J/A+A/675/A23ivo://CDS.VizieR/J/A+A/675/A23doi:10.26093/cds/vizier.36750023CDSNandakumar G.Ryde N.Casagrande L.Mace G.2024-11-28T20:04:13Z2023-06-30T09:23:25ZCDS support team

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

cds-question@unistra.frmilky-way-galaxygiant-starsk-starschemical-abundancesinfrared-astronomyspectroscopyCool stars, such as M giants, can only be analyzed in the near-infrared (NIR) regime due to the ubiquitous titanium oxide features in optical spectra of stars with Teff<4000K. In dust-obscured regions, the inner bulge and Galactic center region, the intrinsically bright M giants observed in the NIR are an optimal option for studying stellar abundances and the chemical evolution of stellar populations. Because of the uncertainties in photometric methods, a method for determining the stellar parameters for M giants from the NIR spectra themselves is needed. We develop a method for determining the stellar parameters for M giants from the NIR spectra. We validate the method by deriving the stellar parameters for nearby well-studied M giants with spectra from the spectral library of the Immersion GRating INfrared Spectrograph (IGRINS). We demonstrate the accuracy and precision of our method by determining the stellar parameters and alpha-element trends versus metallicity for solar neighborhood M giants. We carried out new observations of 44 M giant stars with IGRINS mounted on the Gemini South telescope. We also obtained the full H and K band IGRINS spectra of six nearby well-studied M giants at a spectral resolving power of R=45000 from the IGRINS spectral library. We used the tool called spectroscopy made easy in combination with one-dimensional (1D) model atmospheres in a radiative and convective scheme (MARCS) stellar atmosphere models to model the synthetic spectrum that fits the observed spectrum best. The effective temperatures that we derive from our new method (tested for 3400<=Teff<=4000K here) agree excellently with those of the six nearby well-studied M giants, which indicates that the accuracy is indeed high. For the 43 solar neighborhood M giants, our Teff, logg, [Fe/H], microturbulence, [C/Fe], [N/Fe], and [O/Fe] agree with APOGEE with mean differences and a scatter (our method - APOGEE) of -67+/-33K, -0.31+/-0.15dex, 0.02+/-0.05dex, 0.22+/-0.13km/s, -0.05+/-0.06dex, 0.06+/-0.06dex, and 0.02+/-0.09dex, respectively. Furthermore, the tight offset with a small dispersion compared to the APOGEE Teff indicates a high precision in our derived temperatures and those derived from the APOGEE pipeline. The typical uncertainties in the stellar parameters are found to be +/-100K in Teff, +/-0.2dex in logg, +/-0.1dex in [Fe/H], and +/-0.1km/s in microturbulence. The alpha-element trends versus metallicity for Mg, Si, Ca, and Ti are consistent with the APOGEE DR17 trends for the same stars and with the GILD optical trends. We also find a clear enhancement in the abundances for thick-disk stars.2023A&A...675A..23Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A23CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/675/A23https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/675/A23http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/675/A23https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/675/A23https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/675/A23http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/675/A23GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/675/A23/table3 (Stellar parameters and phosphorus abundances for stars, along with their assumed stellar population and [O/Fe] based on the APOGEE [Mg/Fe] vs. [Fe/H] trend)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/675/A23/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/675/A23/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/675/A23/table3?GETtext/xml+votable180.050000true87.1710772-6.03357720.005555555555555556Cone search capability for table J/A+A/675/A23/tablea6 (Line-by-line Magnesium abundances and mean [Mg/Fe])https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/675/A23/tablea6?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/675/A23/tablea6?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/675/A23/tablea6?GETtext/xml+votable180.050000true87.1710772-6.03357720.0055555555555555566/7533 11519 20959 21370 21375 21457 21464 21472 22112 22120 22144 22179 28912 29066 29113 29456 31419 33088 37135 37408 37417-37418 38132 41589 41591 41596-41597 41760 41762 41768 43132 43288 43553 48041https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/675/A23?format=asciiInfrareddefaultJ/A+A/675/A23/table3Stellar parameters and phosphorus abundances for stars, along with their assumed stellar population and [O/Fe] based on the APOGEE [Mg/Fe] vs. [Fe/H] trendStarName (2M)meta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSimbadSimbad column added by the CDSmeta.ref.urlcharPopDesignated stellar populationmeta.codecharTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]Relative iron abundancephys.abund.FefloatvmicroMicroturbulence velocitykm/sphys.veloc.microTurbfloat[C/Fe]Relative Carbon abundancephys.abundfloat[N/Fe]Relative Nitrogen abundancephys.abundfloat[O/Fe]Relative Oxygen abundancephys.abundfloatCMStars observed by other surveys based on cross match (RAVE and/or GALAH)meta.idcharn_CM[a] Note (1)meta.notechar_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.mainJ/A+A/675/A23/tablea6Line-by-line Magnesium abundances and mean [Mg/Fe]SimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName (2M,HD,HIP)meta.id;meta.maincharAMg21059.76Mg abundance from 21059.76{AA} linephys.abundfloatAMg21060.89Mg abundance from 21060.89{AA} linephys.abundfloatAMg21458.87Mg abundance from 21458.87{AA} linephys.abundfloat[Mg/Fe]Mean Mg abundancephys.abund;stat.meanfloate_[Mg/Fe]Standard mean of errorstat.error;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.mainJ/A+A/675/A23/tablea7Line-by-line Silicon abundances and mean [Si/Fe]recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName (2M,HD,HIP)meta.id;meta.maincharASi16434.93Si abundance from 16434.93{AA} linephys.abundfloatASi20804.20? Si abundance from 20804.20{AA} linephys.abundfloatnullableASi20890.37? Si abundance from 20890.37{AA} linephys.abundfloatnullableASi20926.14? Si abundance from 20926.14{AA} linephys.abundfloatnullable[Si/Fe]Mean Si abundancephys.abund;stat.meanfloate_[Si/Fe]Standard mean of errorstat.error;phys.abundfloatJ/A+A/675/A23/tablea8Line-by-line Calcium abundances and mean [Ca/Fe]recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName (2M,HD,HIP)meta.id;meta.maincharACa16150.76Ca abundance from 16150.76{AA} linephys.abundfloatACa16155.24Ca abundance from 16155.24{AA} linephys.abundfloatACa16157.36Ca abundance from 16157.36{AA} linephys.abundfloatACa20962.57Ca abundance from 20962.57{AA} linephys.abundfloatACa20972.53Ca abundance from 20972.53{AA} linephys.abundfloat[Ca/Fe]Mean Ca abundancephys.abund;stat.meanfloate_[Ca/Fe]Standard mean of errorstat.error;phys.abundfloatJ/A+A/675/A23/tablea9Line-by-line Titanium abundances and mean [Ti/Fe][Ti/Fe]Mean Ti abundancephys.abund;stat.meanfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName (2M,HD,HIP)meta.id;meta.maincharATi16330.54Ti abundance from 16330.54{AA} linephys.abundfloatATi21149.62? Ti abundance from 21149.62{AA} linephys.abundfloatnullablee_[Ti/Fe]Standard mean of errorstat.error;phys.abundfloat