J/ApJ/778/149ivo://CDS.VizieR/J/ApJ/778/149doi:10.26093/cds/vizier.17780149CDSMcWilliam A.Wallerstein G.Mottini M.2017-12-07T07:26:59Z2015-06-08T11:30:35ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frchemical-abundancesline-intensitiesFrom chemical abundance analysis of stars in the Sagittarius dwarf spheroidal galaxy (Sgr), we conclude that the {alpha}-element deficiencies cannot be due to the Type Ia supernova (SN Ia) time-delay scenario of Tinsley. Instead, the evidence points to low [{alpha}/Fe] ratios resulting from an initial mass function (IMF) deficient in the highest mass stars. The critical evidence is the 0.4 dex deficiency of [O/Fe], [Mg/Fe], and other hydrostatic elements, contrasting with the normal trend of r-process [Eu/Fe]_r_ with [Fe/H]. Supporting evidence comes from the hydrostatic element (O, Mg, Na, Al, Cu) [X/Fe] ratios, which are inconsistent with iron added to the Milky Way (MW) disk trends. Also, the ratio of hydrostatic to explosive (Si, Ca, Ti) element abundances suggests a relatively top-light IMF. Abundance similarities with the LMC, Fornax, and IC 1613 suggest that their {alpha}-element deficiencies also resulted from IMFs lacking the most massive SNe II. The top-light IMF, as well as the normal trend of r-process [Eu/Fe]_r_ with [Fe/H] in Sgr, indicates that massive SNe II (>~30M_{sun}_) are not major sources of r-process elements. High [La/Y] ratios, consistent with leaky-box chemical evolution, are confirmed but ~0.3 dex larger than theoretical asymptotic giant branch (AGB) predictions. This suggests that a substantial increase in the theoretical ^13^C pocket in low-mass AGB stars is required. Sgr has the lowest [Rb/Zr] ratios known, consistent with pollution by low-mass (<~2M_{sun}_) AGB stars near [Fe/H]=-0.6, likely resulting from leaky-box chemical evolution. The [Cu/O] trends in Sgr and the MW suggest that Cu yields increase with both metallicity and stellar mass, as expected from Cu production by the weak s-process in massive stars. Finally, we present an updated hyperfine splitting line list, an abundance analysis of Arcturus, and further develop our error analysis formalism.2013ApJ...778..149Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/778/149CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/418/284 : s-process in low-metallicity stars. II. (Bisterzo+, 2011)J/MNRAS/404/1529 : s-process in low-metallicity stars (Bisterzo+, 2010)J/ApJ/708/1290 : A 2MASS view of the Sgr dSph. VI. (Chou+, 2010)J/A+A/520/A95 : Abundances of red giants in M54 & Sgr dSph (Carretta+, 2010)J/A+A/505/117 : Abundances of RGB stars in 15 GCs (Carretta+, 2009)J/A+A/465/815 : Abundances of Sgr dSph stars (Sbordone+, 2007)J/A+A/433/185 : Detailed abundance analysis of F & G dwarfs (Bensby+, 2005)J/A+A/420/183 : Spectroscopy in solar neighborhood (Allende Prieto+ 2004)J/A+A/414/503 : Abundances in the Sgr dSph (Bonifacio+, 2004)J/AJ/118/1245 : Elemental abundances in five stars in M54 (Brown+, 1999)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/778/149https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/778/149http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/778/149https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/778/149https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/778/149http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/778/149GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/778/149/stars (Observations and adopted model atmosphere parameters (tables 1 and 6))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/778/149/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/778/149/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/778/149/stars?GETtext/xml+votable180.050000true283.824583-30.4636110.0055555555555555566/48035https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/778/149?format=asciiOpticaldefaultJ/ApJ/778/149/starsObservations and adopted model atmosphere parameters (tables 1 and 6)DEJ2000Degree of declination (J2000)pos.eq.dec;meta.mainrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLSSF[242/266] Star identifier (1)meta.id;meta.mainintRAJ2000Hour of right ascension (J2000)pos.eq.ra;meta.mainVmag[16.2/16.3] V-band magnitude (1)magphot.mag;em.opt.VfloatExp[5700/8100] Exposure timestime.duration;obs.exposureintS/N[39/50] Signal-to-noise ratiostat.snrintHRV[131.8/145.4] Heliocentric radial velocitykm/sspect.dopplerVeloc;pos.heliocentricfloatTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloat[A/H]Abundance [A/H]phys.abundfloatVtMicroturbulent velocity ({xi})km/sphys.velocfloat[FeI/H]Abundance [FeI/H]phys.abundfloatLink1Display the Equivalent Widths from table2meta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/ApJ/778/149/table2Line Listu_EW-247[:] Uncertainty flag in EW-247meta.code.error;spect.line.eqWidthcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIon identification (1)phys.atmol.ionStagecharlambda[5119.1/8772.9] Wavelength in Angstroms (1)0.1nmem.wlfloatExPot[0/6.2] Lower level excitation potential {chi}eVphys.atmol.excitation;phys.atmol.levelfloatEW-242? Equivalent width in Star 242 (m{AA})1e-13mspect.line.eqWidthintnullableu_EW-242[:] Uncertainty flag in EW-242meta.code.error;spect.line.eqWidthcharDA-242? differential abundance for star 242 (2)phys.abundfloatnullableEW-247? Equivalent width in Star 247 (m{AA})1e-13mspect.line.eqWidthintnullableDA-247? differential abundance for star 247 (2)phys.abundfloatnullableu_DA-247[:] Uncertainty flag in Del-247meta.code.errorcharEW-266? Equivalent width in Star 266 (m{AA})1e-13mspect.line.eqWidthintnullableu_EW-266[:] Uncertainty flag in EW-266meta.code.error;spect.line.eqWidthcharDA-266? differential abundance for star 266 (2)phys.abundfloatnullableu_DA-266[:] Uncertainty flag in Del-266meta.code.errorcharNoteAbundance note(s) (3)meta.notecharJ/ApJ/778/149/table4Hyperfine splitting listrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintA[51/153] Atomic weight (isotope)stat.weight;phys.atmol.weightintIonIon identificationphys.atmol.ionStagecharlambda[5119/8390] Wavelength in Angstroms0.1nmem.wldoublelogFi[-5.4/-0.1] Log of the isotopic fraction times the hyperfine gf valuephys.atmol.oscStrengthfloat