J/A+A/642/A81ivo://CDS.VizieR/J/A+A/642/A81doi:10.26093/cds/vizier.36420081CDSSchultheis M.Rojas-Arriagada A.Cunha K.Zoccali M.Chiappini C.,Zasowski G.Queiroz A.B.A.Minniti D.Fritz T.Garcia-Hernandez D.A.,Nitschelm C.Zamora O.Hasselquist S.Fernandez-Trincado J.G.,Munoz R.R.2021-09-10T12:27:44Z2021-02-10T13:45:56ZCDS support team

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

cds-question@unistra.frgiant-starschemical-abundanceseffective-temperatureThe Galactic center region, including the nuclear disk, has until recently been largely avoided in chemical census studies because of extreme extinction and stellar crowding. Large, near-IR spectroscopic surveys, such as the Apache Point Observatory Galactic Evolution Experiment (APOGEE), allow the measurement of metallicities in the inner region of our Galaxy. Making use of the latest APOGEE data release (DR16), we are able for the first time to study cool Asymptotic Giant branch (AGB) stars and supergiants in this region. The stellar parameters of five known AGB stars and one supergiant star (VR 5-7) show that their location is well above the tip of the red giant branch. We studied metallicities of 157 M giants situated within 150 pc of the Galactic center from observations obtained by the APOGEE survey with reliable stellar parameters from the APOGEE pipeline making use of the cool star grid down to 3200K. Distances, interstellar extinction values, and radial velocities were checked to confirm that these stars are indeed situated in the Galactic center region. We detect a clear bimodal structure in the metallicity distribution function, with a dominant metal-rich peak of [Fe/H]~+0.3dex and a metal-poor peak around {Fe/H]=-0.5dex, which is 0.2dex poorer than Baade's Window. The {alpha}-elements Mg, Si, Ca, and O show a similar trend to the Galactic bulge. The metal-poor component is enhanced in the {alpha}-elements, suggesting that this population could be associated with the classical bulge and a fast formation scenario. We find a clear signature of a rotating nuclear stellar disk and a significant fraction of high-velocity stars with v_gal_>300km/s; the metal-rich stars show a much higher rotation velocity (~200km/s) with respect to the metal-poor stars (~140km/s). The chemical abundances as well as the metallicity distribution function suggest that the nuclear stellar disk and the nuclear star cluster show distinct chemical signatures and might be formed differently.2020A&A...642A..81Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/642/A81CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/642/A81https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/642/A81http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/642/A81https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/642/A81https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/642/A81http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/642/A81GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/642/A81/table1 (Known AGB and supergiants with stellar parameters from APOGEE-DR16)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/642/A81/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/642/A81/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/642/A81/table1?GETtext/xml+votable180.050000true266.3307083-29.23477780.005555555555555556Cone search capability for table J/A+A/642/A81/table2 (Supergiant candidates)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/642/A81/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/642/A81/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/642/A81/table2?GETtext/xml+votable180.050000true266.5310833-28.77822220.005555555555555556Cone search capability for table J/A+A/642/A81/tablea1 (*APOGEE IDs used in this paper for the analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/642/A81/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/642/A81/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/642/A81/tablea1?GETtext/xml+votable180.050000true265.3206667-28.76052780.0055555555555555565/7207 6/28825 28827 28849 28852https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/642/A81?format=asciidefaultJ/A+A/642/A81/table1Known AGB and supergiants with stellar parameters from APOGEE-DR16r_Name? Reference for name (1)meta.ref;pos.frameintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAPOGEEAPOGEE ID (2MHHMMSSss+DDMMSSs)meta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloat[M/H]Metallicityphys.abund.ZfloatNameName, only for table1meta.idcharSNameSimbad name, only for table1meta.idchar_RAPosition from APOGEE name (right ascension part)degpos.eq.ra;meta.main_DEPosition from APOGEE name (declination part)degpos.eq.dec;meta.mainJ/A+A/642/A81/table2Supergiant candidates[M/H]Metallicityphys.abund.ZfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAPOGEEAPOGEE ID (2MHHMMSSss+DDMMSSs)meta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloat_RAPosition from APOGEE name (right ascension part)degpos.eq.ra;meta.main_DEPosition from APOGEE name (declination part)degpos.eq.dec;meta.mainJ/A+A/642/A81/tablea1*APOGEE IDs used in this paper for the analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintAPOGEEAPOGEE ID (2MHHMMSSss+DDMMSSs)meta.id;meta.mainchar_RAPosition from APOGEE name (right ascension part)degpos.eq.ra;meta.main_DEPosition from APOGEE name (declination part)degpos.eq.dec;meta.main