FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Shapiro, SS Davis, JL Lebach, DE Gregory, JS AF Shapiro, SS Davis, JL Lebach, DE Gregory, JS TI Measurement of the solar gravitational deflection of radio waves using geodetic very-long-baseline interferometry data, 1979-1999 SO PHYSICAL REVIEW LETTERS LA English DT Article ID GENERAL-RELATIVITY; VLBI AB We used very-long-baseline interferometry (VLBI) to measure the deflection by the Sun of radio waves emanating from distant compact radio sources. This bending is characterized in the parametrized post-Newtonian formalism by gamma, which is unity in general relativity. Using a large geodetic VLBI data set, we obtained gamma=0.9998(3)+/-0.0004(5) (estimated standard error). We found no systematic biases from our analysis of subgroups of data. C1 Guilford Coll, Dept Phys, Greensboro, NC 27410 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shapiro, SS (reprint author), Guilford Coll, Dept Phys, Greensboro, NC 27410 USA. EM sshapiro@guilford.edu; jdavis@cfa.harvard.edu; dlebach@cfa.harvard.edu RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X NR 21 TC 141 Z9 142 U1 0 U2 1 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 MAR 26 PY 2004 VL 92 IS 12 AR 121101 DI 10.1103/PhysRevLett.92.121101 PG 4 WC Physics, Multidisciplinary SC Physics GA 807TU UT WOS:000220524600009 PM 15089661 ER PT J AU Kirshner, RP AF Kirshner, RP TI The full story on neutrino detection SO SCIENCE LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kirshner, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 0 Z9 0 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 MAR 26 PY 2004 VL 303 IS 5666 BP 1976 EP 1977 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 806JI UT WOS:000220429800019 PM 15044787 ER PT J AU Pogue, MG Harp, CE AF Pogue, MG Harp, CE TI A review of the Schinia tertia (Grote) species complex (Lepidoptera : Noctuidae : Heliothinae) SO ZOOTAXA LA English DT Article DE systematics; genitalia; morphology comparison; host plant; Ericameria nauseosa (Pallas ex Pursh) Nesom & Baird; Ericameria paniculata (A. Gray) H. M. Hall (Asteraceae); Isocoma acradenia var. acradenia (E. Greene) E. Greene (Asteraceae) AB Four closely related species of Schinia are diagnosed using characters of maculation, genitalia, larval host plants, and distribution. The revised status of both Schinia albafascia Smith and Schinia brunnea Barnes and McDunnough are based on differences in wing maculation and male and female genitalic structures. The revised synonymy of Schinia megarena Smith with Schinia tertia (Grote) is discussed. Male and female genitalia are described and illustrated for the first time for all species. C1 NMNH, Smithsonian Inst, Agr Res Serv, USDA,PSI,Systemat Entomol Lab, Washington, DC 20013 USA. RP Pogue, MG (reprint author), NMNH, Smithsonian Inst, Agr Res Serv, USDA,PSI,Systemat Entomol Lab, POB 37012,MRC 168, Washington, DC 20013 USA. EM mpogue@sel.barc.usda.gov; cehmoth@aol.com NR 22 TC 6 Z9 6 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 25 PY 2004 IS 473 BP 1 EP 32 PG 32 WC Zoology SC Zoology GA 868DD UT WOS:000224892300001 ER PT J AU Martin, RV Fiore, AM Van Donkelaar, A AF Martin, RV Fiore, AM Van Donkelaar, A TI Space-based diagnosis of surface ozone sensitivity to anthropogenic emissions SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MONITORING EXPERIMENT; UNITED-STATES; NITROGEN-OXIDES; POLLUTION; GOME; FORMALDEHYDE; MODEL; AIR; HYDROCARBONS; ATMOSPHERE AB We present a novel capability in satellite remote sensing with implications for air pollution control strategy. We show that the ratio of formaldehyde columns to tropospheric nitrogen dioxide columns is an indicator of the relative sensitivity of surface ozone to emissions of nitrogen oxides (NOx = NO + NO2) and volatile organic compounds (VOCs). The diagnosis from these space-based observations is highly consistent with current understanding of surface ozone chemistry based on in situ observations. The satellite-derived ratios indicate that surface ozone is more sensitive to emissions of NOx than of VOCs throughout most continental regions of the Northern Hemisphere during summer. Exceptions include Los Angeles and industrial areas of Germany. A seasonal transition occurs in the fall when surface ozone becomes less sensitive to NOx and more sensitive to VOCs. C1 Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Princeton Univ, Atmospher & Ocean Sci Program, Princeton, NJ 08544 USA. RP Martin, RV (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM rvmartin@fizz.phys.dal.ca RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; NR 32 TC 34 Z9 34 U1 5 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 24 PY 2004 VL 31 IS 6 AR L06120 DI 10.1029/2004GL019416 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 809EW UT WOS:000220621000006 ER PT J AU Laurance, WF Nascimento, HEM Laurance, SG Condit, R D'Angelo, S Andrade, A AF Laurance, WF Nascimento, HEM Laurance, SG Condit, R D'Angelo, S Andrade, A TI Inferred longevity of Amazonian rainforest trees based on a long-term demographic study SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Amazon Basin; demography; growth rate; mortality rate; tree age; tree longevity; tropical forest ID FIRME FOREST; EL-NINO; TROPICAL FORESTS; WOOD DENSITY; COSTA-RICA; GROWTH; MORTALITY; BRAZIL; PATTERNS; DROUGHT AB We used data from a long-term (14-18 years) demographic study to infer the maximum longevity for populations of 93 relatively abundant tree species in central Amazonia. We also assessed the influence of several life-history features (wood density, growth form, mortality rate, recruitment rate, stem diameter, growth increment, population density) on tree longevity. Data on 3159 individual trees were collected in 24 permanent, 1 ha plots in undisturbed forest arrayed across a large (ca. 1000 km(2)) study area. For each species, three estimates of longevity were generated (by dividing the stem diameter of the largest tree by the median, upper quartile, and upper decile of observed diameter-growth rates), and the mean of these three values was used as a longevity estimate. Longevity values ranged from 48 years in the pioneer Pourouma bicolor (Cecropiaceae) to 981 years for the canopy tree Pouteria manaosensis (Sapotaceae), with an overall mean of 336 +/- 196 years. These growth-based estimates of maximum tree age were concordant with those derived from analyses of mean mortality rates. Tree longevity was positively correlated with wood density, maximum stem diameter, and population density, and negatively correlated with annual mortality, recruitment, and growth rates. On average, pioneer species had much lower longevity than did non-pioneers, whereas among old-growth trees, emergent species had greater longevity than did canopy species. Our results are consistent with radiocarbon-based studies that suggest that Amazonian trees can occasionally exceed 1000 years of age. (C) 2003 Elsevier B.V. All rights reserved. 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. EM laurancew@tivoli.si.edu RI Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012; Laurance, Susan/G-6021-2011 OI Laurance, Susan/0000-0002-2831-2933 NR 52 TC 70 Z9 74 U1 1 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 22 PY 2004 VL 190 IS 2-3 BP 131 EP 143 DI 10.1016/j.foreco.2003.09.011 PG 13 WC Forestry SC Forestry GA 806TM UT WOS:000220456200002 ER PT J AU Srygley, RB AF Srygley, RB TI The aerodynamic costs of warning signals in palatable mimetic butterflies and their distasteful models SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE locomotor mimicry; insect flight; aerodynamics; mutualism; communication; Mullerian mimicry ID HOVERING INSECT FLIGHT; LOCOMOTOR MIMICRY; NEOTROPICAL BUTTERFLIES; APOSEMATIC PREY; EVOLUTION; MORPHOLOGY; HELICONIUS; TEMPERATURE; PREDATION; MASS AB Bates hypothesized that some butterfly species that are palatable gain protection from predation by appearing similar to distasteful butterflies. When undisturbed, distasteful butterflies fly slowly and in a straight line, and palatable Batesian mimics also adopt this nonchalant behaviour. When seized by predators, distasteful butterflies are defended by toxic or nauseous chemicals. Lacking chemical defences, Batesian mimics depend on flight to escape attacks. Here, I demonstrate that flight in warning-coloured mimetic butterflies and their distasteful models is more costly than in closely related non-mimetic butterflies. The increased cost is the result of differences in both wing shape and kinematics. Batesian mimics and their models slow the angular velocity of their wings to enhance the colour signal but at an aerodynamic cost. Moreover, the design for flight in Batesian mimics has an additional energetic cost over that of its models. The added cost may cause Batesian mimics to be rare, explaining a general pattern that Bates first observed. C1 Smithsonian Trop Res Inst, Balboa 2072, Panama. Univ Oxford, Dept Zool, Oxford OX1 3PS, England. RP Srygley, RB (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM bob.srygley@zoo.ox.ac.uk NR 29 TC 32 Z9 34 U1 4 U2 21 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 MAR 22 PY 2004 VL 271 IS 1539 BP 589 EP 594 DI 10.1098/rspb.2003.2627 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 808KN UT WOS:000220568100006 PM 15156916 ER PT J AU Su, YN Zhang, QZ Lim, J AF Su, YN Zhang, QZ Lim, J TI Bipolar molecular outflows from high-mass protostars SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (IRAS 21519+5613; IRAS 22506+5944); ISM : jets and outflows; stars : early-type; stars : formation ID ULTRACOMPACT HII-REGIONS; LUMINOUS IRAS SOURCES; STAR-FORMATION; PROTOSTELLAR CANDIDATES; MULTIPLE OUTFLOWS; CO; SAMPLE; SEARCH; CORES; JETS AB We report observations of the bipolar molecular outflows associated with the luminous (similar to2 x 10(4) L-.) far-IR sources IRAS 21519+5613 and IRAS 22506+5944, as well the dust and molecular gas condensations on which these outflows appear to be centered. The observations were made in (CO)-C-12, (CO)-C-13, (CO)-O-18, and continuum at 3 mm with the BIMA array and in (CO)-C-12 and (CO)-C-13 with the NRAO 12 m telescope to recover extended emission filtered out by the interferometric array. We find that the outflow associated with each IRAS source shows a clear bipolar morphology in (CO)-C-12, with properties (i.e., total mass of order 10 - 100 M-., mass-outflow rate greater than or similar to10(-3) M-., dynamical timescale 10(4) - 10(5) yr, and energetics) comparable with those of other massive outflows associated with luminous young stellar objects. Each outflow appears to be centered on a dust and gas condensation with a mass of 200 - 300 M-., likely marking the location of the driving source. The outflow lobes of both sources are fully resolved along their major but not minor axes, and they have collimation factors that may be comparable with young low-mass stars. The mass-velocity diagrams of both outflows change in slope at a velocity of similar to10 km s(-1), suggesting that the high-velocity component (HVC) may drive the low-velocity component (LVC). Although the HVC of IRAS 21519+5613 shows evidence for deceleration, no such signature is seen in the HVC of IRAS 22506+5944. Neither HVC has a momentum supply rate sufficient to drive their corresponding LVCs, although it is possible that the HVC is more highly excited and hence its thrust underestimated. Like for other molecular outflows the primary driving agent cannot be ionized gas, leaving atomic gas as the other remaining candidate. Neither IRAS 21519+5613 nor IRAS 22506+ 5944 exhibits detectable free-free emission, which together with the observed properties of their molecular outflows and surrounding condensations make them credible candidates for high-mass protostars. The mass-accretion rate required to produce their observed IRAS luminosity is greater than or similar to10(-4) M-. yr(-1), which is more than sufficient to quench the development of an UC-H II region. On the other hand, the individual IRAS sources may be associated with a group of stars whose dominant member is a main-sequence star that is responsible for the observed outflow. Such a star would be required to have a spectral type of similar toB2 (luminosity of similar to3000 L-.) or later to not excite a detectable UC-H II region; the time-averaged mass-accretion rate needed to produce this star is then 10(-3) to 10(-4) M-. yr(-1). Thus, regardless of the evolutionary stage of the outflow driving source, the inferred mass-accretion rate is much higher than that allowed by simple inside-out collapse models but can be accommodated by recently proposed variants. C1 Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Su, YN (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM ynsu@asiaa.sinica.edu.tw; qzhang@cfa.harvard.edu; jlim@asiaa.sinica.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 NR 53 TC 32 Z9 32 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 MAR 20 PY 2004 VL 604 IS 1 BP 258 EP 271 DI 10.1086/381880 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LU UT WOS:000220301000021 ER PT J AU Navascues, DBY Mohanty, S Jayawardhana, R AF Navascues, DBY Mohanty, S Jayawardhana, R TI Accretion and outflow in the substellar domain : Magellan spectroscopy of LS-RCrA 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars : formation; stars : low-mass, brown dwarfs; stars : pre-main-sequence ID YOUNG BROWN DWARFS; LOW-MASS STARS; TAURI MAGNETOSPHERIC ACCRETION; SPECTRAL ENERGY-DISTRIBUTIONS; EMISSION-LINE DIAGNOSTICS; MAIN-SEQUENCE TRACKS; CIRCUMSTELLAR DISKS; CORONAE-AUSTRALIS; INFRARED-SPECTRA; ALPHA-PERSEI AB We present low-, medium-, and high-resolution optical spectra, obtained with the Magellan Baade 6.5 m telescope, of LS-RCrA 1, a late-type object identified recently by Fernandez & Comeron in the R Coronae Australis star-forming region. We confirm both pre-main-sequence status and membership in the R CrA region for this object, through the detection of Li I, presence of narrow K I indicative of low gravity, and measurement of radial velocity. The Halpha emission profile is very broad, with a 10% full width of 316 km s(-1) at high resolution, implying the presence of ongoing accretion. Our spectra also exhibit many forbidden emission lines indicative of mass outflow, in agreement with the Fernandez & Comeron results. We derive a spectral type, independent of extinction, of M6.5 +/- 0.5 IV. Using new Two Micron All Sky Survey (2MASS) near-infrared photometry, no significant near-infrared (NIR) excess is found. Our optical veiling measurements yield a mass accretion rate of 10(-10) less than or similar to M less than or similar to 10(-9) M-. yr(-1). The presence of prominent outflow signatures at these low accretion rates is initially puzzling. We consider, and discard as improbable, the possibility that these signatures arise in a line-of-sight Herbig-Haro knot unassociated with LS-RCrA 1 itself. However, if LS-RCrA 1 possesses a nearly edge-on disk, a natural outcome would be the enhancement of any outflow signatures relative to the photosphere; we favor this view. A low accretion/outflow rate, combined with an edge-on orientation, is further supported by the absence of high-velocity components and any significant asymmetries in the forbidden lines. An edge-on geometry is also consistent with the lack of NIR excess in spite of ongoing accretion and explains the relatively large Halpha 10% width compared to other low- mass objects with similar accretion rates. Through comparison with the latest synthetic spectra, we infer T-eff approximate to 2700 +/- 100 K, somewhat lower than the previous estimate (2900 +/- 200 K). Theoretical evolutionary tracks then imply an age of similar to 20 Myr (as derived from T-eff and luminosity) or similar to 8 Myr (T-eff vs. gravity) for LS-RCrA 1. This last value is consistent with the estimated age of other T Tauri stars in R CrA (less than or similar to10 Myr), and it is substantially less than the similar to50 Myr derived previously. Therefore, LS-RCrA 1 indeed appears subluminous relative to expectations for an R CrA member. By comparing its position on the H-R diagram with that of other similarly accreting low-mass objects, we show that accretion-induced effects are unlikely to account for its faintness. We suggest instead that LS-RCrA 1 possesses a nearly edge-on disk and its photosphere is seen predominantly in scattered light, making it appear much fainter (and older) than it really is. The ease with which such a disk simultaneously explains all the puzzling aspects of LS-RCrA 1 - subluminosity, unusually prominent outflow signatures without high-velocity components or asymmetries, very broad Halpha, lack of NIR excess combined with accretion - makes its presence a strong possibility. Finally, the surface gravity and T-eff estimates, combined with the latest evolutionary tracks, indicates a mass of similar to 0.06 or 0.035 +/- 0.010 M-. (depending on the T-eff scale), i.e., at or below the substellar boundary. Our results, together with those of Fernandez & Comeron, imply that young brown dwarfs can not only harbor accretion disks but also generate jets/outflows analogous to those in higer mass classical T Tauri stars. This is further evidence of a common formation mechanism for stars and brown dwarfs. C1 INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Navascues, DBY (reprint author), INTA, Lab Astrofis Espacial & Fis Fundamental, POB 50727, E-28080 Madrid, Spain. EM barrado@laeff.esa.es; smohanty@cfa.harvard.edu; rayjay@umich.edu RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 NR 51 TC 42 Z9 42 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 20 PY 2004 VL 604 IS 1 BP 284 EP 296 DI 10.1086/381747 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LU UT WOS:000220301000023 ER PT J AU Ransom, SM Stairs, IH Backer, DC Greenhill, LJ Bassa, CG Hessels, JWT Kaspi, VM AF Ransom, SM Stairs, IH Backer, DC Greenhill, LJ Bassa, CG Hessels, JWT Kaspi, VM TI Green Bank Telescope discovery of two binary millisecond pulsars in the globular cluster M30 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters : individual (M30); pulsars : individual (PSR J2140-2310A); radio continuum : stars; stars : neutron ID 47 TUCANAE; TIMING OBSERVATIONS; RADIO PULSARS; NGC-6397; 47-TUCANAE; COMPANION; SYSTEMS; SEARCH; WFPC2; VARIABILITY AB We report the discovery of two binary millisecond pulsars in the core-collapsed globular cluster M30 using the Green Bank Telescope (GBT) at 20 cm. PSR J2140 - 2310A (M30A) is an eclipsing 11 ms pulsar in a 4 hr circular orbit, and PSR J2140 - 23B (M30B) is a 13 ms pulsar in an as yet undetermined but most likely highly eccentric (e > 0.5) and relativistic orbit. Timing observations of M30A with a 20 month baseline have provided precise determinations of the pulsar's position (within 4" of the optical centroid of the cluster) and spin and orbital parameters, which constrain the mass of the companion star to be m(2) greater than or similar to 0.1 M-.. The position of M30A is coincident with a possible thermal X-ray point source found in archival Chandra data, which is most likely caused by emission from hot polar caps on the neutron star. In addition, there is a faint (V-555 similar to 23.8) star visible in archival Hubble Space Telescope (HST) F555W data that may be the companion to the pulsar. Eclipses of the pulsed radio emission from M30A by the ionized wind from the compact companion star show a frequency-dependent duration (proportional to nu(-alpha) with alpha similar to 0.4 - 0.5) and delay the pulse arrival times near eclipse ingress and egress by up to 2 - 3 ms. Future observations of M30 may allow both the measurement of post-Keplerian orbital parameters from M30B and the detection of new pulsars through the effects of strong diffractive scintillation. C1 McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. RP Ransom, SM (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM ransom@physics.mcgill.ca OI Ransom, Scott/0000-0001-5799-9714 NR 63 TC 28 Z9 29 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 MAR 20 PY 2004 VL 604 IS 1 BP 328 EP 338 DI 10.1086/381730 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LU UT WOS:000220301000028 ER PT J AU Lenz, DD AF Lenz, DD TI Effects of flow on structure and abundances in multispecies solar coronal loops SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : abundances; Sun : corona; Sun : transition region; Sun : UV radiation ID DIAGNOSTIC SPECTROMETER CDS; ACTIVE-REGION; ELEMENTAL ABUNDANCES; TRANSPORT-EQUATIONS; TRANSITION-REGION; ION TEMPERATURES; MINOR IONS; WIND; STREAMERS; EXPLORER AB We investigate the effects of large-scale bulk flows on coronal abundances using a multispecies numerical model. The model assumes that electrons, protons, and helium are in thermal equilibrium and constitute the bulk of the coronal plasma. Thermal diffusion and Coulomb friction are included. Temperature profiles for the bulk component and for each ion species are assumed, so the model reduces to a solution of mass and force balance for each component. We further assume that the bulk component has an upward bulk velocity at the base, and that ion flow speeds along field lines are negligible relative to the bulk flow. Coulomb coupling of the electrons and ions induces drag that counteracts the tendency of the ions to gravitationally settle. In regions of small delT, such as the outer regions of the corona, Coulomb drag is the only significant force counteracting gravitational settling in this model. We find that relatively modest bulk flows of tens of km s(-1) can enhance ion abundances by 2 - 3 orders of magnitude over their values in low- or no-flow cases. C1 Syst Res Inst, Boulder, CO 80301 USA. Smithsonian Astrophys Lab, Cambridge, MA 02138 USA. RP Lenz, DD (reprint author), Syst Res Inst, 4990 Pearl E Circle, Boulder, CO 80301 USA. EM lenz@oddjob.uchicago.edu NR 39 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 MAR 20 PY 2004 VL 604 IS 1 BP 433 EP 441 DI 10.1086/381879 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LU UT WOS:000220301000038 ER PT J AU Barton, EJ Dave, R Smith, JDT Papovich, C Hernquist, L Springel, V AF Barton, EJ Dave, R Smith, JDT Papovich, C Hernquist, L Springel, V TI Searching for star formation beyond reionization SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : formation; galaxies : high-redshift ID PROBE WMAP OBSERVATIONS; PARTICLE HYDRODYNAMICS SIMULATIONS; LYMAN BREAK GALAXIES; BAND IMAGING SURVEY; HIGH-REDSHIFT; LY-ALPHA; 1ST STARS; EMISSION-LINES; POPULATION-III; UNIVERSE AB The goal of searching back in cosmic time to find star formation during the epoch of reionization will soon be within reach. We assess the detectability of high-redshift galaxies by combining cosmological hydrodynamic simulations of galaxy formation, stellar evolution models appropriate for the first generations of stars, and estimates of the efficiency for Lyalpha to escape from forming galaxies into the intergalactic medium. Our simulated observations show that Lyalpha emission at z similar to 8 may be observable in the near-infrared with 8 m class telescopes and present-day technology. Not only is the detection of early star-forming objects vital to understanding the underlying cause of the reionization of the universe, but the timely discovery of a star-forming population - or even an z 1 7 interesting upper limit on the emergent flux from these objects - will have implications for the design of the next generation of ground- and space-based facilities. C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Barton, EJ (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 41 TC 42 Z9 42 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 20 PY 2004 VL 604 IS 1 BP L1 EP L4 DI 10.1086/383489 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LW UT WOS:000220301200001 ER PT J AU Maslakova, SA Martindale, MQ Norenburg, JL AF Maslakova, SA Martindale, MQ Norenburg, JL TI Fundamental properties of the spiralian developmental program are displayed by the basal nemertean Carinoma tremaphoros (Palaeonemertea, Nemertea) SO DEVELOPMENTAL BIOLOGY LA English DT Article DE nemertean; spiral cleavage; cell lineage; prototroch; molluscan cross; annelid cross ID CELL-LINEAGE; CEREBRATULUS-LACTEUS; DORSOVENTRAL AXIS; PHYLOGENY; CLEAVAGE; ESTABLISHMENT; CONSERVATION; GASTROPODA; EVOLUTION; MOLLUSCA AB The first description of the cleavage program of the palaeonemertean Carinoma tremaphoros (a member of a basal clade of the Nemertea) is illustrated by confocal microscopy and microinjection and compared to development of more derived nemerteans and other eutrochozoans (Annelida, Mollusca, Sipunculida and Echiurida). Lineage tracers were injected into individual blastomeres of C tremaphoros at the 2-, 4-, 8- and 16-cell stage. Subsequent development was followed to the formation of simple (so-called planuliform) planktonic larvae to establish the ultimate fates of the blastomeres. Results of labeling experiments demonstrate that the development of C tremaphoros bears closer similarity to other Eutrochozoa than development of a previously studied hoplonemertean (Nemertopsis bivittata) and a heteronemertean (Cerebratulus lacteus) in that the first cleavage plane bears an invariant relationship to the plane of bilateral symmetry of the larval body. Additionally, our cell-labeling experiments support the earlier suggestion that the transitory pre-oral belt of cells in the larvae of C tremaphoros corresponds to the prototroch of other Eutrochozoa. A unique feature of development of C tremaphoros includes the oblique orientation of the trochal lineages with respect to the anterior-posterior axis of the larva. The significance and application of cleavage characters such as presence of molluscan vs. annelid cross for phylogenetic analyses is reviewed. We argue that molluscan or annelid cross, neither of which are present in nemerteans, are merely two out of much greater variety of patterns created by the differences in the relative size and timing of formation of micromere quartets and none can be considered, by itself, as evidence of close phylogenetic relationship between phyla. (C) 2003 Elsevier Inc. All rights reserved. C1 George Washington Univ, Dept Biol, Washington, DC 20052 USA. Smithsonian Inst, MRC, Natl Museum Nat Hist, Washington, DC 20013 USA. Univ Hawaii, Pacific Biomed Res Ctr, Kewalo Marine Lab, Honolulu, HI 96813 USA. RP Maslakova, SA (reprint author), George Washington Univ, Dept Biol, 2023 G St NW, Washington, DC 20052 USA. EM maslak@gwu.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 60 TC 59 Z9 61 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0012-1606 J9 DEV BIOL JI Dev. Biol. PD MAR 15 PY 2004 VL 267 IS 2 BP 342 EP 360 DI 10.1016/j.ydbio.2003.10.022 PG 19 WC Developmental Biology SC Developmental Biology GA 805FE UT WOS:000220351400006 PM 15013798 ER PT J AU Riley, S AF Riley, S TI The book of Joe. 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 MAR 15 PY 2004 VL 129 IS 5 BP 108 EP 108 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 837VJ UT WOS:000222668800199 ER PT J AU Schlachter, AS Sant'Anna, MM Covington, AM Aguilar, A Gharaibeh, MF Emmons, ED Scully, SWJ Phaneuf, RA Hinojosa, G Alvarez, I Cisneros, C Muller, A McLaughlin, BM AF Schlachter, AS Sant'Anna, MM Covington, AM Aguilar, A Gharaibeh, MF Emmons, ED Scully, SWJ Phaneuf, RA Hinojosa, G Alvarez, I Cisneros, C Muller, A McLaughlin, BM TI Lifetime of a K-shell vacancy in atomic carbon created by 1s -> 2p photoexcitation of C+ SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID FLUORESCENCE YIELDS; AUGER DECAY; PHOTOIONIZATION; SPECTROSCOPY; ELECTRON; SEQUENCE; OXYGEN; PHOTOABSORPTION; TRANSITIONS; IONIZATION AB Lifetimes for K-shell vacancy states in atomic carbon have been determined by measurement of the natural linewidth of the 1s --> 2p photoexcited states of C+ ions. The K-shell vacancy states produced by photoionization of atomic carbon are identical to those produced by 1s --> 2p photoexcitation of a C+ ion: 1s2S(2) 2p(2) D-2, P-2, and S-2 autoionizing states occur in both cases. These vacancy states stabilize by emission of an electron to produce C2+ ions. Measurements are reported for the lifetime of the 1s2s(2) 2p(2) D-2, P-2 and S-2 autoionizing states of C+: 6.3 +/- 0.9 fs, 11.2 +/- 1.1 fs and 5.9 +/- 1.3 fs respectively. Knowledge of such lifetimes is important for comparative studies of the lifetimes of K-shell vacancies in carbon-containing molecules, benchmarking theory, and interpreting satellite x-ray spectra from astrophysical sources such as x-ray binaries. Absolute cross sections were measured for both ground-state and metastable-state ions providing a stringent test of state-of-the-art theoretical calculations. C1 Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Giessen, Inst Kernphys, D-35392 Giessen, Germany. Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. Univ Nevada, Dept Phys, Reno, NV 89557 USA. Lake Tahoe Community Coll, Dept Phys, S Lake Tahoe, CA 96150 USA. RP Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, MS 7-222, Berkeley, CA 94720 USA. EM b.mclaughlin@qub.ac.uk RI Muller, Alfred/A-3548-2009; Sant'Anna, Marcelo/B-9355-2013 OI Muller, Alfred/0000-0002-0030-6929; Sant'Anna, Marcelo/0000-0001-5342-5799 NR 33 TC 42 Z9 43 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAR 14 PY 2004 VL 37 IS 5 BP L103 EP L109 DI 10.1088/0953-4075/37/5/L03 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 809KQ UT WOS:000220636000003 ER PT J AU Van Tassell, JL Baldwin, CC AF Van Tassell, JL Baldwin, CC TI A review of the gobiid genus Akko (Teleostei : Gobiidae) with description of a new species SO ZOOTAXA LA English DT Article DE Gobiidae; new species; Akko; Amblyopus brevis; eastern Pacific ID 7-SPINED GOBIES; ATLANTIC AB Akko was originally described for a highly autapomorphic species of goby, A. dionaea, taken off Brazil. The genus is here recorded for the first time from the eastern Pacific Ocean. The poorly known eastern Pacific goby Amblyopus brevis Gunther is redescribed as Akko brevis based on the study of numerous specimens recently collected off Panama and El Salvador, and Akko rossi is described as new from the coast of El Salvador. Akko dionaea has 11+16 vertebrae, 76 scales in the lateral series, non-overlapping scales on the caudal peduncle, and no melanophores on the pectoral fin or female genital papilla; A. brevis has 11+16 vertebrae, 53 - 60 scales in the lateral series, overlapping scales on the caudal peduncle, and no melanophores on the pectoral fin or female genital papilla; A. rossi has 11+17 vertebrae, 115 scales in the lateral series, overlapping scales on the caudal peduncle, and dense melanophores on the pectoral fin and female genital papilla. C1 114 Hofstra Univ, Dept Biol, Hempstead, NY 11549 USA. Natl Museum Nat Hist, Smithsonian Inst, Div Fisheries, MRC 159, Washington, DC 20013 USA. RP Van Tassell, JL (reprint author), 114 Hofstra Univ, Dept Biol, Hempstead, NY 11549 USA. EM jvantassell@gobiidae.com; baldwin.carole@nmnh.si.edu NR 17 TC 4 Z9 5 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, 1030, NEW ZEALAND SN 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 12 PY 2004 IS 462 BP 1 EP 15 PG 15 WC Zoology SC Zoology GA 867RY UT WOS:000224861100001 ER PT J AU Laurance, WF Oliveira, AA Laurance, SG Condit, R Nascimento, HEM Sanchez-Thorin, AC Lovejoy, TE Andrade, A D'Angelo, S Ribeiro, JE Dick, CW AF Laurance, WF Oliveira, AA Laurance, SG Condit, R Nascimento, HEM Sanchez-Thorin, AC Lovejoy, TE Andrade, A D'Angelo, S Ribeiro, JE Dick, CW TI Pervasive alteration of tree communities in undisturbed Amazonian forests SO NATURE LA English DT Article ID TROPICAL RAIN-FOREST; EL-NINO; GROWTH; VARIABILITY; SEEDLINGS; SOILS; CO2 AB Amazonian rainforests are some of the most species-rich tree communities on earth(1). Here we show that, over the past two decades, forests in a central Amazonian landscape have experienced highly nonrandom changes in dynamics and composition. Our analyses are based on a network of 18 permanent plots unaffected by any detectable disturbance. Within these plots, rates of tree mortality, recruitment and growth have increased over time. Of 115 relatively abundant tree genera, 27 changed significantly in population density or basal area-a value nearly 14 times greater than that expected by chance. An independent, eight-year study in nearby forests corroborates these shifts in composition. Contrary to recent predictions(2-5), we observed no increase in pioneer trees. However, genera of faster-growing trees, including many canopy and emergent species, are increasing in dominance or density, whereas genera of slower-growing trees, including many subcanopy species, are declining. Rising atmospheric CO2 concentrations(6) may explain these changes, although the effects of this and other large-scale environmental alterations remain uncertain. These compositional changes could have important impacts on the carbon storage, dynamics and biota of Amazonian forests. C1 Smithsonian Trop Res Inst, Balboa, Panama. INPA, Dept Bot, BR-69011970 Manaus, Amazonas, Brazil. INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. Univ Sao Paulo, Dept Biol, BR-14040901 Sao Paulo, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM laurancew@tivoli.si.edu RI Dick, Christopher/A-8744-2008; Laurance, William/B-2709-2012; Nascimento, Henrique/F-8612-2012; Oliveira, Alexandre/G-8830-2012; Laurance, Susan/G-6021-2011; Lahoz da Silva Ribeiro, Jose Eduardo/A-8574-2013 OI Oliveira, Alexandre/0000-0001-5526-8109; Laurance, Susan/0000-0002-2831-2933; Lahoz da Silva Ribeiro, Jose Eduardo/0000-0002-2389-5631 NR 29 TC 144 Z9 157 U1 2 U2 39 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 11 PY 2004 VL 428 IS 6979 BP 171 EP 175 DI 10.1038/nature02383 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 801NW UT WOS:000220103600046 PM 15014498 ER PT J AU Silver, E Schnopper, H Austin, G Guth, G Murray, S Madden, N Landis, D Beeman, J Haller, EE Stohlker, T AF Silver, E Schnopper, H Austin, G Guth, G Murray, S Madden, N Landis, D Beeman, J Haller, EE Stohlker, T TI Using a microcalorimeter to measure the Lamb shift in hydrogenic gold and uranium on cooled, decelerated ion beams SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 10th International Workshop on Low Temperature Detectors CY JUL 07-11, 2003 CL Genoa, ITALY DE microcalorimeter; lamb shift AB A precise determination of the Lamb shift from photons emitted by highly charged, one electron ions represents one of the most sensitive tests of QED in strong electromagnetic fields. Recent progress in the production and cooling of intense beams of fully stripped An and U in the SIS/ESR synchrotron storage ring at GSI, Darmstadt has made it possible to obtain precision spectroscopy of these ions. A fully stripped beam of either Au79+ or U92+ ions is injected, stored and cooled in the ESR and interacts with an internal gas target. The capture of an electron and the subsequent population of a 2p or 3p state will lead to a decay by either Lyman or Balmer X-ray emission. Although measurements of the 1 s Lamb shift in U with Ge ionization detectors accurate to similar to3% have provided a test of QED for the high Z domain, the experimental errors (+/-13 eV) are about one order of magnitude larger than the accuracy theoreticians presently claim (1 eV). We present the results from initial broad band experiments using NTD Ge microcalorimeters to measure the 2 s Lamb Shift in An and U at the ESR. The broad band coverage of the microcalorimeter makes it possible to reduce the systematic uncertainties in the Doppler corrections while the high-energy resolution reduces the statistical error in the absolute energy calibration. (C) 2003 Elsevier B.V. All rights reserved. C1 Harvard Univ, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Gesell Schwerionenforsch mbH, D-6100 Darmstadt, Germany. RP Silver, E (reprint author), Harvard Univ, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM esilver@cfa.harvard.edu NR 4 TC 9 Z9 9 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAR 11 PY 2004 VL 520 IS 1-3 BP 60 EP 62 DI 10.1016/j.nima.2003.11.220 PG 3 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 808ZL UT WOS:000220606900015 ER PT J AU Perinati, E Barbera, M Serio, S Silver, E AF Perinati, E Barbera, M Serio, S Silver, E TI Spectral broadening by spatial effects in X-ray microcalorimeters with superconducting absorber and NTD-Ge thermal sensor SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 10th International Workshop on Low Temperature Detectors CY JUL 07-11, 2003 CL Genoa, ITALY DE X-ray spectroscopy; microcalorimeters; numerical simulations AB We discuss how the sensitivity to the position of absorption of the photons can affect the spectral resolution of X-ray microcalorimeters with superconducting Sri absorber and NTD-Ge thermal sensor. Data obtained through the computer simulations are reported for microcalorimeters with different geometries and phonon transmission probabilities at the interface between the absorber and thermistor. (C) 2003 Elsevier B.V. All rights reserved. C1 INAF Osservat Astron GS Vaiana, I-90134 Palermo, Italy. Univ Palermo, Dip Sci Fis & Astr, I-90123 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perinati, E (reprint author), INAF Osservat Astron GS Vaiana, I-90134 Palermo, Italy. EM perinati@astropa.unipa.it OI Barbera, Marco/0000-0002-3188-7420 NR 2 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAR 11 PY 2004 VL 520 IS 1-3 BP 216 EP 219 DI 10.1016/j.nima.2003.11.232 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 808ZL UT WOS:000220606900056 ER PT J AU Barbera, M Perinati, E Serio, S Silver, E AF Barbera, M Perinati, E Serio, S Silver, E TI Spectral broadening by quasiparticle pile-up in X-ray microcalorimeters with superconducting absorbers SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article; Proceedings Paper CT 10th International Workshop on Low Temperature Detectors CY JUL 07-11, 2003 CL Genoa, ITALY DE X-ray spectroscopy; microcalorimeters; superconducting absorbers AB Long-living quasiparticles can pile-up in a superconducting absorber of an X-ray microcalorimeter when photons are detected at high count rate. These quasiparticles can give a non-negligible contribution to the total heat capacity of the detector thus affecting the pulse height spectrum of detected photons. We investigated this effect with numerical simulations and evaluated the resulting spectral broadening as a function of the photon absorption rate, and the heat capacity of the detector for a NTD germanium microcalorimeter with pure Sn absorber. (C) 2003 Elsevier B.V. All rights reserved. C1 INAF, Osservat Astron Palermo GS Vaiana, I-90134 Palermo, Italy. Univ Palermo, Dipartimento Sci Fisiche & Astron, I-90123 Palermo, Italy. Smithsonian Astrophys Observat, Cambridge, MA 02138 USA. RP Barbera, M (reprint author), INAF, Osservat Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy. EM barbera@astropa.unipa.it OI Barbera, Marco/0000-0002-3188-7420 NR 3 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD MAR 11 PY 2004 VL 520 IS 1-3 BP 220 EP 223 DI 10.1016/j.nima.2003.11.233 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 808ZL UT WOS:000220606900057 ER PT J AU Cagnoni, I Nicastro, F Maraschi, L Treves, A Tavecchio, F AF Cagnoni, I Nicastro, F Maraschi, L Treves, A Tavecchio, F TI A view of PKS 2155-304 with XMM-Newton reflection grating spectrometers SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (PKS 2155-304); intergalactic medium; large-scale structure of universe; quasars : absorption lines; X-rays : galaxies ID X-RAY FOREST; HOT INTERGALACTIC MEDIUM; OBJECT PKS 2155-304; CHANDRA DETECTION; ALPHA ABSORPTION; ATOMIC OXYGEN; LOW-REDSHIFT; IONIZED-GAS; LOCAL GROUP; SPECTROSCOPY AB We present the high-resolution X-ray spectrum of the BL Lac object PKS 2155-304 taken with the RGS units on board XMM-Newton in 2000 November. We detect an O VII Kalpha resonant absorption line from warm/hot local gas at 21.59 Angstrom (similar to4.5 sigma detection). The line profile is possibly double peaked. We do not confirm the strong 20.02 Angstrom absorption line seen with Chandra and interpreted as z similar to 0.05 O VIII Kalpha. We set a 3 sigma upper limit of 14 mAngstrom on the equivalent width. We also detect the similar to23.5 Angstrom interstellar O I 1s --> 2p line and derive a factor of less than or equal to1.5 subsolar O/H ratio in the interstellar medium along the PKS 2155-304 line of sight. C1 Univ Insubria, Dipartimento Sci, I-22100 Como, Italy. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Osserv Astron Brera, I-20121 Milan, Italy. RP Cagnoni, I (reprint author), Univ Insubria, Dipartimento Sci, Via Valleggio 11, I-22100 Como, Italy. OI Nicastro, Fabrizio/0000-0002-6896-1364 NR 43 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 MAR 10 PY 2004 VL 603 IS 2 BP 449 EP 455 DI 10.1086/381698 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LQ UT WOS:000220300600008 ER PT J AU Zampieri, L Mucciarelli, P Falomo, R Kaaret, P Di Stefano, R Turolla, R Chieregato, M Treves, A AF Zampieri, L Mucciarelli, P Falomo, R Kaaret, P Di Stefano, R Turolla, R Chieregato, M Treves, A TI The ultraluminous X-ray source NGC 1313 X-2 (MS 0317.7-6647) and its environment SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 1313); stars : individual (NGC 1313 X-2/MS 0317.7-6647); X-rays : binaries; X-rays : galaxies ID NEARBY SPIRAL GALAXIES; ISOLATED NEUTRON-STAR; SOURCE NGC-5204 X-1; OPTICAL COUNTERPART; BLACK-HOLES; NGC 1313; ACCRETION DISKS; SUPERNOVA; EMISSION; IDENTIFICATION AB We present new optical and Chandra observations of the field containing the ultraluminous X-ray source NGC 1313 X-2. On an ESO 3.6 m image, the Chandra error box embraces an R = 21.6 pointlike object and excludes a previously proposed optical counterpart. The resulting X-ray/optical flux ratio of NGC 1313 X-2 is similar to500. The value of f(X)/f(opt), the X-ray variability history, and the spectral distribution derived from a reanalysis of the ROSAT, ASCA, and XMM-Newton data indicate a luminous X-ray binary in NGC 1313 as a likely explanation for NGC 1313 X-2. If the X-ray soft component observed in the XMM-Newton EPIC spectrum originates from an accretion disk, the inferred mass of the compact remnant is approximate to100 M-circle dot, making it an intermediate-mass black hole. The derived optical luminosity (L approximate to 10(5) L-circle dot) is consistent with that of a approximate to15-20 M-circle dot companion. The properties of the environment of NGC 1313 X-2 are briefly discussed. C1 Astron Observ Padova, INAF, I-35122 Padua, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. Univ Padua, Dipartimento Fis, I-35131 Padua, Italy. Univ Insubria, Dipartimento Sci, I-22100 Como, Italy. SISSA, I-34014 Trieste, Italy. RP Zampieri, L (reprint author), Astron Observ Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. OI Falomo, Renato/0000-0003-4137-6541; Zampieri, Luca/0000-0002-6516-1329 NR 45 TC 50 Z9 50 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 2004 VL 603 IS 2 BP 523 EP 530 DI 10.1086/381541 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LQ UT WOS:000220300600014 ER PT J AU Schlegel, EM Kong, A Kaaret, P DiStefano, R Murray, S AF Schlegel, EM Kong, A Kaaret, P DiStefano, R Murray, S TI Chandra ACIS and XMM-Newton EPIC observations of the X-ray-luminous SN 1978K in NGC 1313 SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae : individual (SN 1978K); X-rays : stars ID NGC 1313; CIRCUMSTELLAR INTERACTION; SPIRAL GALAXIES; EMISSION; SUPERNOVA; INSTRUMENT; RADIATION; SPECTRUM; 1993J AB We describe an observation of the X-ray-luminous SN 1978K in NGC 1313 using the ACIS detector on board Chandra and an archival XMM-Newton EPIC observation. The models that provided good fits to the ASCA SIS and GIS and the ROSAT PSPC spectra no longer do so for the ACIS and EPIC spectra. The best-fit models to the ACIS and EPIC spectra are dual hot plasma models (VMEKAL); one component is soft (T = 0.61(-0.05)(+0.04) keV, 90% errors), and the other is harder (T = 3.16(-0.40)(+0.44) keV). For the varying abundances permitted within the model, only the Si abundance of the soft component differs from solar, with a value n(SN 78K)(Si)/n(solar)(Si) = solar = 3.20(-1.90)(+1.80) (90% errors). From a ratio of the low- and high-T model fits to the Chandra and XMM-Newton spectra, we infer an exponent n of the ejecta density distribution, rho(ejecta) proportional to r(-n), of similar to5.2, adopting a circumstellar matter distribution exponent of s = 2 (rho(cs) proportional to r(-s)). The 0.5 - 2 keV light curve shows essentially no decline; the 2 - 10 keV light curve, comprised of only the ASCA, XMM-Newton, and Chandra observations, shows a drop of 1.5 from the ASCA epoch. The hard-band decline, together with the apparently enhanced Si emission, signal the start of the X-ray decline of SN 1978K. C1 Smithsonian Astrophys Observ, High Energy Astrophys Div, Cambridge, MA 02138 USA. RP Schlegel, EM (reprint author), Smithsonian Astrophys Observ, High Energy Astrophys Div, 60 Garden St, Cambridge, MA 02138 USA. NR 34 TC 15 Z9 15 U1 0 U2 0 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 2004 VL 603 IS 2 BP 644 EP 651 DI 10.1086/381571 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LQ UT WOS:000220300600024 ER PT J AU Uzzo, M Ko, YK Raymond, JC AF Uzzo, M Ko, YK Raymond, JC TI Active region streamer diagnostics 2001 September 14-16 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : abundances; Sun : activity; Sun : corona; Sun : coronal mass ejections (CMEs); Sun : UV radiation ID SLOW SOLAR-WIND; ULTRAVIOLET CORONAGRAPH SPECTROMETER; ELEMENTAL ABUNDANCES; ATOMIC DATABASE; EMISSION-LINES; SOHO; UVCS/SOHO; CHIANTI; WAVELENGTHS; TEMPERATURE AB From 2001 September 14 to 16 the Ultraviolet Coronal Spectrometer aboard the Solar and Heliospheric Observatory conducted a series of observations designed to study the absolute elemental abundances of an active region streamer. The absolute elemental abundances for O, Si, Fe, Mg, N, S, and Ar were calculated utilizing a constant electron temperature technique and an alternative approach to the emission measure technique, both producing complementary results. The manifestation of the first ionization potential ( FIP) effect was observed here as in previous streamers. Two aspects of this streamer make it unusual and worth special attention. The active region streamer observed possessed an abundance-depleted core typically, although not exclusively, seen in quiescent streamers. A coronal mass ejection (CME) occurred at the active region during the observations. This event resulted in the second unexpected aspect of this streamer, its quick return to the same general abundance characteristics that existed before the CME occurred. The re-formation of a depleted core and the presence of the FIP effect immediately after a highly disruptive event are surprising given the 1 day timescale predicted by streamer theories. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 35 TC 12 Z9 12 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 MAR 10 PY 2004 VL 603 IS 2 BP 760 EP 775 DI 10.1086/381525 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LQ UT WOS:000220300600036 ER PT J AU Zhao, JH Herrnstein, RM Bower, GC Goss, WM Liu, SM AF Zhao, JH Herrnstein, RM Bower, GC Goss, WM Liu, SM TI A radio outburst nearly coincident with the large X-ray flare from Sagittarius A* on 2002 October 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : active; Galaxy : center; radio continuum : galaxies ID SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; FLUX-DENSITY; VARIABILITY; SPECTRUM; JET; MILLIMETER; MODEL AB A large radio outburst from Sgr A* was observed during the Very Large Array weekly monitoring program at 2 cm, 1.3 cm, and 7 mm, nearly coincident with the brightest X-ray flare detected to date with the XMM-Newton X-ray observatory on 2002 October 3. The flux density of 1.9 +/- 0.2 Jy measured at 7 mm exceeds the mean value (1.00 +/- 0.01 Jy) by a factor of similar to2, one of the two highest increases observed during the past 3 yr (2000 June - 2003 October), while less significant increases in flux densities were observed at 1.3 and 2 cm. The radio observation started 13.5 hr after the onset of the X-ray flare ( which had occurred over a 45 minute duration) and continued for 1.3 hr. During the observation, there was no significant (<3 σ) change in the radio flux densities at all three wavelengths, indicating that the radio outburst varied on a timescale of greater than 1 hr. A spectral index of α = 2.4(-0.6)(+0.3) (Sproportional tonu(alpha)) was derived for the outburst component, consistent with an optically thick non-thermal synchrotron source. These results suggest that energetic electrons responsible for the radio outburst might be produced via a process associated with the X-ray flare then transported to large radii, producing the observed radio outburst. The observation is the first evidence for a correlated variation in the radio and X-ray emissions from Sgr A*. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Columbia Univ, Dept Astron, New York, NY 10027 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, MS 78, 60 Garden St, Cambridge, MA 02138 USA. EM jzhao@cfa.harvard.edu RI liu, siming/B-5389-2011 NR 27 TC 28 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 MAR 10 PY 2004 VL 603 IS 2 BP L85 EP L88 DI 10.1086/383128 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 804LS UT WOS:000220300800006 ER PT J AU Crayn, DM Winter, K Smith, JAC AF Crayn, DM Winter, K Smith, JAC TI Multiple origins of crassulacean acid metabolism and the epiphytic habit in the Neotropical family Bromeliaceae SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID SUBFAMILY PITCAIRNIOIDEAE BROMELIACEAE; PHYLOGENETIC-RELATIONSHIPS; PHOTOSYNTHETIC PATHWAYS; TILLANDSIOIDEAE BROMELIACEAE; PHYSIOLOGICAL ECOLOGY; NDHF SEQUENCES; CO2 FIXATION; EVOLUTION; CAM; CLASSIFICATION AB The large Neotropical family Bromeliaceae presents an outstanding example of adaptive radiation in plants, containing a wide range of terrestrial and epiphytic life-forms occupying many distinct habitats. Diversification in bromeliads has been linked to several key innovations, including water- and nutrient-impounding phytotelmata, absorptive epidermal trichomes, and the water-conserving mode of photosynthesis known as crassulacean acid metabolism (CAM). To clarify the origins of CAM and the epiphytic habit, we conducted a phylogenetic analysis of nucleotide sequences for 51 bromeliad taxa by using the plastid loci matK and the rps16 intron, combined with a survey of photosynthetic pathway determined by carbon-isotope ratios for 1,873 species representing 65% of the family. Optimization of character-states onto the strict consensus tree indicated that the last common ancestor of Bromeliaceae was a terrestrial C(3) mesophyte, probably adapted to moist, exposed, nutrient-poor habitats. Both CAM photosynthesis and the epiphytic habit evolved a minimum of three times in the family, most likely in response to geological and climatic changes in the late Tertiary. The great majority of epiphytic forms are now found in two lineages: in subfamily Tillandsioideae, in which C(3) photosynthesis was the ancestral state and CAM developed later in the most extreme epiphytes, and in subfamily Bromelioideae, in which CAM photosynthesis predated the appearance of epiphytism. Subsequent radiation of the bromelioid line into less xeric habitats has led to reversion to C(3) photosynthesis in some taxa, showing that both gain and loss of CAM have occurred in the complex evolutionary history of this family. C1 Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. Royal Bot Gardens, Sydney, NSW 2000, Australia. Smithsonian Trop Res Inst, Ancon, Panama. RP Smith, JAC (reprint author), Univ Oxford, Dept Plant Sci, S Parks Rd, Oxford OX1 3RB, England. EM andrew.smith@plants.ox.ac.uk RI Crayn, Darren/A-7386-2011 OI Crayn, Darren/0000-0001-6614-4216 NR 66 TC 134 Z9 145 U1 5 U2 39 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 MAR 9 PY 2004 VL 101 IS 10 BP 3703 EP 3708 DI 10.1073/pnas.0400366101 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 802LA UT WOS:000220163800068 PM 14982989 ER PT J AU Fallon, SM Ricklefs, RE Latta, SC Bermingham, E AF Fallon, SM Ricklefs, RE Latta, SC Bermingham, E TI Temporal stability of insular avian malarial parasite communities SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE avian malaria; temporal stability; community; turnover; Plasmodium; Haemoproteus ID PLASMODIUM-FALCIPARUM; VERTEBRATE HOST; TAXON CYCLES; CYTOCHROME-B; PREVALENCE; LIZARD; POPULATION; EVOLUTION; ECOLOGY; ISLAND AB Avian malaria is caused by a diverse community of genetically differentiated parasites of the genera Plasmodium and Haemoproteus. Rapid seasonal and annual antigenic allele turnover resulting from selection by host immune systems, as observed in some parasite populations infecting humans, may extend analogously to dynamic species compositions within communities of avian malarial parasites. To address this issue, we examined the stability of avian malarial parasite lineages across multiple time-scales within two insular host communities. Parasite communities in Puerto Rico and St Lucia included 20 and 14 genetically distinct parasite lineages, respectively. Lineage composition of the parasite community in Puerto Rico did not vary seasonally or over a 1 year interval. However, over intervals approaching a decade, the avian communities of both islands experienced an apparent loss or gain of one malarial parasite lineage, indicating the potential for relatively frequent lineage turnover. Patterns of temporal variation of parasite lineages in this study suggest periodic colonization and extinction events driven by a combination of host-specific immune responses, competition between lineages and drift. However, the occasional and ecologically dynamic lineage turnover exhibited by insular avian parasite communities is not as rapid as antigenic allele turnover within populations of human malaria. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Fallon, SM (reprint author), Smithsonian Inst, Genet Program, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM fallon.sylvia@nmnh.si.edu NR 46 TC 46 Z9 47 U1 0 U2 24 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 MAR 7 PY 2004 VL 271 IS 1538 BP 493 EP 500 DI 10.1098/rspb.2003.2621 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 779LV UT WOS:000189299600008 PM 15129959 ER PT J AU DeVorkin, D AF DeVorkin, D TI The Cambridge Encyclopedia of Space - Missions, applications and exploration SO SCIENCE LA English DT Book Review C1 Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20013 USA. RP DeVorkin, D (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, POB 37012, Washington, DC 20013 USA. EM David.DeVorkin@nasm.si.edu NR 1 TC 0 Z9 0 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 MAR 5 PY 2004 VL 303 IS 5663 BP 1470 EP 1471 DI 10.1126/science.1094780 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 800AA UT WOS:000220000100022 ER PT J AU Fonseca, DM Keyghobadi, N Malcolm, CA Mehmet, C Schaffner, F Mogi, M Fleischer, RC Wilkerson, RC AF Fonseca, DM Keyghobadi, N Malcolm, CA Mehmet, C Schaffner, F Mogi, M Fleischer, RC Wilkerson, RC TI Emerging vectors in the Culex pipiens complex SO SCIENCE LA English DT Article ID WEST-NILE-VIRUS; NEW-YORK-CITY; MOSQUITOS; CULICIDAE; DIPTERA; QUINQUEFASCIATUS; POPULATIONS; INFECTION; BIRDS AB In the Old World, some mosquitoes in the Culex pipiens complex are excellent enzootic vectors of West Nile virus, circulating the virus among birds, whereas others bite mainly humans and other mammals. Here we show that, in northern Europe, such forms differing in behavior and physiology have unique microsatellite fingerprints with no evidence of gene flow between them, as would be expected from distinct species. In the United States, however, hybrids between these forms are ubiquitous. Such hybrids between human-biters and bird-biters may be the bridge vectors contributing to the unprecedented severity and range of the West Nile virus epidemic in North America. C1 Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. Walter Reed Army Inst Res, Dept Entomol, Div Communicable Dis & Immunol, Silver Spring, MD 20910 USA. Univ London, Queen Mary, Sch Biol Sci, London E1 4NS, England. Adege, Entente Interdept Demousticat Mediterranee, F-34184 Montpellier 4, France. Saga Med Sch, Dept Microbiol, Div Parasitol, Saga 8498501, Japan. RP Fonseca, DM (reprint author), Acad Nat Sci Philadelphia, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. EM fonseca@acnatsci.org OI Fonseca, Dina/0000-0003-4726-7100 FU NIGMS NIH HHS [1R01GM063258]; ODCDC CDC HHS [U50/CCU220532] NR 31 TC 240 Z9 253 U1 5 U2 32 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 MAR 5 PY 2004 VL 303 IS 5663 BP 1535 EP 1538 DI 10.1126/science.1094247 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 800AA UT WOS:000220000100048 PM 15001783 ER PT J AU Sumner, S Hughes, WOH Pedersen, JS Boomsma, JJ AF Sumner, S Hughes, WOH Pedersen, JS Boomsma, JJ TI Ant parasite queens revert to mating singly SO NATURE LA English DT Editorial Material ID FUNGUS-GROWING ANTS; SOCIAL HYMENOPTERA; TRANSITION; NUMBER C1 Univ Copenhagen, Dept Populat Biol, Inst Biol, DK-2100 Copenhagen, Denmark. RP Sumner, S (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM jjboomsma@zi.ku.dk RI Sumner, Seirian/E-6611-2011; Hughes, William/A-6957-2014; Pedersen, Jes Soe/J-6337-2014; Boomsma, Jacobus/M-2785-2014 OI Hughes, William/0000-0003-0951-9768; Pedersen, Jes Soe/0000-0002-4439-2638; Boomsma, Jacobus/0000-0002-3598-1609 NR 11 TC 69 Z9 71 U1 1 U2 11 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 4 PY 2004 VL 428 IS 6978 BP 35 EP 36 DI 10.1038/428035a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 780GK UT WOS:000189363800026 PM 14999273 ER PT J AU Potts, R AF Potts, R TI Paleoenvironmental basis of cognitive evolution in great apes SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article; Proceedings Paper CT 71st Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 10-13, 2002 CL BUFFALO, NY SP Amer Assoc Phys Anthropol DE great apes; cognition; environment; fruit-habitat hypothesis; extinction; variability selection ID EUROPEAN MIOCENE CATARRHINES; DENTAL MICROWEAR; BEHAVIORAL ECOLOGY; SEASONAL-VARIATION; DIETARY-RESPONSE; FRUIT ABUNDANCE; MIDDLE MIOCENE; LOPE RESERVE; LIFE-HISTORY; FORT TERNAN AB A bias favoring tree-dominated habitats and ripe-fruit frugivory has persisted in great ape evolution since the early Miocene. This bias is indicated by fossil ape paleoenvironments, molar morphology, dental microwear, the geographic pattern of extinctions, and extant apes' reliance on wooded settings. The ephemeral aspect of high-quality fruit has placed a premium on cognitive and social means of finding and defending food sources, and appears related to great apes' affinity since the Miocene for wooded, fruit-rich environments. These habitats have, however, undergone a severe withdrawal toward the low latitudes of Africa and Southeast Asia since the late Miocene, corresponding to a decline in the diversity of great apes beginning 9.5 million years ago. Plio-Pleistocene records imply that wooded settings of Africa anal SE Asia were prone to substantial fragmentation and coalescence. Once apes were confined to equatorial settings, therefore, habitat instability heightened the spatial/temporal uncertainty of ripe-fruit sources. Prolonged learning, the assignment of attributes to distant places, mental representation, and reliance on fallback foods were all favored in this dynamic environmental context. These abilities helped sustain forest frugivory in most lineages. Fluid social grouping afforded the animals opportunities to locate ephemeral foods in continuous and fragmented forests. Fission-fusion grouping also magnified the problems of object impermanence (of individuals) and dispersion manifested by food sources in the ecological realm. Thus the spatial and temporal dynamics of fruit and wooded habitats since the Miocene are reflected in important components of great ape cognition, foraging, and sociality. In contrast to great apes, cercopithecoid monkeys have increased their plant dietary options and diversified in seasonal environments since the late Miocene. Early hominins eventually severed the habitat bias that characterized the evolution of great apes, and later expanded into diverse environments. (C) 2004 Whiley-Liss, Inc. C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Potts, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. EM potts.rick@nmnh.si.edu NR 78 TC 32 Z9 33 U1 2 U2 19 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 MAR PY 2004 VL 62 IS 3 BP 209 EP 228 DI 10.1002/ajp.20016 PG 20 WC Zoology SC Zoology GA 812CA UT WOS:000220816400006 PM 15027093 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, WN Zatwarnicki, T TI Tronamyia, a new genus of shore flies, and a phylogenetic reassessment of the tribe Lipochaetini Becker (Diptera : Ephydridae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Diptera; Ephydridae; Lipochaetini; Tronamyia; phylogeny ID REVISION AB The genus Tronamyia is described in the tribe Lipochaetini (subfamily Gymnomyzinae) with Asmeringa lindsleyi Sturtevant & Wheeler (new combination) as its type species. The type species had previously been listed as an unplaced species in the tribe Atissini (subfamily Hydrelliinae). In a phylogenetic analysis of the tribe Lipochaetini, Tronamyia is the sister group of Lipochaeta Coquillett, a genus that also occurs along maritime beaches or inland saline or alkaline playas of the New World. C1 Smithsonian Inst, Entomol Sect, Dept Systemat Biol, Washington, DC 20013 USA. Polish Acad Sci, Museum Zool, PL-00679 Warsaw, Poland. Polish Acad Sci, Inst Zool, PL-00679 Warsaw, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Entomol Sect, Dept Systemat Biol, POB 37012, Washington, DC 20013 USA. OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 NR 17 TC 4 Z9 4 U1 0 U2 0 PU ENTOMOLOGICAL SOC AMER PI LANHAM PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAR PY 2004 VL 97 IS 2 BP 259 EP 270 DI 10.1603/0013-8746(2004)097[0259:TANGOS]2.0.CO;2 PG 12 WC Entomology SC Entomology GA 803AI UT WOS:000220203600010 ER PT J AU Hall, JPW Harvey, DJ Janzen, DH AF Hall, JPW Harvey, DJ Janzen, DH TI Life history of Calydna sturnula with a review of larval and pupal balloon setae in the Riodinidae (Lepidoptera) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE balloon setae; Calydna; Helicopini; larval defenses; Nymphidiini ID BUTTERFLIES; THISBE; NYMPHIDIINI; PHYLOGENY; ECOLOGY; ANTS AB The immature stages of Calydna sturnula, from the second instar onwards, are described and illustrated from tropical dry forest in the Area de Conservacion Guanacaste in northwestern Costa Rica. The foodplant in all cases was Schoepfia schreberi (Olacaceae). Only six of the 219 individual caterpillars and pupae collected during the last 15 yr were parasitized by braconid and chalcid wasps and a tachinid fly. The larval ultrastructure of C. sturnula was studied by means of scanning electron microscopy, with emphasis placed on their prothoracic balloon setae, rare structures in the Riodinidae. The occurrence of larval and pupal balloon setae in the Riodinidae is reviewed. Larval balloon setae are currently known from all three genera of the Helicopini, at least Calydna in the incertae sedis section of the Riodininae, and at least three genera of the Nymphidiini. Larval material was examined for all but one of these genera, and the macro and ultrastructure of their balloon setae are described, illustrated, and compared. Pupal balloon setae are currently known only from Helicopis and Calydna. The balloon setae of Calydna and the genera of the Helicopini are found to be more similar to each other than to those of the Nymphidiini genera. Because balloon setae occur in nonmyrmecophilous (such as Calydna) as well as myrmecophilous species, we hypothesize that they are used to store and disperse a noxious chemical when the caterpillar or pupa is grabbed by a predator, rather than to facilitate a symbiotic relationship with ants, as previously suggested. Internally, balloon setae are filled with a spongy yellowish material that consists of a dense latticework of tiny strands. We suggest that as these strands enter the otherwise hollow external acanthae, the acanthae discharge the noxious chemical when the balloon setae are squeezed. C1 Smithsonian Inst, Natl Museum Amer Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA. NR 47 TC 8 Z9 8 U1 0 U2 0 PU ENTOMOL SOC AMER PI LANHAM PA 9301 ANNAPOLIS RD, LANHAM, MD 20706 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAR PY 2004 VL 97 IS 2 BP 310 EP 321 DI 10.1603/0013-8746(2004)097[0310:LHOCSW]2.0.CO;2 PG 12 WC Entomology SC Entomology GA 803AI UT WOS:000220203600016 ER PT J AU Calzetti, D Harris, J Gallagher, JS Smith, DA Conselice, CJ Homeier, N Kewley, L AF Calzetti, D Harris, J Gallagher, JS Smith, DA Conselice, CJ Homeier, N Kewley, L TI Ionized gas in local starburst galaxies: Global and small-scale feedback from star formation SO ASTRONOMICAL JOURNAL LA English DT Review DE galaxies : ISM; galaxies : interactions; galaxies : starburst; ISM : structure ID H-II REGIONS; HUBBLE-SPACE-TELESCOPE; INFRARED SPECTRAL DISTRIBUTIONS; CHARGE-TRANSFER EFFICIENCY; X-RAY OBSERVATIONS; INTERSTELLAR-MEDIUM; DWARF GALAXIES; SPIRAL GALAXIES; IRREGULAR GALAXIES; FORMING GALAXIES AB The small- and intermediate-scale structure and the fraction of the interstellar medium (ISM) ionized by nonradiative processes are investigated in a small sample of four local starburst galaxies, imaged with the Hubble Space Telescope (HST) Wide Field Planetary Camera 2. The sample comprises three dwarf galaxies, NGC 3077, 4214, and 5253, and one giant spiral, NGC 5236 (M83). The galaxies span a range in metallicity (similar to0.2 - 2 Z(.)), luminosity (M-B similar to - 17 to - 20), and environment (isolated, interacting), enabling the investigation of nonradiative ionization processes in a variety of galactic conditions. For this purpose, the four galaxies were imaged in the lines of Hbeta (4861 Angstrom), [O III] (5007 Angstrom), Halpha (6563 Angstrom), and [S II] (6717, 6731 Angstrom). This is a unique set of data, as very few galaxies ( and only our four starbursts) have ever been imaged by HST in the relatively faint lines of Hbeta and [S II]. The use of HST has allowed us to trace nonphotoionized gas in these galaxies on scales ranging from a few tens of parsecs to a few hundred parsecs and, thus, to provide a full budget for this ionized gas component. Using the "maximum starburst line'' of Kewley et al. to discriminate between photoionized and nonphotoionized gas, we find that in all four galaxies non-photoionization processes are responsible for a small fraction of the total Halpha emission, at the level of 3% - 4%. Because the nonphotoionized gas is associated with low Halpha surface brightness, it occupies between one-sixth and one-quarter of the total imaged area. The central starbursts yield enough mechanical energy to produce the nonphotoionized gas in the four galaxies, by means of shocks from massive star winds and supernova explosions. In particular, the starbursts in the three dwarf galaxies must deposit a significant fraction, 70% - 100%, of their mechanical energy into the surrounding ISM, in order to account for the observed luminosity of the nonphotoionized gas. The morphology of the nonphotoionized regions is different in the dwarfs and the giant spiral. As already established in previous works, nonphotoionized gas in dwarfs is mainly associated with extended "shells'' or filamentary regions, likely areas of supernova- driven expanding gas. In all three dwarfs, star formation has been an ongoing process for the last few times 10(7) yr to similar to 10(8) yr; time-extended star formation episodes are a requirement to sustain the observed luminosity of the nonphotoionized gas. In the massive spiral, the nonphotoionized gas is concentrated in localized areas surrounded by active star formation, with no evidence of extended structures on the same ( or smaller) spatial scales as the "shells'' in the dwarfs. The two Halpha cavities in NGC 5236 may be evolved regions within the starburst. This confirms the picture that starbursts remain confined events in massive galaxies, likely as a consequence of the deep potential well. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Calzetti, D (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM calzetti@stsci.edu; jharris@stsci.edu RI Conselice, Christopher/B-4348-2013; OI Conselice, Christopher/0000-0003-1949-7638 NR 119 TC 57 Z9 57 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 2004 VL 127 IS 3 BP 1405 EP 1430 DI 10.1086/382095 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 801FL UT WOS:000220081700013 ER PT J AU Schiavon, RP Caldwell, N Rose, JA AF Schiavon, RP Caldwell, N Rose, JA TI The integrated spectrum of M67 and the spectroscopic age of M32 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : individual (M32); galaxies : stellar content; open clusters and associations : individual (M67); stars : evolution ID EARLY-TYPE GALAXIES; OLD STELLAR POPULATIONS; COLOR-MAGNITUDE DIAGRAM; HORIZONTAL-BRANCH STARS; DIGITAL SKY SURVEY; OPEN CLUSTER M67; BLUE STRAGGLERS; CHEMICAL-COMPOSITION; GLOBULAR-CLUSTERS; 47 TUCANAE AB We construct an integrated spectrum of the intermediate-age, solar-metallicity Galactic cluster M67, from individual spectroscopic observations of bona fide cluster members. The spectrum so obtained is used as a template to test our stellar population synthesis models, in an age and metallicity regime where such models remain largely untested. As a result, we demonstrate that our models predict a spectroscopic age of 3.5 +/- 0.5 Gyr for M67, which is the same age we obtain from fitting isochrones to the color-magnitude diagram of the cluster. Full consistency is reached when using either Hbeta, Hgamma, or Hdelta as the age indicator. We also check if the models, when applied to the cluster integrated spectrum, predict elemental abundances in agreement with the known detailed abundance pattern of the cluster. The models also pass the latter test, by predicting the abundances of iron, magnesium, carbon, and nitrogen in agreement with detailed abundance analyses of cluster stars to within 0.1 dex. Encouraged by the high degree of consistency of our models, we apply them to the study of the integrated spectrum of the central 3" of the compact elliptical galaxy M32. The resulting luminosity-weighted age of the galaxy ranges between 2 and 3.5 Gyr, depending on the age indicator adopted. According to our models, the center of M32 seems to have a supersolar iron abundance, ranging between [Fe/H] similar to +0.1 and + 0.3, depending on the spectral index adopted. The light element magnesium seems to be underabundant in the center of M32 relative to iron by aboutsimilar to 0.1 - 0.2 dex, whereas the data are consistent with nearly solar carbon and nitrogen abundances relative to iron. We find that single- age, single-metallicity stellar population models with solar-scaled abundance patterns cannot fit all the Balmer and metal lines in the integrated spectrum of M32. In particular, there is a systematic trend in the sense that bluer absorption lines indicate a younger age and a higher metallicity. This slight inconsistency can be due either to ( unaccounted for) abundance ratio effects on blue iron and Balmer line indices or to a spread of the ages of the stellar populations in M32. Current stellar population models cannot break this degeneracy at the level of accuracy required to address this problem. C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. RP Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA. EM ripisc@ucolick.org; caldwell@cfa.harvard.edu; jim@physics.unc.edu NR 75 TC 50 Z9 51 U1 1 U2 3 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 MAR PY 2004 VL 127 IS 3 BP 1513 EP 1530 DI 10.1086/381950 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 801FL UT WOS:000220081700020 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ Beers, TC Kurtz, MJ Roll, JB AF Brown, WR Geller, MJ Kenyon, SJ Beers, TC Kurtz, MJ Roll, JB TI Mapping the inner halo of the Galaxy with 2MASS-selected horizontal-branch candidates SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy : halo; Galaxy : stellar content; stars : early-type ID RR LYRAE STARS; A-TYPE STARS; SAGITTARIUS DWARF GALAXY; DIGITAL SKY SURVEY; SURVEY COMMISSIONING DATA; GALACTIC HALO; MILKY-WAY; STELLAR HALO; STATISTICAL PARALLAX; SOLAR NEIGHBORHOOD AB We use Two Micron All Sky Survey (2MASS) photometry to select blue horizontal-branch (BHB) candidates covering the sky, |b| > 15degrees. A 12.5< J(0) < 15.5 sample of BHB stars traces the thick disk and inner halo to d(.) < 9 kpc, with a density comparable to that of M giant stars. We base our sample selection strategy on the Century Survey Galactic Halo Project, a survey that provides a complete, spectroscopically identified sample of blue stars to a similar depth as the 2MASS catalog. We show that a - 0.20 < (J - H)(0) < 0.10, - 0.10 < ( H - K)(0) < 0.10 color-selected sample of stars is 65% complete for BHB stars and is composed of 47% BHB stars. We apply this photometric selection to the full 2MASS catalog and see no spatial overdensities of BHB candidates at high Galactic latitude, | b| > 50degrees. We insert simulated star streams into the data and conclude that the high Galactic latitude BHB candidates are consistent with having no similar to5degrees wide star stream with density greater than 0.33 objects deg(-2) at the 95% confidence level. The absence of observed structure suggests that there have been no major accretion events in the inner halo in the last few Gyr. However, at low Galactic latitudes a two-point angular correlation analysis reveals structure on angular scales theta less than or similar to 1degrees. This structure is apparently associated with stars in the thick disk and has a physical scale of 10 - 100 pc. Interestingly, such structures are expected by cosmological simulations that predict the majority of the thick disk may arise from accretion and disruption of satellite mergers. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI KURTZ, Michael /B-3890-2009; OI Kenyon, Scott/0000-0003-0214-609X; Kurtz, Michael/0000-0002-6949-0090 NR 65 TC 20 Z9 20 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 MAR PY 2004 VL 127 IS 3 BP 1555 EP 1566 DI 10.1086/381910 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 801FL UT WOS:000220081700023 ER PT J AU Paulson, DB Saar, SH Cochran, WD Henry, GW AF Paulson, DB Saar, SH Cochran, WD Henry, GW TI Searching for planets in the Hyades. III. The quest for short-period planets SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations : individual (Hyades); planetary systems : general; stars : activity; stars : spots; techniques : photometric; techniques : radial velocities ID RADIAL-VELOCITY VARIATIONS; ACTIVE-REGION EVOLUTION; HOBBY-EBERLY TELESCOPE; MAGNETIC ACTIVITY; TIME-SERIES; COOL STARS; DWARFS; VARIABILITY; LONGITUDES; PHOTOMETRY AB We have been using the Keck I High Resolution Spectrograph to search for planetary companions in the Hyades cluster. We selected four stars from this sample that showed significant radial velocity variability on short timescales to search for short-period planetary companions. The radial velocities of these four stars were monitored regularly with the Hobby-Eberly Telescope for approximately 2 months, while sparse data were also taken over similar to4 months: we also obtained near-simultaneous photometric observations with one of the automatic photoelectric telescopes at Fairborn Observatory. For three of the stars, we detect photometric variability with the same period present in the radial velocity (v(r)) measurements, compatible with the expected rotation rates for Hyades members. The fourth star continues to show vr variations and minimal photometric variability but with no significant periodicity. This study shows that for the three stars with periodic behavior, a significant portion of the v(r) fluctuations are likely due primarily to magnetic activity modulated by stellar rotation rather than planetary companions. Using simple models for the v(r) perturbations arising from spot and plage, we demonstrate that both are likely to contribute to the observed v(r) variations. Thus, simultaneous monitoring of photometric (photospheric) and spectroscopic (chromospheric) variations is essential for identifying the cause of Doppler-shifted absorption lines in more active stars. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37203 USA. RP Paulson, DB (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg, Ann Arbor, MI 48109 USA. EM apodis@astro.as.utexas.edu; ssaar@cfa.harvard.edu; wdc@astro.as.utexas.edu; henry@schwab.tsuniv.edu NR 40 TC 63 Z9 63 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 2004 VL 127 IS 3 BP 1644 EP 1652 DI 10.1086/381948 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 801FL UT WOS:000220081700031 ER PT J AU Hernandez, J Calvet, N Briceno, C Hartmann, L Berlind, P AF Hernandez, J Calvet, N Briceno, C Hartmann, L Berlind, P TI Spectral analysis and classification of Herbig Ae/Be stars SO ASTRONOMICAL JOURNAL LA English DT Review DE Hertzsprung-Russell diagram; stars : emission-line, Be; stars : pre-main-sequence; techniques : spectroscopic ID MAIN-SEQUENCE STARS; INTERMEDIATE-MASS STARS; YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DISKS; EMISSION-LINE; MOLECULAR CLOUDS; PHOTOMETRIC-OBSERVATIONS; ROTATIONAL VELOCITIES; V633 CASSIOPEIAE; FORBIDDEN LINES AB We present an analysis of the optical spectra of 75 early-type emission-line stars, many of which have been classified previously as Herbig Ae/Be (HAeBe) stars. Accurate spectral types were derived for 58 members of the sample; high continuum veiling, contamination by nonphotospheric absorption features, or a composite binary spectrum prevented accurate spectral typing for the rest. Approximately half of our sample exhibited [O I] lambda6300 forbidden-line emission down to our detection limit of 0.1 Angstrom equivalent width; a third of the sample exhibited Fe II emission ( multiplet 42). A subset of 11 of the HAeBe sample showed abnormally strong Fe II absorption; 75% of this subset are confirmed UX Ori objects. Combining our spectral typing results with photometry from the literature, we confirm previous findings of high values of total-to-selective extinction (R-V similar to 5) in our larger sample, suggesting significant grain growth in the environments of HAeBe stars. With this high value of RV, the vast majority of HAeBe stars appear younger than with the standard R-V = 3.1 extinction law and are more consistent with being pre-main-sequence objects. C1 Univ Los Andes, Merida 5101A, Venezuela. Ctr Invest Astron CIDA, Merida 5101A, Venezuela. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hernandez, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jesush@cida.ve; ncalvet@cfa.harvard.edu; briceno@cida.ve; hartmann@cfa.harvard.edu; pberlind@cfa.harvard.edu NR 116 TC 189 Z9 190 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 2004 VL 127 IS 3 BP 1682 EP 1701 DI 10.1086/381908 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 801FL UT WOS:000220081700034 ER PT J AU Natta, A Testi, L Neri, R Shepherd, DS Wilner, DJ AF Natta, A Testi, L Neri, R Shepherd, DS Wilner, DJ TI A search for evolved dust in Herbig Ae stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : planetary systems : protoplanetary disks; stars : planetary systems : formation; stars : formation ID T-TAURI STARS; INTERMEDIATE-MASS STARS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS; HIGH-RESOLUTION; SYSTEMS; ACCRETION; GAS; EVOLUTION AB We present observations of six isolated, pre-main-sequence, intermediate mass stars selected for shallow spectra at submillimeter wavelengths at 1.3, 2.6, 7.0, and 36 millimeters from the IRAM PdBI and the VLA. We analyze the new observations of these stars (HD 34282, HD 35187, HD 142666, HD 143006, HD 150193, HD 163296) together with similar observations of three additional stars from the literature (CQ Tau, UX Ori, TW Hya), in the context of self-consistent irradiated disk models. Our aim is to constrain the wavelength dependence of the dust opacity and the total dust mass in the disks. The shallow wavelength dependence of the opacity is confirmed and for a few stars extended to significantly longer wavelengths. For any plausible dust properties, this requires grain growth from interstellar sizes to maximum sizes of at least a few millimeters, and very likely to several centimeters or more. For four of the stars (HD 34282, HD 163296, CQ Tau, TW Hya), the millimeter emission has been spatially resolved, and the large disk radii (>100 AU) rule out that high optical depths play a role. The mass of dust that has been processed into large grains is substantial, and in some cases implies a disk mass comparable to the mass of the central star. C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. Natl Radio Astron Observ, Socorro, NM 87801 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Natta, A (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM natta@arcetri.astro.it NR 31 TC 115 Z9 117 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 2004 VL 416 IS 1 BP 179 EP 186 DI 10.1051/0004-6361:20035620 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 807XZ UT WOS:000220535500017 ER PT J AU Tafalla, M Myers, PC Caselli, P Walmsley, CM AF Tafalla, M Myers, PC Caselli, P Walmsley, CM TI On the internal structure of starless cores - I. Physical conditions and the distribution of CO, CS, N2H+, and NH3 in L1498 and L1517B SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM : abundances; ISM : clouds; ISM : molecules; stars : formation; ISM : individual objects : L1498, L1517B ID MOLECULAR CLOUD CORES; PRE-STELLAR CORES; DENSE CORES; DARK CLOUDS; PROTOSTELLAR CORES; HYPERFINE-STRUCTURE; INITIAL CONDITIONS; PRESTELLAR CORES; CHEMICAL-MODELS; MILLIMETER-WAVE AB We have characterized the physical structure and chemical composition of two close-to-round starless cores in Taurus-Auriga, L1498 and L1517B. Our analysis is based on high angular resolution observations in at least two transitions of NH3, N2H+, CS, (CS)-S-34, (CO)-O-18, and (CO)-O-17, together with maps of the 1.2 mm continuum. For both cores, we derive radial profiles of constant temperature and constant turbulence, together with density distributions close to those of non-singular isothermal spheres. Using these physical conditions and a Monte Carlo radiative transfer model, we derive abundance profiles for all species and model the strong chemical differentiation of the core interiors. According to our models, the NH3 abundance increases toward the core centers by a factor of several (approximate to5) while N2H+ has a constant abundance over most of the cores. In contrast, both (CO)-O-18 and CS (and isotopomers) are strongly depleted in the core interiors, most likely due to their freeze out onto grains at densities of a few 10(4) cm(-3). Concerning the kinematics of the dense gas, we find (in addition to constant turbulence) a pattern of internal motions at the level of 0.1 km s(-1). These motions seem correlated with asymmetries in the pattern of molecular depletion, and we interpret them as residuals of core contraction. Their distribution and size suggest that core formation occurs in a rather irregular manner and with a time scale of a Myr. A comparison of our derived core properties with those predicted by supersonic turbulence models of core formation shows that our Taurus cores are much more quiescent than representative predictions from these models. In two appendices at the end of the paper we present a simple and accurate approximation to the density profile of an isothermal (Bonnor-Ebert) sphere, and a Monte Carlo-calibrated method to derive Gas kinetic temperatures using NH3 data. C1 Observ Astron Nacl, Madrid, Spain. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. RP Observ Astron Nacl, Alfonso XII 3, Madrid, Spain. EM m.tafalla@oan.es NR 91 TC 273 Z9 273 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2004 VL 416 IS 1 BP 191 EP 212 DI 10.1051/0004-6361:20031704 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 807XZ UT WOS:000220535500019 ER PT J AU Beltran, MT Gueth, F Guilloteau, S Dutrey, A AF Beltran, MT Gueth, F Guilloteau, S Dutrey, A TI L1157: Interaction of the molecular outflow with the Class 0 environment SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : individual : L1157; stars : formation; stars : circumstellar matter; ISM : dust, extinction; ISM : molecules ID YOUNG STELLAR OBJECTS; STAR-FORMATION; BIPOLAR OUTFLOWS; ACCRETION DISKS; DUST OPACITIES; EMISSION; CLOUDS; ENVELOPE; L-1157; SIO AB We present high angular resolution interferometric observations [*] of the dust continuum at 2.7 and 1.3 mm, and of the HC3N (J = 12 --> 11) and (CO)-O-18 (J = 2 --> 1) emission around L1157-mm, a Class 0 object that drives a spectacular molecular outflow. The millimeter dust emission is clearly resolved into two components, a flattened compact source of similar to450 x 250 AU at 1.3 mm, and mass similar to0.1 M-., plus an extended envelope of similar to3000 AU at 1.3 mm, and mass similar to1.1 M-.. The millimeter spectral index varies throughout the region, with the lower value found toward the compact protostar, possibly indicating grain growth in the denser regions. A strong interaction between the molecular outflow and the close protostellar environment is taking place and affects the structure of the innermost parts of the envelope. This is shown by the spatial coincidence between the molecular outflow and the dust (1.3 mm continuum) and HC3N emission: both tracers show structures associated to the edges of the outflow lobes. Basically, the global picture sketched for the Class 0 object L1157-mm by Gueth et al. (1997) is supported. We find possible evidence of infall, but we do not detect any velocity gradient indicative of a rotating circumstellar disk. C1 Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astrofis Arcetri, I-50125 Florence, Italy. Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. RP Gueth, F (reprint author), Inst Radio Astron Millimetr, 300 Rue Piscine, F-38406 St Martin Dheres, France. EM gueth@iram.fr OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626 NR 51 TC 23 Z9 23 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 2004 VL 416 IS 2 BP 631 EP 640 DI 10.1051/0004-6361:20034123 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811PG UT WOS:000220783200020 ER PT J AU Perez, MR van den Ancker, ME de Winter, D Bopp, BW AF Perez, MR van den Ancker, ME de Winter, D Bopp, BW TI A young and complex binary star - HD 144432 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : circumstellar matter; stars : emission-line, Be; stars : individual : HD 144432; stars : binaries : visual; stars : pre-main sequence ID HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; BETA-PICTORIS PHENOMENON; INTERMEDIATE-MASS STARS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; SHELL STARS; FU ORIONIS; AE-TYPE; SPECTROSCOPY AB The southern emission-line star HD 144432 has received considerable attention due to its relative brightness (Vsimilar to8.17), its late spectral type (late A-type or perhaps early F) and its relative isolation from a bona-fide active star formation region. We present new imaging and spectroscopic data of this star, which in the past has been classified as both an evolved (post-AGB) object and an isolated Herbig Ae/Be star. We confirm the presence of a faint companion source located 1.4" north. which appears physically associated with HD 144432. New infrared spectroscopy reveals this companion to be a late-type (early-mid K) star, devoid of any emission lines. Furthermore, we confirm the pre-main sequence nature of this object, report the detection of Li I 6707.8 Angstrom absorption toward the HD 144432 system, and its apparent association with Sco OB2-2 located at 145 pc. C1 Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. TNO, TPD, NL-2600 AD Delft, Netherlands. Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. RP Perez, MR (reprint author), Los Alamos Natl Lab, POB 1663,ISR-DO,Mail Stop F650, Los Alamos, NM 87545 USA. EM mperez@lanl.gov; mvandena@eso.org; dolf@xiada.ft.uam.es; bbopp@uoft02.utoledo.edu NR 47 TC 19 Z9 19 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 MAR PY 2004 VL 416 IS 2 BP 647 EP 654 DI 10.1051/0004-6361:20034390 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811PG UT WOS:000220783200022 ER PT J AU Kervella, P Nardetto, N Bersier, D Mourard, D du Foresto, VC AF Kervella, P Nardetto, N Bersier, D Mourard, D du Foresto, VC TI Cepheid distances from infrared long-baseline interferometry - I. VINCI/VLTI observations of seven Galactic Cepheids SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques : interferometric; stars : variables : Cepheids; stars : oscillations ID PERIOD-LUMINOSITY RELATION; PROTOTYPE OPTICAL INTERFEROMETER; LIMB-DARKENING COEFFICIENTS; HUBBLE-SPACE-TELESCOPE; RADIAL-VELOCITY CURVE; CLASSICAL CEPHEIDS; FUNDAMENTAL PARAMETERS; ANGULAR DIAMETER; FE/H DETERMINATIONS; VLT INTERFEROMETER AB We report the angular diameter measurements of seven classical Cepheids, X Sgr, eta Aql, W Sgr, zeta Gem, beta Dor, Y Oph and l Car that we have obtained with the VINCI instrument, installed at ESO's VLT Interferometer (VLTI). We also present reprocessed archive data obtained with the FLUOR/IOTA instrument on zeta Gem, in order to improve the phase coverage of our observations. We obtain average limb darkened angular diameter values of (θ(LD)) over bar [X SGR] =1.471 +/- 0.033 mas, (θ(LD)) over bar[etaAql] = 1.839 +/- 0.028 mas, (θ(LD)) over bar [W Sgr] =1.312 +/- 0.029 mas, (θ(LD)) over bar [beta Dor] = 1.891 +/- 0.024 mas, (θ(LD)) over bar[zetaGem] = 1.747 +/- 0.061 mas, (θ(LD)) over bar [Y Oph] = 1.437 +/- 0.040 mas, and (θ(LD)) over bar [lCar] = 2.988 +/-0.012 mas.For four of these stars, eta Aql, WSgr, beta Dor, and l car, we detect the pulsational variation of their angular diameter. This enables us to compute directly their distances, using a modified version of the Baade-Wesselink method: d[eta Aql] = 276(-38)(+55) pc, d[W Sgr] = 379(-130)(+216) pc, d[betaDor] = 345(-80)(+175) pc, d[l Car] = 603(-19)(+24) pc. The stated error bars are statistical in nature. Applying a hybrid method, that makes use of the Gieren et al. (1998) Period-Radius relation to estimate the linear diameters, we obtain the following distances (statistical and systematic error bars are mentioned): d[X Sgr] = 324 +/- 7 +/- 17 pc, d[eta Aql] = 264 +/- 4 +/-14 pc, d[W Sgr] = 386 +/- 9 +/- 21 pc, d[betaDor] = 326 +/- 4 +/- 19 pc, d[zeta Gem] = 360 +/- 13 +/- 22 pc d[Y Oph] = 648 +/- 17 +/- 47 pc, d[l Car] = 542 +/- 2 +/- 49 pc. C1 European So Observ, Santiago 19, Chile. Observ Cote Azur, Dept Fresnel, CNRS, UMR 6528, F-06304 Nice 4, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Paris, LESIA, F-92195 Meudon, France. RP Kervella, P (reprint author), European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile. EM pkervell@eso.org NR 91 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 MAR PY 2004 VL 416 IS 3 BP 941 EP 953 DI 10.1051/0004-6361:20031743 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 809UP UT WOS:000220661900019 ER PT J AU Horan, D Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cui, W Daniel, M D'Vali, M Perez, IDC Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Evans, JL Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J AF Horan, D Badran, HM Bond, IH Boyle, PJ Bradbury, SM Buckley, JH Carter-Lewis, DA Catanese, M Celik, O Cui, W Daniel, M D'Vali, M Perez, IDC Duke, C Falcone, A Fegan, DJ Fegan, SJ Finley, JP Fortson, LF Gaidos, JA Gammell, S Gibbs, K Gillanders, GH Grube, J Hall, J Hall, TA Hanna, D Hillas, AM Holder, J Jarvis, A Jordan, M Kenny, GE Kertzman, M Kieda, D Kildea, J Knapp, J Kosack, K Krawczynski, H Krennrich, F Lang, MJ Le Bohec, S Linton, E Evans, JL Milovanovic, A Moriarty, P Muller, D Nagai, T Nolan, S Ong, RA Pallassini, R Petry, D Power-Mooney, B Quinn, J Quinn, M Ragan, K Rebillot, P Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Swordy, SP Syson, A Vassiliev, VV Wakely, SP Walker, G Weekes, TC Zweerink, J TI Constraints on the very high energy emission from BL Lacertae objects SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : general; galaxies : jets; gamma rays : observations ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; X-RAY; LAC OBJECTS; MARKARIAN 501; BLAZARS; MODEL; SEARCH; SAMPLE; JET AB We present results from observations of 29 BL Lacertae objects, taken with the Whipple Observatory 10 m gamma-ray telescope between 1995 and 2000. The observed objects are mostly at low redshift (z<0.2), but observations of objects of up to z=0.444 are also reported. Five of the objects are EGRET sources and two are unconfirmed TeV sources. Three of the confirmed sources of extragalactic TeV gamma rays were originally observed as part of this survey and have been reported elsewhere. No significant excesses are detected from any of the other objects observed, on timescales of days, months, or years. We report 99.9% confidence level flux upper limits for the objects for each observing season. The flux upper limits are typically 20% of the Crab flux, although for some sources, limits as sensitive as 6% of the Crab flux were derived. The results are consistent with the synchrotron self-Compton model predictions considered in this work. C1 Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Tanta Univ, Dept Phys, Tanta, Egypt. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Calif Los Angeles, Dept Phys, Los Angeles, CA 90095 USA. Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Univ Ireland, Expt Phys Dept, Dublin 4, Ireland. Natl Univ Ireland, Dept Phys, Galway, Ireland. Univ Utah, High Energy Astrophys Inst, Salt Lake City, UT 84112 USA. Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA. McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. Galway Mayo Inst Technol, Sch Sci, Galway, Ireland. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Horan, D (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, POB 97, Amado, AZ 85645 USA. EM dhoran@cfa.harvard.edu RI Hall, Jeter/E-9294-2015; Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Cui, Wei/0000-0002-6324-5772; Knapp, Johannes/0000-0003-1519-1383; Lang, Mark/0000-0003-4641-4201 NR 69 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 MAR 1 PY 2004 VL 603 IS 1 BP 51 EP 61 DI 10.1086/381430 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779ZM UT WOS:000189343900008 ER PT J AU Yoo, J DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Udalski, A Soszynski, I Wyrzykowski, L Kubiak, M Szymanski, M Pietrzynski, G Szewczyk, O Zebrun, K AF Yoo, J DePoy, DL Gal-Yam, A Gaudi, BS Gould, A Han, C Lipkin, Y Maoz, D Ofek, EO Park, BG Pogge, RW Udalski, A Soszynski, I Wyrzykowski, L Kubiak, M Szymanski, M Pietrzynski, G Szewczyk, O Zebrun, K CA muFUN Collaboration OGLE Collaboration TI OGLE-2003-BLG-262: Finite-source effects from a point-mass lens SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing; stars : low-mass, brown dwarfs ID BINARY MICROLENSING EVENTS; LIMB-DARKENING MEASUREMENT; GALACTIC BULGE; PLANET PHOTOMETRY; GALACTOCENTRIC DISTANCE; PROPER MOTIONS; MACHO 98-SMC-1; BAADES WINDOW; STELLAR; PARALLAX AB We analyze OGLE-2003-BLG-262, a relatively short (t(E)=12.5+/-0.1 day) microlensing event generated by a point-mass lens transiting the face of a K giant source in the Galactic bulge. We use the resulting finite-source effects to measure the angular Einstein radius, theta(E)=195+/-17 muas, and so constrain the lens mass to the FWHM interval 0.08 70) over the eight generations since founding. Results suggest a moderate bottleneck in the early establishment phase but with more than seven effective founders. Individuals in the UCSD population have shorter wings and tails than those in the nearby mountains and a common garden experiment indicates that the morphological differences are genetically based. The moderate effective population size is not sufficient for the observed morphological differences to have evolved as a consequence of genetic drift, indicating a major role for selection subsequent to the founding of the UCSD population. C1 Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. Univ Calif San Diego, Sect Ecol Behav & Evolut 0116, Div Biol Sci, La Jolla, CA 92093 USA. Smithsonian Inst, Mol Genet Lab, Washington, DC 20008 USA. RP Price, TD (reprint author), Univ Chicago, Dept Ecol & Evolut, 1101 E 57th St, Chicago, IL 60637 USA. EM pricet@uchicago.edu NR 50 TC 50 Z9 52 U1 1 U2 23 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 2004 VL 13 IS 3 BP 671 EP 681 DI 10.1046/j.1365-294X.2004.02104.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 772DQ UT WOS:000188825700014 PM 14871370 ER PT J AU Jones, FA Poelchau, MF Bouck, AC Hubbell, P AF Jones, FA Poelchau, MF Bouck, AC Hubbell, P TI Eight microsatellite markers for the neotropical tree Luehea seemannii (Tiliaceae) SO MOLECULAR ECOLOGY NOTES LA English DT Article DE Barro Colorado Island; gene flow; maternity and paternity analysis; Panama; seed dispersal ID POPULATIONS; FOREST AB We isolated eight polymorphic microsatellites from the neotropical tree Luehea seemannii for gene flow and genetic structure studies. We used a streptavidin subtractive enrichment technique to develop a library of CA/GT repeats. Eight loci were screened for diversity from 96 individuals from Barro Colorado Island (BCI) and neighbouring Gigante peninsula in Panama. Luehea seemannii shows moderate levels of genetic diversity within these two populations. Allelic richness ranged from four to nine alleles and averaged 6.44 alleles per locus. Average expected heterozygosity was 0.65 on BCI and 0.60 on Gigante. Results are compared to microsatellite data from another wind-dispersed gap colonizing species common in Panama. C1 Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Univ Georgia, Dept Genet, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Jones, FA (reprint author), Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. EM fajones@plantbio.uga.edu RI Jones, Andy/C-3460-2009 NR 13 TC 5 Z9 5 U1 0 U2 6 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD MAR PY 2004 VL 4 IS 1 BP 5 EP 8 DI 10.1046/j.1471-8286.2003.00543.x PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 777DJ UT WOS:000189159500002 ER PT J AU Keyghobadi, N Matrone, MA Ebel, GD Kramer, LD Fonseca, DM AF Keyghobadi, N Matrone, MA Ebel, GD Kramer, LD Fonseca, DM TI Microsatellite loci from the northern house mosquito (Culex pipiens), a principal vector of West Nile virus in North America SO MOLECULAR ECOLOGY NOTES LA English DT Article DE Culex pipiens; Culex quinquefasciatus; microsatellite; null allele; West Nile virus ID COMPETENCE AB Microsatellites were isolated and characterized in the northern house mosquito, Culex pipiens, a widespread pest species and important vector of diseases such as West Nile virus. An enrichment protocol yielded 150 positive clones. We designed primers to amplify 17 unique (GT)(n) microsatellites, eight of which amplified cleanly and were polymorphic. A survey of 29 individuals showed that these loci are highly variable with the number of alleles ranging from seven to 19 and expected heterozygosity ranging from 0.66 to 0.93. These markers will be useful for studies of population structure and intraspecific variation in epidemiological characteristics of Cx. pipiens. C1 Acad Nat Sci Philadelphia, Philadelphia, PA 19103 USA. Smithsonian Inst, NMHN, Genet Program, Washington, DC 20008 USA. NY State Dept Hlth, Wadsworth Ctr, Slingerlands, NY 12159 USA. RP Fonseca, DM (reprint author), Acad Nat Sci Philadelphia, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA. EM fonseca@acnatsci.org RI Ebel, Gregory/D-8324-2017; OI Fonseca, Dina/0000-0003-4726-7100 NR 9 TC 36 Z9 36 U1 0 U2 2 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1471-8278 J9 MOL ECOL NOTES JI Mol. Ecol. Notes PD MAR PY 2004 VL 4 IS 1 BP 20 EP 22 DI 10.1046/j.1471-8286.2003.00557.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 777DJ UT WOS:000189159500007 ER PT J AU Steppan, SJ Storz, BL Hoffmann, RS AF Steppan, SJ Storz, BL Hoffmann, RS TI Nuclear DNA phylogeny of the squirrels (Mammalia : Rodentia) and the evolution of arboreality from c-myc and RAG1 SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID B GENE-SEQUENCES; MOLECULAR PHYLOGENY; PLACENTAL MAMMALS; PASSERINE BIRDS; SCIURIDAE; INFERENCE; ORIGIN; RECOMBINATION; DIVERGENCES; SYSTEMATICS AB Although the family Sciuridae is large and well known, phylogenetic analyses are scarce. We report on a comprehensive molecular phylogeny for the family. Two nuclear genes (c-myc and RAG1) comprising approximately 4500 bp of data (most in exons) are applied for the first time to rodent phylogenetics. Parsimony, likelihood, and Bayesian analyses of the separate gene regions and combined data reveal five major lineages and refute the conventional elevation of the flying squirrels (Pteromyinae) to subfamily status. Instead, flying squirrels are derived from one of the tree squirrel lineages. C-myc indels corroborate the sequence-based topologies. The common ancestor of extant squirrels appears to have been arboreal, confirming the fossil evidence. The results also reveal an unexpected clade of mostly terrestrial squirrels with African and Holarctic centers of diversity. We present a revised classification of squirrels. Our results demonstrate the phylogenetic utility of relatively slowly evolving nuclear exonic data even for relatively recent clades. (C) 2003 Elsevier Science (USA). All rights reserved. C1 Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. Smithsonian Inst, Museum Natl Hist Nat, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Steppan, SJ (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA. EM steppan@bio.fsu.edu NR 66 TC 108 Z9 124 U1 3 U2 22 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2004 VL 30 IS 3 BP 703 EP 719 DI 10.1016/S1055-7903(03)00204-5 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 774AW UT WOS:000188958400017 PM 15012949 ER PT J AU Pavlovic, Z Roos, BO Cote, R Sadeghpour, HR AF Pavlovic, Z Roos, BO Cote, R Sadeghpour, HR TI Collisional properties of trapped cold chromium atoms SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; PERTURBATION-THEORY; DIPOLAR GASES; GROUND-STATE; CR-2; SPECTRA; LEVEL AB We report on calculations of the elastic cross section and thermalization rate for collision between two maximally spin-polarized chromium atoms in the cold and ultracold regimes, relevant to buffer-gas and magneto-optical cooling. We calculate ab initio potential-energy curves for Cr-2 and the van der Waals coefficient C-6, and construct interaction potentials between two colliding Cr atoms. We explore the effect of shape resonances on the elastic cross section, and find that they dramatically affect the thermalization rate. Our calculated value for the s-wave scattering length is compared in magnitude with a recent measurement. We propose that a dip in the elastic rate coefficient could be experimentally exploited to obtain an accurate value for the scattering length. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Chem Ctr Lund, Dept Theoret Chem, S-22100 Lund, Sweden. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Pavlovic, Z (reprint author), Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA. NR 34 TC 14 Z9 14 U1 0 U2 4 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 2004 VL 69 IS 3 AR 030701 DI 10.1103/PhysRevA.69.030701 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 808YU UT WOS:000220605200005 ER PT J AU Johnson, EA Rossman, GR AF Johnson, EA Rossman, GR TI An infrared and (1)H MAS NMR investigation of strong hydrogen bonding in ussingite, Na(2)AlSi(3)O(8)(OH) SO PHYSICS AND CHEMISTRY OF MINERALS LA English DT Article DE infrared spectroscopy; NMR spectroscopy; ussingite; low albite; hydrogen ID STRETCHING FREQUENCIES; CHEMICAL-SHIFT; LOW ALBITE; SPECTROSCOPY; FELDSPAR; MINERALS; LENGTHS; WATER; SI-29; FTIR AB The mineral ussingite, Na(2)AlSi(3)O(8)(OH), an "interrupted" tectosilicate, has strong hydrogen bonding between OH and the other nonbridging oxygen atom in the structure. Infrared spectra contain a strongly polarized, very broad OH-stretching band with an ill-defined maximum between 1500 and 1800 cm(-1), and a possible OH librational bending mode at 1295 cm(-1). The IR spectra confirm the orientation of the OH vector within the triclinic unit cell as determined from X-ray refinement (Rossi et al. 1974). There are three distinct bands in the (1)H NMR spectrum of ussingite: a predominant band at 13.5 ppm (TMS) representing 90% of the structural hydrogen, a second band at 15.9 ppm corresponding to 8% of the protons, and a third band at 11.0 ppm accounting for the remaining 2% of structural hydrogen. From the correlation between hydrogen bond length and (1)H NMR chemical shift (Sternberg and Brunner 1994), the predominant hydrogen bond length (H...O) was calculated to be 1.49 Angstrom, in comparison to the hydrogen bond length determined from X-ray refinement (1.54 Angstrom). The population of protons at 15.9 ppm is consistent with 5-8% Al-Si disorder. Although the ussingite crystal structure and composition are similar to those of low albite, the bonding environment of OH in low albite and other feldspars, as characterized through IR and (1)H NMR, is fundamentally different from the strong hydrogen bonding found in ussingite. C1 CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Johnson, EA (reprint author), Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, MRC 0119, Washington, DC 20119 USA. EM johnson.elizabeth@nmnh.si.edu OI Rossman, George/0000-0002-4571-6884 NR 28 TC 6 Z9 7 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0342-1791 J9 PHYS CHEM MINER JI Phys. Chem. Miner. PD MAR PY 2004 VL 31 IS 2 BP 115 EP 121 DI 10.1007/s00269-003-0368-5 PG 7 WC Materials Science, Multidisciplinary; Mineralogy SC Materials Science; Mineralogy GA 803RW UT WOS:000220249200006 ER PT J AU Bakos, G Noyes, RW Kovacs, G Stanek, KZ Sasselov, DD Domsa, I AF Bakos, G Noyes, RW Kovacs, G Stanek, KZ Sasselov, DD Domsa, I TI Wide-field millimagnitude photometry with the HAT: A tool for extrasolar planet detection SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID SEARCH; STAR; TELESCOPE; TRANSITS; SKY; ATMOSPHERE; ALGORITHM; ERRORS; DISK AB We discuss the system requirements for obtaining millimagnitude photometric precision over a wide field using small-aperture, short focal length telescope systems such as those being developed by a number of research groups to search for transiting extrasolar planets. We describe a Hungarian Automated Telescope ( HAT) system, which attempts to meet these requirements. The attainable precision of HAT has been significantly improved by a technique in which the telescope is made to execute small pointing steps during each exposure so as to broaden the effective point-spread function (PSF) of the system to a value more compatible with the pixel size of our CCD detector. Experiments during a preliminary survey ( spring 2003) of two star fields with the HAT-5 instrument allowed us to optimize the HAT photometric precision using this method of PSF broadening; in this way we have been able to achieve a precision as good as 2 mmag on brighter stars. We briefly describe development of a network of longitudinally spaced HAT telescopes (HATNet). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Konkoly Observ Budapest, H-1525 Budapest, Hungary. RP Bakos, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu; rnoyes@cfa.harvard.edu; kovacs@konkoly.hu; kstanek@cfa.harvard.edu; dsasselov@cfa.harvard.edu; domsa@konkoly.hu NR 28 TC 262 Z9 264 U1 2 U2 3 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 MAR PY 2004 VL 116 IS 817 BP 266 EP 277 DI 10.1086/382735 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 802ZF UT WOS:000220200700002 ER PT J AU Groce, N AF Groce, N TI Local culture in the global city - The folklife of New York SO VOICES-THE JOURNAL OF NEW YORK FOLKLORE LA English DT Article C1 Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. RP Groce, N (reprint author), Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA. EM grocen@folklife.si.edu RI Chesters, Heather/C-6089-2009 NR 1 TC 0 Z9 0 U1 0 U2 2 PU NEW YORK FOLKLORE SOC PI SCHENECTADY PA 133 JAY ST, PO BOX 764, SCHENECTADY, NY 12301 USA SN 0361-204X J9 VOICES JI Voices-J N. Y. Folk. PD SPR-SUM PY 2004 VL 30 IS 1-2 BP 8 EP 12 PG 5 WC Folklore SC Arts & Humanities - Other Topics GA 832IN UT WOS:000222261000004 ER PT J AU Jehl, JR Johnson, E AF Jehl, JR Johnson, E TI Wing and tail molts of the Ruddy Duck SO WATERBIRDS LA English DT Article DE Ruddy Duck; Oxyura jamaicensis; wing molt; tail molt AB Stiff-tailed ducks (Oxyurini) are reputed to be unique among waterfowl in having two complete wing and tail molts annually. We examined molt patterns in wild Ruddy Ducks (Oxyura jamaicensis) and in captives of known age. Adults of both groups underwent a complete wing molt in early autumn. A spring wing molt was very rare in wild Ruddy Ducks, but occurred more often in captives, especially in adult females. Ruddy Ducks replace rectrices twice annually. These molts are complete but unusual in that feathers are typically replaced in two waves, in which (1) every other rectrix is lost and largely re-grown before (2) the intervening feathers are molted. As a result, the molt is protracted and the tail plumage, at times, includes feathers of two generations. The pattern ensures that a functional tail is maintained at all times. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. Univ San Diego, Dept Biol & Marine Studies, San Diego, CA 92110 USA. RP Jehl, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. EM Grebe5K@cs.com NR 14 TC 2 Z9 3 U1 1 U2 5 PU WATERBIRD SOC PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 1524-4695 J9 WATERBIRDS JI Waterbirds PD MAR PY 2004 VL 27 IS 1 BP 54 EP 59 DI 10.1675/1524-4695(2004)027[0054:WATMOT]2.0.CO;2 PG 6 WC Ornithology SC Zoology GA 803NU UT WOS:000220238600009 ER PT J AU Milne, GA Mitrovica, JX Scherneck, HG Davis, JL Johansson, JM Koivula, H Vermeer, M AF Milne, GA Mitrovica, JX Scherneck, HG Davis, JL Johansson, JM Koivula, H Vermeer, M TI Continuous GPS measurements of postglacial adjustment in Fennoscandia: 2. Modeling results SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE glacial isostasy; space geodesy; mantle viscosity ID GLACIAL-ISOSTATIC-ADJUSTMENT; SEA-LEVEL CHANGE; COMPUTING 3-DIMENSIONAL DEFORMATIONS; MANTLE VISCOSITY; EARTHS ROTATION; PLEISTOCENE DEGLACIATION; GEODETIC CONSTRAINTS; SPECTRAL FORMALISM; SURFACE LOADS; RHEOLOGY AB [1] Data collected under the auspices of the BIFROST GPS project yield a geographically dense suite of estimates of present-day, three-dimensional (3-D) crustal deformation rates in Fennoscandia [Johansson et al., 2002]. A preliminary forward analysis of these estimates [Milne et al., 2001] has indicated that models of ongoing glacial isostatic adjustment (GIA) in response to the final deglaciation event of the current ice age are able to provide an excellent fit to the observed 3-D velocity field. In this study we revisit our previous GIA analysis by considering a more extensive suite of forward calculations and by performing the first formal joint inversion of the BIFROST rate estimates. To establish insight into the physics of the GIA response in the region, we begin by decomposing a forward prediction into the three contributions associated with the ice, ocean, and rotational forcings. From this analysis we demonstrate that recent advances in postglacial sea level theory, in particular the inclusion of rotational effects and improvements in the treatment of the ocean load in the vicinity of an evolving continental margin, involve peak signals that are larger than the observational uncertainties in the BIFROST network. The forward analysis is completed by presenting predictions for a pair of Fennoscandian ice histories and an extensive suite of viscoelastic Earth models. The former indicates that the BIFROST data set provides a powerful discriminant of such histories. The latter yields bounds on the ( assumed constant) upper and lower mantle viscosity (nu(UM), nu(LM)); specifically, we derive a 95% confidence interval of 5 x 10(20) less than or equal to nu(UM) less than or equal to 10(21) Pa s and 5 x 10(21) less than or equal to nu(LM) less than or equal to 5 x 10(22) Pa s, with some preference for (elastic) lithospheric thickness in excess of 100 km. The main goal of the ( Bayesian) inverse analysis is to estimate the radial resolving power of the BIFROST GPS data as a function of depth in the mantle. Assuming a reasonably accurate ice history, we demonstrate that this resolving power varies from similar to 200 km near the base of the upper mantle to similar to 700 km in the top portion of the lower mantle. We conclude that the BIFROST data are able to resolve structure on radial length scale significantly smaller than a single upper mantle layer. However, these data provide little constraint on viscosity in the bottom half of the mantle. Finally, elements of both the forward and inverse analyses indicate that radial and horizontal velocity estimates provide distinct constraints on mantle viscosity. C1 Univ Durham, Dept Earth Sci, Sci Labs, Durham DH1 3LE, England. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Finnish Geodet Inst, FIN-02431 Masala, Finland. Helsinki Univ Technol, Inst Geodesy, FIN-02015 Espoo, Finland. RP Milne, GA (reprint author), Univ Durham, Dept Earth Sci, Sci Labs, Durham DH1 3LE, England. EM g.a.milne@durham.ac.uk; jxm@physics.utoronto.ca; hgs@oso.chalmers.se; jdavis@cfa.harvard.edu; hannu.koivula@fgi.fi; martin.vermeer@hut.fi RI Davis, James/D-8766-2013; Vermeer, Martin/G-2468-2013 OI Davis, James/0000-0003-3057-477X; Vermeer, Martin/0000-0003-3107-6342 NR 47 TC 63 Z9 63 U1 1 U2 4 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 FEB 28 PY 2004 VL 109 IS B2 AR B02412 DI 10.1029/2003JB002619 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 803GB UT WOS:000220218500003 ER PT J AU Fukami, H Budd, AF Paulay, G Sole-Cava, A Chen, CLA Iwao, K Knowlton, N AF Fukami, H Budd, AF Paulay, G Sole-Cava, A Chen, CLA Iwao, K Knowlton, N TI Conventional taxonomy obscures deep divergence between Pacific and Atlantic corals SO NATURE LA English DT Article ID EVOLUTIONARY RELATIONSHIPS; SCLERACTINIAN CORALS; NUCLEOTIDE-SEQUENCES; MITOCHONDRIAL-DNA; SUBSTITUTIONS; REGION; REEFS AB Only 17% of 111 reef-building coral genera and none of the 18 coral families with reef-builders are considered endemic to the Atlantic, whereas the corresponding percentages for the Indowest Pacific are 76% and 39%(1,2). These figures depend on the assumption that genera and families spanning the two provinces belong to the same lineages ( that is, they are monophyletic). Here we show that this assumption is incorrect on the basis of analyses of mitochondrial and nuclear genes. Pervasive morphological convergence at the family level has obscured the evolutionary distinctiveness of Atlantic corals. Some Atlantic genera conventionally assigned to different families are more closely related to each other than they are to their respective Pacific 'congeners'. Nine of the 27 genera of reef-building Atlantic corals belong to this previously unrecognized lineage, which probably diverged over 34 million years ago. Although Pacific reefs have larger numbers of more narrowly distributed species, and therefore rank higher in biodiversity hotspot analyses(3), the deep evolutionary distinctiveness of many Atlantic corals should also be considered when setting conservation priorities. C1 Smithsonian Trop Res Inst, Naos Marine Lab, Balboa, Panama. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. Univ Fed Rio de Janeiro, Dept Genet, Rio De Janeiro, Brazil. Acad Sinica, Inst Zool, Taipei 115, Taiwan. Akajima Marine Sci Lab, Okinawa 9013311, Japan. RP Knowlton, N (reprint author), Smithsonian Trop Res Inst, Naos Marine Lab, Box 2072, Balboa, Panama. EM nknowlton@ucsd.edu RI Sole-Cava, Antonio /G-4209-2011 OI Sole-Cava, Antonio /0000-0003-0363-5821 NR 24 TC 161 Z9 176 U1 3 U2 41 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 26 PY 2004 VL 427 IS 6977 BP 832 EP 835 DI 10.1038/nature02339 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 777WU UT WOS:000189207500038 PM 14985760 ER PT J AU Bhattacharya, A AF Bhattacharya, A TI Novel mechanism of distance-oriented bee movement, secondary pollen dispersal and reticulate pollination - a case study in Melipona panamica SO CURRENT SCIENCE LA English DT Article ID OILSEED RAPE; HYMENOPTERA; PLANT AB The efficiency of secondary pollen dispersal, effect of distance isolation, and possible consequence of reticulate pollination were assessed specifically by movements of stingless bees (Melipona panamica) in lowland Neotropical forest vegetation in Panama, because this insect is one of the predominant pollen vectors there. The trial consisted of two identical strips (9 m X 45 m) along the forest ground-level discrete vegetation having herbaceous diversity. The design was a 'V', truncated in such a way that the zone, without any vegetation, between the two strips varied from 4.5 to 18 m in width. A nest of M. panamica colony was placed at 12 m from the top of the 'V'. Three equal sectors (135 m(2)) were identified in each strip. The bees were marked with different colours according to each sector of one strip, named the donor strip. Almost all bees were marked until their number was nearly balanced between the three sectors. Then, marked and unmarked bees were counted on the donor and recipient strips. Results showed that the foraging area in a given strip is about 405 m(2) and that a mean proportion of 3.45% of marked bees/total number of bees in colony was recovered in the recipient strip. It was found that a barren zone from 4.5 to 18 m in width was not sufficient to completely discourage bees from crossing between two identical resources, but that it significantly reduced cross-pollination. The bees dispersed pollens by bee-bee interactions within the nest, showing high diversity of pollens from outgoing bees, rather than incoming ones. The pollen viability study along the body of exiting bees showed that the pollens remained viable (48-51 %) within the bee nest, indicating a possibility of out-crossing by exiting bees at the time of their forage patch and trip change. C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Bhattacharya, A (reprint author), Natl Bot Res Inst, Palynol Lab, Lucknow 226001, Uttar Pradesh, India. EM bhattacharyaa@hotmail.com NR 18 TC 1 Z9 1 U1 0 U2 3 PU INDIAN ACAD SCIENCES PI BANGALORE PA C V RAMAN AVENUE, SADASHIVANAGAR, P B #8005, BANGALORE 560 080, INDIA SN 0011-3891 J9 CURR SCI INDIA JI Curr. Sci. PD FEB 25 PY 2004 VL 86 IS 4 BP 576 EP 580 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 823HA UT WOS:000221599600026 ER PT J AU Parker, GG Russ, ME AF Parker, GG Russ, ME TI The canopy surface and stand development: assessing forest canopy structure and complexity with near-surface altimetry SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE complexity; forest structure; fractal dimension; laser altimetry; leaf area density; leaf area index; outer canopy; rugosity AB A first-return laser rangefinder deployed from a low-flying helicopter provided inexpensive, repeatable, and high-resolution measurements of the shape of the outer forest canopy in stands of four successional stages on the Maryland coastal plain. The traces of canopy height in these stands revealed structural characteristics such as cover, maximum and mean heights which were consistent with corresponding ground measurements. Differences in the statistics on canopy structure corresponded to general developmental trends in these stands, including the development of maximum height and surface rugosity. Furthermore, some of the outer canopy statistics related to measures of internal organization, such as the shape of the foliage height profile and the leaf area index. These observations suggest that such measurements could be used readily to classify stand structure and developmental stage, and to deduce some aspects of internal organization of vegetation. Published by Elsevier B.V. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. Univ Maryland, Coll Life Sci, College Pk, MD 20742 USA. RP Parker, GG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM parkerg@si.edu OI Parker, Geoffrey/0000-0001-7055-6491 NR 21 TC 55 Z9 55 U1 1 U2 17 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 FEB 23 PY 2004 VL 189 IS 1-3 BP 307 EP 315 DI 10.1016/j.foreco.2003.09.001 PG 9 WC Forestry SC Forestry GA 774GG UT WOS:000188971000023 ER PT J AU Nagamine, K Springel, V Hernquist, L AF Nagamine, K Springel, V Hernquist, L TI Abundance of damped Lyman alpha absorbers in cosmological smoothed particle hydrodynamics simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : evolution; galaxies : formation; cosmology : theory ID COLD DARK-MATTER; HIGH-REDSHIFT GALAXIES; ULTRAVIOLET LUMINOSITY DENSITY; COSMIC STAR-FORMATION; LOW-MASS GALAXIES; LY-ALPHA; BREAK GALAXIES; INTERGALACTIC MEDIUM; METAL ENRICHMENT; UNIVERSE AB We use cosmological smoothed particle hydrodynamics (SPH) simulations of the Lambda cold dark matter (CDM) model to study the abundance of damped Lyman alpha absorbers (DLAs) in the redshift range z= 0-4.5. We compute the cumulative DLA abundance by using the relation between the DLA cross-section and the total halo mass inferred from the simulations. Our approach includes standard radiative cooling and heating with a uniform ultraviolet background, star formation, supernova feedback and a phenomenological model for feedback by galactic winds. The latter allows us to examine, in particular, the effect of galactic outflows on the abundance of DLAs. We employ the 'conservative entropy' formulation of SPH developed by Springel & Hernquist, which mitigates against the systematic overcooling that affected earlier simulations. In addition, we utilize a series of simulations of varying box-size and particle number to isolate the impact of numerical resolution on our results. We show that the DLA abundance was overestimated in previous studies for three reasons: (i) the overcooling of gas occurring with non-conservative formulations of SPH, (ii) a lack of numerical resolution and (iii) an inadequate treatment of feedback. Our new results for the total neutral hydrogen mass density, DLA abundance and column density distribution function all agree reasonably well with observational estimates at redshift z= 3, indicating that DLAs arise naturally from radiatively cooled gas in dark matter haloes that form in a LambdaCDM universe. Our simulations suggest a moderate decrease in DLA abundance by roughly a factor of 2 from z= 4.5 to 3, consistent with observations. A significant decline in abundance from z= 3 to 1, followed by weak evolution from z= 1 to 0, is also indicated, but our low-redshift results need to be interpreted with caution because they are based on coarser simulations than those employed at high redshift. Our highest resolution simulation also suggests that the halo mass-scale below which DLAs do not exist is slightly above 10(8)h(-1) M-. at z= 3-4, somewhat lower than previously estimated. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Nagamine, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM knagamin@cfa.harvard.edu; volker@mpa-garching.mpg.de; lars@cfa.harvard.edu NR 67 TC 79 Z9 79 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 FEB 21 PY 2004 VL 348 IS 2 BP 421 EP 434 DI 10.1111/j.1365-2966.2004.07393.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 775CY UT WOS:000189024200008 ER PT J AU Nagamine, K Springel, V Hernquist, L AF Nagamine, K Springel, V Hernquist, L TI Star formation rate and metallicity of damped Lyman alpha absorbers in cosmological smoothed particle hydrodynamics simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : numerical; galaxies : evolution; galaxies : formation; cosmology : theory ID HIGH-REDSHIFT GALAXIES; ULTRAVIOLET LUMINOSITY DENSITY; CHEMICAL ENRICHMENT HISTORY; II-ASTERISK ABSORPTION; DARK-MATTER UNIVERSE; SURFACE MASS DENSITY; LY-ALPHA; BREAK GALAXIES; SUPERNOVA EXPLOSIONS; FORMATION MODELS AB We study the distribution of the star formation rate (SFR) and metallicity of damped Lyman alpha absorbers (DLAs) in the redshift range z= 0-4.5 using cosmological smoothed particle hydrodynamics (SPH) simulations of the Lambda cold dark matter model. Our simulations include standard radiative cooling and heating with a uniform ultraviolet background, star formation, supernova (SN) feedback, as well as a phenomenological model for feedback by galactic winds. The latter allows us to examine, in particular, the effect of galactic outflows on the distribution of the SFR and metallicity of DLAs. We employ a 'conservative entropy' formulation of SPH which alleviates numerical overcooling effects that affected earlier simulations. In addition, we utilize a series of simulations of varying box-size and particle number to investigate the impact of numerical resolution on our results. We find that there is a positive correlation between the projected stellar mass density and the neutral hydrogen column density (N(H I)) of DLAs for high N(H I) systems, and that there is a good correspondence in the spatial distribution of stars and DLAs in the simulations. The evolution of typical star-to-gas mass ratios in DLAs can be characterized by an increase from approximately 2 at z= 4.5 to 3 at z= 3, to 10 at z= 1 and finally to 20 at z= 0. We also find that the projected SFR density in DLAs follows the Kennicutt law well at all redshifts, and the simulated values are consistent with the recent observational estimates of this quantity by Wolfe, Prochaska & Gawiser. The rate of evolution in the mean metallicity of simulated DLAs as a function of redshift is mild, and is consistent with the rate estimated from observations. The predicted metallicity of DLAs is generally subsolar in our simulations, and there is a significant scatter in the distribution of DLA metallicity for a given N(H I). However, we find that the median metallicity of simulated DLAs is close to that of Lyman-break galaxies, and is higher than the values typically observed for DLAs by nearly an order of magnitude. This discrepancy with observations could be due to an inadequate treatment of the SN feedback or the multiphase structure of the gas in our current simulations. Alternatively, the current observations might be missing the majority of the high metallicity DLAs due to selection effects. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. RP Nagamine, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM knagamin@cfa.harvard.edu; volker@mpa-garching.mpg.de; lars@cfa.harvard.edu NR 79 TC 75 Z9 75 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 FEB 21 PY 2004 VL 348 IS 2 BP 435 EP 450 DI 10.1111/j.1365-2966.2004.07180.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 775CY UT WOS:000189024200009 ER PT J AU Kaaret, P Alonso-Herrero, A Gallagher, JS Fabbiano, G Zezas, A Rieke, MJ AF Kaaret, P Alonso-Herrero, A Gallagher, JS Fabbiano, G Zezas, A Rieke, MJ TI Displacement of X-ray sources from star clusters in starburst galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : M82; galaxies : individual : NGC 1569; galaxies : individual : NGC 5253; galaxies : starburst; galaxies : stellar content; X-rays : galaxies ID GLOBULAR-CLUSTERS; BLACK-HOLES; CHANDRA OBSERVATIONS; EXTERNAL GALAXIES; FOSSIL STARBURST; POINT SOURCES; NGC 5253; M82; BINARIES; SPECTROSCOPY AB We examine the spatial offsets between X-ray point sources and star clusters in three starburst galaxies. We find that the X-ray sources are preferentially located near the star clusters. Because the star clusters are very good tracers of the star formation activity in the galaxies, this indicates that the X-ray sources are young objects associated with current star formation. We find significant displacements of the X-ray sources from the clusters. These displacements are likely due to motion of the X-ray sources and indicates that they are X-ray binaries. We find that brighter X-ray sources preferentially occur closer to clusters. The absence of very bright sources at large displacements from clusters may help constrain models of the sources. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Consejo Super Invest Cient, IEM, Dept Astrofis Mol & Infrarroja, Madrid 28006, Spain. Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pkaaret@cfa.harvard.edu RI Alonso-Herrero, Almudena/H-1426-2015; Zezas, Andreas/C-7543-2011 OI Alonso-Herrero, Almudena/0000-0001-6794-2519; Zezas, Andreas/0000-0001-8952-676X NR 43 TC 52 Z9 52 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 FEB 21 PY 2004 VL 348 IS 2 BP L28 EP + DI 10.1111/j.1365-2966.2004.07516.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 775CY UT WOS:000189024200004 ER PT J AU Barris, BJ Tonry, JL Blondin, S Challis, P Chornock, R Clocchiatti, A Filippenko, AV Garnavich, P Holland, ST Jha, S Kirshner, RP Krisciunas, K Leibundgut, B Li, WD Matheson, T Miknaitis, G Riess, AG Schmidt, BP Smith, RC Sollerman, J Spyromilio, J Stubbs, CW Suntzeff, NB Aussel, H Chambers, KC Connelley, MS Donovan, D Henry, JP Kaiser, N Liu, MC Martin, EL Wainscoat, RJ AF Barris, BJ Tonry, JL Blondin, S Challis, P Chornock, R Clocchiatti, A Filippenko, AV Garnavich, P Holland, ST Jha, S Kirshner, RP Krisciunas, K Leibundgut, B Li, WD Matheson, T Miknaitis, G Riess, AG Schmidt, BP Smith, RC Sollerman, J Spyromilio, J Stubbs, CW Suntzeff, NB Aussel, H Chambers, KC Connelley, MS Donovan, D Henry, JP Kaiser, N Liu, MC Martin, EL Wainscoat, RJ TI Twenty-three high-redshift supernovae from the Institute for Astronomy Deep Survey: Doubling the supernova sample at z > 0.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; distance scale; galaxies : distances and redshifts; supernovae : general ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; FARTHEST KNOWN SUPERNOVA; BVRI LIGHT CURVES; IA SUPERNOVAE; LOCKMAN-HOLE; ACCELERATING UNIVERSE; COSMOLOGICAL CONSTANT; INTERGALACTIC MEDIUM AB We present photometric and spectroscopic observations of 23 high-redshift supernovae (SNe) spanning a range of z = 0.34-1.03, nine of which are unambiguously classified as Type Ia. These SNe were discovered during the IfA Deep Survey, which began in 2001 September and observed a total of 2.5 deg(2) to a depth of approximately m approximate to 25-26 in RIZ over 9-17 visits, typically every 1-3 weeks for nearly 5 months, with additional observations continuing until 2002 April. We give a brief description of the survey motivations, observational strategy, and reduction process. This sample of 23 high-redshift SNe includes 15 at z greater than or equal to 0.7, doubling the published number of objects at these redshifts, and indicates that the evidence for acceleration of the universe is not due to a systematic effect proportional to redshift. In combination with the recent compilation of Tonry et al. (2003), we calculate cosmological parameter density contours that are consistent with the flat universe indicated by the cosmic microwave background (Spergel et al. 2003). Adopting the constraint that Omega(total) = 1.0, we obtain best-fit values of (Omega(m), Omega(Lambda)) = (0.33, 0.67) using 22 SNe from this survey augmented by the literature compilation. We show that using the empty-beam model for gravitational lensing does not eliminate the need for Omega(Lambda) > 0. Experience from this survey indicates great potential for similar large-scale surveys while also revealing the limitations of performing surveys for z > 1 SNe from the ground. C1 Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. European So Observ, D-85748 Garching, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Cerro Tololo Interamer Observ, La Serena, Chile. Las Campanas Observ, La Serena, Chile. Univ Washington, Dept Astron, Seattle, WA 98195 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Australian Natl Univ, Res Sch Astron & Astrophys, Weston 2611, Australia. AlbaNova, Stockholm Observ, SE-10691 Stockholm, Sweden. RP Barris, BJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM barris@ifa.hawaii.edu; jt@ifa.hawaii.edu; sblondin@eso.org; pchallis@cfa.harvard.edu; rchornock@astro.berkeley.edu; aclocchi@astro.puc.cl; alex@astroberkeley.edu; pgarnavi@miranda.phys.nd.edu; sholland@milkyway.gsfc.nasa.gov; sjha@astro.berkeley.edu; kirshner@cfa.harvard.edu; kkrisciunas@noao.edu; bleibund@eso.org; weidong@astro.berkeley.edu; tmatheson@cfa.harvard.edu; gm@u.washington.edu; ariess@stsci.edu; brian@mso.anu.edu.au; csmith@ctio.noao.edu; jesper@astro.su.se; jspyromi@eso.org; stubbs@astro.washington.edu; nsuntzeff@noao.edu; aussel@ifa.hawaii.edu; chambers@ifa.hawaii.edu; msc@galileo.ifa.hawaii.edu; donovan@ifa.hawaii.edu; henry@ifa.hawaii.edu; kaiser@ifa.hawaii.edu; liu@ifa.hawaii.edu; ege@ifa.hawaii.edu; rjw@ifa.hawaii.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Sollerman, Jesper/0000-0003-1546-6615; Chambers, Kenneth /0000-0001-6965-7789; Schmidt, Brian/0000-0002-8538-9195 NR 96 TC 364 Z9 366 U1 0 U2 4 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 FEB 20 PY 2004 VL 602 IS 2 BP 571 EP 594 DI 10.1086/381122 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779ZK UT WOS:000189343700004 ER PT J AU Janiuk, A Czerny, B Siemiginowska, A Szczerba, R AF Janiuk, A Czerny, B Siemiginowska, A Szczerba, R TI On the turbulent alpha-disks and the intermittent activity in active galactic nuclei SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies : evolution; MHD ID SUPERMASSIVE BLACK-HOLES; X-RAY TRANSIENTS; ACCRETION DISKS; VERTICAL STRUCTURE; INSTABILITY MODEL; RADIO GALAXIES; THIN DISK; EVOLUTION; AGN; TRANSITION AB We consider effects of MHD turbulence on viscosity during the evolution of the thermal-viscous ionization instability in standard alpha-accretion disks. We consider the possibility that accretion onto a supermassive black hole proceeds through an outer standard accretion disk and an inner radiatively inefficient and advection-dominated flow. In this scenario we follow the time evolution of the accretion disk, in which the viscosity parameter alpha is constant throughout the whole instability cycle, as implied by the strength of MHD turbulence. We conclude that the hydrogen ionization instability is a promising mechanism to explain the intermittent activity in AGNs. C1 Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Janiuk, A (reprint author), Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. EM agnes@camk.edu.pl; bcz@camk.edu.pl; asiemiginowska@cfa.harvard.edu; szczerba@ncac.torun.pl RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 NR 56 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 FEB 20 PY 2004 VL 602 IS 2 BP 595 EP 602 DI 10.1086/381159 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779ZK UT WOS:000189343700005 ER PT J AU Luhman, KL AF Luhman, KL TI A census of the Chamaeleon I star-forming region SO ASTROPHYSICAL JOURNAL LA English DT Review DE infrared : stars; stars : evolution; stars : formation; stars : low-mass, brown dwarfs; stars : luminosity function, mass function; stars : pre-main-sequence ID T-TAURI STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; YOUNG STELLAR OBJECTS; ALL-SKY SURVEY; INFRARED PHOTOMETRIC VARIABILITY; DARK CLOUD COMPLEX; X-RAY OBSERVATIONS; H-ALPHA EMISSION; MOLECULAR CLOUD AB I present a new census of the members of the Chamaeleon I star-forming region. Optical spectroscopy has been obtained for 179 objects that have been previously identified as possible members of the cluster, that lack either accurate spectral types or clear evidence of membership, and that are optically visible (I less than or similar to18). I have used these spectroscopic data and all other available constraints to evaluate the spectral classifications and membership status of a total sample of 288 candidate members of Chamaeleon I that have appeared in published studies of the cluster. The latest census of Chamaeleon I now contains 158 members, eight of which are later than M6 and thus are likely to be brown dwarfs. I find that many of the objects identified as members of Chamaeleon I in recent surveys are actually field stars. Meanwhile, seven of nine candidates discovered by Carpenter and coworkers are confirmed as members, one of which is the coolest known member of Chamaeleon I at a spectral type of M8 (similar to0.03 M-circle dot). I have estimated extinctions, luminosities, and effective temperatures for the members and used these data to construct an H-R diagram for the cluster. Chamaeleon I has a median age of similar to2 Myr according to evolutionary models and hence is similar in age to IC 348 and is slightly older than Taurus (similar to1 Myr). The measurement of an initial mass function for Chamaeleon I from this census is not possible because of the disparate methods with which the known members were originally selected and must await an unbiased, magnitude-limited survey of the cluster. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kluhman@cfa.harvard.edu NR 114 TC 145 Z9 145 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 FEB 20 PY 2004 VL 602 IS 2 BP 816 EP 842 DI 10.1086/381146 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779ZK UT WOS:000189343700022 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, SJ Bromley, BC TI Detecting the dusty debris of terrestrial planet formation SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; solar system : formation; stars : formation ID T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; MAIN-SEQUENCE STARS; EARLY KUIPER-BELT; SOLAR NEBULA; GRAIN-GROWTH; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; HR 4796A AB We use a multiannulus accretion code to investigate debris disks in the terrestrial zone at 0.7 - 1.3 AU around a 1 M. star. Terrestrial planet formation produces a bright dusty ring of debris with a lifetime of greater than or similar to 10(6) yr. The early phases of terrestrial planet formation are observable with current facilities; the late stages require more advanced instruments with adaptive optics. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X NR 61 TC 88 Z9 88 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 FEB 20 PY 2004 VL 602 IS 2 BP L133 EP L136 DI 10.1086/382693 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779ZL UT WOS:000189343800016 ER PT J AU Winget, DE Sullivan, DJ Metcalfe, TS Kawaler, SD Montgomery, MH AF Winget, DE Sullivan, DJ Metcalfe, TS Kawaler, SD Montgomery, MH TI A strong test of electroweak theory using pulsating DB white dwarf stars as plasmon neutrino detectors SO ASTROPHYSICAL JOURNAL LA English DT Article DE neutrinos; stars : interiors; stars : oscillations; white dwarfs ID EVOLUTIONARY PERIOD CHANGES; HOT; ASTEROSEISMOLOGY AB We demonstrate that plasmon neutrinos are the dominant form of energy loss in model white dwarf stars down to T(eff) similar to 25,000 K, depending on the stellar mass. The lower end of this range overlaps the observed temperatures for the V777 Her star ( DBV) instability strip. The evolution of white dwarfs at these temperatures is driven predominantly by cooling, so this directly affects the stellar evolutionary timescale in proportion to the ratio of the neutrino energy loss to the photon energy loss. This evolutionary timescale is observable through the time rate of change of the pulsation periods. Although the unified electroweak theory of lepton interactions that is crucial for understanding neutrino production has been well tested in the high- energy regime, the approach presented here should result in an interesting low- energy test of the theory. We discuss observational strategies to achieve this goal. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6001, New Zealand. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Winget, DE (reprint author), Univ Texas, Dept Astron, RLM 15-308,C-1400, Austin, TX 78712 USA. RI Metcalfe, Travis/A-9388-2008; OI Metcalfe, Travis/0000-0003-4034-0416; Kawaler, Steven/0000-0002-6536-6367 NR 23 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 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2004 VL 602 IS 2 BP L109 EP L112 DI 10.1086/382591 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779ZL UT WOS:000189343800010 ER PT J AU Beuther, H Schilke, P AF Beuther, H Schilke, P TI Fragmentation in massive star formation SO SCIENCE LA English DT Article ID PROTOSTELLAR CANDIDATES; EMISSION; CONTINUUM; MASSES; CLOUD AB Studies of evolved massive stars indicate that they form in a clustered mode. During the earliest evolutionary stages, these regions are embedded within their natal cores. Here we present high-spatial-resolution interferometric dust continuum observations disentangling the cluster-like structure of a young massive star-forming region. The derived protocluster mass distribution is consistent with the stellar initial mass function. Thus, fragmentation of the initial massive cores may determine the initial mass function and the masses of the final stars. This implies that stars of all masses can form via accretion processes, and coalescence of intermediate-mass protostars appears not to be necessary. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-53121 Bonn, Germany. RP Beuther, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hbeuther@cfa.harvard.edu NR 16 TC 56 Z9 56 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 FEB 20 PY 2004 VL 303 IS 5661 BP 1167 EP 1169 DI 10.1126/science.1094014 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 775RP UT WOS:000189074700038 PM 14976307 ER PT J AU Volkov, I Banavar, JR Maritan, A Hubbell, SP AF Volkov, I Banavar, JR Maritan, A Hubbell, SP TI The stability of forest biodiversity SO NATURE LA English DT Editorial Material C1 Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. INFM, I-35131 Padua, Italy. Abdus Salam Int Ctr Theoret Phys, I-34014 Trieste, Italy. Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Volkov, I (reprint author), Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. EM banavar@psu.edu NR 6 TC 21 Z9 21 U1 0 U2 16 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 19 PY 2004 VL 427 IS 6976 BP 696 EP 696 DI 10.1038/427696a PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 775DT UT WOS:000189026000029 PM 14973471 ER PT J AU Watters, TR Robinson, MS Bina, CR Spudis, PD AF Watters, TR Robinson, MS Bina, CR Spudis, PD TI Thrust faults and the global contraction of Mercury SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID STAGNANT LID CONVECTION; TERRESTRIAL PLANETS; LOBATE SCARPS; TECTONICS; VOLCANISM; MANTLE; MOON AB [1] Lobate scarps on Mercury are the surface expression of thrust faults and are generally thought to be the result of global contraction. Our analysis indicates that these thrust faults are not uniformly distributed and exhibit non-random patterns on the imaged hemisphere. The greatest area normalized cumulative length of the faults occurs in the southern hemisphere, below 50degreesS. The thrust faults in this region dip to the north, indicating a broad zone where the crust has been displaced to the south. Widespread thrust faulting may not have initiated before the emplacement of Calorian smooth plains, well after the emplacement of pre-Tolstojan intercrater plains. Our observations suggest that regional-scale tectonic stresses on Mercury dominated over stresses resulting from global contraction. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. Northwestern Univ, Dept Geol Sci, Evanston, IL 60208 USA. Northwestern Univ, Ctr Planetary Sci, Evanston, IL 60208 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Watters, TR (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. EM twatters@nasm.si.edu NR 20 TC 24 Z9 25 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD FEB 18 PY 2004 VL 31 IS 4 AR L04701 DI 10.1029/2003GL019171 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 780GX UT WOS:000189372900004 ER PT J AU Schroll, S AF Schroll, S TI A sweeper-up after artists: A memoir. SO LIBRARY JOURNAL LA English DT Book Review C1 Smithsonian Inst Lib, Washington, DC USA. RP Schroll, 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 FEB 15 PY 2004 VL 129 IS 3 BP 123 EP 123 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 772TC UT WOS:000188856500055 ER PT J AU Soon, WWH Legates, DR Baliunas, SL AF Soon, WWH Legates, DR Baliunas, SL TI Estimation and representation of long-term (> 40 year) trends of Northern-Hemisphere-gridded surface temperature: A note of caution SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WAVELET ANALYSIS; CLIMATE AB Several quantitative estimates of surface instrumental temperature trends in the late 20th century are compared by using published results and our independent analyses. These estimates highlight a significant sensitivity to the method of analysis, the treatment of data, and the choice of data presentation (i.e., size of the smoothing filter window). Providing an accurate description of both quantitative uncertainties and sensitivity to the treatment of data is recommended as well as avoiding subjective data-padding procedures. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Delaware, Ctr Climat Res, Newark, DE USA. RP Soon, WWH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wsoon@cfa.harvard.edu; legates@udel.edu; sbaliunas@cfa.harvard.edu NR 16 TC 22 Z9 23 U1 4 U2 12 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 FEB 14 PY 2004 VL 31 IS 3 AR L03209 DI 10.1029/2003GL019141 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 775PX UT WOS:000189051500005 ER PT J AU Zdanska, PR Sadeghpour, HR Moiseyev, N AF Zdanska, PR Sadeghpour, HR Moiseyev, N TI Non-Hermitian diabatic formulation of antiproton collision: protonium formation SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID METASTABLE STATES; HELIUM; ATOMS; H-2; ELECTRON; CAPTURE AB We present a non-Hermitian coupled-channel resonant diabatic approach to Rydberg protonium formation in the ultraslow rearrangement collision p - H --> Pn + e(-), where the kinetic coupling between the electronic and the nuclear motions is strong. We calculate complex diabatic potential energy curves and associated coupling matrix elements that vary smoothly with pp distance. The [Pn-e](-) resonances split into two groups converging to the first and second hydrogen thresholds. C1 Technion Israel Inst Technol, Dept Chem, IL-32000 Haifa, Israel. Technion Israel Inst Technol, Minerva Ctr Non Linear Phys, IL-32000 Haifa, Israel. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Technion Israel Inst Technol, Dept Chem, IL-32000 Haifa, Israel. RI Kapralova, Petra/F-5605-2014 NR 29 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD FEB 14 PY 2004 VL 37 IS 3 BP L35 EP L41 AR PII S0953-4075(04)70330-2 DI 10.1088/0953-4075/37/3/L01 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 822WW UT WOS:000221572300001 ER PT J AU Sorensen, AS van der Wal, CH Childress, LI Lukin, MD AF Sorensen, AS van der Wal, CH Childress, LI Lukin, MD TI Capacitive coupling of atomic systems to mesoscopic conductors SO PHYSICAL REVIEW LETTERS LA English DT Article ID QUANTUM COMPUTATION; CAVITY; ENTANGLEMENT; STATES; IONS AB We describe a technique that enables a strong, coherent coupling between isolated neutral atoms and mesoscopic conductors. The coupling is achieved by exciting atoms trapped above the surface of a superconducting transmission line into Rydberg states with large electric dipole moments that induce voltage fluctuations in the transmission line. Using a mechanism analogous to cavity quantum electrodynamics, an atomic state can be transferred to a long-lived mode of the fluctuating voltage, atoms separated by millimeters can be entangled, or the quantum state of a solid-state device can be mapped onto atomic or photonic states. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Childress, Lilian/H-1359-2012; van der Wal, Caspar/D-9206-2013; Sorensen, Anders/L-1868-2013 OI Childress, Lilian/0000-0002-0507-6392; van der Wal, Caspar/0000-0002-9843-3220; Sorensen, Anders/0000-0003-1337-9163 NR 33 TC 114 Z9 115 U1 1 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 13 PY 2004 VL 92 IS 6 AR 063601 DI 10.1103/PhysRevLett.92.063601 PG 4 WC Physics, Multidisciplinary SC Physics GA 773WM UT WOS:000188947700019 PM 14995237 ER PT J AU Winn, JN Rusin, D Kochanek, CS AF Winn, JN Rusin, D Kochanek, CS TI The central image of a gravitationally lensed quasar SO NATURE LA English DT Article ID EARLY-TYPE GALAXIES; MASS MODELS; QUINTUPLE QUASAR; RADIO; CENTERS; CORE AB A galaxy can act as a gravitational lens, producing multiple images of a background object. Theory predicts that there should be an odd number of images produced by the lens(1,2), but hitherto almost all lensed objects have two or four images. The missing 'central' images, which should be faint and appear near the centre of the lensing galaxy, have long been sought as probes of galactic cores too distant to resolve with ordinary observations(3-7). There are five candidates for central images, but in one case the third image is not necessarily the central one(8-10), and in the others the putative central images might be foreground sources(11-15). Here we report a secure identification of a central image, based on radio observations of one of the candidates(14). Lens models using the central image reveal that the massive black hole at the centre of the lensing galaxy has a mass of <2x10(8) solar masses (M-&ODOT;), and the galaxy's surface density at the location of the central image is >20,000 M-circle dot pc(-2); which is in agreement with expections based on observations of galaxies that are much closer to the Earth. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jwinn@cfa.harvard.edu NR 29 TC 54 Z9 54 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 12 PY 2004 VL 427 IS 6975 BP 613 EP 615 DI 10.1038/nature02279 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 773AJ UT WOS:000188875300034 PM 14961114 ER PT J AU Hynes, RI Charles, PA van Zyl, L Barnes, A Steeghs, D O'Brien, K Casares, J AF Hynes, RI Charles, PA van Zyl, L Barnes, A Steeghs, D O'Brien, K Casares, J TI Spectroscopy of the optical counterpart to Ser X-1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries : close; stars : individual : MM Ser ID X-RAY BINARIES; OPTIMAL EXTRACTION; EMISSION; SPECTRA AB We present William Herschel Telescope (WHT) and Very Large Telescope (VLT) spectroscopy of MM Ser, the optical counterpart to Ser X-1. We deblend the red spectra of the two close stars identified by Wachter and show that the brighter of the two is responsible for the H and He I emission, hence confirming that this is the true counterpart of the X-ray source. We also identify several He II and N III lines in the blue spectrum. The isolated emission lines are all remarkably narrow, with FWHM 200-300 km s(-1). The Bowen blend has structure suggesting that the individual components are also narrow. These narrow lines could be from the disc if the binary inclination is quite low, or they could come from a more localized region such as the heated face of the companion star. Several interstellar lines are detected and indicate that the reddening is moderate, and consistent with the neutral hydrogen column density inferred in X-rays. C1 Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Univ Keele, Sch Chem & Phys, Astrophys Grp, Keele ST5 5BG, Staffs, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. European So Observ, Santiago, Chile. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Inst Astrofis Canarias, Tenerife 38200, Spain. RP Hynes, RI (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM rih@astro.as.utexas.edu RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 25 TC 12 Z9 12 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 FEB 11 PY 2004 VL 348 IS 1 BP 100 EP 104 DI 10.1111/j.1365-2966.2004.07347.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769JC UT WOS:000188646100013 ER PT J AU De Lucia, G Kauffmann, G Springel, V White, SDM Lanzoni, B Stoehr, F Tormen, G Yoshida, N AF De Lucia, G Kauffmann, G Springel, V White, SDM Lanzoni, B Stoehr, F Tormen, G Yoshida, N TI Substructures in cold dark matter haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : clusters : general; galaxies : evolution; galaxies : formation; cosmology : dark matter ID N-BODY SIMULATIONS; COSMOLOGICAL SIMULATIONS; GALACTIC SATELLITES; GALAXY FORMATION; LENS GALAXIES; EVOLUTION; CLUSTERS; FLUCTUATIONS; ABUNDANCE; CODE AB We analyse the properties of substructures within dark matter haloes (subhaloes) using a set of high-resolution numerical simulations of the formation of structure in a CDM universe. Our simulation set includes 11 high-resolution simulations of massive clusters as well as a region of mean density, allowing us to study the spatial and mass distribution of substructures down to a mass resolution limit of 10(9) h(-1) M-circle dot. We also investigate how the properties of substructures vary as a function of the mass of the 'parent' halo in which they are located. We find that the substructure mass function depends at most weakly on the mass of the parent halo and is well described by a power law. The radial number density profiles of substructures are steeper in low mass haloes than in high-mass haloes. More massive substructures tend to avoid the centres of haloes and are preferentially located in the external regions of their parent haloes. We also study the mass accretion and merging histories of substructures, which we find to be largely independent of environment. We find that a significant fraction of the substructures residing in clusters at the present day were accreted at redshifts z < 1. This implies that a significant fraction of present-day 'passive' cluster galaxies were still outside the cluster progenitor and were more active at z &SIM; 1. C1 Max Planck Inst Astrophys, D-85748 Garching, Germany. INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP De Lucia, G (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. EM gdelucia@mpa-garching.mpg.de RI Yoshida, Naoki/A-4305-2011 NR 43 TC 219 Z9 219 U1 0 U2 4 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 FEB 11 PY 2004 VL 348 IS 1 BP 333 EP 344 DI 10.1111/j.1365-2966.2004.07372.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769JC UT WOS:000188646100038 ER PT J AU Maness, HL Taylor, GB Zavala, RT Peck, AB Pollack, LK AF Maness, HL Taylor, GB Zavala, RT Peck, AB Pollack, LK TI Breaking all the rules: The compact symmetric object 0402+379 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (0402+379); radio continuum : galaxies; radio lines : galaxies ID RADIO-SOURCES; OBJECTS; GALAXY; VLBI; IDENTIFICATIONS; REDSHIFTS; SEARCH; RING AB We present results of multifrequency Very Long Baseline Array (VLBA) observations of the compact symmetric object (CSO) 0402+379. The parsec-scale morphology of 0402+379 allows us to confirm it as a CSO, while VLA data clearly show the presence of kiloparsec-scale structure. Thus, 0402+379 is only the second known CSO to possess large-scale structure. Another puzzling morphological characteristic found from our observations is the presence of two central, compact, flat-spectrum components, which we identify as possible active nuclei. We also present the discovery of neutral hydrogen absorption along the southern hot spot of 0402+379 with a central velocity similar to1000 km s(-1) greater than the systemic velocity. Multiepoch observations from the VLA archive, the Caltech-Jodrell Bank Survey, and the VLBA Calibrator Survey allow us to further analyze these anomalous features. Results of this analysis reveal significant motion in the northern hot spot, as well as appreciable variability in both of the core candidates. We consider the possibility that 0402+379 was formed during a recent merger. In this case, the two candidate cores could be interpreted as binary supermassive black holes that have not yet coalesced, whereas the large-scale radio emission could be attributed to interactions directly linked to the merger or to previous activity associated with one of the cores. C1 Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. Natl Radio Astron Observ, Socorro, NM 87801 USA. New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. Harvard Smithsonian Ctr Astrophys, SMA Project, Hilo, HI 96721 USA. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Grinnell Coll, Dept Phys, POB 805, Grinnell, IA 50112 USA. RI Zavala, Robert/D-7821-2011 OI Zavala, Robert/0000-0002-9402-2870 NR 27 TC 39 Z9 39 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 FEB 10 PY 2004 VL 602 IS 1 BP 123 EP 134 DI 10.1086/380919 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MT UT WOS:000189304900012 ER PT J AU Lazendic, JS Slane, PO Gaensler, BM Reynolds, SP Plucinsky, PP Hughes, JP AF Lazendic, JS Slane, PO Gaensler, BM Reynolds, SP Plucinsky, PP Hughes, JP TI A high-resolution study of nonthermal radio and X-ray emission from supernova remnant G347.3-0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; ISM : individual (G347.3-0.5) radiation; mechanisms : nonthermal; supernova remnants; X-rays : ISM ID CHARGE-TRANSFER INEFFICIENCY; SHOCK-ACCELERATED ELECTRONS; CCD IMAGING SPECTROMETER; HIGH-ENERGY ELECTRONS; SNR RX J1713.7-3946; COSMIC-RAYS; MAXIMUM ENERGIES; SHELL; SN-1006; RX-J1713.7-3946 AB G347.3-0.5 is one of three shell-type supernova remnants (SNRs) in the Galaxy whose X-ray spectrum is dominated by nonthermal emission. This puts G347.3-0.5 in the small but growing class of SNRs for which the X-ray emission reveals directly the presence of extremely energetic electrons accelerated by the SNR shock. We have obtained new high-resolution X-ray and radio data on G347.3-0.5 using the Chandra X-Ray Observatory and the Australia Telescope Compact Array (ATCA), respectively. The bright northwestern peak of the SNR seen in ROSAT and ASCA images is resolved with Chandra into bright filaments and fainter diffuse emission. These features show good correspondence with the radio morphological structure, providing strong evidence that the same population of electrons is responsible for the synchrotron emission in both bands in this part of the remnant. Spectral index information from both observations is presented. We found significant difference in photon index value between bright and faint regions of the SNR shell. Spectral properties of these regions support the notion that efficient particle acceleration is occurring in the bright SNR filaments. We report the detection of linear radio polarization toward the SNR, which is most ordered at the northwestern shell where particle acceleration is presumably occurring. Using our new Chandra and ATCA data, we model the broadband emission from G347.3-0.5 with the synchrotron and inverse Compton mechanisms and discuss the conditions under which this is a plausible scenario. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Lazendic, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 53 TC 94 Z9 95 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 FEB 10 PY 2004 VL 602 IS 1 BP 271 EP 285 DI 10.1086/380956 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MT UT WOS:000189304900024 ER PT J AU Chen, Y Esser, R Strachan, L Hu, Y AF Chen, Y Esser, R Strachan, L Hu, Y TI Stagnated outflow of O+5 ions in the source region of the slow solar wind at solar minimum SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun : corona ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; ANISOTROPIC VELOCITY DISTRIBUTIONS; FLOW SPEEDS; MODEL; STREAMER; TEMPERATURE; O5+; ORIGINS; HOLES AB Using recent coordinated UVCS and LASCO measurements by Strachan and coworkers to constrain the heating parameters of a one-dimensional single-fluid minor ion model, we calculate the outflow velocity profile of O+5 ions in the flow tube overlying the helmet streamer, which has been supposed to be the source region of the slow solar wind at least during solar minimum. The background solar wind parameters and the flow tube geometry are taken from a recent two-dimensional magnetohydrodynamic solar wind model. We show that in this slow-wind source region the O+5 outflow speed varies nonmonotonically with increasing heliocentric distance. There is a local minimum of the outflow speed near the streamer cusp point (about 3 R-.), which is below the current observational sensitivity. This type of ion outflow in the slow solar wind is termed "stagnated outflow" in this paper. We also show that the observed effective temperature in the perpendicular direction (to the magnetic field) and the outflow speed of the O+5 ions can be used to put limits on their parallel thermal temperature. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Sci & Technol China, China Ctr Astrophys, Anhua 230026, Peoples R China. Univ Tromso, Astrophys Grp, NO-9037 Tromso, Norway. RP Chen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yachen@cfa.harvard.edu RI Chen, Yao/B-7255-2011 NR 29 TC 14 Z9 16 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 FEB 10 PY 2004 VL 602 IS 1 BP 415 EP 421 DI 10.1086/380960 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MT UT WOS:000189304900039 ER PT J AU Lin, J Raymond, JC Van Ballegooijen, AA AF Lin, J Raymond, JC Van Ballegooijen, AA TI The role of magnetic reconnection in the observable features of solar eruptions SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; plasmas; Sun : coronal mass ejections (CMEs); Sun : filaments; Sun : magnetic fields ID CORONAL MASS EJECTIONS; FLUX ROPE MODEL; MAGNETOHYDRODYNAMIC MODEL; DYNAMICAL EVOLUTION; ACTIVE-REGION; CURRENT SHEET; FLARE MYTH; 1 AU; FIELD; MECHANISMS AB There are two competing classes of models for coronal mass ejections (CMEs): those that assume a preexisting magnetic flux rope and those that can make a flux rope during the eruption by magnetic reconnection. The present work is based on the model with a preexisting flux rope. We investigate the evolution of morphological features of the magnetic configuration in a CME according to a catastrophe model of flux rope CMEs developed previously. For the parameters chosen for the present work, roughly half of the total mass and magnetic flux are contained in the initial flux rope, while the remaining plasma and poloidal magnetic flux are brought by magnetic reconnection from the corona into the current sheet and from there into the CME bubble. These features and the corresponding physical processes are identical to those described by the non-flux rope models. Thus, the flux rope and non-flux rope models are less distinct than is generally assumed. The reconnected magnetic flux can account for the rapid expansion of the ejecta, and the plasma flowing out of the current sheet fills the outer shell of the ejecta. We tentatively identify the outer shell, the expanded bubble, and the flux rope with the leading edge, void, and core of the three-component CME structure, respectively. Thus, the final mass, speed, and magnetic energy-the quantities that determine the geoeffectiveness of the CME-are determined not in the initial eruption but during the CME expansion, at heights of a few solar radii. The aspects of this explanation that need improvement are also discussed. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI LIN, JUN/B-9890-2017; OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 75 TC 97 Z9 103 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2004 VL 602 IS 1 BP 422 EP 435 DI 10.1086/380900 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MT UT WOS:000189304900040 ER PT J AU Korzennik, SG Rabello-Soares, MC Schou, J AF Korzennik, SG Rabello-Soares, MC Schou, J TI On the determination of Michelson Doppler Imager high-degree mode frequencies SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun : activity; Sun : helioseismology; Sun : oscillations ID SOLAR OSCILLATION FREQUENCIES; DIFFERENTIAL ROTATION; F-MODE; EIGENFUNCTIONS; PARAMETERS; VELOCITY; PROFILES; FLOWS; GONG AB The characteristics of the solar acoustic spectrum are such that mode lifetimes get shorter and spatial leaks get closer in frequency as the degree of a mode increases for a given order. A direct consequence of this property is that individual p-modes are resolved only at low and intermediate degrees and that at high degrees individual modes blend into ridges. Once modes have blended into ridges, the power distribution of the ridge defines the ridge central frequency, and it will mask the true underlying mode frequency. An accurate model of the amplitude of the peaks that contribute to the ridge power distribution is needed to recover the underlying mode frequency from fitting the ridge. We present the results of fitting high-degree power ridges (up to l = 900) computed from several 2-3 month long time series of full-disk observations taken with the Michelson Doppler Imager (MDI) on board the Solar and Heliospheric Observatory between 1996 and 1999. We also present a detailed discussion of the modeling of the ridge power distribution, and the contribution of the various observational and instrumental effects on the spatial leakage, in the context of the MDI instrument. We have constructed a physically motivated model (rather than some ad hoc correction scheme) that we believe results in a methodology that can produce an unbiased determination of high-degree modes once the instrumental characteristics are well understood. Finally, we present preliminary estimates of changes in high-degree mode parameters with epoch and thus solar activity level and discuss their significance. These estimates are preliminary because they rely on a simple-if not simplistic-ridge-to-mode correction scheme to account for errors in the plate scale used for the spherical harmonic decomposition. Such a correction scheme produced residual systematics that, as we show, are not always constant with time. These cannot be properly corrected without reprocessing the data back to the level of the spherical harmonic decomposition. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Stanford Univ, Hansen Expt Phys Lab, Stanford, CA 94305 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Rabello Soares, Maria Cristina/C-3207-2013; OI Rabello Soares, Maria Cristina/0000-0003-0172-3713 NR 32 TC 58 Z9 58 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 FEB 10 PY 2004 VL 602 IS 1 BP 481 EP 515 DI 10.1086/381021 PN 1 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MT UT WOS:000189304900044 ER PT J AU Monnier, JD Traub, WA Schloerb, FP Millan-Gabet, R Berger, JP Pedretti, E Carleton, NP Kraus, S Lacasse, MG Brewer, M Ragland, S Ahearn, A Coldwell, C Haguenauer, P Kern, P Labeye, P Lagny, L Malbet, F Malin, D Maymounkov, P Morel, S Papaliolios, C Perraut, K Pearlman, M Porro, IL Schanen, I Souccar, K Torres, G Wallace, G AF Monnier, JD Traub, WA Schloerb, FP Millan-Gabet, R Berger, JP Pedretti, E Carleton, NP Kraus, S Lacasse, MG Brewer, M Ragland, S Ahearn, A Coldwell, C Haguenauer, P Kern, P Labeye, P Lagny, L Malbet, F Malin, D Maymounkov, P Morel, S Papaliolios, C Perraut, K Pearlman, M Porro, IL Schanen, I Souccar, K Torres, G Wallace, G TI First results with the IOTA3 imaging interferometer: The spectroscopic binaries lambda Virginis and WR 140 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : spectroscopic; instrumentation : interferorneters; stars : individual (lambda Virginis, WR 140); techniques : interferometric ID OPTICAL APERTURE SYNTHESIS; INTEGRATED-OPTICS; BEAM-COMBINATION; STARS; ORBIT; VISIBILITIES; CAPELLA; IMAGES; WR-140; DUST AB We report the first spatially resolved observations of the spectroscopic binaries lambda Vir and WR 140, including the debut of aperture-synthesis imaging with the upgraded three-telescope IOTA interferometer. Using IONIC-3, a new integrated optics beam combiner capable of a precise closure phase measurement, short observations were sufficient to extract the angular separation and orientation of each binary system and the component brightness ratio. Most notably, the underlying binary in the prototypical colliding-wind source WR 140 (WC7 + O4/O5) was found to have a separation of similar to 13 mas with a position angle of 152degrees, consistent with previous interpretations of the 2001 dust shell ejection only if the Wolf-Rayet star is fainter than the 0 star at 1.65 mum. We also highlight lambda Vir, whose peculiar stellar properties of the Am star components will permit direct testing of current theories of tidal evolution when the full orbit is determined. C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. Lab Astrophys Grenoble, F-38400 St Martin Dheres, France. Alcatel Space Ind, Cannes, France. CEA, LETI, Grenoble, France. European So Observ, D-85748 Garching, Germany. MIT, Cambridge, MA 02139 USA. IMEP, INPG, Grenoble, France. RP Monnier, JD (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM monnier@umich.edu NR 32 TC 53 Z9 53 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 FEB 10 PY 2004 VL 602 IS 1 BP L57 EP L60 DI 10.1086/382213 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MU UT WOS:000189305000015 ER PT J AU Park, S Hughes, JP Slane, PO Burrows, DN Roming, PWA Nousek, JA Garmire, GP AF Park, S Hughes, JP Slane, PO Burrows, DN Roming, PWA Nousek, JA Garmire, GP TI Nucleosynthesis in the oxygen-rich supernova remnant G292.0+1.8 from Chandra X-ray spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : abundances; ISM : indivdiual (G292.0+1.8, MSH 11-54); supernova remnants; X-rays : ISM ID CCD IMAGING SPECTROMETER; CHARGE-TRANSFER INEFFICIENCY; PULSAR WIND NEBULA; ABUNDANCES; G292.0&1.8; PROGENITOR AB We continue our analysis of the Galactic oxygen-rich supernova remnant (SNR) G292.0+1.8, which was observed with the Chandra X-Ray Observatory. The high angular resolution Chandra data resolve metal-rich ejecta knots as well as the shocked circumstellar medium. X-ray emission from the ejecta material in G292.0+1.8 is dominated by highly ionized O, Ne, and Mg. Measured abundance ratios suggest that this material was produced during the hydrostatic evolution of the massive progenitor star. In contrast to Cassiopeia A, there is little evidence for X-ray-emitting ejecta from explosive nucleosynthesis, i.e., material enriched in Si, S, and particularly, Fe. This limits the amount of mixing or overturning of deep ejecta material in G292.0+1.8 and suggests that the ejecta are strongly stratified by composition and that the reverse shock has not propagated to the Si/S- or Fe-rich zones. On the other hand, the bright equatorial belt is dominated by X-ray emission with normal chemical composition, which supports shocked dense circumstellar material for its origin. We find that the thermal pressure in the SNR is much higher than the pressure in the pulsar wind nebula (PWN), indicating that the reverse shock has not yet begun to interact with the PWN. C1 Penn State Univ, Dept Astron & Astrophys, 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, 525 Davey Lab, University Pk, PA 16802 USA. EM park@astro.psu.edu NR 16 TC 37 Z9 38 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 FEB 10 PY 2004 VL 602 IS 1 BP L33 EP L36 DI 10.1086/382276 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MU UT WOS:000189305000009 ER PT J AU Patel, SK Kouveliotou, C Tennant, A Woods, PM King, A Finger, MH Ubertini, P Winkler, C Courvoisier, TJL van der Klis, M Wachter, S Gaensler, BM Phillips, CJ AF Patel, SK Kouveliotou, C Tennant, A Woods, PM King, A Finger, MH Ubertini, P Winkler, C Courvoisier, TJL van der Klis, M Wachter, S Gaensler, BM Phillips, CJ TI The peculiar X-ray transient IGR J16358-4726 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars : individual (IGR J16358-4726) ID BLACK-HOLE; J16318-4848; IMAGER AB The new transient IGR J16358-4726 was discovered on 2003 March 19 with INTEGRAL. We detected the source serendipitously during our 2003 March 24 observation of SGR 1627-41 with the Chandra X-Ray Observatory at the 1.7 x 10(-10) ergs s(-1) cm(-2) flux level (2-10 keV) with a very high absorption column (N-H = 3.3 x 10(23) cm(-2)) and a hard power-law spectrum of index 0.5(1). We discovered a very strong flux modulation with a period of 5880(50) s and peak-to-peak Pulse fraction of 70(6)% (2-10 keV), clearly visible in the X-ray data. The nature of IGR J16358-4726 remains unresolved. The only neutron star systems known with similar spin periods are low-luminosity persistent wind-fed pulsars; if this is a spin period, this transient is a new kind of object. If this is an orbital period, then the system could be a compact low-mass X-ray binary. C1 Univ Space Res Assoc, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol, Huntsville, AL 35805 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. ESA, European Space Res & Technol Ctr, NL-2201 AZ Noordwijk, Netherlands. ISDC, CH-1290 Versoix, Switzerland. Observ Geneva, CH-1290 Sauverny, Switzerland. Univ Amsterdam, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Australia Telescope Natl Facil, Epping, NSW 1710, Australia. EM sandeep.patel@nsste.nasa.gov RI Gaensler, Bryan/F-8655-2010 NR 19 TC 44 Z9 44 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 FEB 10 PY 2004 VL 602 IS 1 BP L45 EP L48 DI 10.1086/382210 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 779MU UT WOS:000189305000012 ER PT J AU Heyer, WR AF Heyer, WR TI Paulo Emilio Vanzolini SO COPEIA LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20013 USA. RP Heyer, WR (reprint author), SUNY Albany, Dept Biol Sci, Albany, NY 12222 USA. EM heyer.ron@nmnh.si.edu NR 0 TC 1 Z9 1 U1 0 U2 0 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 FEB 9 PY 2004 IS 1 BP 184 EP 189 PG 6 WC Zoology SC Zoology GA 774LX UT WOS:000188981900025 ER PT J AU Sanchez, JA Lasker, HR AF Sanchez, JA Lasker, HR TI Do multi-branched colonial organisms exceed normal growth after partial mortality? SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE gorgonian coral; Octocorallia; branching; growth; regeneration; overcompensation ID PSEUDOPTEROGORGIA-ELISABETHAE; CORAL; REGENERATION; POPULATION; TRANSPORT; OCTOCORAL AB One of the advantages of modular colonial growth is the capability to recover after partial mortality. Tolerance to partial mortality is a known property of some resistant species of plants that respond to mortality with vigorous regrowth or overcompensation. It is not clear whether modular marine invertebrates such as octocorals overcompensate. This study provides evidence that following injury to colonies (by breaking apical dominance), new growth exceeds normal rates of branching, as observed in some plants, in a degree correlated to the original multi-branched network setting (e.g. the number of original branches connected to main stem), in colonies of the Caribbean gorgonian octocoral Pseudopterogorgia bipinnata. This can be explained by the network of communicating vessels and canals inside octocoral colonies, which provide the structure for effective allocation of resources to regenerating parts. C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA. Smithsonian Inst, Lab Analyt Biol, Washington, DC 20013 USA. SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. RP Sanchez, JA (reprint author), Natl Inst Water & Atmospher Res, POB 14901, Wellington, New Zealand. EM j.sanchez@niwa.co.nz RI Johnson, Selena/K-3541-2013 NR 22 TC 16 Z9 16 U1 0 U2 8 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD FEB 7 PY 2004 VL 271 SU 3 BP S117 EP S120 DI 10.1098/rsbl.2003.0108 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 771LK UT WOS:000188786700036 PM 15101437 ER PT J AU Sharma, DK Maldonado, JE Jhala, YV Fleischer, RC AF Sharma, DK Maldonado, JE Jhala, YV Fleischer, RC TI Ancient wolf lineages in India SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Canis lupus; India; wolf; mitochondrial DNA; evolution ID MITOCHONDRIAL-DNA; BROWN BEARS; CANIS-LUPUS; DOGS; MULTIPLE; WOLVES; ORIGIN AB All previously obtained wolf (Canis lupus) and dog (Canis familiaris) mitochondrial (mt) DNA sequences fall within an intertwined and shallow clade (the 'wolf-dog' clade). We sequenced mtDNA of recent and historical samples from 45 wolves from throughout lowland peninsular India and 23 wolves from the Himalayas and Tibetan Plateau and compared these sequences with all available wolf and dog sequences. All 45 lowland Indian wolves have one of four closely related haplotypes that form a well-supported, divergent sister lineage to the wolf-dog clade. This unique lineage may have been independent for more than 400 000 years. Although seven Himalayan wolves from western and central Kashmir fall within the widespread wolf-dog clade, one from Ladakh in eastern Kashmir, nine from Himachal Pradesh, four from Nepal and two from Tibet form a very different basal clade. This lineage contains five related haplotypes that probably diverged from other canids more than 800 000 years ago, but we find no evidence of current barriers to admixture. Thus, the Indian subcontinent has three divergent, ancient and apparently parapatric mtDNA lineages within the morphologically delineated wolf. No haplotypes of either novel lineage are found within a sample of 37 Indian (or other) dogs. Thus, we find no evidence that these two taxa played a part in the domestication of canids. C1 Smithsonian Inst, Natl Museum Nat Hist, Systemat Biol Dept, Genet Program, Washington, DC 20008 USA. Univ Durham, Dept Biol Sci, Durham DH1 3LE, England. Wildlife Inst India, Dehra Dun 248001, Uttar Pradesh, India. RP Fleischer, RC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Biol Dept, Genet Program, 3001 Connecticut Ave,NW, Washington, DC 20008 USA. EM fleischer.robert@nmnh.si.edu NR 23 TC 34 Z9 35 U1 1 U2 14 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD FEB 7 PY 2004 VL 271 SU 3 BP S1 EP S4 DI 10.1098/rsbl.2003.0071 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 771LK UT WOS:000188786700001 PM 15101402 ER PT J AU Zayed, A Roubik, DW Packer, L AF Zayed, A Roubik, DW Packer, L TI Use of diploid male frequency data as an indicator of pollinator decline SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE pollinator decline; diploid males; Euglossini; Hymenoptera ID EFFECTIVE POPULATION-SIZE; ANT SOLENOPSIS-INVICTA; SEX DETERMINATION; BEES HYMENOPTERA; EUGLOSSINE BEES; METAPOPULATION; APIDAE; CONSERVATION; ACCUMULATION; EXTINCTION AB Pollination deficits in agricultural and natural systems are suggestive of large reductions in pollinator populations. However, actual declines are difficult to demonstrate using census data. Here, we show census data to be misleading because many abundant pollinators exhibit high levels of production of sterile diploid males usually found only in small inbred hymenopteran populations; Euglossa imperialis exhibits high levels of diploid male production induced by low effective population sizes (N(e)approximate to15), despite being the most abundant orchid bee in lowland tropical forests in Panama. We caution that although some pollinators appear abundant on the basis of census data, their long-term persistence may be highly tenuous based on genetic evidence. We propose the use of diploid male frequency data as a metric for assessing the sustainability of bee populations. C1 York Univ, Dept Biol, N York, ON M3J 1P3, Canada. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Zayed, A (reprint author), York Univ, Dept Biol, 4700 Keele St, N York, ON M3J 1P3, Canada. EM amro@torontodigital.com RI Zayed, Amro/G-6405-2011; OI Zayed, Amro/0000-0003-3233-4585; packer, laurence/0000-0002-1711-8203 NR 42 TC 49 Z9 51 U1 4 U2 14 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD FEB 7 PY 2004 VL 271 SU 3 BP S9 EP S12 DI 10.1098/rsbl.2003.0109 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 771LK UT WOS:000188786700003 PM 15101404 ER PT J AU Martin, ST Hung, HM Park, RJ Jacob, DJ Spurr, RJD Chance, KV Chin, M AF Martin, ST Hung, HM Park, RJ Jacob, DJ Spurr, RJD Chance, KV Chin, M TI Effects of the physical state of tropospheric ammonium-sulfate-nitrate particles on global aerosol direct radiative forcing SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Review ID GENERAL-CIRCULATION MODEL; COMMUNITY CLIMATE MODEL; EFFLORESCENCE RELATIVE HUMIDITIES; AQUEOUS-PHASE-TRANSITIONS; BLACK CARBON AEROSOLS; ANTHROPOGENIC SULFATE; ATMOSPHERIC AEROSOLS; CORUNDUM INCLUSIONS; INORGANIC AEROSOLS; OPTICAL-THICKNESS AB The effect of aqueous versus crystalline sulfate-nitrate-ammonium tropospheric particles on global aerosol direct radiative forcing is assessed. A global three-dimensional chemical transport model predicts sulfate, nitrate, and ammonium aerosol mass. An aerosol thermodynamics model is called twice, once for the upper side (US) and once for lower side (LS) of the hysteresis loop of particle phase. On the LS, the sulfate mass budget is 40% solid ammonium sulfate, 12% letovicite, 11% ammonium bisulfate, and 37% aqueous. The LS nitrate mass budget is 26% solid ammonium nitrate, 7% aqueous, and 67% gas-phase nitric acid release due to increased volatility upon crystallization. The LS ammonium budget is 45% solid ammonium sulfate, 10% letovicite, 6% ammonium bisulfate, 4% ammonium nitrate, 7% ammonia release due to increased volatility, and 28% aqueous. LS aerosol water mass partitions as 22% effloresced to the gas-phase and 78% remaining as aerosol mass. The predicted US/LS global fields of aerosol mass are employed in a Mie scattering model to generate global US/LS aerosol optical properties, including scattering efficiency, single scattering albedo, and asymmetry parameter. Global annual average LS optical depth and mass scattering efficiency are, respectively, 0.023 and 10.7 m(2) (g SO4-2)(-1), which compare to US values of 0.030 and 13.9 m(2) (g SO42-)(-1). Radiative transport is computed, first for a base case having no aerosol and then for the two global fields corresponding to the US and LS of the hysteresis loop. Regional, global, seasonal, and annual averages of top-of-the-atmosphere aerosol radiative forcing on the LS and US (F-L and F-U, respectively, in Wm(-2)) are calculated. Including both anthropogenic and natural emissions, we obtain global annual averages of F-L = - 0.750, F-U = - 0.930, and DeltaF(U,L) = 24% for full sky calculations without clouds and F-L = - 0.485, F-U = - 0.605, and DeltaF(U,L) = 25% when clouds are included. Regionally, DeltaF(U,L) = 48% over the USA, 55% over Europe, and 34% over East Asia. Seasonally, DeltaF(U,L) varies from 18% in DJF to 75% in SON over the USA. The global annual average contribution from anthropogenic aerosol is F-L = - 0.314 and F-U = - 0.404, which yield normalized direct radiative forcings (G) of G(L) = - 205 W (g SO42-)(-1) and G(U) = - 264W (g SO42-)(-1). C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Martin, ST (reprint author), Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA. EM scot_martin@harvard.edu RI Chin, Mian/J-8354-2012; Martin, Scot/G-1094-2015; Park, Rokjin/I-5055-2012; Hung, Hui-Ming/E-3851-2016; OI Martin, Scot/0000-0002-8996-7554; Park, Rokjin/0000-0001-8922-0234; Hung, Hui-Ming/0000-0002-6755-6359; Chance, Kelly/0000-0002-7339-7577 NR 105 TC 100 Z9 101 U1 5 U2 45 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 FEB 4 PY 2004 VL 4 BP 183 EP 214 PG 32 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 771GA UT WOS:000188776200001 ER PT J AU Hunt, DR AF Hunt, DR TI Obituary: Lucile E. St. Hoyme (1924-2001) SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Biographical-Item C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Div Phys Anthropol, Washington, DC 20013 USA. RP Hunt, DR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Div Phys Anthropol, MRC112,POB 37012, Washington, DC 20013 USA. EM hunt.david@nmnh.si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 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 FEB PY 2004 VL 123 IS 2 BP 103 EP 105 DI 10.1002/ajpa.10338 PG 3 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 768YB UT WOS:000188616200001 PM 14730644 ER PT J AU Corbett, Y Herrera, L Gonzalez, J Cubilla, L Capson, TL Coley, PD Kursar, TA Romero, LI Ortega-Barria, E AF Corbett, Y Herrera, L Gonzalez, J Cubilla, L Capson, TL Coley, PD Kursar, TA Romero, LI Ortega-Barria, E TI A novel DNA-based microfluorimetric method to evaluate antimalarial drug activity SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID LACTATE-DEHYDROGENASE ACTIVITY; PLASMODIUM-FALCIPARUM; MALARIA; ASSAY; SUSCEPTIBILITY; CULTURE AB This paper describes the development of a novel microfluorimetric assay to measure the inhibition of Plasmodium falciparum based on the detection of parasitic DNA by intercalation with PicoGreen(R). The method was used to determine parasite inhibition profiles and 50% inhibitory concentration values of known or potential antimalarial drugs. Values for parasite inhibition with known anti-malarial drugs using the PicoGreen(R) assay were comparable with those determined by the standard method based upon the uptake of (3)H-hypoxanthine and the Giemsa stain microscopic technique. The PicoGreen(R) assay is rapid, sensitive, reproducible, easily interpreted, and ideally suited for screening of large numbers of samples for anti-malarial drug development. C1 Inst Invest Cient Avanzadas & Serv Alta Tecnol, Panama City, Panama. Univ Panama, Lab Prod Nat, Panama City, Panama. Smithsonian Trop Res Inst, Ancon, Panama. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. RP Ortega-Barria, E (reprint author), Inst Invest Cient Avanzadas & Serv Alta Tecnol, Ciudad Saber,POB 7250,Zona 5,Clayton, Panama City, Panama. EM eortega@senacyt.gob.pa FU FIC NIH HHS [1R03 TW01076, 1U01 TW01021-01] NR 17 TC 97 Z9 100 U1 0 U2 5 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD FEB PY 2004 VL 70 IS 2 BP 119 EP 124 PG 6 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 773BZ UT WOS:000188879000004 PM 14993620 ER PT J AU De, S Heaney, PJ Fei, YW Vicenzi, EP AF De, S Heaney, PJ Fei, YW Vicenzi, EP TI Microstructural study of synthetic sintered diamond and comparison with carbonado, a natural polycrystalline diamond SO AMERICAN MINERALOGIST LA English DT Article ID HIGH-PRESSURE; SUPERHARD MATERIALS; DIRECT CONVERSION; STATIC PRESSURE; DEFORMATION; GRAPHITE; TEMPERATURE; CONSTRAINTS; MINERALOGY; PARTICLES AB Efforts to simulate the extreme toughness of the polycrystalline diamond variety known as carbonado typically entail the sintering of diamond powders in the presence of metal solvent-catalysts. In this study, we have attempted to duplicate the carbonado microstructure by sintering diamond powders without catalysts in a multi-anvil press at pressures of 6 to 9 GPa, temperatures of 1200 to 1800 degreesC, and times up to 6 h. The resultant microstructural defect assemblages for each experimental condition were characterized by transmission electron microscopy (TEM). Despite the absence of catalysts, sintered compacts were successfully produced for all runs, though intergranular porosity was significantly higher than that observed in natural carbonado. Primary grain sizes were reduced by more than 50% from their original dimensions in some experiments due to surface fracturing and abrasion, and aperiodic slip planes rigorously parallel to {111} consistently emerged in high densities, with lamellar spacings of 3 to 30 nm. In addition, sintering over all conditions produced polysynthetic spinel twinning in close association with the partial slip defects. Compacts compressed at 8 GPa produced some euhedral crystals with very low dislocation densities surrounded by grains in which dislocation densities were quite high. In addition, curviplanar defects loosely constrained to {111} were visible within some specimens sintered at the highest pressures. These textures resembled the polygonalization fabrics and defect microstructures observed in natural carbonado (De et al. 1998), and the appearance of these features suggests that our experiments at their most extreme pressure and temperature parameters reproduced carbonado-like defect assemblages. The formation of such textures in quasi-hydrostatic experiments suggests that shock metamorphism is not required to produce the periodic defect lamellae observed in carbonado. C1 NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP De, S (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. EM sde@alumni.princeton.edu RI Fei, Yingwei/F-3709-2011 OI Fei, Yingwei/0000-0001-9955-5353 NR 46 TC 9 Z9 9 U1 0 U2 5 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD FEB-MAR PY 2004 VL 89 IS 2-3 BP 438 EP 446 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 776HU UT WOS:000189111200025 ER PT J AU Ricklefs, RE Bermingham, E AF Ricklefs, RE Bermingham, E TI History and the species-area relationship in Lesser Antillean birds SO AMERICAN NATURALIST LA English DT Article DE colonization; equilibrium theory; extinction; island biogeography; Lesser Antilles; species-area relationship ID WEST-INDIES; SOLOMON ISLANDS; TAXON CYCLES; AVIFAUNA; COMMUNITIES; HABITAT; BIOGEOGRAPHY; DIVERSITY; PATTERNS; BARBADOS AB We examined the species-area relationship for three historically distinct subsets of Lesser Antillean birds identified by molecular phylogenetic analysis of island and continental populations. The groups comprised recent colonists from continental or Greater Antillean source populations, old taxa having recently expanded distributions within the Lesser Antilles, and old endemic taxa lacking evidence of recent dispersal between. islands. The number of young taxa was primarily related to distance from the source of colonists in South America. In a multiple regression, the logarithmic slope of the species-area relationship for this group was shallow (0.066 +/- 0.016). Old endemic taxa were restricted to islands with high elevation, and within this subset, species richness was related primarily to island area, with a steep slope (0.719 +/- 0.110). The number of recently spread endemic taxa was related primarily to island elevation, apparently reflecting the persistence, of such populations on islands with large areas of forested and montane habitats. Historical analysis of the Lesser Antillean avifauna supports the dynamic concept of island biogeography of MacArthur and Wilson, rather than the more static view of David Lack, in that colonists exhibit dispersal limitation and extinction plays a role in shaping patterns of diversity. However, the avifauna of the Lesser Antilles is probably not in equilibrium at present, and the overall species-area relationship might reflect changing proportions of historically distinguishable subsets of species. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Ricklefs, RE (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. EM ricklefs@umsl.edu; eb@naos.si.edu NR 46 TC 42 Z9 46 U1 3 U2 24 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 FEB PY 2004 VL 163 IS 2 BP 227 EP 239 DI 10.1086/381002 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 805PR UT WOS:000220378700005 PM 14970924 ER PT J AU Towe, KM AF Towe, KM TI The vinland map ink is NOT medieval SO ANALYTICAL CHEMISTRY LA English DT Letter C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Towe, KM (reprint author), 230 W Adams St, Tennille, GA 31089 USA. EM ken.towe@alumni.duke.edu NR 15 TC 10 Z9 10 U1 1 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 J9 ANAL CHEM JI Anal. Chem. PD FEB 1 PY 2004 VL 76 IS 3 BP 863 EP 865 DI 10.1021/ac0354488 PG 3 WC Chemistry, Analytical SC Chemistry GA 772CW UT WOS:000188823900054 PM 14750887 ER PT J AU Bonanos, AZ Stanek, KZ Szentgyorgyi, AH Sasselov, DD Bakos, GA AF Bonanos, AZ Stanek, KZ Szentgyorgyi, AH Sasselov, DD Bakos, GA TI The RR Lyrae distance to the Draco dwarf spheroidal galaxy SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; galaxies : dwarf; galaxies : individual (Draco); Local Group ID PHOTOMETRIC STANDARD STARS; IMAGE SUBTRACTION; LOCAL GROUP AB We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2 m telescope on 22 nights, over a period of 10 months, covering a 22' x 22' field centered at alpha = 17(h)19(m)57.(s)5, delta = 57degrees50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould & Popowski and 94 RRab stars from our field, we obtain a distance modulus of (m - M)(0) = 19.40 +/- 0.02 (stat) +/- 0.15 (syst) mag for Draco, corresponding to a distance of 75.8 +/- 0.7 (stat) +/- 5.4 (syst) kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all 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. RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abonanos@cfa.harvard.edu; kstanek@cfa.harvard.edu; aszentgyorgyi@cfa.harvard.edu; sasselov@cfa.harvard.edu; gbakos@cfa.harvard.edu RI Bonanos, Alceste/K-5392-2013 OI Bonanos, Alceste/0000-0003-2851-1905 NR 28 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 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2004 VL 127 IS 2 BP 861 EP 867 DI 10.1086/381073 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 801FG UT WOS:000220081200023 ER PT J AU Torres, G AF Torres, G TI A double-lined spectroscopic orbit for the young star HD 34700 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : spectroscopic; stars : evolution; stars : individual (HD 34700); stars : pre-main-sequence; techniques : spectroscopic ID MAIN-SEQUENCE STARS; T-TAURI STARS; HIGH-RESOLUTION SPECTROSCOPY; MILLIMETER-WAVE PROPERTIES; VEGA-LIKE SYSTEMS; RADIAL-VELOCITIES; FORMING REGIONS; SOURCE CATALOG; BINARY STARS; MULTIPLICITY AB We report high-resolution spectroscopic observations of the young star HD 34700, which confirm it to be a double-lined spectroscopic binary. We derive an accurate orbital solution with a period of 23.4877 +/- 0.0013 days and an eccentricity of e = 0.2501 +/- 0.0068. The stars are found to be of similar mass (M(2)/M(1) = 0.987 +/- 0.014) and luminosity. We derive also the effective temperatures (5900 and 5800 K) and projected rotational velocities (28 and 22 km s(-1)) of the components. These values of v sin i are much higher than expected for main-sequence stars of similar spectral type (G0) and are not due to tidal synchronization. We also discuss the indicators of youth available for the object. Although there is considerable evidence that the system is young strong infrared excess, X-ray emission, Li i lambda6708 absorption (0.17 Angstrom equivalent width), Halpha emission (similar to 0.6 Angstrom), rapid rotation - the precise age cannot yet be established because the distance is unknown. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 20,60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu NR 51 TC 9 Z9 9 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 FEB PY 2004 VL 127 IS 2 BP 1187 EP 1193 DI 10.1086/381066 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 801FG UT WOS:000220081200049 ER PT J AU Storm, J Carney, BW Gieren, WP Fouque, P Latham, DW Fry, AM AF Storm, J Carney, BW Gieren, WP Fouque, P Latham, DW Fry, AM TI The effect of metallicity on the Cepheid Period-Luminosity relation from a Baade-Wesselink analysis of Cepheids in the Galaxy and in the Small Magellanic Cloud SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars : distances; stars : fundamental parameters; Cepheids; Magellanic Clouds; distance scale ID GRAVITATIONAL LENSING EXPERIMENT; HUBBLE-SPACE-TELESCOPE; MILKY-WAY CEPHEIDS; EXTRAGALACTIC DISTANCE SCALE; SURFACE BRIGHTNESS TECHNIQUE; CLASSICAL CEPHEIDS; RADIAL-VELOCITY; INTERFEROMETRIC OBSERVATIONS; FUNDAMENTAL PARAMETERS; IMPROVED CALIBRATION AB We have applied the near-IR Barnes-Evans realization of the Baade-Wesselink method as calibrated by Fouque & Gieren (1997) to five metal-poor Cepheids with periods between 13 and 17 days in the Small Magellanic Cloud as well as to a sample of 34 Galactic Cepheids to determine the effect of metallicity on the period-luminosity (P-L) relation. For ten of the Galactic Cepheids we present new accurate and well sampled radial-velocity curves. The Baade-Wesselink analysis provides accurate individual distances and luminosities for the Cepheids in the two samples, allowing us to constrain directly, in a purely differential way, the metallicity effect on the Cepheid P-L relation. For the Galactic Cepheids we provide a new set of P-L relations which have zero-points in excellent agreement with astrometric and interferometric determinations. These relations can be used directly for the determination of distances to solar-metallicity samples of Cepheids in distant galaxies, circumventing any corrections for metallicity effects on the zero-point and slope of the P-L relation. We find evidence for both such metallicity effects in Our data. Comparing our two samples of Cepheids at a mean period of about 15 days, we find a weak effect of metallicity on the luminosity similar to that adopted by the HST Key Project on the Extragalactic Distance Scale. The effect is smaller for the V band, where we find DeltaM(V)/Delta[Fe/H]=-0.21+/-0.19, and larger for the Wesenheit index W, where we find DeltaM(W)/Delta[Fe/H]=-0.29+/-0.19. For the I and K bands we find DeltaM(I)/Delta[Fe/H]=-0.23+/-0.19 and DeltaM(K)/Delta[Fe/H]=-0.21+/-0.19, respectively. The error estimates are 1 sigma statistical errors. It seems now well established that metal-poor Cepheids with periods longer than about 10 days are intrinsically fainter in all these bands than their metal-rich counterparts of identical period. Correcting the LMC distance estimate of Fouque et al. (2003) for this metal licit effect leads to a revised LMC distance modulus of (m-M)(0)=18.48+/-0.07, which is also in excellent agreement with the value of (m-M)(0) 18.50+/-0.10 adopted by the Key Project. From our SMC Cepheid distances we determine the SMC distance to be 18.88+/-0.13 mag irrespective of metallicity. C1 Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. Univ Concepcion, Dept Fis, Concepcion, Chile. Observ Paris, LESIA, F-92195 Meudon, France. European So Observ, Santiago 19, Chile. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Storm, J (reprint author), Astrophys Inst Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. EM jstorm@aip.de; bruce@physics.unc.edu; wgieren@coma.cfm.udec.cl; pfouque@eso.org; dlatham@cfa.harvard.edu; anne.fry@integraonline.com OI Storm, Jesper/0000-0002-8627-6096 NR 94 TC 93 Z9 95 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2004 VL 415 IS 2 BP 531 EP 547 DI 10.1051/0004-6361:30034634 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 773RG UT WOS:000188936100020 ER PT J AU Voevodkin, A Vikhlinin, A AF Voevodkin, A Vikhlinin, A TI Constraining amplitude and slope of the mass fluctuation spectrum using a cluster baryon mass function SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; galaxies : clusters : general; surveys; X-rays : galaxies : clusters ID NEARBY GALAXY CLUSTERS; MICROWAVE BACKGROUND ANISOTROPIES; RAY SCALING RELATIONS; DARK-MATTER HALOES; DIGITAL SKY SURVEY; M-T RELATION; COSMOLOGICAL CONSTRAINTS; INFLATIONARY UNIVERSE; TEMPERATURE PROFILES; INTRACLUSTER MEDIUM AB We derive the baryon mass function for a complete sample of low-redshift clusters and argue that it is an excellent proxy for the total mass function if the ratio f(b)=M-b/M-tot in all clusters is close to its universal value, Omega(b)/Omega(M). Under this assumption, the baryon mass function can be used to constrain the amplitude and slope of the density fluctuation power spectrum on cluster scales. This method does not use observational determinations of the total mass and thus bypasses major uncertainties in the traditional analyses based on the X-ray temperature function. However, it is sensitive to possible systematic variations of the baryon fraction as a function of cluster mass. Adapting a weak dependence f(b)(M), suggested by observations and numerical simulations by Bialek et al., we derive sigma(8)=0.72+/-0.04 and the shape parameter Omega(M)h=0.13+/-0.07, in good agreement with a number of independent methods. We discuss the sensitivity of these values to other cosmological parameters and to different assumptions about variations in f(b). C1 Space Res Inst, Moscow, Russia. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Space Res Inst, Moscow, Russia. RP Voevodkin, A (reprint author), Space Res Inst, Profsoyuznaya 84-32, Moscow, Russia. EM voevodkin@hea.iki.rssi.ru NR 69 TC 56 Z9 56 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 FEB 1 PY 2004 VL 601 IS 2 BP 610 EP 620 DI 10.1086/380818 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769PC UT WOS:000188658100002 ER PT J AU Dale, DA Roussel, H Contursi, A Helou, G Dinerstein, HL Hunter, DA Hollenbach, DJ Egami, E Matthews, K Murphy, TW Lafon, CE Rubin, RH AF Dale, DA Roussel, H Contursi, A Helou, G Dinerstein, HL Hunter, DA Hollenbach, DJ Egami, E Matthews, K Murphy, TW Lafon, CE Rubin, RH TI Near-infrared integral field spectroscopy of star-forming galaxies SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : ISM; HII regions; infrared : galaxies; stars : formation ID SPECTRAL ENERGY-DISTRIBUTIONS; BLUE COMPACT GALAXIES; EMISSION-LINE SPECTRA; H-II REGIONS; INTERSTELLAR-MEDIUM; SPIRAL GALAXIES; FE-II; PHYSICAL CONDITIONS; STARBURST GALAXIES; ORION NEBULA AB The Palomar Integral Field Spectrograph was used to probe a variety of environments in nine nearby galaxies that span a range of morphological types, luminosities, metallicities, and infrared-to-blue ratios. For the first time, near-infrared spectroscopy was obtained for nuclear or bright H II regions in star-forming galaxies over two spatial dimensions (5."7x10."0) in the [Fe II] (1.257 mum), [Fe II] (1.644 mum), Pabeta (1.282 mum), H-2 (2.122 mum), and Brgamma (2.166 mum) transition lines. These data yield constraints on various characteristics of the star-forming episodes in these regions, including their strength, maturity, spatial variability, and extinction. The H II regions stand out from the nuclei. Unlike observations of nuclear regions, H II region near-infrared observations do not show a spatial coincidence of the line and continuum emission; the continuum and line maps of H II regions usually show distinct and sometimes spatially separated morphologies. Gauging from Pabeta and Brgamma equivalent widths and luminosities, the H II regions have younger episodes of star formation than the nuclei and more intense radiation fields. Near-infrared line ratio diagnostics suggest that H II regions have "purer'' starbursting properties. The correlation between ionizing photon density and mid-infrared color is consistent with the star formation activity level being higher for H II regions than for nuclei. And though the interpretation is complicated, on a purely empirical basis the H II regions show lower Fe1+ abundances than nuclei by an order of magnitude. C1 Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. CALTECH, Pasadena, CA 91125 USA. Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Lowell Observ, Flagstaff, AZ 86001 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Washington, Dept Phys, Seattle, WA 98195 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dale, DA (reprint author), Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. EM ddale@uwyo.edu NR 84 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 FEB 1 PY 2004 VL 601 IS 2 BP 813 EP 830 DI 10.1086/380753 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769PC UT WOS:000188658100017 ER PT J AU La Parola, V Fabbiano, G Elvis, M Nicastro, F Kim, DW Peres, G AF La Parola, V Fabbiano, G Elvis, M Nicastro, F Kim, DW Peres, G TI Long-term X-ray spectral variability of the nucleus of M81 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M81); galaxies : nuclei; X-rays : galaxies ID ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEUS; DUSTY WARM ABSORBERS; SPIRAL GALAXY M81; GAS; DISCOVERY; EMISSION; BINARIES; CHANDRA; QUASARS AB We have analyzed the soft X-ray emission from the nuclear source of the nearby spiral galaxy M81, using the available data collected with ROSAT, ASCA, BeppoSAX, and Chandra. The source flux is highly variable (sometimes dramatic: a factor of 4 in 20 days), showing variability at different timescales, from 2 days to 4 yr, and in particular a steady increase of the flux by a factor of greater than or similar to2 over 4 yr, broken by rapid flares. After accounting for the extended component resolved by Chandra, the nuclear soft X-ray spectrum (from ROSAT/PSPC, BeppoSAX/LECS, and Chandra data) cannot be fitted well with a single absorbed power-law model. Acceptable fits are obtained by adding an extra component, either a multicolor blackbody (MCBB) or an absorption feature. In the MCBB case, the inner accretion disk would be far smaller than the Schwartzchild radius for the 3-60x10(6) M-circle dot nucleus, requiring a strictly edge-on inclination of the disk, even if the nucleus is a rotating Kerr black hole. The temperature is 0.27 keV, larger than expected from the accretion disk of a Schwartzchild black hole but consistent with that expected from a Kerr black hole. In the power law+absorption feature model, we have either high-velocity (0.3c) infalling C V clouds or neutral C I absorption at rest. In both cases the C:O overabundance is a factor of 10. C1 Dipartimento Sci Fis & Astron, Sez Astron, I-90134 Palermo, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP La Parola, V (reprint author), Dipartimento Sci Fis & Astron, Sez Astron, Piazza Parlamento 1, I-90134 Palermo, Italy. EM laparola@oapa.astropa.unipa.it OI Nicastro, Fabrizio/0000-0002-6896-1364; PERES, Giovanni/0000-0002-6033-8180; La Parola, Valentina/0000-0002-8087-6488 NR 44 TC 10 Z9 10 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 FEB 1 PY 2004 VL 601 IS 2 BP 831 EP 844 DI 10.1086/380786 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769PC UT WOS:000188658100018 ER PT J AU Shinnaga, H Ohashi, N Lee, SW Moriarty-Schieven, GH AF Shinnaga, H Ohashi, N Lee, SW Moriarty-Schieven, GH TI Physical properties and kinetic structure of a starless core in the Taurus molecular cloud SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : clouds; ISM : individual (L1521F); ISM : molecules; radio lines : ISM; stars : formation ID SUBMILLIMETER CONTINUUM OBSERVATIONS; CLERK-MAXWELL-TELESCOPE; PRE-PROTOSTELLAR CORES; DENSE CORES; DARK CLOUDS; SCUBA DATA; L1544; AMMONIA; MASS; CCS AB We have made synthesis imaging of a starless core in the Taurus molecular cloud L1521F, with two key chemical evolutionary tracers, CCS (J(N) = 3(2)-2(1)), which traces young evolutionary phase of cores, and N2H+ (J = 1-0), which traces until the late evolutionary phase, as well as mapping observations of submillimeter dust continuum. The peak positions, as well as the radial distributions, of N2H+ and dust continuum coincide with each other. Unlike the other tracers, CCS shows a dip at the dust continuum center, suggesting that the abundance of the molecule decreases at the core center because of depletion and chemical reactions. The channel maps of both molecular lines clearly revealed clumpy substructures inside the core. Using an automatic and objective routine, eight and four clumps have been identified in the CCS and N2H+ channel maps, respectively. The abundances of the molecules are estimated toward the dust continuum center. Using our derived abundances, the LTE masses for each clump are estimated. The CCS components, which appear to trace the envelope, show an overall velocity gradient from east to west, whereas a N2H+ clump located at the core center shows a gradient from west to east. Assuming that the velocity gradients are due to rotation, the observational results indicate that the rotation of the outer envelope (size less than or similar to 0.08 pc similar to 16,000 AU) and that of the central compact region (size less than or similar to 0.03 pc similar to 6000 AU) have different axes with almost opposite senses of rotation. The velocity gradients of the southern and northern CCS components are estimated to be 7.2 and 9.2 km s(-1) pc(-1) at size scales of 0.05 and 0.04 pc, respectively. The velocity gradient of the N2H+ components at the core center is estimated to be 15 km s(-1) pc(-1) at a size scale of 0.01 pc (similar to2000 AU). Examining the line width-size correlation of these clumps and of other cold ( kinetic temperature T-K less than or similar to 10 K) starless cores, the slope index is found to be slightly shallower than those values for cores containing stars. Assuming a spherical, homogeneous sphere, the ratios of rotational to gravitational energy, beta, of these cores are calculated to be similar to0.3 for the CCS and similar to1.0 for the N2H+ components, respectively. The relation of the specific angular momentum (J/M) to size seen at scales larger than similar to0.03 pc (similar to6000 AU) appears to flatten out at sizes smaller than similar to6000 AU, for which the specific angular momentum is relatively constant at similar to0.002. This is consistent with results reported by Ohashi et al. Based on a chemical evolutionary model, the core may be in a young starless cores phase, assuming that the dip of CCS at the core center is caused by depletion and chemical reaction. L1521F may be in a younger starless-core phase than L1544. C1 Harvard Smithsonian Ctr Astrophys, Submillimeter Array, Hilo, HI 96721 USA. Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. Joint Astron Ctr, Natl Res Council Canada, Hilo, HI 96720 USA. RP Shinnaga, H (reprint author), Harvard Smithsonian Ctr Astrophys, Submillimeter Array, POB 824, Hilo, HI 96721 USA. EM hshinnaga@cfa.harvard.edu NR 56 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 FEB 1 PY 2004 VL 601 IS 2 BP 962 EP 978 DI 10.1086/379760 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769PC UT WOS:000188658100028 ER PT J AU Slane, P Zimmerman, ER Hughes, JP Seward, FD Gaensler, BM Clarke, MJ AF Slane, P Zimmerman, ER Hughes, JP Seward, FD Gaensler, BM Clarke, MJ TI X-ray observations of the compact source in CTA 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM : individual (CTA 1); stars : individual (RX J0007.0+7302; 3EG J0010+7309); stars : neutron; supernova remnants; X-rays : ISM ID SUPERNOVA REMNANT G292.0+1.8; CENTRAL OBJECT; NEUTRON-STARS; PULSAR; PULSATIONS; DISCOVERY; EMISSION; NEBULAE; 3C-58 AB We have studied the point source RX J0007.0+7302, at the center of supernova remnant CTA 1, using the X-Ray Multi-mirror Mission (XMM-Newton). The X-ray spectrum of the source is consistent with that of a neutron star and is well described by a power law with the addition of a soft thermal component that may correspond to emission from hot polar cap regions or to cooling emission from a light-element atmosphere over the entire star. There is evidence of extended emission on small spatial scales, which may correspond to structure in the underlying synchrotron nebula. No pulsations are observed. Extrapolation of the nonthermal spectrum of RX J0007.0+7302 to gamma-ray energies yields a flux consistent with that of EGRET source 3EG J0010+7309, supporting the proposition that there is a gamma-ray-emitting pulsar at the center of CTA 1. Observations of the outer regions of CTA 1 with ASCA confirm earlier detections of thermal emission from the supernova remnant and show that the synchrotron nebula extends to the outermost reaches of the remnant. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Cambridge, MA 02138 USA. Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 NR 28 TC 31 Z9 31 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 FEB 1 PY 2004 VL 601 IS 2 BP 1045 EP 1049 DI 10.1086/380498 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769PC UT WOS:000188658100035 ER PT J AU Belczynski, K Kalogera, V Zezas, A Fabbiano, G AF Belczynski, K Kalogera, V Zezas, A Fabbiano, G TI X-ray binary populations: The luminosity function of NGC 1569 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; galaxies : individual (NGC 1569); stars : evolution; X-rays : binaries ID STARBURST GALAXY NGC-1569; CHANDRA OBSERVATIONS; STELLAR POPULATION; STARS; EVOLUTION; PULSARS; SYSTEMS; HISTORY AB Using the population synthesis code StarTrack we construct the first synthetic X-ray binary populations for direct comparison with the X-ray luminosity function (XLF) of NGC 1569 observed with Chandra. Our main goal is to examine whether it is possible to reproduce the XLF shape with our models, given the current knowledge of the star formation history of this starburst galaxy. We thus produce hybrid models meant to represent the two stellar populations: one old and metal-poor, with continuous star formation for similar to1.5 Gyr; and another a recent and metal-rich population. To examine the validity of the models, we compare XLFs calculated for varying ages of the populations and varying relative weights for the star formation rates in the two populations. We find that for typical binary evolution parameters, it is indeed possible to quite closely match the observed XLF shape. The robust match is achieved for an age of the young population and a ratio of star formation rates in the two populations that are within factors of 1.5 and 2, respectively, of those inferred from Hubble Space Telescope observations of NGC 1569. In view of this encouraging first step, we discuss the implications of our X-ray binary models and their potential as tools to study binary populations in galaxies. C1 Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Belczynski, K (reprint author), Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM belczynski@northwestern.edu; vicky@northwestern.edu; azezas@head.cfa.harvard.edu; pepi@head.cfa.harvard.edu RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X NR 28 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 FEB 1 PY 2004 VL 601 IS 2 BP L147 EP L150 DI 10.1086/382131 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769PE UT WOS:000188658300010 ER PT J AU Miller, J Hormiga, G AF Miller, J Hormiga, G TI The unbearable lightness of being monophyletic: Clade stability and the addition of data: A case study from erigonine spiders (Araneae : Linyphiidae, Erigoninae) SO CLADISTICS LA English DT Meeting Abstract CT 22nd Annual Meeting of the Willi-Hennig-Society CY JUL 20-24, 2003 CL New York Botan Garden, Bronx, NY SP Willi Hennig Soc HO New York Botan Garden C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol Entomol, Washington, DC 20560 USA. George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RI Hormiga, Gustavo/C-3874-2009 NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0748-3007 EI 1096-0031 J9 CLADISTICS JI Cladistics PD FEB PY 2004 VL 20 IS 1 BP 89 EP 89 PG 1 WC Evolutionary Biology SC Evolutionary Biology GA 806PZ UT WOS:000220447100054 ER PT J AU Fauchald, K AF Fauchald, K TI So many worms, so little time ... SO CLADISTICS-THE INTERNATIONAL JOURNAL OF THE WILLI HENNIG SOCIETY LA English DT Meeting Abstract CT 22nd Annual Meeting of the Willi-Hennig-Society CY JUL 20-24, 2003 CL New York Botan Garden, Bronx, NY SP Willi Hennig Soc HO New York Botan Garden C1 Smithsonian Inst, Natl Museum Nat Hist, Sect Invertebrate Zool, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0748-3007 J9 CLADISTICS JI Cladistics-Int. J. Willi Hennig Soc. PD FEB PY 2004 VL 20 IS 1 BP 82 EP 82 PG 1 WC Evolutionary Biology SC Evolutionary Biology GA 806PZ UT WOS:000220447100030 ER PT J AU Sanchez, CR Murray, S Montali, RJ AF Sanchez, CR Murray, S Montali, RJ TI Use of desferoxamine and S-adenosylmethionine to treat hemochromatosis in a red ruffed lemur (Varecia variegata ruber) SO COMPARATIVE MEDICINE LA English DT Article ID ADENOSYL-L-METHIONINE; ALCOHOLIC LIVER-DISEASE; IRON STORAGE DISEASE; CHELATION-THERAPY; DEFEROXAMINE; HEMOSIDEROSIS; OVERLOAD; PHARMACOKINETICS; EFFICACY; MODELS AB Hemochromatosis was diagnosed in a 14-year-old, male, red ruffed lemur (Varecia variegata ruber) on the basis of abnormal results of serum biochemical analysis, including high serum ferritin and transferrin saturation values, and of liver biopsy. Therapy included chelation, using desferoxamine to remove excess iron and S-adenosylmethionine to improve liver function, and monthly peripheral blood removal by phlebotomy to reduce total body iron content. Response to treatment was assessed by changes in the lemur's attitude and appetite, as well as variations in serum biochemical and iron panel values. Initial improvement was associated with the onset of therapy. After 56 days of treatment, results of serum biochemical analysis indicated a decrease in iron panel values Treatment was temporarily discontinued from days 56 to 65, and the lemur's condition worsened, so therapy was re-instituted. However, the lemur died of hepatocellular carcinoma on day 110 of treatment. C1 Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Sanchez, CR (reprint author), Smithsonian Inst, Natl Zool Pk, 3001 Connecticut Ave, Washington, DC 20008 USA. NR 35 TC 3 Z9 4 U1 0 U2 3 PU AMER ASSOC LABORATORY ANIMAL SCIENCE PI MEMPHIS PA 9190 CRESTWYN HILLS DR, MEMPHIS, TN 38125 USA SN 1532-0820 J9 COMPARATIVE MED JI Comparative Med. PD FEB PY 2004 VL 54 IS 1 BP 100 EP 103 PG 4 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 780EA UT WOS:000189358000017 PM 15027625 ER PT J AU Miller, B Conway, W Reading, RP Wemmer, C Wildt, D Kleiman, D Monfort, S Rabinowitz, A Armstrong, B Hutchins, M AF Miller, B Conway, W Reading, RP Wemmer, C Wildt, D Kleiman, D Monfort, S Rabinowitz, A Armstrong, B Hutchins, M TI Evaluating the conservation mission of zoos, aquariums, botanical gardens, and natural history museums SO CONSERVATION BIOLOGY LA English DT Article ID ATTITUDE-CHANGE AB Collection-based institutions-zoos, aquariums, museums, and botanical gardens-exhibit wildlife and thus have a special connection with nature. Many of these institutions emphasize a mission of conservation, and, undeniably, they do contribute directly to conservation education and conservation science. They present an exceptional opportunity for many urban residents to see the wonders of life, and they can contribute to education and habitat preservation. Because many collection-based institutions now hold a stated mission of conservation, we suggest eight potential questions to evaluate actions toward that mission: (1) Does conservation thought define policy decisions? (2) Is there sufficient organizational funding for conservation activities? (3) Is there a functional conservation department? (4) Does the institution advocate for conservation? (5) Do conservation education programs effectively target children and adults? (6) Does the institution contribute directly to habitat protection locally and internationally? (7) Do exhibits explain and promote conservation efforts? and (8) Do internal policies and activities protect the environment? These questions are offered as a place to begin discussion. We hope they will help employees and administrators of a collection-based institution (and citizens of the surrounding community) think about and support their institution's conservation activities. Public support and praise for institutions that are striving toward solutions for conservation problems and pressure on organizations that are moving more slowly toward a conservation orientation can help shift more resources toward saving nature. C1 Denver Zool Fdn, Denver, CO 80205 USA. Wildlife Conservat Soc, Bronx, NY 10460 USA. Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. Natl Zool Pk, Washington, DC 20008 USA. Brevard Zoo, Melbourne, FL 32940 USA. Amer Zoo & Aquarium Assoc, Silver Spring, MD 20910 USA. RP Miller, B (reprint author), Denver Zool Fdn, 2300 Steele St, Denver, CO 80205 USA. EM zooconservation@denverzoo.org NR 47 TC 29 Z9 36 U1 27 U2 148 PU BLACKWELL PUBLISHING INC PI MALDEN PA 350 MAIN ST, MALDEN, MA 02148 USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2004 VL 18 IS 1 BP 86 EP 93 DI 10.1111/j.1523-1739.2004.00181.x PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 769HL UT WOS:000188644500018 ER PT J AU Novotny, V Basset, Y Miller, SE Kitching, RL Laidlaw, M Drozd, P Cizek, L AF Novotny, V Basset, Y Miller, SE Kitching, RL Laidlaw, M Drozd, P Cizek, L TI Local species richness of leaf-chewing insects feeding on woody plants from one hectare of a lowland rainforest SO CONSERVATION BIOLOGY LA English DT Article ID PAPUA-NEW-GUINEA; QUANTIFYING BIODIVERSITY; HOST-SPECIFICITY; TROPICAL FOREST; HERBIVORES; DIVERSITY; COMMUNITIES; LEPIDOPTERA; ARTHROPODS; ABUNDANCE AB Local species diversity of insect herbivores feeding on rainforest vegetation remains poorly known. This ignorance limits evaluation of species extinction patterns following various deforestation scenarios. We studied leaf-chewing insects feeding on 59 species of woody plants from 39 genera and 18 families in a lowland rainforest in Papua New Guinea and surveyed all plants with a stem diameter at breast height of greater than or equal to5 cm in a 1-ha plot within the same area. We used two extrapolation methods, based on randomized species-accumulation curves, to combine these two data sets and estimate the number of species of leaf-chewing herbivores feeding on woody plants from the 1-ha area. We recorded 58,483 feeding individuals from 940 species of leaf-chewing insects. The extrapolation estimated that there were 1567-2559 species of leaf-chewing herbivores feeding on the 152 plant species from 97 genera and 45 families found in 1 ha of the forest. Most of the herbivore diversity was associated with plant diversity on the familial and generic levels. We predicted that, on average, the selection of 45 plant species each representing a different family supported 39% of all herbivore species, the 52 plant species each representing a different additional genus from these families supported another 39% of herbivore species, and the remaining 55 plant species from these genera supported 22% of herbivore species. Lepidoptera was the most speciose taxon in the local fauna, followed by Coleoptera and orthopteroids (Orthoptera and Phasmatodea). The ratio of herbivore to plant species and the estimated relative species richness of the Lepidoptera, Coleoptera, and orthopteroids remained constant on the spatial scale from 0.25 to 1 ha. However, the utility of local taxon-to-taxon species ratios for extrapolations to geographic scales requires further study. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, MRC 105, Washington, DC 20013 USA. Acad Sci Czech Republic, Inst Entomol, Branisovska 31, CR-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice 37005, Czech Republic. Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Griffith Univ, Cooperat Res Ctr Trop Rainforest Ecol & Managemen, Nathan, Qld 4111, Australia. Univ Ostrava, Dept Biol, Ostrava 70103, Czech Republic. RP Miller, SE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, MRC 105, Washington, DC 20013 USA. EM miller.scott@nmnh.si.edu RI Kitching, Roger/C-5102-2009; Drozd, Pavel/J-3943-2013; Basset, Yves/B-6642-2014; Cizek, Lukas/G-7905-2014; Novotny, Vojtech/G-9434-2014; Cizek, Lukas/K-7111-2015; OI Drozd, Pavel/0000-0002-4602-8856; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 46 TC 29 Z9 30 U1 3 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2004 VL 18 IS 1 BP 227 EP 237 DI 10.1111/j.1523-1739.2004.00293.x PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 769HL UT WOS:000188644500031 ER PT J AU Wright, SJ Calderon, O Hernandez, A Paton, S AF Wright, SJ Calderon, O Hernandez, A Paton, S TI Are lianas increasing in importance in tropical forests? A 17-year record from Panama SO ECOLOGY LA English DT Article DE Barro Colorado Island; El Nino; leaf litter; leaf production; lianas; seedlings; seeds; temporal trends; tropical forests ID TREE; DIVERSITY; BIOMASS; GROWTH; CONSEQUENCES; RECRUITMENT; ABUNDANCE; DYNAMICS; IMPACT; PLANTS AB The relative importance of large lianas (woody vines) increased by 100% for stem enumerations conducted during the 1980s and 1990s in widely scattered Neotropical forests. We use three independent types of data to evaluate the hypothesis that lianas have increased in importance in old growth forests on Barro Colorado Island, Panama. Liana leaf litter production and the proportion of forest-wide leaf litter composed of lianas increased between 1986 and 2002. In contrast, liana seed production and liana seedling densities were much more variable through time with particularly high levels during and immediately after El Nino years. Longer time series will be required to detect shifts in life-form composition for highly dynamic seed and seedling communities. The Barro Colorado Island leaf production data are, however, consistent with the hypothesis that lianas are increasing in importance in Neotropical forests. C1 Smithsonian Trop Res Inst, Balboa 2072, Ancon, Panama. RP Wright, SJ (reprint author), APO AA, Unit 0948, Miami, FL 34002 USA. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 31 TC 145 Z9 156 U1 2 U2 16 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 FEB PY 2004 VL 85 IS 2 BP 484 EP 489 DI 10.1890/02-0757 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 801PV UT WOS:000220108700018 ER PT J AU Crockett, C AF Crockett, C TI What do kids know - and misunderstand - about science? SO EDUCATIONAL LEADERSHIP LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Crockett, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-71, Cambridge, MA 02138 USA. EM ccrockett@cfa.harvard.edu NR 6 TC 2 Z9 2 U1 0 U2 0 PU ASSOC SUPERVISION CURRICULUM DEVELOPMENT PI ALEXANDRIA PA 1703 N BEAUREGARD ST, ALEXANDRIA, VA 22311-1717 USA SN 0013-1784 J9 EDUC LEADERSHIP JI Educ. Leadership PD FEB PY 2004 VL 61 IS 5 BP 34 EP 37 PG 4 WC Education & Educational Research SC Education & Educational Research GA 771ZB UT WOS:000188815000007 ER PT J AU Levitan, DR Fukami, H Jara, J Kline, D McGovern, TM McGhee, KE Swanson, CA Knowlton, N AF Levitan, DR Fukami, H Jara, J Kline, D McGovern, TM McGhee, KE Swanson, CA Knowlton, N TI Mechanisms of reproductive isolation among sympatric broadcast-spawning corals of the Montastraea annularis species complex SO EVOLUTION LA English DT Article DE coral reef; fertilization; hybridization; mass-spawning; speciation ID CONGENERIC SEA-URCHINS; REEF BUILDING CORAL; SEXUAL CONFLICT; FERTILIZATION KINETICS; RETICULATE EVOLUTION; ACROPORA-HYACINTHUS; FAVEOLATA ELLIS; GENUS PLATYGYRA; HYBRIDIZATION; SCLERACTINIA AB Many coral species spawn simultaneously and have compatible gametes, leading to controversy over the nature of species boundaries and the frequency with which hybridization occurs. Three western Atlantic corals, Montastraea annularis, M. faveolata, and M. franksi, typify this controversy; they all spawn sympatrically on the same evenings after the fall full moons. Here we show, in both Panama and the Bahamas for multiple years, how a variety of mechanisms may act in concert to reproductively isolate all three species. Field studies indicate that M. franksi spawns two hours earlier than the other two species, and the eggs released during this earlier period disperse an average of 500 m by the time the other species spawn. Field measures of fertilization indicate that peak fertilization occurs when spawning synchrony is high and that corals that spawn at the tails of the spawning distributions have greatly reduced fertilization success. Laboratory studies indicate that there is a gametic incompatibility between M. faveolata and the other two species. There are regional differences in the gametic compatibility of M. franksi and M. annularis. In Panama, the two species are completely compatible, whereas in the Bahamas, M. franksi sperm can fertilize M. annularis eggs but the reciprocal cross often fails. Gamete age influences patterns of fertilization, such that very young eggs seem resistant to fertilization and old sperm lose viability after two hours. In sum, the combination of temporal differences in spawning, sperm aging, gamete dispersal and dilution, and gametic incompatibility act in various combinations among the three species, making it unlikely that hybrid fertilization would occur. C1 Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. Smithsonian Trop Res Inst, Balboa 2072, Panama. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. RP Levitan, DR (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA. EM levitan@bio.fsu.edu NR 58 TC 125 Z9 131 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 FEB PY 2004 VL 58 IS 2 BP 308 EP 323 DI 10.1111/j.0014-3820.2004.tb01647.x PG 16 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 802WS UT WOS:000220194200009 PM 15068348 ER PT J AU Fukami, H Budd, AF Levitan, DR Jara, J Kersanach, R Knowlton, N AF Fukami, H Budd, AF Levitan, DR Jara, J Kersanach, R Knowlton, N TI Geographic differences in species boundaries among members of the Montastraea annularis complex based on molecular and morphological markers SO EVOLUTION LA English DT Article DE Caribbean; coral reef; hybridization; Montastraea; sibling species complex ID REEF-BUILDING CORAL; GENUS ACROPORA; REPRODUCTIVE CHARACTERISTICS; MITOCHONDRIAL-DNA; GENETIC-EVIDENCE; EVOLUTIONARY HISTORY; SPAWNING TIMES; HYBRID ZONE; HYBRIDIZATION; SCLERACTINIA AB The three members of the Montastraea annularis complex (M. annularis, M. franksi, and M. faveolata) are dominant reef builders in the western Atlantic whose species status has been controversial for over a decade. Although differences in colony morphology and reproductive characteristics exist, interspecific fertilizations are possible in the laboratory and genetic differentiation is slight. Here we compare the three taxa genetically and morphologically in Panama and the Bahamas, widely separated locations spanning most of their geographic ranges. In Panama, analyses of three AFLP loci, a noncoding region of the mitochondrial genome, and ITS sequences reveal that M. faveolata is strongly differentiated genetically. Discriminant function analysis also indicates no overlap with the other two species in the fine structure of the corallites that comprise the colony. Genetic analyses of larvae from interspecific crosses between M. faveolata and the other two taxa confirmed the hybrid status of the larvae, but no examples of the most probable F, genotype were observed in the field. Although M. annularis and M. franksi were more similar, they also exhibited strong frequency differences at two AFLP loci and in the mitochondrial noncoding region, as well as distinct corallite structure. In the Bahamas, in contrast, the three taxa exhibited overlapping morphologies. Montastraea franksi and M. annularis were indistinguishable genetically, and M. faveolata was distinct at fewer genetic loci. Once again, however, the most probable F, genotype involving M. faveolata was not observed. Geographic differences between Panama and the Bahamas explain why past studies have come to different conclusions concerning the status of the three species. In general, the genetic and morphological data suggest a north to south hybridization gradient, with evidence for introgression strongest in the north. However, reproductive data show no such trend, with intrinsic barriers to gene flow comparable or stronger in the north. C1 Smithsonian Trop Res Inst, Naos Marine Lab, Balboa, Panama. Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. RP Fukami, H (reprint author), Smithsonian Trop Res Inst, Naos Marine Lab, Box 2072, Balboa, Panama. EM nknowlton@ucsd.edu NR 65 TC 129 Z9 137 U1 0 U2 18 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA SN 0014-3820 J9 EVOLUTION JI Evolution PD FEB PY 2004 VL 58 IS 2 BP 324 EP 337 DI 10.1111/j.0014-3820.2004.tb01648.x PG 14 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 802WS UT WOS:000220194200010 PM 15068349 ER PT J AU Lovelock, CE Feller, IC Mckee, KL Engelbrecht, BMJ Ball, MC AF Lovelock, CE Feller, IC Mckee, KL Engelbrecht, BMJ Ball, MC TI The effect of nutrient enrichment on growth, photosynthesis and hydraulic conductance of dwarf mangroves in Panama SO FUNCTIONAL ECOLOGY LA English DT Article DE Bocas del Toro; fertilization experiment; herbivory; Rhizophora mangle ID VS. PHOSPHORUS LIMITATION; NITROGEN-USE EFFICIENCY; RHIZOPHORA MANGLE L.; COASTAL PEAT SWAMP; BOCAS DEL TORO; SPARTINA-ALTERNIFLORA; GAS-EXCHANGE; AVICENNIA-GERMINANS; WATER TRANSPORT; PLANT-GROWTH AB 1. Dwarf stands of the mangrove Rhizophora mangle L. are extensive in the Caribbean. We fertilized dwarf trees in Almirante Bay, Bocas del Toro Province, north-eastern Panama with nitrogen (N) and phosphorus (P) to determine (1) if growth limitations are due to nutrient deficiency; and (2) what morphological and/or physiological factors underlie nutrient limitations to growth. 2. Shoot growth was 10-fold when fertilized with P and twofold with N fertilization, indicating that stunted growth of these mangroves is partially due to nutrient deficiency. 3. Growth enhancements caused by N or P enrichment could not be attributed to increases in photosynthesis on a leaf area basis, although photosynthetic nutrient-use efficiency was improved. The most dramatic effect was on stem hydraulic conductance, which was increased sixfold by P and 2.5-fold with N enrichment. Fertilization with P enhanced leaf and stem P concentrations and reduced C : N ratio, but did not alter leaf damage by herbivores. 4. Our findings indicate that addition of N and P significantly alter tree growth and internal nutrient dynamics of mangroves at Bocas del Toro, but also that the magnitude, pattern and mechanisms of change will be differentially affected by each nutrient. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Australian Natl Univ, Res Sch Biol Sci, Canberra, ACT 0200, Australia. RP Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM lovelockc@si.edu RI Ball, Marilyn/D-1180-2009; Engelbrecht, Bettina/E-9914-2012; McKee, Karen/D-1365-2014; Lovelock, Catherine/G-7370-2012; OI McKee, Karen/0000-0001-7042-670X; Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 NR 57 TC 79 Z9 87 U1 2 U2 50 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2004 VL 18 IS 1 BP 25 EP 33 DI 10.1046/j.0269-8463.2004.00805.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 772BT UT WOS:000188821200003 ER PT J AU Stiling, P Moon, D Hymus, G Drake, B AF Stiling, P Moon, D Hymus, G Drake, B TI Differential effects of elevated CO2 on acorn density, weight, germination, and predation among three oak species in a scrub-oak forest SO GLOBAL CHANGE BIOLOGY LA English DT Article DE acorn density; acorn weight; elevated CO2; germination rate; Kennedy Space Center; Quercus chapmanii; Quercus geminata; Quercus myrtifolia; seed predation ID METAANALYSIS; RECRUITMENT; ENRICHMENT; ECOSYSTEM; RESPONSES; CARBON; TREES AB Much research on the effects of elevated CO2 on forest trees has focused on quantitative changes in photosynthesis, secondary chemistry, and plant biomass. However, plant fitness responses to rising CO2 should also include quantitative measures of reproduction, since most forest systems are recruitment limited. Until now, it has proved very difficult to grow forest trees to sexual maturity in a CO2-enriched environment. This paper is the first of its kind to address the effects of elevated CO2 on the reproduction of hardwood trees in a natural forest. Beginning in 1996, scrub-oak vegetation, predominantly three species of scrub-oaks, Quercus myrtifolia, Q. chapmanii, and Q. geminata, were grown inside eight chambers with elevated CO2 (704 parts per million (ppm)) and eight with ambient CO2 (379 ppm) at Kennedy Space Center, Florida. In elevated CO2, acorn production increased significantly for the dominant species Q. myrtifolia and for Q. chapmanii, but it did not increase for the subdominant, Q. geminata. Acorn weight, germination rate, and predation by weevils were unaffected by CO2. Thus, recruitment of some forest tree species into the Florida scrub-oak community is likely to be accelerated in an atmosphere of increased CO2. However, because the acceleration of recruitment differs among species, over the long term, Q. myrtifolia and Q. chapmanii will be favored over Q. geminata and this is likely to change patterns of species diversity. C1 Univ S Florida, Dept Biol, Tampa, FL 33620 USA. Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Stiling, P (reprint author), Univ S Florida, Dept Biol, Tampa, FL 33620 USA. EM pstiling@chuma1.cas.usf.edu NR 18 TC 13 Z9 17 U1 0 U2 5 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD FEB PY 2004 VL 10 IS 2 BP 228 EP 232 DI 10.1111/j.1529-8817.2003.00728.x PG 5 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 775DN UT WOS:000189025600008 ER PT J AU Parenti, LR Soeroto, B AF Parenti, LR Soeroto, B TI Adrianichthys roseni and Oryzias nebulosus, two new ricefishes (Atherinomorpha : Beloniformes : Adrianichthyidae) from Lake Poso, Sulawesi, Indonesia SO ICHTHYOLOGICAL RESEARCH LA English DT Article DE ricefishes; Sulawesi; Buntingi; Adrianichthys roseni sp nov; Oryzias nebulosus sp nov. ID TELEOSTEI; FISH AB Two new species of ricefishes or buntingi, Adrianichthys roseni and Oryzias nebulosus, are described from Lake Poso, Sulawesi Tengah, Indonesia, bringing to 12 the number of endemic ricefishes known from Sulawesi. Adrianichthys roseni and its sole congener, A. kruyti, are distinguished from other relatively large-bodied ricefishes, Xenopoecilus, in having orbits that project beyond the dorsal profile of the head; paired preethmoid cartilages (versus single or absent in Xenopoecilus); and 13-16 (versus 8-13) dorsal fin rays. Also, as in A. kruyti, the lower jaw of A. roseni is enclosed in the upper jaw when the mouth is closed; however, the upper jaw is not as large and broadly expanded as in A. kruyti. Adrianichthys roseni differs further from A. kruyti in having fewer scales in a lateral series (approximately 63-65 versus 70-75), attaining a smaller maximum recorded standard length (90 mm versus 109 mm), and having the lateral process of the pelvic bone in line with the fifth, rather than the eighth, pleural rib. Oryzias nebulosus shares with O. nigrimas, also from Lake Poso, a unique sexual dichromatism in preserved specimens: adult males are dark gray to black, whereas females are a lighter grayish-yellow to brown. Relative to O. nigrimas, O. nebulosus is a small species (maximum recorded SL 33 mm versus 51 mm), with pelvic fins relatively anterior (lateral process of pelvic bone is in line with the third, fourth, or fifth, modally fourth, rather than the fourth or fifth, modally fifth, pleural rib), dorsal fin relatively anterior (origin above the 12-14th anal fin ray as opposed to the 15-17th anal fin ray), precaudal vertebrae 11-13, modally 12 (versus 13-14, modally 13), and relatively straight, narrow and slender (as opposed to curved, broad, and robust) ossified and cartilaginous portions of the gill arches. Endemic buntingi are threatened by introduction of exotic species, overfishing, and pollution. A conservation plan includes rearing native fishes for local use as ornamental fishes and possible reintroduction. C1 Smithsonian Inst, MRC 159, Natl Museum Nat Hist,Div Fishes, Dept Systemat Biol,Sect Vertebrate Zool, Washington, DC 20013 USA. Univ Sam Ratulangi, Dept Biol, Manado, Sulawesi, Indonesia. RP Parenti, LR (reprint author), Smithsonian Inst, MRC 159, Natl Museum Nat Hist,Div Fishes, Dept Systemat Biol,Sect Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM parenti.lynne@nmnh.si.edu; bam@manado.wasantara.net.id NR 38 TC 18 Z9 20 U1 0 U2 1 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 1341-8998 EI 1616-3915 J9 ICHTHYOL RES JI Ichthyol. Res. PD FEB PY 2004 VL 51 IS 1 BP 10 EP 19 DI 10.1007/s10228-003-0187-1 PG 10 WC Zoology SC Zoology GA 777JC UT WOS:000189173400003 ER PT J AU Muchhala, N Munroe, TA AF Muchhala, N Munroe, TA TI A new species of Soleichthys (Soleidae : Pleuronectiformes) from tropical seas off northern Australia SO ICHTHYOLOGICAL RESEARCH LA English DT Article DE Soleidae; Soleichthys; new species; Pleuronectiformes AB Soleichthys maculosus, described from six specimens collected in shallow waters (37-63 m) off northern Australia, is readily distinguished from congeners by its unique ocular-side pigmentation featuring numerous, conspicuous white spots and blotches nearly as large as the eye diameter on a uniformly dark brown background without any crossbands, and in having two elongated, ocular-side pectoral-fin rays, with the second dorsalmost ray longer than the first, and without scales on the pectoral-fin rays. Soleichthys maculosus is most similar to S. siammakuti, a poorly-known species collected in the Gulf of Thailand, but differs from S. siammakuti in having the second dorsalmost ocular-side pectoral-fin ray longer than the first (vs. first ocular-side pectoral-fin ray longer in S. siammakuti), and in having different ocular-side pigmentation than that of S. siammakuti, which features yellow spots on dorsal and anal fins, two conspicuous white spots arranged in longitudinal series on the lateral line, and also a series of nine, light brown crossbands on a dark brown body. C1 Smithsonian Inst, NOAA, NMFS, Natl Systemat Lab,NHB,WC 57, Washington, DC 20013 USA. Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. RP Munroe, TA (reprint author), Smithsonian Inst, NOAA, NMFS, Natl Systemat Lab,NHB,WC 57, POB 37012,MRC-153, Washington, DC 20013 USA. EM munroe.thomas@nmnh.si.edu NR 26 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER-VERLAG TOKYO PI TOKYO PA 3-3-13, HONGO, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 1341-8998 J9 ICHTHYOL RES JI Ichthyol. Res. PD FEB PY 2004 VL 51 IS 1 BP 57 EP 62 DI 10.1007/s10228-003-0196-0 PG 6 WC Zoology SC Zoology GA 777JC UT WOS:000189173400009 ER PT J AU Hoshino, K Amaoka, K Munroe, TA AF Hoshino, K Amaoka, K Munroe, TA TI New records of sexual dimorphisms among the Pleuronectiformes exhibited by differences in urogenital papilla structure of Citharichthys platophrys (Paralichthyidae : Pleuronectiformes) SO ICHTHYOLOGICAL RESEARCH LA English DT Article DE Citharichthys platophrys; sexual dimorphism; urogenital papilla ID BEHAVIOR; FLOUNDER AB Sexual dimorphisms of the urogenital papilla are reported in the eastern Pacific paralichthyid flounder Citharichthys platophrys. In males, the urogenital papilla is longer than that in females, and it has several (2-7) obvious lateral projections. Urogenital papilla length is not sexually dimorphic among related flatfishes (species of Paralichthyidae and Bothidae) examined. Several species of Citharichthys and Etropus have small, poorly developed lateral projections, which may suggest that these species share a common ancestry. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 0159, Washington, DC 20013 USA. Marine Ecol Inst, Osaka 5610808, Japan. Natl Marine Fisheries Serv, Natl Museum Nat Hist, MRC 0159, Washington, DC 20013 USA. RP Hoshino, K (reprint author), Natl Sci Museum, Shinjuku Ku, 3-23-1 Hyakunin Cho, Tokyo 1690073, Japan. EM khoshino@kahaku.go.jp; amaoka@fish.hokudai.ac.jp NR 11 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER-VERLAG TOKYO PI TOKYO PA 3-3-13, HONGO, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 1341-8998 J9 ICHTHYOL RES JI Ichthyol. Res. PD FEB PY 2004 VL 51 IS 1 BP 81 EP 83 DI 10.1007/s10228-003-0193-3 PG 3 WC Zoology SC Zoology GA 777JC UT WOS:000189173400014 ER PT J AU Gingerich, O AF Gingerich, O TI A catalogue Raisonne of scientific instruments from the Louvain school, 1530 to 1600 SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD FEB PY 2004 VL 35 BP 113 EP 115 PN 1 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 863LE UT WOS:000224562400007 ER PT J AU Basset, Y Novotny, V Miller, SE Weiblen, GD Missa, O Stewart, AJA AF Basset, Y Novotny, V Miller, SE Weiblen, GD Missa, O Stewart, AJA TI Conservation and biological monitoring of tropical forests: the role of parataxonomists SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE arthropods; biodiversity; rain forests; taxonomy ID PAPUA-NEW-GUINEA; SPECIES-ABUNDANCE MODELS; RAIN-FOREST; INSECT HERBIVORES; BIODIVERSITY CONSERVATION; DIVERSITY; DISTURBANCE; INDICATOR; FICUS; INVERTEBRATES AB 1. The demise of tropical rain forests will lead to a large-scale extinction of genetic diversity, particularly of arthropods. Curtailing these trends might be facilitated by (i) reducing rates of habitat loss and degradation, (ii) enhancing systematics and (iii) increasing the flow of primary information on tropical biodiversity. 2. We emphasize the need to examine alternative approaches that could generate a constant stream of data from tropical ecosystems. We argue that data collecting by parataxonomists (local assistants trained by professional biologists) represents one of the most efficient approaches to the study of tropical ecosystems available to date. 3. Parataxonomists can provide high-quality biological specimens and ecological information; statistical power will be high due to large sample sizes of data; database growth will be rapid and results will be published in a timely manner; and there will be collateral education of local people in conservation biology by the parataxonomists themselves. 4. We stress that training local parataxonomists to inventory and monitor biodiversity is a promising and efficient strategy that deserves more attention in conservation biology. In particular, it may be one of the most feasible approaches for the biological monitoring of small and cryptic organisms in species-rich environments, such as invertebrates in tropical rain forests. 5. Synthesis and applications. Permanent botanical plots yield a wealth of data on the organization of tropical forests, and their numbers should be increased to monitor tropical biodiversity. Likewise, augmenting the number of local parataxonomist groups in various tropical countries and networking these contingents to monitor functionally diverse taxa may provide an efficient biological monitoring system in tropical forests. C1 Smithsonian Trop Res Inst, Panama City, Panama. Acad Sci Czech Republ, Inst Entomol, CR-37005 Ceske Budejovice, Czech Republic. Univ S Bohemia, Fac Biol, Ceske Budejovice 37005, Czech Republic. Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA. Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. Griffith Univ, Australian Sch Environm Studies, Brisbane, Qld 4111, Australia. Univ Sussex, Sch Life Sci, Brighton BN1 9QG, E Sussex, England. RP Basset, Y (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Panama City, Panama. EM bassety@tivoli.si.edu RI Missa, Olivier/G-2687-2012; Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; OI Missa, Olivier/0000-0002-4330-5192; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 NR 99 TC 57 Z9 61 U1 3 U2 24 PU BLACKWELL PUBLISHING LTD PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD FEB PY 2004 VL 41 IS 1 BP 163 EP 174 DI 10.1111/j.1365-2664.2004.00878.x PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 768KJ UT WOS:000188541900015 ER PT J AU Krems, RV Dalgarno, A AF Krems, RV Dalgarno, A TI Quantum-mechanical theory of atom-molecule and molecular collisions in a magnetic field: Spin depolarization SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID RELAXATION RATES; AB-INITIO; PHOTOASSOCIATION; SPECTROSCOPY; TEMPERATURES; SCATTERING; EXCHANGE; GASES; TRAP AB A theory for quantum-mechanical calculations of cross sections for atom-molecule and molecular collisions in a magnetic field is presented. The formalism is based on the representation of the wave function as an expansion in a fully uncoupled space-fixed basis. The systems considered include S-1-atom-(2)Sigma-molecule, S-1-atom-(3)Sigma-molecule, (2)Sigma-molecule-(2)Sigma-molecule, and (3)Sigma-molecule-(3)Sigma-molecule. The theory is used to elucidate the mechanisms for collisionally induced spin depolarization. (C) 2004 American Institute of Physics. C1 Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. Harvard Smithsonian Ctr Astrophys, ITAMP, Inst Theoret Atom Mol & Opt Phys, 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 42 TC 99 Z9 99 U1 1 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD FEB 1 PY 2004 VL 120 IS 5 BP 2296 EP 2307 DI 10.1063/1.1636691 PG 12 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 767XD UT WOS:000188498400025 PM 15268368 ER PT J AU Kornicker, LS AF Kornicker, LS TI Morphology and musculature of a new species of Thaumatocypris (Ostracoda, Halocyprida, Thaumatocypridoidea) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article ID CRUSTACEA AB A new species, Thaumatocypris rudjakovi, from near Madagascar is described and illustrated. The specimens studied previously had been referred to T. echinata Mailer, 1906 by Rudjakov (1993). The description includes the analysis of appendage muscles. The species T. echinata is discussed, and a key is presented to genera of the Thaumatocyprididae. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. RP Kornicker, LS (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA. EM kornicker.louis@nmnh.si.edu NR 21 TC 3 Z9 3 U1 1 U2 1 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD FEB PY 2004 VL 24 IS 1 BP 54 EP 71 DI 10.1651/C-2397 PG 18 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 774VL UT WOS:000189006300005 ER PT J AU Roberts, SP Harrison, JF Dudley, R AF Roberts, SP Harrison, JF Dudley, R TI Allometry of kinematics and energetics in carpenter bees (Xylocopa varipuncta) hovering in variable-density gases SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE aerodynamics; allometry; energetics; flight; reserve capacity; Xylocopa; bee ID FLY DROSOPHILA-MELANOGASTER; INSECT FLIGHT; POWER REQUIREMENTS; OXYGEN-CONSUMPTION; MUSCLE EFFICIENCY; THERMAL-STABILITY; WATER-LOSS; AERODYNAMICS; PERFORMANCE; HUMMINGBIRDS AB We assessed the energetic and aerodynamic limits of hovering flight in the carpenter bee Xylocopa varipuncta. Using normoxic, variable-density mixtures Of O-2, N-2 and He, we were able to elicit maximal hovering performance and aerodynamic failure in the majority of bees sampled. Bees were not isometric regarding thorax mass and wing area, both of which were disproportionately lower in heavier individuals. The minimal gas density necessary for hovering (MGD) increased with body mass and decreased with relative thoracic muscle mass. Only the four bees in our sample with the highest body mass-specific thorax masses were able to hover in pure heliox. Wingbeat frequency and stroke amplitude during maximal hovering were significantly greater than in normodense hovering, increased significantly with body mass during normodense hovering but were mass independent during maximal hovering. Reserve capacity for wingbeat frequency and stroke amplitude decreased significantly with increasing body mass, although reserve capacity in stroke amplitude (10-30%) exceeded that of wingbeat frequency (0-8%). Stroke plane angle during normodense hovering was significantly greater than during maximal hovering, whereas body angle was significantly greater during maximal hovering than during normodense hovering. Power production during normodense hovering was significantly less than during maximal hovering. Metabolic rates, were significantly greater during maximal hovering than during normodense hovering and were inversely related to body mass during maximal and normodense hovering. Metabolic reserve capacity averaged 34% and was independent of body mass. Muscle efficiencies were slightly higher during normodense hovering. The allometry of power production, power reserve capacity and muscle efficiency were dependent on the assumed coefficient of drag (CD), with significant allometries most often at lower values of CD. Larger bees operate near the envelope of maximal performance even in normodense hovering due to smaller body mass-specific flight muscles and limited reserve capacities for kinematics and power production. C1 Univ Nevada, Dept Biol Sci, Las Vegas, NV 89154 USA. Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Roberts, SP (reprint author), Univ Nevada, Dept Biol Sci, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA. EM sroberts@ccmail.nevada.edu NR 46 TC 30 Z9 31 U1 1 U2 10 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD FEB PY 2004 VL 207 IS 6 BP 993 EP 1004 DI 10.1242/jeb.00850 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 804ZL UT WOS:000220336500016 PM 14766958 ER PT J AU Schroll, S AF Schroll, S TI Only skin deep: Changing visions of the American self. SO LIBRARY JOURNAL LA English DT Book Review C1 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 FEB 1 PY 2004 VL 129 IS 2 BP 83 EP 83 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 768BC UT WOS:000188507500062 ER PT J AU Riley, S AF Riley, S TI Late bloomer. 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 FEB 1 PY 2004 VL 129 IS 2 BP 125 EP 125 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 768BC UT WOS:000188507500270 ER PT J AU Bernardi, G Bucciarelli, G Costagliola, D Robertson, DR Heiser, JB AF Bernardi, G Bucciarelli, G Costagliola, D Robertson, DR Heiser, JB TI Evolution of coral reef fish Thalassoma spp. (Labridae). 1. Molecular phylogeny and biogeography SO MARINE BIOLOGY LA English DT Article ID INDO-WEST PACIFIC; SPECIES BOUNDARIES; MITOCHONDRIAL-DNA; WRASSE; SEQUENCE; PATTERNS; PRIMERS AB Wrasses in the genus Thalassoma comprise 27 recognized species that occur predominantly on coral reefs and subtropical rocky reefs worldwide. The phylogenetic relationships for 26 species were examined based on two mitochondrial genes (cytochrome b and 16S rRNA) and one nuclear intron (the first intron of the ribosomal protein S7). Two closely related species, the bird-wrasses (Gomphosus varius Lacepede, 1801 and G. caerulaeus Lacepede, 1801), were also included in the analysis. These species grouped within the genus Thalassoma. Thalassoma newtoni (Osorio, 1891) from Sao Tome, which is generally synonymized with the Atlantic/Mediterranean Thalassoma pavo (Linnaeus, 1758) appears to be a valid species. Using a molecular clock, the genus was estimated to have originally diverged 8-13 million years ago, with Thalassoma ballieui (Vaillant and Sauvage, 1875) from Hawaii and Thalassoma septemfasciata Scott, 1959 from Western Australia as the ancestral species. Approximately 5-10 million years ago, a sudden burst of speciation resulted in seven clades, which were resolved with the sequence data. The terminal Tethyan event and the closing of the Isthmus of Panama were probably the major historical factors shaping the evolution of species in the genus Thalassoma. These data on the spatio-temporal pattern of speciation in the Indo-Pacific indicate that peripheral species have been generated at various times throughout the history of the genus, and that none of the widespread species are relatively young. Thus, there is no clear support for centrifugal (youngest at the periphery) versus centripetal (oldest at the periphery) modes of generation of species, two theories which have been used to account for geographic gradients in species diversity. C1 Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. Univ Naples 2, Dipartimento Sci Vita, I-81100 Caserta, Italy. Smithsonian Trop Res Inst, Balboa, Panama. Cornell Univ, Shoals Marine Lab, Ithaca, NY 14853 USA. Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. RP Bernardi, G (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, 100 Shaffer Rd, Santa Cruz, CA 95060 USA. EM bernardi@biology.ucsc.edu RI Bernardi, Giacomo/F-6346-2011 OI Bernardi, Giacomo/0000-0002-8249-4678 NR 45 TC 72 Z9 74 U1 2 U2 16 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 FEB PY 2004 VL 144 IS 2 BP 369 EP 375 DI 10.1007/s00227-003-1199-0 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 767WE UT WOS:000188496200017 ER PT J AU Costagliola, D Robertson, DR Guidetti, P Stefanni, S Wirtz, P Heiser, JB Bernardi, G AF Costagliola, D Robertson, DR Guidetti, P Stefanni, S Wirtz, P Heiser, JB Bernardi, G TI Evolution of coral reef fish Thalassoma spp. (Labridae). 2. Evolution of the eastern Atlantic species SO MARINE BIOLOGY LA English DT Article ID MITOCHONDRIAL-DNA DIFFERENCES; MEDITERRANEAN SEA; GENE FLOW; POPULATIONS; PHYLOGEOGRAPHY; VARIABILITY; WESTERN; SCALES; PISCES AB The genetic relationships within and among congeneric species of marine fish from the Atlantic and the Mediterranean are poorly known. Relationships among all five species of the wrasse genus Thalassoma present in the Atlantic and the Mediterranean were examined using sequence data from the mitochondrial control region. Sampling was focused on the mid-Atlantic T. sanctaehelenae (Valenciennes, 1839) and T. ascensionis (Quoy & Gaimard, 1834), the eastern Atlantic T. newtoni (Osorio, 1891) from Sao Tome, and the eastern Atlantic/Mediterranean T. pavo (Linnaeus, 1758). Two western Atlantic species T. bifasciatum (Bloch, 1791) from the Caribbean and T. noronhanum (Boulenger, 1890) from Brazil served as outgroups. Tissues from a total of 132 individuals were sequenced. T. newtoni from Sao Tome preferentially grouped with the central Atlantic T. sanctaehelenae and T. ascensionis. T. pavo exhibits two distinct coloration patterns, one in the Cape Verde Islands and one in the eastern Atlantic Islands and Mediterranean. However, no genetic discontinuities between the Cape Verde Islands and the remaining samples or between Atlantic and Mediterranean individuals were found. Within Mediterranean populations of T. pavo, our data suggested the presence of a genetic break between eastern and western regions. C1 Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. Univ Naples 2, Dipartimento Sci Vita, I-81100 Caserta, Italy. Smithsonian Trop Res Inst, Balboa, Panama. Univ Lecce, CoNISMa, DiSTeBA, Lab Zool & Marine Biol, I-73100 Lecce, Italy. Univ Acores, Dept Oceanog & Pesca, Ctr IMAR, PT-99018862 Horta Azores, Portugal. Univ Algarve, Ctr Ciencias Mar, P-8000117 Faro, Portugal. Cornell Univ, Shoals Marine Lab, Ithaca, NY 14853 USA. Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. RP Bernardi, G (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, 100 Shaffer Rd, Santa Cruz, CA 95060 USA. EM bernardi@biology.ucsc.edu RI Stefanni, Sergio/A-5476-2009; Bernardi, Giacomo/F-6346-2011; OI Bernardi, Giacomo/0000-0002-8249-4678; Guidetti, Paolo/0000-0002-7983-8775 NR 28 TC 28 Z9 29 U1 1 U2 8 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 FEB PY 2004 VL 144 IS 2 BP 377 EP 383 DI 10.1007/s00227-003-1200-y PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 767WE UT WOS:000188496200018 ER PT J AU French, BM AF French, BM TI The importance of being cratered: The new role of meteorite impact as a normal geological process SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CRETACEOUS-TERTIARY BOUNDARY; SUDBURY IGNEOUS COMPLEX; INDUCED HYDROTHERMAL ACTIVITY; PRECAMBRIAN HAMERSLEY BASIN; PERMIAN-TRIASSIC BOUNDARY; BARBERTON MOUNTAIN LAND; ARCHEAN SPHERULE BEDS; TEKTITE STREWN FIELD; SOUTH-AFRICA; SHOCK METAMORPHISM AB This paper is a personal (and, in many ways, incomplete) view of the past development of impact geology and of the newly recognized importance of impact events in terrestrial geological history. It also identifies some exciting scientific challenges for future investigators: to determine the full range of impact effects preserved on the Earth, to apply the knowledge obtained from impact phenomena to more general geological problems, and to continue the merger of the once exotic field of impact geology with mainstream geosciences. Since the recognition of an impact event at the Cretaceous-Tertiary (K-T) boundary, much current activity in impact geology has been promoted by traditionally trained geoscientists who have unexpectedly encountered impact effects in the course of their work. Their studies have involved: 1) the recognition of additional major impact effects in the geological record (the Chesapeake Bay crater, the Alamo breccia, and multiple layers of impact spherules in Precambrian rocks); and 2) the use of impact structures as laboratories to study general geological processes (e.g., igneous petrogenesis at Sudbury, Canada and Archean crustal evolution at Vredefort, South Africa). Other research areas, in which impact studies could contribute to major geoscience problems in the future, include: 1) comparative studies between low-level (less than or equal to 7 GPa) shock deformation of quartz, and the production of quartz cleavage, in both impact and tectonic environments; and 2) the nature, origin, and significance of bulk organic carbon ("kerogen") and other carbon species in some impact structures (Gardnos, Norway, and Sudbury, Canada). C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP French, BM (reprint author), 7408 Wyndale Lane, Chevy Chase, MD 20815 USA. EM french.bevan@nmnh.si.edu NR 294 TC 21 Z9 23 U1 2 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD FEB PY 2004 VL 39 IS 2 BP 169 EP 197 PG 29 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 804XB UT WOS:000220330300002 ER PT J AU Uttley, P Taylor, RD McHardy, IM Page, MJ Mason, KO Lamer, G Fruscione, A AF Uttley, P Taylor, RD McHardy, IM Page, MJ Mason, KO Lamer, G Fruscione, A TI Complex X-ray spectral behaviour of NGC 4051 in the low flux state SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies : individual : NGC 4051; galaxies : Seyfert; X-rays : galaxies ID SEYFERT-1 GALAXY NGC-4051; CYGNUS X-1; NGC 4051; XMM-NEWTON; SOFT STATE; SWAN SONG; IRON LINE; VARIABILITY; MCG-6-30-15; NUCLEUS AB The narrow-line Seyfert 1 galaxy, NGC 4051, was observed in one of its prolonged low flux states by XMM-Newton in 2002 November. Here we present the results of an analysis of the European Photon Imaging Camera (EPIC) pn data obtained during the observation. Within the low state, the source shows complex spectral variability which cannot easily be explained by any simple model. However, by making a 'flux-flux' plot which combines the low state data with data obtained during a normal flux state, we demonstrate that the extremely hard spectrum observed above 2 keV results from a continuation of the spectral variability seen in the normal state, which is caused by spectral pivoting of the power-law continuum. The pivoting power law appears to be attached to a Comptonized thermal component of variable flux (blackbody temperature kT similar to 0.1 keV, consistent with the small black hole mass in NGC 4051) which dominates the soft X-ray band in the low state, and is probably the source of seed photons for Comptonization. Additional constant thermal and reflection components, together with absorption by ionized gas, seem to be required to complete the picture and explain the complex X-ray spectral variability seen in the low state of NGC 4051. C1 Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Uttley, P (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM pu@astro.soton.ac.uk NR 25 TC 34 Z9 34 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 FEB 1 PY 2004 VL 347 IS 4 BP 1345 EP 1356 DI 10.1111/j.1365-2966.2004.07321.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765VP UT WOS:000188305300035 ER PT J AU Paul, VJ Puglisi, MP AF Paul, VJ Puglisi, MP TI Chemical mediation of interactions among marine organisms SO NATURAL PRODUCT REPORTS LA English DT Review ID SPONGE APLYSINA-FISTULARIS; CARIBBEAN GORGONIAN CORALS; BROWN ALGAL PHLOROTANNINS; ANTARCTIC SOFT CORALS; PREDATORY REEF FISH; BIOLOGICALLY-ACTIVE METABOLITES; PARERYTHROPODIUM-FULVUM-FULVUM; SEAWEED SECONDARY METABOLITES; CYPHOMA-GIBBOSUM GASTROPODA; NORTHEASTERN PACIFIC KELPS AB This review covers the recent marine chemical ecology literature for macroalgae, sponges, octocorals and other benthic invertebrates; 332 references are cited. C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. Lake Erie Coll Osteopath Med, Sch Pharm, Erie, PA 16509 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. NR 330 TC 92 Z9 106 U1 0 U2 25 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0265-0568 EI 1460-4752 J9 NAT PROD REP JI Nat. Prod. Rep. PD FEB PY 2004 VL 21 IS 1 BP 189 EP 209 DI 10.1039/b302334f PG 21 WC Biochemistry & Molecular Biology; Chemistry, Medicinal; Chemistry, Organic SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy; Chemistry GA 803TP UT WOS:000220253700012 PM 15039843 ER PT J AU Thies, W Kalko, EKV AF Thies, W Kalko, EKV TI Phenology of neotropical pepper plants (Piperaceae) and their association with their main dispersers, two short-tailed fruit bats, Carollia perspicillata and C. castanea (Phyllostomidae) SO OIKOS LA English DT Review ID TROPICAL UNDERSTORY COMMUNITY; EATING BIRDS STAY; SEED DISPERSAL; COSTA-RICA; RAIN-FOREST; RESOURCE AVAILABILITY; FLOWERING PHENOLOGIES; ANT DISPERSAL; DRY FOREST; PATTERNS AB To relate differences in phenological strategies of a group of closely related plants to biotic (pollinators, dispersers) and abiotic (water, light) factors, we studied leafing, flowering, and fruiting phenology of 12 species of Piper (Piperaceae) in a neotropical lowland forest in Panama for 28 months. We asked how Piper may partition time and vertebrate frugivores to minimize possible competition for dispersal agents. Based on habitat preferences and physiological characteristics we discriminate between forest Piper species (eight species) and gap Piper species (four species). Forest Piper species flowered synchronously mostly at the end of the dry season. Gap Piper species had broader or multiple flowering peaks distributed throughout the year with a trend towards the wet season. Both groups of Piper species showed continuous fruit production. Fruiting peaks of forest Piper species were short and staggered. Gap Piper species had extended fruiting seasons with multiple or broad peaks. Both groups of Piper species also differed in their time of ripening and disperser spectrum. Forest Piper species ripened in late afternoon and had a narrow spectrum consisting mainly of two species of frugivorous bats: Carollia perspicillata and C. castanea (Phyllostomidae). Fruits of gap Piper species, in contrast, ripened early in the morning and were eaten by a broader range of diurnal and nocturnal visitors, including bats, birds, and ants. We conclude that the differences in flowering phenology of forest and gap Piper species are primarily caused by abiotic factors, particularly the availability of water and light, whereas differences in fruiting patterns are mostly influenced by biotic factors. The staggered fruiting pattern of forest Piper species may reflect competition for a limited spectrum of dispersers. The long and overlapping fruiting periods of gap Piper species are associated with a larger spectrum of dispersers and may be a strategy to overcome the difficulty of seed dispersal into spatially unpredictable germination sites with suitable light conditions. C1 Univ Tubingen, DE-72076 Tubingen, Germany. Univ Ulm, DE-89069 Ulm, Germany. Smithsonian Trop Res Inst, Balboa, Panama. RP Thies, W (reprint author), Univ Tubingen, Morgenstelle 28, DE-72076 Tubingen, Germany. EM elisabeth.kalko@biologie.uni-ulm.de NR 123 TC 102 Z9 112 U1 3 U2 30 PU BLACKWELL MUNKSGAARD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0030-1299 J9 OIKOS JI Oikos PD FEB PY 2004 VL 104 IS 2 BP 362 EP 376 DI 10.1111/j.0030-1299.2004.12747.x PG 15 WC Ecology SC Environmental Sciences & Ecology GA 772NV UT WOS:000188848900013 ER PT J AU Gahn, FJ Baumiller, TK AF Gahn, FJ Baumiller, TK TI A bootstrap analysis for comparative taphonomy, applied to Early Mississippian (Kinderhookian) crinoids from the Wassonville Cycle of Iowa SO PALAIOS LA English DT Article ID FUNCTIONAL-MORPHOLOGY; ECHINODERMATA; SHALE; DECAY AB Morphological and environmental taphonomic gradient analysis provides insights into morphological, behavioral, and environmental influences on the preservation of fossil organisms. This paper explores morphological and environmental taphonomic gradients in six crinoid morphotypes (diplobathrids, monobathrids, dichocrinids, plalycrinitids, cladids, and flexibles) from three stratigraphic units (the Maynes Creek Formation and the Starrs Cave and "Ollie" Members of the Wassonville Formation) representing distinct depositional environments along an onshore-offshore transect within the Early Mississippian (Kinder-hookian) Wassonville Cycle of southeast Iowa. Taphonomic differences in stalk, calyx, and arm disarticulation, calyx compression, and arm orientation were categorized independently and subjected to a non-parametric ranking test with bootstrapping (rather than a parametric approach, due to the non-additive nature of the data analyzed herein) to explore taphonomic patterns. The results suggest that the disarticulation of the stalk, calyx, and arms behave independently, although patterns of arm disarticulation may be influenced by the disarticulation of the calyx. In general, preservational integrity in fossil crinoids appears to be a function of the relative proportion of articular to non-articular surface area, skeletal innovations, tissue type and properties, survival response behavior, and thickness and rapidity of burial. Furthermore, these results demonstrate a general decrease in preservational integrity from onshore to offshore environments in the Wassonville Cycle and that sedimentation dynamics associated with episodic events are more influential than background deposition in determining preservation in fossil Lagerstatten. The methodology employed herein also could be used effectively to identify morphological, behavioral, and environmental taphonomic influences on other fossil organisms. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. Polish Acad Sci, Inst Paleobiol, PAN, PL-00818 Warsaw, Poland. Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. RP Gahn, FJ (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. EM gahn.forest@nmnh.si.edu RI Baumiller, Tomasz/C-3596-2012 NR 48 TC 12 Z9 15 U1 0 U2 2 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD FEB PY 2004 VL 19 IS 1 BP 17 EP 38 DI 10.1669/0883-1351(2004)019<0017:ABAFCT>2.0.CO;2 PG 22 WC Geology; Paleontology SC Geology; Paleontology GA 773VN UT WOS:000188945000003 ER PT J AU Marian, P Marian, TA Scutaru, H AF Marian, P Marian, TA Scutaru, H TI Distinguishability and nonclassicality of one-mode Gaussian states SO PHYSICAL REVIEW A LA English DT Article ID MIXED QUANTUM STATES; THERMAL NOISE; RADIATION-FIELD; SQUEEZED STATES; DISTANCE; COHERENT; CLASSICALITY; ENTANGLEMENT; DESTRUCTION; FIDELITY AB We consider the class of the one-mode Gaussian states of the quantum radiation field. The relative entropy of such a state with respect to a similar one is derived. We analyze the entropic amount of nonclassicality of a Gaussian state defined as the minimal relative entropy of any classical Gaussian state with respect to it. A similar quantity built with the Hilbert-Schmidt distance is also calculated. Both nonclassicality measures are then compared with the Bures-metric degree of nonclassicality evaluated previously. The properties of the closest classical Gaussian state, as well as the decrease of the nonclassicality under thermal noise mappings are carefully examined in each case. For mixed states we find that only the Bures-distance amount of nonclassicality is equivalent to the nonclassical depth. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. Univ Bucharest, Dept Chem, R-030018 Bucharest, Romania. Univ Bucharest, Dept Phys, R-077125 Bucharest, Romania. Romanian Acad, Ctr Adv Studies Phys, R-050711 Bucharest, Romania. RP Marian, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. NR 41 TC 21 Z9 21 U1 1 U2 4 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 FEB PY 2004 VL 69 IS 2 AR 022104 DI 10.1103/PhysRevA.69.022104 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 780MZ UT WOS:000189386300013 ER PT J AU Vrinceanu, D Kotochigova, S Sadeghpour, HR AF Vrinceanu, D Kotochigova, S Sadeghpour, HR TI Pressure broadening and shift of He(2 P-3(0,1,2))-He(2 S-3) lines SO PHYSICAL REVIEW A LA English DT Article ID DENSITY-MATRIX; CROSS-SECTIONS; REDISTRIBUTION; FORMULATION; COLLISIONS; INTERVAL; HELIUM AB The collisional broadening and shift of metastable helium fine-structure lines are calculated within the impact approximation. Ab initio Born-Oppenheimer potential energy curves correlating to He(1 S-1(0)) and He(2 P-3(j)) atomic levels are obtained using the configuration interaction valence bond method and combined with semiempirically calculated van der Waals interaction terms between these atoms to also study j-specific and j-changing collisions. A long-range van der Waals potential well exists in the (3)Pi(u) potential correlated to the He(1 S-1(0))+He(2 P-3(j)) limit, whose influence on the scattering phase shift is assessed. At T=310 K, the broadening and shift parameters are practically j independent and have average values of 12.60 and 1.87 MHz/Torr, respectively. The j-changing collisions have cross sections roughly five times smaller than the j-specific cross sections. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. NR 37 TC 16 Z9 16 U1 1 U2 6 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 FEB PY 2004 VL 69 IS 2 AR 022714 DI 10.1103/PhysRevA.69.022714 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 780MZ UT WOS:000189386300073 ER PT J AU Lokvam, J Coley, PD Kursar, TA AF Lokvam, J Coley, PD Kursar, TA TI Cinnamoyl glucosides of catechin and dimeric procyanidins from young leaves of Inga umbellifera (Fabaceae) SO PHYTOCHEMISTRY LA English DT Article DE Inga umbellifera; Fabaceae; young leaf secondary chemistry; acetylated flavan-3-ol glycoside; acetylated procyanidin glycoside; cinnamoyl glycoside ID GLYCOSIDE; TANNINS; FLAVAN-3-OLS; BARK AB The rapidly growing, nearly achlorophyllous, young leaves of Inga umbellifera express high concentrations of mono and dimeric 3-O-gluco-cinnamoyl catechin/epicatechin, rare forms of substituted flavan-3-ols. Here we present structures for five novel compounds in this class: three monomers [catechin-3-O-beta-D-gluco(2-cinnamoyl)pyranoside, catechin-3-O-beta-D-gluco(6-cinnamoyl) pyranoside, catechin-3-O-beta-D-gluco(2,6-biscinnamoyl)pyranoside] and two dimeric procyanidins [catechin-3-O-beta-D-glucopyrano(4alpha-->8)-catechin-3-O-beta-D-gluco(2-cinnamoyl)pyranoside and catechin-3-O-beta-D-glucopyrano-(4alpha-->8)-epicatechin-3-O-beta-D-gluco(6-cinnamoyl)pyranoside]. The young leaves of Inga umbellifera express high concentrations of 3-O-(cinnamoyl)glucosides of catechin and epicatechin. (C) 2004 Elsevier Ltd. All rights reserved. C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Lokvam, J (reprint author), Univ Utah, Dept Biol, 257 S 1400 E, Salt Lake City, UT 84112 USA. EM lokvam@biology.utah.edu NR 20 TC 23 Z9 24 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0031-9422 J9 PHYTOCHEMISTRY JI Phytochemistry PD FEB PY 2004 VL 65 IS 3 BP 351 EP 358 DI 10.1016/j.phytochem.2003.11.012 PG 8 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA 773JX UT WOS:000188921600010 PM 14751307 ER PT J AU Bromm, V AF Bromm, V TI The first sources of light SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Review ID INITIAL MASS FUNCTION; POPULATION-III STARS; MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; PRIMORDIAL GAS CLOUDS; HIGH-REDSHIFT UNIVERSE; EARLY METAL ENRICHMENT; COLD DARK-MATTER; GAMMA-RAY BURSTS; 1ST STARS AB I review recent progress in understanding the formation of the first stars and quasars. The initial conditions for their emergence are given by the now firmly established model of cosmological structure formation. Numerical simulations of the collapse and fragmentation of primordial gas indicate that the first stars formed at redshifts z similar or equal to 20-30 and that they were predominantly very massive, with M-* greater than or similar to 100 M-circle dot. Important uncertainties, however, remain. Paramount among them is the accretion process, which builds up the final stellar mass by incorporating part of the diffuse, dust-free envelope into the central protostellar core. The first quasars, on the other hand, are predicted to have formed later on, at z similar to 10, in more massive dark matter halos, with total masses similar to10(8) M-circle dot, characteristic of dwarf galaxies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bromm, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vbromm@cfa.harvard.edu NR 138 TC 21 Z9 21 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 FEB PY 2004 VL 116 IS 816 BP 103 EP 114 DI 10.1086/381304 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 770TD UT WOS:000188746200001 ER PT J AU Clarke, GKC Leverington, DW Teller, JT Dyke, AS AF Clarke, GKC Leverington, DW Teller, JT Dyke, AS TI Paleohydraulics of the last outburst flood from glacial Lake Agassiz and the 8200 BP cold event SO QUATERNARY SCIENCE REVIEWS LA English DT Article ID LAURENTIDE ICE-SHEET; C-14 YR BP; CLIMATE-CHANGE; HUDSON STRAIT; DEGLACIATION; JOKULHLAUPS; VOLUME; ICELAND; EUROPE; RUNOFF AB During the last deglaciation of North America, huge proglacial lakes formed along the southern margin of the Laurentide Ice Sheet. The largest of these was glacial Lake Agassiz, which formed about 11.7 C-14 kyr and drained into Hudson Bay about 7.7 C-14 kyr (8.45 cal kyr). Overflow from these lakes was variably directed to the Mississippi, St. Lawrence and Mackenzie drainage systems and it is thought that switches in routing were accompanied by a response in ocean circulation that produced abrupt climate events. When the ice dam across Hudson Bay finally was breached, a massive flood drained Lake Agassiz, which was routed through Hudson Strait to the Labrador Sea. In terms of stored water volume the largest reservoir was associated with the Kinojevis level of Lake Agassiz. For this maximum filling, the impounded water volume available to produce floods is estimated as 40,000-151,000 km(3), depending on the location of the ice margin and route used. The timing of this rapid release of stored freshwater just precedes the early Holocene cooling event at 8.2 cal kyr BP. We use the Spring-Hutter theory to simulate flood hydrographs for floods that originate in subglacial drainage conduits and find that flood magnitude and duration are similar to5 Sv and similar to0.5 yr. Multiple fillings and floods are possible as are single floods having a complex multipulse structure. Modelling results suggest that the outburst flood from Lake Agassiz may have terminated before the lake surface elevation dropped to sea level and that the flood ended when a stable drainage channel was established, connecting Lake Agassiz to the Tyrrell Sea. (C) 2003 Elsevier Ltd. All rights reserved. C1 Univ British Columbia, Vancouver, BC V6T 1Z4, Canada. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. Geol Survey Canada, Terrain Sci Div, Ottawa, ON K1A 0E8, Canada. RP Clarke, GKC (reprint author), Univ British Columbia, 6339 Stores Rd,219 Main Mall, Vancouver, BC V6T 1Z4, Canada. EM clarke@eos.ubc.ca NR 76 TC 157 Z9 161 U1 6 U2 45 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD FEB PY 2004 VL 23 IS 3-4 BP 389 EP 407 DI 10.1016/j.quascirev.2003.06.004 PG 19 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 778HC UT WOS:000189232700010 ER PT J AU Ricklefs, RE Fallon, SM Bermingham, E AF Ricklefs, RE Fallon, SM Bermingham, E TI Evolutionary relationships, cospeciation, and host switching in avian malaria parasites SO SYSTEMATIC BIOLOGY LA English DT Article DE avian malaria; component; cospeciation; cytochrome b; Haemoproteus; host-parasite relationships; ParaFit; phylogeny; plasmodium; speciation; TreeFitter ID SYMPATRIC SPECIATION; PHYLOGENETIC-RELATIONSHIPS; PLASMODIUM-ELONGATUM; BLOOD PARASITES; GENE-SEQUENCES; CYTOCHROME-B; BIRDS; COEVOLUTION; HAEMOPROTEUS; FLORIDA AB We used phylogenetic analyses of cytochrome b sequences of malaria parasites and their avian hosts to assess the coevolutionary relationships between host and parasite lineages. Many lineages of avian malaria parasites have broad host distributions, which tend to obscure cospeciation events. The hosts of a single parasite or of closely related parasites were nonetheless most frequently recovered from members of the same host taxonomic family, more so than expected by chance. However, global assessments of the relationship between parasite and host phylogenetic trees, using Component and ParaFit, failed to detect significant cospeciation. The event-based approach employed by TreeFitter revealed significant cospeciation and duplication with certain cost assignments for these events, but host switching was consistently more prominent in matching the parasite tree to the host tree. The absence of a global cospeciation signal despite conservative host distribution most likely reflects relatively frequent acquisition of new hosts by individual parasite lineages. Understanding these processes will require a more refined species concept for malaria parasites and more extensive sampling of parasite distributions across hosts. If parasites can disperse between allopatric host populations through alternative hosts, cospeciation may not have a strong influence on the architecture of host - parasite relationships. Rather, parasite speciation may happen more often in conjunction with the acquisition of new hosts followed by divergent selection between host lineages in sympatry. Detailed studies of the phylogeographic distributions of hosts and parasites are needed to characterize these events. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Smithsonian Trop Res Inst, Balboa, Panama. RP Ricklefs, RE (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA. EM ricklefs@umsl.edu NR 69 TC 157 Z9 159 U1 3 U2 44 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD FEB PY 2004 VL 53 IS 1 BP 111 EP 119 DI 10.1080/10635150490264987 PG 9 WC Evolutionary Biology SC Evolutionary Biology GA 773JC UT WOS:000188895000010 PM 14965906 ER PT J AU Barkley, TM DePriest, P Funk, V Kiger, RW Kress, WJ Moore, G AF Barkley, TM DePriest, P Funk, V Kiger, RW Kress, WJ Moore, G TI Linnaean nomenclature in the 21(st) Century: a report from a workshop on integrating traditional nomenclature and phylogenetic classification SO TAXON LA English DT Article AB As a follow-up to the 2001 Smithsonian Botanical Symposium, in late June of 2002 a group of 15 taxonomists took part in a Workshop entitled "Linnaean Nomenclature in the 21(st) Century" at the Hunt Institute for Botanical Documentation in Pittsburgh to discuss integrating phylogenetic information into the current systems of naming plants, animals, and microorganisms. The Hunt Group included a diversity of taxonomists, including traditional and phylogenetic practitioners as well as authorities on the current codes and end-users of nomenclatural rules. The discussion ranged from identifying problems and possible solutions to devising strategies for implementing change. It was concluded that the central problems revolve around the concepts of (1) circumscribing taxa, (2) hierarchical ranking, and (3) the use of binomials. In a critical article-by-article examination of the current edition of the International Code of Botanical Nomenclature it was found that only 14 of the total 62 articles (plus appendices) are relevant to whether or not classification is phylogenetic. Furthermore, each of these potentially problematic articles is either amenable to conveying phylogenetic information or neutral to phylogenetic considerations. There is nothing in the current Linnaean nomenclature that prevents cladistic information from being incorporated into the naming procedure. We suggest that a major effort is needed to educate the botanical community as well as lay persons on the implications and use of these pertinent articles in phylogenetic nomenclature. C1 Natl Museum Nat Hist, US Natl Herbarium, Smithsonian Inst, Washington, DC 20013 USA. Bot Res Inst Texas, Ft Worth, TX 76102 USA. Carnegie Mellon Univ, Hunt Inst Bot Documentat, Pittsburgh, PA 15213 USA. Brooklyn Bot Garden, Brooklyn, NY 11225 USA. RP Kress, WJ (reprint author), Natl Museum Nat Hist, US Natl Herbarium, Smithsonian Inst, POB 37012,MRC-166, Washington, DC 20013 USA. EM rkiger@andrew.cmu.edu; kress.john@nmnh.si.edu RI DePriest, Paula/K-6633-2015 NR 3 TC 12 Z9 13 U1 0 U2 4 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD FEB PY 2004 VL 53 IS 1 BP 153 EP 158 DI 10.2307/4135501 PG 6 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 804FJ UT WOS:000220284300019 ER PT J AU Barkley, TM DePriest, P Funk, V Kiger, RW Kress, WJ McNeill, J Moore, G Nicolson, DH Stevenson, DW Wheeler, QD AF Barkley, TM DePriest, P Funk, V Kiger, RW Kress, WJ McNeill, J Moore, G Nicolson, DH Stevenson, DW Wheeler, QD TI A review of the International Code of Botanical Nomenclature with respect to its compatibility with phylogenetic classification SO TAXON LA English DT Editorial Material C1 Brooklyn Bot Garden, Brooklyn, NY 11225 USA. Bot Res Inst Texas, Ft Worth, TX 76102 USA. Natl Museum Nat Hist, US Natl Herbarium, Smithsonian Inst, Washington, DC 20013 USA. Carnegie Mellon Univ, Hunt Inst Bot Documentat, Pittsburgh, PA 15213 USA. Royal Bot Gardens, Edinburgh EH3 5LR, Midlothian, Scotland. New York Bot Garden, Bronx, NY 10458 USA. Natl Sci Fdn, Div Environm Biol, Arlington, VA 22230 USA. RP Barkley, TM (reprint author), Brooklyn Bot Garden, 1000 Washington Ave, Brooklyn, NY 11225 USA. EM barkley@brit.org; depriest.paula@nmnh.si.edu; junk.vicki@nmnh.si.edu; rkiger@andrew.emu.edu; kress.john@nmnh.si.edu; jmcneill@rbge.org.uk; gerrymoore@bbg.org; nicolson.dan@nmnh.si.edu; dws@nybg.org; qwheeler@nsf.gov RI DePriest, Paula/K-6633-2015 NR 3 TC 9 Z9 9 U1 0 U2 4 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD FEB PY 2004 VL 53 IS 1 BP 159 EP 161 DI 10.2307/4135502 PG 3 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 804FJ UT WOS:000220284300020 ER PT J AU Chernova, OF Hoffmann, RS AF Chernova, OF Hoffmann, RS TI A comparative study of thin structure of Tenrec spines (Mammalia, Tenrecidae) SO ZOOLOGICHESKY ZHURNAL LA Russian DT Article ID INSECTIVORA ERINACEIDAE; ACICULAR INTEGUMENT; TRANSFORMATION; RODENTIA AB The architectonics of tenrec (Tenrecidae) spines has a convergent similarity to that in porcupine (Erethizontidae) quills and is also species specific. Like in Erethizontidae species, in tenrecs of the genus Hemicentetes using the tactics of active front defense, defensive spines of the trunk and crown fan are covered with an inverted cuticle, which serves as a particular harpoon. In Echinops and Setifer tenrecs using the tactics of passive defense (they can roll into a ball), spines of the trunk have no such cuticle. Spines of the stridulation organ in Hemicentetes are specialized to produce ultrasonic sounds due to rubbing against each other, and the spine structure reflects this peculiarity. The cuticle of trunk spines in Echipops telfairi is unique. C1 Russian Acad Sci, Severtsov Inst Ecol & Evolut, Moscow 119071, Russia. Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Chernova, OF (reprint author), Russian Acad Sci, Severtsov Inst Ecol & Evolut, Moscow 119071, Russia. EM chernova_o@sevin.ru; hoffmann.robert@NMNH.SI.EDU NR 24 TC 0 Z9 0 U1 17 U2 54 PU MEZHDUNARODNAYA KNIGA PI MOSCOW PA 39 DIMITROVA UL., 113095 MOSCOW, RUSSIA SN 0044-5134 J9 ZOOL ZH JI Zool. Zhurnal PD FEB PY 2004 VL 83 IS 2 BP 159 EP 165 PG 7 WC Zoology SC Zoology GA 806OF UT WOS:000220442500002 ER PT J AU Dietsch, TV Philpott, SM Rice, RA Greenberg, R Bichier, P AF Dietsch, TV Philpott, SM Rice, RA Greenberg, R Bichier, P TI Conservation policy in coffee landscapes SO SCIENCE LA English DT Letter C1 Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Dietsch, TV (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk,3001Connecticut Ave NW, Washington, DC 20008 USA. RI Philpott, Stacy/F-2330-2011 NR 7 TC 19 Z9 19 U1 0 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 JAN 30 PY 2004 VL 303 IS 5658 BP 625 EP 625 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 768EN UT WOS:000188530800015 PM 14752143 ER PT J AU Lapointe, BE Barile, PJ Yentsch, CS Littler, MM Littler, DS Kakuk, B AF Lapointe, BE Barile, PJ Yentsch, CS Littler, MM Littler, DS Kakuk, B TI The relative importance of nutrient enrichment and herbivory on macroalgal communities near Norman's Pond Cay, Exumas Cays, Bahamas: a "natural" enrichment experiment SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE nitrogen; phosphorus; herbivores; macroalgae; coral; groundwater ID CORAL-REEF MACROALGAE; GRACILARIA-TIKVAHIAE; FLORIDA KEYS; STROMBUS-GIGAS; SEAGRASS MEADOWS; STANDING CROP; BARRIER-REEF; PHASE-SHIFTS; NITROGEN; GROWTH AB The simultaneous effects of grazing and nutrient enrichment on macroalgal communities were experimentally investigated using plastic mesh enclosure/exclosure cages along a natural nutrient (DIN, SPP) gradient from the discharge of a tidal mangrove creek on the west side of Norman's Pond Cay, Exumas Cays, Bahamas. Nutrient enrichment was the only factor affecting total biomass of macroalgae whereas selective herbivory moderated species composition. Biomass ranged from >2 kg dry weight m(-2) at the DIN-enriched Waterfall to < 600 g dry weight m(-2) in the DIN-limited Algal Halo. Grazing by the queen conch Strombus gigas and the sea hare Aplysia dactylomela significantly reduced biomass of the epiphyte Laurencia intricata, but not its host Digenea simplex at the DIN-enriched Waterfall. These two rhodophytes dominated the macroalgal community at the DIN-enriched Waterfall and inner Algal Halo, whereas the chlorophytes Microdictyon marinum and Cladophora catenata dominated the relatively DIN-depleted outer Algal Halo. Higher grazing rates by S. gigas, A. dactylomela, and juvenile parrotfish and surgeonfish at the DIN-enriched Waterfall compared to the more oligotrophic Algal Halo suggested selective grazing on higher quality (nitrogen) diets by these herbivores. A pronounced increase in the carbon/nitrogen (C:N) ratios of D. simplex and L. intricata from the Water-fall to the Algal Halo indicated increased DIN-limitation of growth in the more offshore, lower DIN macroalgal communities. In contrast, only modest increases in C:N ratios of M. marinum and C. catenata between the Water-fall and Algal Halo suggested that these species are better adapted to growth in reef environments with lower levels of DIN enrichment. Low coral cover (<2%) co-occurred with high macroalgal cover (>35%) at DIN-enriched reef sites around Norman's Pond Cay (Waterfall, Patch Reef, North Perry Reef) compared to relatively high coral cover (10-20%) and low macroalgal cover (<20%) at the lower DIN reef sites (Rainbow Reef, Lang's Reef). These results support ecological theory that bottom-up control via nutrient enrichment is a primary factor regulating overall biomass and taxonomic assemblages of macroalgae on coral reefs, whereas grazing is more important in controlling relative species composition via dietary preferences. (C) 2003 Elsevier B.V. All rights reserved. C1 Harbor Branch Oceanog Inst Inc, Div Marine Sci, Ft Pierce, FL 34946 USA. Bigelow Lab Ocean Sci, Boothbay Harbor, ME 04575 USA. Natl Museum Nat Hist, Dept Syst Biol, Smithsonian Inst, Washington, DC 20560 USA. Caribbean Marine Res Ctr, Exumas Cays, Bahamas. RP Lapointe, BE (reprint author), Harbor Branch Oceanog Inst Inc, Div Marine Sci, 5600 US 1 N, Ft Pierce, FL 34946 USA. EM lapointe@hboi.edu NR 62 TC 64 Z9 67 U1 5 U2 40 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 JAN 28 PY 2004 VL 298 IS 2 BP 275 EP 301 DI 10.1016/S0022-0981(03)00363-0 PG 27 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 771HV UT WOS:000188780300008 ER PT J AU Dorta, E Diaz-Marrero, AR Cueto, M D'Croz, L Mate, JL San-Martin, A Darias, J AF Dorta, E Diaz-Marrero, AR Cueto, M D'Croz, L Mate, JL San-Martin, A Darias, J TI Unusual chlorinated pregnanes from the eastern Pacific octocoral Carijoa multiflora SO TETRAHEDRON LETTERS LA English DT Article DE halogenated metabolites; steroids; octocorals ID SCLERACTINIAN CORAL; XESTOSPONGIA SP; SOFT CORALS; STEROIDS; SPONGE; DERIVATIVES; GLYCOSIDES AB Two unique chloro-pregnane steroids have been isolated from the eastern Pacific octocoral Carijoa multiflora and their structures and stereochemistries were determined on the basis of spectral studies and molecular mechanics calculations. (C) 2003 Elsevier Ltd. All rights reserved. C1 CSIC, Inst Prod Nat & Agrobiol, Tenerife 38206, Spain. Smithsonian Trop Res Inst, Balboa, Panama. Estafeta Univ, Dept Biol Marina & Limnol, Panama City, Panama. Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. Univ Chile, Fac Ciencias, Dept Quim, Santiago, Chile. RP Darias, J (reprint author), CSIC, Inst Prod Nat & Agrobiol, Avda Astrofis F Sanchez,3,Apdo 195, Tenerife 38206, Spain. EM jdarias@ipna.csic.es RI Diaz-Marrero, Ana/L-2899-2014; Cueto, MERCEDES/L-3185-2014 OI Diaz-Marrero, Ana/0000-0002-8886-7519; Cueto, MERCEDES/0000-0002-9112-6877 NR 24 TC 17 Z9 17 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0040-4039 J9 TETRAHEDRON LETT JI Tetrahedron Lett. PD JAN 26 PY 2004 VL 45 IS 5 BP 915 EP 918 DI 10.1016/j.tetlet.2003.11.113 PG 4 WC Chemistry, Organic SC Chemistry GA 766MP UT WOS:000188380400005 ER PT J AU Astrakharchik, GE Blume, D Giorgini, S Granger, BE AF Astrakharchik, GE Blume, D Giorgini, S Granger, BE TI Quasi-one-dimensional Bose gases with a large scattering length SO PHYSICAL REVIEW LETTERS LA English DT Article ID IMPENETRABLE BOSONS; MONTE-CARLO; CONDENSATE AB Bose gases confined in highly elongated harmonic traps are investigated over a wide range of interaction strengths using quantum Monte Carlo techniques. We find that the properties of a Bose gas under tight transverse confinement are well reproduced by a 1D model Hamiltonian with contact interactions. We point out the existence of a unitary regime, where the properties of the quasi-1D Bose gas become independent of the actual value of the 3D scattering length a(3D). In this unitary regime, the energy of the system is well described by a hard-rod equation of state. We investigate the stability of quasi-1D Bose gases with positive and negative a(3D). C1 Univ Trent, Dipartimento Fis, I-38050 Povo, Italy. BEC, INFM, I-38050 Povo, Italy. Inst Spect, Troitsk 142190, Moscow Region, Russia. Washington State Univ, Dept Phys, Pullman, WA 99164 USA. Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Astrakharchik, GE (reprint author), Univ Trent, Dipartimento Fis, I-38050 Povo, Italy. RI Astrakharchik, Gregory/L-6181-2014 OI Astrakharchik, Gregory/0000-0003-0394-8094 NR 24 TC 53 Z9 53 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JAN 23 PY 2004 VL 92 IS 3 AR 030402 DI 10.1103/PhysRevLett.92.030402 PG 4 WC Physics, Multidisciplinary SC Physics GA 766TZ UT WOS:000188392800002 PM 14753852 ER PT J AU Kaaret, P AF Kaaret, P TI X-ray clues to viability of loop quantum gravity SO NATURE LA English DT Letter ID CRAB-NEBULA; POLARIZATION C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaaret, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 8 Z9 8 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 22 PY 2004 VL 427 IS 6972 BP 287 EP 287 DI 10.1038/427287b PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 765KE UT WOS:000188266200015 PM 14737141 ER PT J AU Weinberg, DH Dave, R Katz, N Hernquist, L AF Weinberg, DH Dave, R Katz, N Hernquist, L TI Galaxy clustering and galaxy bias in a Lambda CDM universe SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology : theory; galaxies : formation; large-scale structure of universe; methods : numerical ID DIGITAL SKY SURVEY; COLD DARK-MATTER; LARGE-SCALE STRUCTURE; LY-ALPHA FOREST; PAIRWISE VELOCITY DISPERSION; HALO OCCUPATION DISTRIBUTION; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; HUBBLE DEEP FIELD; POWER SPECTRUM AB We investigate galaxy clustering and the correlations between galaxies and mass in the LambdaCDM cosmological model (inflationary cold dark matter with Omegam = 0.4, Omega(Lambda) = 0.65, h = 0.65, n = 0.95, and sigma(8) = 0.8), using a large, smoothed particle hydrodynamics simulation (SPH; with 2 x 144(3) particles in a 50 h(-1) Mpc cube). Simulated galaxies can be unambiguously identified as clumps of stars and cold gas a few kpc to a few tens of kpc across, residing in extended halos of hot gas and dark matter; the space density of the resolved galaxy population at z = 0 corresponds to that of observed galaxies with luminosity L greater than or similar to L-*/4. We investigate the galaxy correlation function, the pairwise velocity dispersion and mean pairwise velocity, and the second and third moments of counts in cells; we also investigate the galaxy-mass correlation function and the average extended mass distributions around galaxies, both of which can be measured via galaxy-galaxy lensing. For the most part, the predicted biases between galaxies and dark matter lead to good agreement with current observations, including (1) a nearly constant comoving correlation length from z = 3 to 0 for mass-selected galaxy samples of constant comoving space density; (2) an rms bias factor b(sigma) approximate to 1 at z = 0; (3) a scale-dependent bias on small scales that transforms the curved dark matter correlation function into a nearly power-law galaxy correlation function; (4) galaxy pairwise dispersion and hierarchical skewness ratio S-3 in good agreement with observed values, lower than values for the dark matter by similar to20%; (5) a ratio of galaxy-galaxy to galaxy-mass correlation functions consistent with recent measurements from the Red Cluster Sequence survey; and (6) a mean excess mass DeltaM(260 h(-1) kpc) approximately proportional to galaxy baryon mass M-b, in agreement with estimates from the Sloan Digital Sky Survey (SDSS). All these clustering properties vary with galaxy baryon mass and, more strongly, with the age of a galaxy's stellar population. The predicted dependences are in good qualitative agreement with the observed dependence of galaxy clustering and the galaxy-mass correlation function on galaxy type. The predicted ratio DeltaM(260 h(-1) kpc)/M-b is lower than the SDSS estimates by a factor of similar to1.5-3 for galaxies with M-b greater than or similar to 2 x 10(11) M-circle dot. A test with a higher resolution (smaller volume) simulation suggests that this discrepancy is largely a numerical artifact; if so, then the SDSS weak-lensing comparison leaves limited room for feedback or other astrophysical processes to reduce the stellar masses of luminous galaxies, at least given our adopted cosmological parameters. On the whole, our results show that the DeltaCDM model and the galaxy formation physics incorporated in the SPH simulation give a good account of observed galaxy clustering, but anticipated improvements in clustering and weak-lensing measurements will soon test this picture in much greater detail. C1 Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM dhw@astronomy.ohio-state.edu; rad@as.arizona.edu; nsk@kaka.astro.umass.edu; lars@cfa.harvard.edu NR 151 TC 80 Z9 81 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2004 VL 601 IS 1 BP 1 EP 21 DI 10.1086/380481 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600001 ER PT J AU Krawczynski, H Hughes, SB Horan, D Aharonian, F Aller, MF Aller, H Boltwood, P Buckley, J Coppi, P Fossati, G Gotting, N Holder, J Horns, D Kurtanidze, OM Marscher, AP Nikolashvili, M Remillard, RA Sadun, A Schroder, M AF Krawczynski, H Hughes, SB Horan, D Aharonian, F Aller, MF Aller, H Boltwood, P Buckley, J Coppi, P Fossati, G Gotting, N Holder, J Horns, D Kurtanidze, OM Marscher, AP Nikolashvili, M Remillard, RA Sadun, A Schroder, M TI Multiwavelength observations of strong flares from the TeV blazar 1ES 1959+650 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects : individual (1ES 1959+650); galaxies : jets; gamma rays : observations ID CHERENKOV TELESCOPE SYSTEM; BL-LACERTAE OBJECTS; ENERGY GAMMA-RAYS; ACTIVE GALAXY MARKARIAN-421; SIMULTANEOUS X-RAY; LAC OBJECTS; SPECTRAL VARIABILITY; COMPTON EMISSION; TIMING EXPLORER; 4.85 GHZ AB Following the detection of strong TeV gamma-ray flares from the BL Lac object 1ES 1959+650 with theWhipple 10 m Cerenkov telescope on 2002 May 16 and 17, we performed intensive target of opportunity radio, optical, X-ray, and TeV gamma-ray observations from 2002 May 18 to August 14. Observations with the X-ray telescope Rossi X-Ray Timing Explorer and the Whipple and HEGRA gamma-ray telescopes revealed several strong flares, enabling us to sensitively test the X-ray-gamma-ray flux correlation properties. Although the X-ray and gamma-ray fluxes seemed to be correlated in general, we found an "orphan'' gamma-ray flare that was not accompanied by an X-ray flare. While we detected optical flux variability with the Boltwood and Abastumani observatories, the data did not give evidence for a correlation of the optical flux variability with the observed X-ray and gamma-ray flares. Within statistical errors of about 0.03 Jy at 14.5 GHz and 0.05 Jy at 4.8 GHz, the radio fluxes measured with the University of Michigan Radio Astronomy Observatory stayed constant throughout the campaign; the mean values agreed well with the values measured on 2002 May 7 and June 7 at 4.9 and 15 GHz with the Very Large Array and at 4.8 GHz with archival flux measurements. After describing in detail the radio, optical, X-ray and gamma-ray light curves, and spectral energy distributions (SEDs), we present initial modeling of the SED with a simple synchrotron self-Compton model. With the addition of another TeV blazar with good broadband data, we consider the set of all TeV blazars, to begin to look for a connection of the jet properties to the properties of the central accreting black hole thought to drive the jet. Remarkably, the temporal and spectral X-ray and gamma-ray emission characteristics of TeV blazars are very similar, even though the mass estimates of their central black holes differ by up to 1 order of magnitude. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. Yale Univ, New Haven, CT 06520 USA. Rice Univ, Houston, TX 77005 USA. Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany. Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England. Abastumani Astrophys Observ, GE-383762 Abastumani, Rep of Georgia. Landessternwarte Heidelberg Konigstuhl, Heidelberg, Germany. Astrophys Inst Potsdam, Potsdam, Germany. Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Colorado, Dept Phys, Denver, CO 80217 USA. RP Krawczynski, H (reprint author), Washington Univ, Dept Phys, 1 Brookings Dr,CB 1105, St Louis, MO 63130 USA. RI Fossati, Giovanni/A-5841-2009; Horns, Dieter/C-9727-2011; Kurtanidze, Omar/J-6237-2014 NR 63 TC 206 Z9 206 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 JAN 20 PY 2004 VL 601 IS 1 BP 151 EP 164 DI 10.1086/380393 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600014 ER PT J AU McNamara, BR Wise, MW Murray, SS AF McNamara, BR Wise, MW Murray, SS TI The insignificance of global reheating in the A1068 cluster: Multiwavelength analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general ID COOLING-FLOW CLUSTERS; RAY LUMINOUS CLUSTERS; EMISSION-LINE NEBULAE; INTRACLUSTER MEDIUM; RADIO-SOURCES; MOLECULAR-HYDROGEN; ELLIPTIC GALAXIES; STAR-FORMATION; THERMAL CONDUCTION; SURFACE PHOTOMETRY AB In this paper and in a companion paper by Wise, McNamara, & Murray, we present a detailed, multi-wavelength study of the A1068 galaxy cluster, and we use this data to test cooling and energy feedback models of galaxy clusters. Near-ultraviolet and infrared images of the cluster show that the cD galaxy is experiencing star formation at a rate of similar to20-70 M-circle dot yr(-1) over the past less than or similar to100 Myr. The dusty starburst is concentrated toward the nucleus of the cD galaxy and in filamentary structures projecting 60 kpc into its halo. The Chandra X-ray image presented in Wise, McNamara, & Murray reveals a steep temperature gradient that drops from roughly 4.8 keV beyond 120 kpc to roughly 2.3 keV in the inner 10 kpc of the galaxy, where the starburst peaks. Over 95% of the ultraviolet and Halpha photons associated with the starburst are emerging from regions cloaked in keV gas with very short cooling times (similar to100 Myr), as would be expected from star formation fueled by cooling condensations in the intracluster medium. However, the Chandra spectrum is consistent with but does not require cooling at a rate of 114-145 M-circle dot yr(-1), factors of several below the rates found with the ROSAT observatory. The local cooling rate in the vicinity of the central starburst is less than or similar to40M(circle dot) yr(-1), which is consistent with the star formation rate determined with U-band and infrared data. We consider energy feedback into the intracluster medium by the radio source, heat conduction, and supernova explosions associated with the starburst. We find that energy feedback from both the radio source and thermal conduction are inconsequential in A1068. Although supernova explosions associated with the starburst may be able to retard cooling in the inner 10 kpc of the cluster by similar to18% or so, they are incapable of maintaining the cooling gas at keV temperatures. Therefore, it is plausible that the star formation in A1068 is being fueled by the cooling intracluster medium. Finally, we present circumstantial evidence for the contrary view that at least some and perhaps all of the star formation may have been fueled by an interaction between the cD and one or more companion galaxies. C1 Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McNamara, BR (reprint author), Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. EM mcnamarb@ohio.edu; wise@space.mit.edu; ssm@head-cfa.harvard.edu NR 70 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 JAN 20 PY 2004 VL 601 IS 1 BP 173 EP 183 DI 10.1086/380114 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600016 ER PT J AU Wise, MW McNamara, BR Murray, SS AF Wise, MW McNamara, BR Murray, SS TI The insignificance of global reheating in the A1068 cluster: X-ray analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : elliptical and lenticular, cD; intergalactic medium; X-rays : galaxies ID COOLING FLOW GALAXIES; INTRACLUSTER MEDIUM; MOLECULAR-HYDROGEN; HIGH-RESOLUTION; STAR-FORMATION; BETA-MODEL; HYDRA-A; CHANDRA; CONDUCTION; GAS AB We report on a Chandra observation of the massive, medium redshift (z = 0.1386) cooling flow cluster A1068. We detect a clear temperature gradient in the X-ray-emitting gas from kT similar to 5 keV in the outer part of the cluster down to roughly 2 keV in the core and a striking increase in the metallicity of the gas toward the cluster center. The total spectrum from the cluster can be fitted by a cooling flow model with a total mass deposition rate of similar to150 M-circle dot yr(-1). Within the core (r < 30 kpc), the mass deposition rate of &SIM;40 M-&ODOT; yr(-1) is comparable to estimates for the star formation rate from optical data. We find an apparent correlation between the cD galaxy's optical isophotes and enhanced metallicity isocontours in the central &SIM;100 kpc of the cluster. We show that the approximate doubling of the metallicity associated with the cD galaxy can be plausibly explained by supernova explosions associated with the cD galaxy's ambient stellar population and the recent starburst. Finally, we calculate the amount of heating due to thermal conduction and show that this process is unlikely to offset cooling in A1068. C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA. Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wise, MW (reprint author), MIT, Ctr Space Res, Bldg 37,70 Vassar St, Cambridge, MA 02139 USA. EM wise@space.mit.edu NR 43 TC 44 Z9 46 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 JAN 20 PY 2004 VL 601 IS 1 BP 184 EP 196 DI 10.1086/380115 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600017 ER PT J AU Kraft, RP Forman, WR Churazov, E Laslo, N Jones, C Markevitch, M Murray, SS Vikhlinin, A AF Kraft, RP Forman, WR Churazov, E Laslo, N Jones, C Markevitch, M Murray, SS Vikhlinin, A TI An unusual discontinuity in the X-ray surface brightness profile of NGC 507: Evidence of an abundance gradient? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 507); galaxies : ISM; X-rays : galaxies ID LUMINOSITY RADIO GALAXIES; XMM-NEWTON OBSERVATIONS; CHANDRA OBSERVATION; INTRACLUSTER MEDIUM; ASCA OBSERVATIONS; VLA OBSERVATIONS; ELLIPTIC GALAXY; CLUSTER; GAS; ROSAT AB We present results from a 45 ks Chandra ACIS-I observation of the nearby (z = 0.01646) NGC 507 group. The X-ray surface brightness profile of the outer region of the group is well described by an isothermal beta-profile consistent with earlier ROSAT observations. We find a sharp edge or discontinuity in the radial surface brightness profile 55 kpc east and southeast of NGC 507 covering an similar to125degrees arc. At the sharpest part of the discontinuity, the surface brightness declines by a factor of similar to2 over a distance of 6.9 kpc (similar to15"). The inner and outer gas temperatures across the discontinuity differ by only about 0.2 keV (interior and exterior gas temperatures are 1.2 and 1.4 keV, respectively). Spectral analysis indicates that there is a gradient in the elemental abundance across the discontinuity, and comparison with the low-resolution NRAO VLA Sky Survey radio maps suggests that the discontinuity is aligned with a low surface brightness radio lobe. We conclude that the appearance of this discontinuity may be the result of two phenomena: the transonic (M similar to 0.75-1) expansion/inflation of the radio lobe close to our line of sight and the transport of high-abundance material from the center of the galaxy due to this expansion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Max Planck Inst Astrophys, D-85740 Garching, Germany. Moscow Space Res Inst, Moscow 117810, Russia. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA. RI Churazov, Eugene/A-7783-2013 NR 35 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 JAN 20 PY 2004 VL 601 IS 1 BP 221 EP 227 DI 10.1086/380427 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600020 ER PT J AU Li, LX Narayan, R AF Li, LX Narayan, R TI Quasi-periodic oscillations from Rayleigh-Taylor and Kelvin-Helmholtz instability at a disk-magnetosphere interface SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; instabilities; magnetic fields; MHD; stars : oscillations ID X-RAY BINARIES; MAGNETIC NEUTRON-STARS; G-MODE OSCILLATIONS; PROBING ACCRETION DISKS; THIN RELATIVISTIC DISKS; ACTIVE GALACTIC NUCLEI; INTERCHANGE INSTABILITY; MILLISECOND PULSAR; COLLAPSING STAR; GRO J1655-40 AB We consider the interface between an accretion disk and a magnetosphere surrounding the accreting mass. We argue that such an interface can occur not only with a magnetized neutron star but also sometimes with an unmagnetized neutron star or a black hole. The gas at the magnetospheric interface is generally Rayleigh-Taylor unstable and may also be Kelvin-Helmholtz unstable. Because of these instabilities, modes with low azimuthal wavenumbers m are expected to grow to large amplitude. It is proposed that the resulting nonaxisymmetric structures contribute to the high-frequency quasi-periodic oscillations that have been seen in neutron star and black hole X-ray binaries. The mode oscillation frequencies are calculated to be approximately equal to mOmega(m), where Omega(m) is the angular velocity of the accreting gas at the magnetospheric radius. Thus, mode frequencies should often be in the approximate ratio 1 : 2 : 3, etc. If the pressure of the gas in the disk is not large, then the m = 1 mode will be stable. In this case, the mode frequencies should be in the approximate ratio 2 : 3, etc. There is some observational evidence for such simple frequency ratios. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, LX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lli@cfa.harvard.edu; rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 75 TC 47 Z9 48 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 JAN 20 PY 2004 VL 601 IS 1 BP 414 EP 427 DI 10.1086/380446 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600035 ER PT J AU Tomsick, JA Kalemci, E Kaaret, P AF Tomsick, JA Kalemci, E Kaaret, P TI Detection of low-hard state spectral and timing signatures from the black hole X-ray transient XTE J1650-500 at low X-ray luminosities 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; NOVA-MUSCAE 1991; GX 339-4; LOW/HARD STATE; XTE J1650-500; CYGNUS X-1; BINARIES; QUIESCENCE; EMISSION; JET AB Using the Chandra X-Ray Observatory and the Rossi X-Ray Timing Explorer, we have studied the black hole candidate (BHC) X-ray transient XTE J1650 - 500 near the end of its 2001 - 2002 outburst after its transition to the low-hard state at X-ray luminosities down to L = 1.5 x 10(34) ergs s(-1) (1 - 9 keV, assuming a source distance of 4 kpc). Our results include a characterization of the spectral and timing properties. At the lowest sampled luminosity, we used an 18 ks Chandra observation to measure the power spectrum at low frequencies. For the three epochs at which we obtained Chandra/RXTE observations, the 0.5 - 20 keV energy spectrum is consistent with a spectral model consisting of a power law with interstellar absorption. We detect evolution in the powerlaw photon index from Gamma = 1.66 +/- 0.05 to 1.93 +/- 0.13 (90% confidence errors), indicating that the source softens at low luminosities. The power spectra are characterized by strong (20% - 35% fractional rms) band-limited noise, which we model as a zero-centered Lorentzian. Including results from an RXTE study of XTE J1650 - 500 near the transition to the low-hard state by Kalemci and coworkers the half-width of the zero-centered Lorentzian (roughly where the band-limited noise cuts off) drops from 4 Hz at L = 7 x 10(36) ergs s(-1) (1 - 9 keV, absorbed) to 0.067 +/- 0.007 Hz at L = 9 x 10(34) ergs s(-1) to 0.0035 +/- 0.0010 Hz at the lowest luminosity. While the spectral and timing parameters evolve with luminosity, it is notable that the general shapes of the energy and power spectra remain the same, indicating that the source stays in the low-hard state. This implies that the X-ray - emitting region of the system likely keeps the same overall structure, while the luminosity changes by a factor of 470. We discuss how these results may constrain theoretical black hole accretion models. C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, Code 0424,9500 Gilman Dr, La Jolla, CA 92093 USA. EM jtomsick@ucsd.edu NR 49 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 JAN 20 PY 2004 VL 601 IS 1 BP 439 EP 449 DI 10.1086/380484 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600037 ER PT J AU Miller, JM Raymond, J Fabian, AC Homan, J Nowak, MA Wijnands, R van der Klis, M Belloni, T Tomsick, JA Smith, DM Charles, PA Lewin, WHG AF Miller, JM Raymond, J Fabian, AC Homan, J Nowak, MA Wijnands, R van der Klis, M Belloni, T Tomsick, JA Smith, DM Charles, PA Lewin, WHG TI Chandra/High Energy Transmission Grating Spectrometer spectroscopy of the Galactic black hole GX 339-4: A relativistic iron emission line and evidence for a Seyfert-like warm absorber SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; relativity; stars : individual (GX 339-4, XTE J1650-500) ID ADVECTION-DOMINATED ACCRETION; QUASI-PERIODIC OSCILLATIONS; X-RAY BINARIES; GX 339-4; XTE J1550-564; CANDIDATE GX-339-4; GRO J1655-40; CYGNUS X-1; HIGH STATE; H I AB We observed the Galactic black hole GX 339 - 4 with the Chandra High Energy Transmission Grating Spectrometer (HETGS) for 75 ks during the decline of its 2002 - 2003 outburst. The sensitivity of this observation provides an unprecedented glimpse of a Galactic black hole at about a tenth of the luminosity of the outburst peak. The continuum spectrum is well described by a model consisting of multicolor disk blackbody (kT similar or equal to 0.6 keV) and power-law (Gamma similar or equal to 2.5) components. X-ray reflection models yield improved fits. A strong, relativistic Fe Kalpha emission line is revealed, indicating that the inner disk extends to the innermost stable circular orbit. The breadth of the line is sufficient to suggest that GX 339 - 4 may harbor a black hole with significant angular momentum. Absorption lines from H- and He-like O and He-like Ne and Mg are detected, as well as lines that are likely due to Ne II and Ne III. The measured line properties make it difficult to associate the absorption with the coronal phase of the interstellar medium. A scenario wherein the absorption lines are due to an intrinsic AGN-like warm-absorber geometry - perhaps produced by a disk wind in an extended disk-dominated state - may be more viable. We compare our results to Chandra observations of the Galactic black hole candidate XTE J1650 - 500 and discuss our findings in terms of prominent models for Galactic black hole accretion flows and connections to supermassive black holes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. Osserv Astron Brera, INAF, I-23807 Merate, Italy. MIT, Space Res Ctr, Cambridge, MA 02139 USA. MIT, Dept Phys, Cambridge, MA 02139 USA. Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jmmiller@cfa.harvard.edu NR 73 TC 114 Z9 114 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 JAN 20 PY 2004 VL 601 IS 1 BP 450 EP 465 DI 10.1086/380196 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600038 ER PT J AU Wood, BE Karovska, M AF Wood, BE Karovska, M TI Molecular hydrogen emission lines in Far Ultraviolet Spectroscopic Explorer observations of Mira B SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries : close; stars : individual (o Ceti); ultraviolet : stars ID HUBBLE-SPACE-TELESCOPE; H-2 EMISSION; T-TAURI; EVOLVED STARS; BAND SYSTEM; MASS-LOSS; SPECTRUM; CETI; COMPANION; VARIABLES AB We present new Far Ultraviolet Spectroscopic Explorer (FUSE) observations of Mira A's wind-accreting companion star, Mira B. We find that the strongest lines in the FUSE spectrum are H-2 lines fluoresced by H I Lyalpha. A previously analyzed Hubble Space Telescope (HST) spectrum also shows numerous Lyalpha-fluoresced H-2 lines. The HST lines are all Lyman band lines, while the FUSE H-2 lines are mostly Werner band lines, many of them never before identified in an astrophysical spectrum. We combine the FUSE and HST data to refine estimates of the physical properties of the emitting H-2 gas. We find that the emission can be reproduced by an H-2 layer with a temperature and column density of T = 3900 K and log N(H-2) = 17: 1, respectively. Another similarity between the HST and FUSE data, besides the prevalence of H-2 emission, is the surprising weakness of the continuum and high-temperature emission lines, suggesting that accretion onto Mira B has weakened dramatically. The UV fluxes observed by HST on 1999 August 2 were previously reported to be over an order of magnitude lower than those observed by HST and the International Ultraviolet Explorer (IUE) from 1979-1995. Analysis of the FUSE data reveals that Mira B was still in a similarly low state on 2001 November 22. C1 Univ Colorado, JILA, Boulder, CO 80309 USA. NIST, Boulder, CO 80309 USA. Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Wood, BE (reprint author), Univ Colorado, JILA, Boulder, CO 80309 USA. EM woodb@origins.colorado.edu; mkarovska@cfa.harvard.edu NR 33 TC 23 Z9 23 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 JAN 20 PY 2004 VL 601 IS 1 BP 502 EP 511 DI 10.1086/380197 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769NX UT WOS:000188657600044 ER PT J AU Nimmo, F Watters, TR AF Nimmo, F Watters, TR TI Depth of faulting on Mercury: Implications for heat flux and crustal and effective elastic thickness SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LOBATE SCARPS; PLANET; RADAR AB Topographic profiles across a lobate fault scarp on Mercury have been used to constrain the depth of faulting to 30-40 km. Here we use this depth to place constraints on the crustal thickness and heat flow into the base of the crust. With no crustal heat production, the mantle heat flux on Mercury at the time of scarp formation was 30-50 mWm(-2). However, higher crustal heat production rates allow significantly lower mantle heat fluxes. In all cases the mantle heat flux exceeds the likely radiogenic heat flux 4 Gyr ago; it is likely that secular cooling accounted for the remainder. Irrespective of crustal heat generation, a crustal thickness of less than or equal to140 km is required to satisfy both the faulting observations and the requirement that the base of the crust does not melt. The effective elastic thickness of the lithosphere at the time of faulting is predicted to be 25-30 km. C1 UCL, Dept Earth Sci, London WC1E 6BT, England. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Nimmo, F (reprint author), Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. EM nimmo@ess.ucla.edu; twatters@nasm.si.edu NR 25 TC 42 Z9 42 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 JAN 20 PY 2004 VL 31 IS 2 AR L02701 DI 10.1029/2003GL018847 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 769VU UT WOS:000188671100005 ER PT J AU Miller, SE Kress, WJ K, CS AF Miller, SE Kress, WJ K, CS TI Crisis for biodiversity collections SO SCIENCE LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Miller, SE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. NR 6 TC 2 Z9 2 U1 0 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 16 PY 2004 VL 303 IS 5656 BP 310 EP 310 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 763QK UT WOS:000188111800017 PM 14726573 ER PT J AU Williams, KK Greeley, R AF Williams, KK Greeley, R TI Laboratory and field measurements of the modification of radar backscatter by sand SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE radar backscatter; SAR; radar penetration; AIRSAR; sand ID SHUTTLE IMAGING RADAR; EASTERN SAHARA; SYSTEM; PENETRATION; ATTENUATION; FEATURES; DESERT AB Over the last two decades, the use of synthetic aperture radar (SAR) to address geologic problems has expanded as new applications for radar have been developed. One of the earliest and perhaps most surprising results from orbital SAR images of the Sahara was that, under certain conditions, radar signals penetrated up to several meters of sand to reveal subsurface features such as ancient river channels. Subsequent studies of radar penetration of and sand deposits have dealt with factors that govern the ability of radar to penetrate a sand cover. This paper presents results from a laboratory experiment in which radar backscatter from a surface of rocks was measured under controlled conditions as a function of frequency, polarization, incidence angle, and sand cover thickness. The sand used in the experiment had a moisture content of 0.28 vol.% and caused calculated average attenuations of 4.2 +/- 1 dB/m for C-band and similar to 11 +/- 2 dB/m for X-band. Results from the experiment were compared to field measurements of sand thickness during acquisition of airborne radar images. In AIRSAR images, the extent of dry sand in a dune field appears best in C-band because longer wavelength L- and P-band signals penetrate thinner sand deposits. Images of wet sand (4.9 vol.%) suggest that L-band was able to penetrate thin sand even though that sand was wet. Together, these laboratory and field measurements contribute towards a better understanding of how a sand cover modifies the radar backscatter of a surface. (C) 2003 Elsevier Inc. All rights reserved. C1 Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. RP Williams, KK (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20013 USA. EM williamsk@nasm.si.edu NR 24 TC 4 Z9 5 U1 0 U2 3 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD JAN 15 PY 2004 VL 89 IS 1 BP 29 EP 40 DI 10.1016/j.rse.2003.09.006 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 761BH UT WOS:000187879000002 ER PT J AU Brocksopp, C Sokoloski, JL Kaiser, C Richards, AM Muxlow, TWB Seymour, N AF Brocksopp, C Sokoloski, JL Kaiser, C Richards, AM Muxlow, TWB Seymour, N TI A radio jet in the prototypical symbiotic star Z And? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : symbiotic; circumstellar matter; stars : individual : Z And; stars : winds, outflows ID X-RAY SOURCE; LARGE-MAGELLANIC-CLOUD; SOURCE RX J0019.8+2156; BINARY Z ANDROMEDAE; CH-CYGNI; BIPOLAR JETS; SYSTEM PARAMETERS; HOT COMPONENT; WHITE-DWARF; EMISSION AB As part of a multiwavelength campaign to observe the 2000-2002 outburst of the prototypical symbiotic star Z Andromedae, we observed this object six times each with the Multi-Element Radio Linked Interferometer Network (MERLIN) and Very Large Array (VLA). The radio flux varied significantly during the course of the optical outburst at all three observation frequencies (1.4, 5, and 15 GHz). A jet-like extension was present in the 2001 September MERLIN image and appeared to be aligned perpendicularly to the plane of the binary orbit. Assuming that the ejection took place at the beginning of the optical outburst, the 0.06-arcsec separation between the peak of the extended emission and the central core implies that the ejected material was moving with a velocity of similar to400 km s(-1). This extended emission faded on a time-scale of months and was not detected at any other epoch. We consider the implications of jets being a component of a 'prototypical' symbiotic system and compare properties of the observed jet of Z And with those of the jets in X-ray binary systems. C1 UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. Inst Astrophys, F-75014 Paris, France. RP Brocksopp, C (reprint author), UCL, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM cb4@mssl.ucl.ac.uk OI Richards, Anita/0000-0002-3880-2450; Muxlow, Thomas/0000-0001-5797-8796; Seymour, Nicholas/0000-0003-3506-5536 NR 56 TC 38 Z9 38 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 JAN 11 PY 2004 VL 347 IS 2 BP 430 EP 436 DI 10.1111/j.1365-2966.2004.07213.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EB UT WOS:000187451900015 ER PT J AU Petit, JM Holman, M Scholl, H Kavelaars, J Gladman, B AF Petit, JM Holman, M Scholl, H Kavelaars, J Gladman, B TI A highly automated moving object detection package SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods : data analysis; Kuiper Belt; Solar system : general ID TRANS-NEPTUNIAN OBJECTS; KUIPER-BELT OBJECTS; FRANCE-HAWAII-TELESCOPE; WAVELET ANALYSIS; SOLAR-SYSTEM; SEARCH; GENERATION; CENTAURS; CAMERA AB With the deployment of large CCD mosaic cameras and their use in large-scale surveys to discover Solar system objects, there is a need for fast detection algorithms that can handle large data loads in a nearly automatic way. We present here an algorithm that we have developed. Our approach, by using two independent detection algorithms and combining the results, maintains high efficiency while producing low false-detection rates. These properties are crucial in order to reduce the operator time associated with searching these huge data sets. We have used this algorithm on two different mosaic data sets obtained using the CFH12K camera at the Canada-France-Hawaii Telescope (CFHT). Comparing the detection efficiency and false-detection rate of each individual algorithm with the combination of both, we show that our approach decreases the false detection rate by a factor of a few hundred to a thousand, while decreasing the 'limiting magnitude' (where the detection rate drops to 50 per cent) by only 0.1-0.3 mag. The limiting magnitude is similar to that of a human operator blinking the images. Our full pipeline also characterizes the magnitude efficiency of the entire system by implanting artificial objects in the data set. The detection portion of the package is publicly available. C1 Observ Besancon, F-25010 Besancon, France. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Observ Cote Azur, F-06304 Nice, France. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Petit, JM (reprint author), Observ Besancon, BP 1615, F-25010 Besancon, France. NR 30 TC 20 Z9 20 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 JAN 11 PY 2004 VL 347 IS 2 BP 471 EP 480 DI 10.1111/j.1365-2966.2004.07217.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EB UT WOS:000187451900019 ER PT J AU Worrall, DM Hardcastle, MJ Pearson, TJ Readhead, ACS AF Worrall, DM Hardcastle, MJ Pearson, TJ Readhead, ACS TI The relationship between the X-ray and radio components in the compact steep-spectrum quasar 3C 48 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms : non-thermal; quasars : individual : 3C 48; radio continuum : galaxies; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; 3C 48; ENERGY-DISTRIBUTIONS; CHANDRA OBSERVATIONS; LOUD QUASARS; EMISSION; GALAXIES; CLUSTERS; JET; VARIABILITY AB We combine results from ROSAT, Chandra and multifrequency VLBA observations of the compact steep-spectrum quasar 3C 48 in an attempt to understand why the radio source is so small and unusual. The X-ray spectrum shows no evidence for the excess absorption which might have allowed us to conclude that 3C 48 is small because it is bottled up by cold neutral gas. We infer that the X-ray spectrum of the nucleus is made up of a soft, variable, steep-spectrum component, and harder, power-law emission of slope consistent with the 1-GHz radio spectrum. The similarity of the X-ray-to-radio ratio of 3C 48 to that seen in core-dominated radio-loud quasars leads us to examine the possibility that the harder X-ray emission is inverse Compton radiation from the radio source, which is more than 99 per cent resolved in our VLBA data. The weak (3sigma) evidence that we find for a proper motion of 0.5+/-0.2c in a compact radio component about 0.05 arcsec from the core implies that if this component has a highly relativistic bulk motion, it is at a very small angle to the line of sight. However, stringent requirements on the jet opening angle make it unlikely that all the X-ray emission is from a fast jet which sees boosted cosmic microwave background emission and emits beamed X-rays in the observer's frame. If the unusual radio structures are intrinsically one-sided and unbeamed, the inverse Compton mechanism can provide an appreciable fraction of the X-ray emission if the magnetic field strength is a factor of 6-10 below that which gives equal energy in radiating relativistic particles and magnetic fields and roughly minimizes the total energy in the source. It remains possible that the unresolved X-ray emission arises from close to the central engine, either as an embedded blazar or associated with the accretion processes. C1 Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. CALTECH, Pasadena, CA 91125 USA. RP Univ Bristol, Dept Phys, Tyndall Ave, Bristol BS8 1TL, Avon, England. EM D.Worrall@bristol.ac.uk RI Hardcastle, Martin/E-2264-2012; Pearson, Timothy/N-2376-2015 OI Hardcastle, Martin/0000-0003-4223-1117; Pearson, Timothy/0000-0001-5213-6231 NR 65 TC 16 Z9 17 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 JAN 11 PY 2004 VL 347 IS 2 BP 632 EP 644 DI 10.1111/j.1365-2966.2004.07243.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 756EB UT WOS:000187451900032 ER PT J AU Viel, M Matarrese, S Heavens, A Haehnelt, MG Kim, TS Springel, V Hernquist, L AF Viel, M Matarrese, S Heavens, A Haehnelt, MG Kim, TS Springel, V Hernquist, L TI The bispectrum of the Lyman alpha forest at z similar to 2-2.4 from a large sample of UVES QSO absorption spectra (LUQAS) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE intergalactic medium; quasars : absorption lines; cosmology : miscellaneous; large-scale structure of Universe ID PARTICLE HYDRODYNAMICS SIMULATIONS; LARGE-SCALE BIAS; INTERGALACTIC MEDIUM; POWER SPECTRUM; GRAVITATIONAL-INSTABILITY; STAR-FORMATION; UNIVERSE; REDSHIFT; MODEL AB We present a determination of the bispectrum of the flux in the Lyman alpha forest of quasistellar object (QSO) absorption spectra obtained from a large sample of Ultraviolet Echelle Spectrograph (UVES) QSO absorption spectra (LUQAS), which consists of spectra observed with the high-resolution UVES. Typical errors on the observed bispectrum as obtained from a jack-knife estimator are similar to50 per cent. For wavenumbers in the range 0.031 and the photometric diagnostic used to discriminate them from other types of SNe detected during the Great Observatories Origins Deep Survey (GOODS) Hubble Space Telescope Treasury Program with the Advanced Camera for Surveys (ACS). Photometric redshift measurements of the hosts combined with deep F606W, F775W, and F850LP imaging discriminates hydrogen-rich SNe II from SNe I at z>1 by exploiting the UV deficit in the energy distributions of SNe Ia. This sorting allows rapid follow-up of space-based discoveries. Subsequent spectroscopy of 11 GOODS SNe Ia obtained from the ground and with the grism on ACS confirmed the reliability of our photometric screening. We present the highest redshift spectrum of any SN published to date, SN Ia 2002fw at z=1.3 observed near maximum brightness with the ACS grism. The lack of UV flux for true SNe Ia provides an effective tool for our ongoing efforts to build a sample of SNe Ia a 1.2