J/A+A/630/A104ivo://CDS.VizieR/J/A+A/630/A104doi:10.26093/cds/vizier.36300104CDSAmarsi A.M.Nissen P.E.Skuladottir A.2020-03-26T14:19:11Z2019-11-12T15:37:59ZCDS support team

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

cds-question@unistra.frlate-type-starschemical-abundancesThe abundances of carbon, oxygen, and iron in late-type stars are important parameters in exoplanetary and stellar physics, as well as key tracers of stellar populations and Galactic chemical evolution. However, standard spectroscopic abundance analyses can be prone to severe systematic errors, by the assumption that the stellar atmosphere is one-dimensional (1D) and hydrostatic, and by ignoring departures from local thermodynamic equilibrium (LTE). To address this, we carry out 3D non-LTE radiative transfer calculations for CI and OI, and 3D LTE radiative transfer calculations for FeII, across the stagger-grid of 3D hydrodynamic model atmospheres. The absolute 3D non-LTE versus 1D LTE abundance corrections can be as severe as ~0.3dex for CI lines in low-metallicity F dwarfs, and ~0.6dex for OI lines in high-metallicity F dwarfs. The 3D LTE versus 1D LTE abundance corrections for FeII lines are less severe, typically less than +0.15dex. We use the corrections in a re-analysis of carbon, oxygen, and iron in 187 F and G dwarfs in the Galactic disk and halo. Applying the differential 3D non-LTE corrections to 1D LTE abundances visibly reduces the scatter in the abundance plots. The thick disk and high- halo population rise in carbon and oxygen with decreasing metallicity, reaching a maximum of [C/Fe]~=0.2 and a plateau of [O/Fe]~=0.6 at [Fe/H]~=~1.0. The low- halo population is qualitatively similar, albeit offset towards lower metallicities and with larger scatter. Nevertheless, these populations overlap in the [C/O] versus [O/H] plane, decreasing to a plateau of [C/O]~=0.6 below [O/H]~=1.0. In the thin-disk, stars having confirmed planet detections tend to have higher values of C/O at given [O/H]; this potential signature of planet formation is only apparent after applying the abundance corrections to the 1D LTE results. Our grids of line-by-line abundance corrections are publicly available and can readily be used to improve the accuracy of spectroscopic analyses of late-type stars.2019A&A...630A.104Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/630/A104CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/630/A104https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/630/A104http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/630/A104https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/630/A104https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/630/A104http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/630/A104GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/630/A104/table7 (Parameters/abundances of 187 stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/630/A104/table7?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/630/A104/table7?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/630/A104/table7?GETtext/xml+votable180.050000true285.180558319.07456030.0055555555555555566/146 200 208 373 436 488 953 1053 1425 1614 4376 4603 5413 5622 6681 7286 7334 8235 8999 9537 9831 10313 12451 12621 12645 12793 13020 13162 13348 14385 16652 16883 16935 17136 17245 17332 17726 17730 17768 17782 18053 18548 18614 18887 19003 19347 19385 21477 21926 22036 22118 22590 22754 22909 23015 23096 23978 24442 24775 24824 24827 24924 24942 25225 25385 25444 25554 25862 25891 25948 26025 26284 26289 26768 27018 27162 27323 27330 27394 27826 27857 27975 27991 28154 28258 28265 28459 28763 29490 29541 29596 29765 30051 30179 30196 30233 30296 30359 30526 30878 31029 31094 31470 31503 31874 32100 32335 32930 33063 33273 33456 33508 33630 33923 35954 36840 37232 37573 37595 38072 38238 38279 38288 38986 39157 39257 39647 39692 39984 40101 40442 40692 40716 40921 40924 41259 41607 41721 41861 41912 41941 42146 42248 42331 42700 43012 43228 43258 43310 43575 43639 43641 43760 43813 43911 44131 44243 44281 44542 44653 44740 45121 45168 45364 45485 45669 45865 46053 46297 46302 46306 46640 46828 46967 47347 47389 47512 47530 48105 48281 48394 48545 48705 48719 48736https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/630/A104?format=asciidefaultJ/A+A/630/A104/table7Parameters/abundances of 187 starsSimbadNameSimbad column added by the CDSmeta.idchar_DEExplain (declination part)degpos.eq.dec;meta.mainnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName of starmeta.id;meta.maincharPopPopulation assigned in the papersrc.classcharNplanetNumber of planet detectionsmeta.numberintMaxmassMaximum planet mass in system(1.898187x10+27kg)phys.massfloatTeffEffective temperatureKphys.temperature.effectiveintloggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloatvmic1D microturbulence parameterkm/sphys.veloc.microTurbfloat[Fe/H]3L? 3D LTE iron abundance (1)phys.abund.Fedoublenullablee_[Fe/H]3L? Uncertainty on [Fe/H]3L (1)stat.error;phys.abund.Fedoublenullable[Fe/H]1L? 1D LTE iron abundance (1)phys.abund.Fedoublenullablee_[Fe/H]1L? Uncertainty on [Fe/H]1L (1)stat.error;phys.abund.Fedoublenullable[C/H]3N? 3D non-LTE carbon abundance (1)phys.abunddoublenullablee_[C/H]3N? Uncertainty on [C/H]3N (1)stat.error;phys.abunddoublenullable[C/H]1N? 1D non-LTE carbon abundance (1)phys.abunddoublenullablee_[C/H]1N? Uncertainty on [C/H]1N (1)stat.error;phys.abunddoublenullable[C/H]3L? 3D LTE carbon abundance (1)phys.abunddoublenullablee_[C/H]3L? Uncertainty on [C/H]3L (1)stat.error;phys.abunddoublenullable[C/H]1L? 1D LTE carbon abundance (1)phys.abunddoublenullablee_[C/H]1L? Uncertainty on [C/H]1L (1)stat.error;phys.abunddoublenullable[O/H]3N? 3D non-LTE oxygen abundance (1)phys.abunddoublenullablee_[O/H]3N? Uncertainty on [O/H]3N (1)stat.error;phys.abunddoublenullable[O/H]1N? 1D non-LTE carbon abundance (1)phys.abunddoublenullablee_[O/H]1N? Uncertainty on [O/H]1N (1)stat.error;phys.abunddoublenullable[O/H]3L? 3D LTE carbon abundance (1)phys.abunddoublenullablee_[O/H]3L? Uncertainty on [O/H]3L (1)stat.error;phys.abunddoublenullable[O/H]1L? 1D LTE carbon abundance (1)phys.abunddoublenullablee_[O/H]1L? Uncertainty on [O/H]1L (1)stat.error;phys.abunddoublenullable_RAExplain (right ascension part)degpos.eq.ra;meta.mainnullableJ/A+A/630/A104/table1Line parameterschipotExcitation potentialeVphys.atmol.excitationdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSpeciesSpecies identifier (CI, OI or FeII)meta.id;meta.maincharLineLine labelmeta.id;spect.linecharwlairAir wavelengthnmem.wldoublewlvacVacuum wavelengthnmem.wldoubleloggfLogarithm of lower level statistical weight times oscillator strengthstat.weight;phys.atmol.oscStrength;phys.atmol.leveldoubleloggamnatLogarithm of natural broadeninglog(s**-1)spect.line.broaddoublesigmaABO? ABO cross-section at 10^4^m/s in a0^2^ unit (1)phys.atmol.crossSectionintnullablealphaABO? ABO velocity exponent (1)arith.factor;phys.velocfloatnullableJ/A+A/630/A104/table23N-1L abundance corrections for CIrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffEffective temperatureKphys.temperature.effectiveintloggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]Iron abundance relative to the Sunphys.abund.Fefloatvmic1D microturbulence parameterkm/sphys.veloc.microTurbfloatlogepsAbsolute abundancephys.abundfloatLineCI line labelmeta.id;spect.linecharDelta3D non-LTE versus 1D LTE correctionarith.factordoubleJ/A+A/630/A104/table33N-1L abundance corrections for OIrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffEffective temperatureKphys.temperature.effectiveintlogggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]Iron abundance relative to the Sunphys.abund.Fefloatvmic1D microturbulence parameterkm/sphys.veloc.microTurbfloatlogepsAbsolute abundancephys.abundfloatLineOI line label (1)meta.id;spect.linecharDelta3D non-LTE versus 1D LTE correctionarith.factordoubleJ/A+A/630/A104/table43L-1L abundance corrections for FeIIrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffEffective temperatureKphys.temperature.effectiveintloggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloatvmic1D microturbulence parameterkm/sphys.veloc.microTurbfloatlogepsAbsolute abundancephys.abundfloatLineFeII line labelmeta.id;spect.linecharDelta3D LTE versus 1D LTE correctionarith.factordoubleJ/A+A/630/A104/table61N-1L abundance corrections for OIrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffEffective temperatureKphys.temperature.effectiveintloggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]Iron abundance relative to the Sunphys.abund.Fefloatvmic1D microturbulence parameterkm/sphys.veloc.microTurbfloatlogepsAbsolute abundancephys.abundfloatLineOI line label (1)meta.id;spect.linecharDelta1D non-LTE versus 1D LTE correctionarith.factordoubleJ/A+A/630/A104/table51N-1L abundance corrections for CIrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTeffEffective temperatureKphys.temperature.effectiveintloggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]Iron abundance relative to the Sunphys.abund.Fefloatvmic1D microturbulence parameterkm/sphys.veloc.microTurbfloatlogepsAbsolute abundancephys.abundfloatLineCI line labelmeta.id;spect.linecharDelta1D non-LTE versus 1D LTE correctionarith.factordouble