J/MNRAS/382/553ivo://CDS.VizieR/J/MNRAS/382/553doi:10.26093/cds/vizier.73820553CDSLiu Y.J.Zhao G.Shi J.R.Pietrzynski G.Gieren W.2024-07-05T20:15:57Z2009-01-28T13:33:07ZCDS support team

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

cds-question@unistra.frgiant-starschemical-abundancesBased on the analysis of high-resolution spectra with a high signal-to-noise ratio, we have determined the abundances of the alpha-elements O, Si, Ca and Ti, the iron peak elements V, Fe and Ni, and the heavy element Ba without the consideration of non-local thermodynamic equilibrium (NLTE) effect and the light neutron-rich elements Na, Mg and Al with an NLTE analysis for 63 nearby red clump giants. Fe abundances cover a logarithmic range between 0.60 and +0.35 relative to solar. All abundance ratios with respect to Fe are similar to those found in the Sun. Hyperfine structure (HFS) was taken into account when calculating V lines. The difference in abundances obtained with and without HFS can be as large as 0.5 dex.2007MNRAS.382..553Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/382/553CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/402/343 : IR O I triplet, [O I] lines in F-K dwarfs/giants (Takeda, 2003)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/382/553https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/382/553http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/382/553https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/382/553https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/382/553http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/382/553GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/382/553/stars (Results for the 63 red clump stars studied)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/382/553/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/382/553/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/382/553/stars?GETtext/xml+votable180.050000true2.0730519-8.82411220.0055555555555555566/8536 16704 16895 17262 17286 17391 17568 17582 17585 17764 18688 18893 18911 19985 28892 28948 28968 29001 30344 30953 31091 31428 31445 31475 32922 33205 34353 34392 35025 35185 35191 35254 35382 35415 35494 35532 35602 35680 35984 36001 36433 41051 41068 42172 42361 42514 42942 44333 44372 44485 44722 45668 46176 46502 46582 46903 46918 47423-47424 47640 47728 48519 48687https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/382/553?format=asciiOpticaldefaultJ/MNRAS/382/553/starsResults for the 63 red clump stars studiedVmagV magnitudemagphot.mag;em.opt.VfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarHD namemeta.id;meta.maincharprimaryn_StarSimbad column added by the CDSmeta.notecharTeff(B-V)Effective temperature derived from B-V colour indexKphys.temperature.effectiveintTeff(b-y)? Effective temperature derived from b-y colour indexKphys.temperature.effectiveintnullableTeff(V-K)Effective temperature derived from V-K colour indexKphys.temperature.effectiveintVMAGAbsolute V magnitudemagphys.magAbs;em.opt.VfloatTeffEffective temperatureKphys.temperature.effectiveint[Fe/H]Metallicitylog(Sun)phys.abund.ZfloatEWDisplay the 226 equivalent widths for this starmeta.ref.urlcharSimbadSimbad column added by the CDSchar[Na/Fe]eNa abundance relative to Fe from LTE analysislog(Sun)phys.abundfloat[Na/Fe]nNa abundance relative to Fe from NLTE analysislog(Sun)phys.abundfloat[Mg/Fe]eMg abundance relative to Fe from LTE analysislog(Sun)phys.abundfloat[Mg/Fe]nMg abundance relative to Fe from NLTE analysislog(Sun)phys.abundfloat[Al/Fe]eAl abundance relative to Fe from LTE analysislog(Sun)phys.abund.Zfloat[Al/Fe]nAl abundance relative to Fe from NLTE analysislog(Sun)phys.abund.Zfloat[Ca/Fe]Ca abundance relative to Felog(Sun)phys.abundfloat[Si/Fe]Si abundance relative to Felog(Sun)phys.abundfloat[Ti/Fe]Ti abundance relative to Felog(Sun)phys.abundfloat[Ni/Fe]Ni abundance relative to Felog(Sun)phys.abundfloat[V/Fe]V abundance relative to Felog(Sun)phys.abundfloat[Ba/Fe]Ba abundance relative to Felog(Sun)phys.abundfloatEW7772? [O/Fe]7772{AA} equivalent width0.1nmspect.line.eqWidthfloatnullableEW7774? [O/Fe]7774{AA} equivalent width0.1nmspect.line.eqWidthfloatnullableEW7775? [O/Fe]7775{AA} equivalent width0.1nmspect.line.eqWidthfloatnullable[O/Fe]7772LTE [O/Fe]7772 abundancelog(Sun)phys.abundfloat[O/Fe]7774? LTE [O/Fe]7774{AA} abundancelog(Sun)phys.abundfloatnullable[O/Fe]7775LTE [O/Fe]7775{AA} abundancelog(Sun)phys.abundfloat[O/Fe]LTE [O/Fe] abundancelog(Sun)phys.abundfloat[O/Fe]7772cLTE [O/Fe]7772{AA} abundance after correction according to Takeda (2003, J/A+A/402/343)log(Sun)phys.abundfloat[O/Fe]7774cLTE [O/Fe]7774{AA} abundance after correction according to Takeda (2003, J/A+A/402/343)log(Sun)phys.abundfloat[O/Fe]7775cLTE [O/Fe]7775{AA} abundance after correction according to Takeda (2003, J/A+A/402/343)log(Sun)phys.abundfloat[O/Fe]cLTE [O/Fe]{AA} abundance after correction according to Takeda (2003, J/A+A/402/343)log(Sun)phys.abundfloat_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainHIPHIP numbermeta.idintloggSurface gravitylog(cm.s**-2)phys.gravityfloat[M/H]Metal abundancelog(Sun)phys.abund.ZfloatvtMicroturbulent velocitykm/sphys.velocfloatMassMasssolMassphys.massfloatplxParallaxmaspos.parallax.trigfloate_plxrms uncertainty on Plxmasstat.error;pos.parallaxfloatBCBolometric correctionmagphot.mag.bcfloatJ/MNRAS/382/553/table1All atomic-line data used and EW values of programme starsStarHD namemeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonIon designationmeta.id;phys.atmol.ionStagecharlambdaWavelength0.1nmem.wldoubleEPExcitation potentialeVphys.atmol.excitationfloatloggflog of Oscillator Strengthphys.atmol.oscStrengthfloatf6Enhancement factorphys.dampingfloatEW? Line equivalent width0.1nmspect.line.eqWidthfloatnullableJ/MNRAS/382/553/table4The comparison of stellar parameters of 22 stars common with the sample McW90 (1990ApJS...74.1075M)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarHD namemeta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveintTeffMcEffective temperature from 1990ApJS...74.1075MKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloatloggMcSurface gravity from 1990ApJS...74.1075Mlog(cm.s**-2)phys.gravityfloat[Fe/H]Metallicitylog(Sun)phys.abund.Zfloat[Fe/H]McMetallicity from 1990ApJS...74.1075Mlog(Sun)phys.abund.FefloatvtMicroturbulent velocitykm/sphys.velocfloatvtMcMicroturbulent velocity in 1990ApJS...74.1075Mkm/sphys.velocfloatDTeffEffective temperature differenceKphys.temperatureintDloggSurface gravity differencelog(cm.s**-2)phys.gravity;arith.difffloatD[Fe/H]Metallicity differencelog(Sun)phys.abund.FefloatDvtMicroturbulent velocity differencekm/sphys.veloc;arith.difffloat