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dc.contributor.authorSchultheis, M.
dc.contributor.authorRojas-Arriagada, A.
dc.contributor.authorCunha, K.
dc.contributor.authorZoccali, M.
dc.contributor.authorChiappini, C.
dc.contributor.authorZasowski, G.
dc.contributor.authorQueiroz, A. B. A.
dc.contributor.authorMinniti, D.
dc.contributor.authorFritz, T.
dc.contributor.authorGarcía-Hernández, D. A.
dc.contributor.authorNitschelm, C.
dc.contributor.authorZamora, O.
dc.contributor.authorHasselquist, S.
dc.contributor.authorFernández-Trincado, J. G.
dc.contributor.authorMunoz, R. R.
dc.date.accessioned2021-01-13T02:18:35Z
dc.date.available2021-01-13T02:18:35Z
dc.date.issued2020-10-08
dc.identifier.citationSchultheis, M., Rojas-Arriagada, A., Cunha, K., Zoccali, M., Chiappini, C., Queiroz, A. B. A., ... & Munoz, R. R. (2020). Cool stars in the Galactic Center as seen by APOGEE: M giants, AGB stars and supergiant stars/candidates. A&A, 642 (2020) A81.en_US
dc.identifier.issn0004-6361
dc.identifier.doi10.1051/0004-6361/202038327
dc.identifier.urihttp://hdl.handle.net/10150/650745
dc.description.abstractThe 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 3200 K. 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] similar to +0.3 dex and a metal-poor peak around {Fe/H] = -0.5 dex, which is 0.2 dex 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)> 300 km s(-1); the metal-rich stars show a much higher rotation velocity (similar to 200 km s(-1)) with respect to the metal-poor stars (similar to 140 km s(-1)). 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.en_US
dc.language.isoenen_US
dc.publisherE D P SCIENCES S Aen_US
dc.rights© M. Schultheis et al. 2020. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0).en_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_US
dc.subjectGalaxy: bulgeen_US
dc.subjectGalaxy: stellar contenten_US
dc.subjectstars: fundamental parametersen_US
dc.subjectstars: abundancesen_US
dc.titleCool stars in the Galactic center as seen by APOGEE: M giants, AGB stars, and supergiant stars and candidatesen_US
dc.typeArticleen_US
dc.identifier.eissn1432-0746
dc.contributor.departmentUniv Arizonaen_US
dc.identifier.journalASTRONOMY & ASTROPHYSICSen_US
dc.description.noteOpen access articleen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleAstronomy & Astrophysics
dc.source.volume642
dc.source.beginpageA81
refterms.dateFOA2021-01-13T02:18:52Z


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© M. Schultheis et al. 2020. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0).
Except where otherwise noted, this item's license is described as © M. Schultheis et al. 2020. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0).