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dc.contributor.authorBragança, G. A.
dc.contributor.authorDaflon, S.
dc.contributor.authorLanz, T.
dc.contributor.authorCunha, K.
dc.contributor.authorBensby, T.
dc.contributor.authorMcMillan, P. J.
dc.contributor.authorGarmany, C. D.
dc.contributor.authorGlaspey, J. W.
dc.contributor.authorBorges Fernandes, M.
dc.contributor.authorOey, M. S.
dc.contributor.authorHubeny, I.
dc.date.accessioned2019-08-30T21:17:18Z
dc.date.available2019-08-30T21:17:18Z
dc.date.issued2019-05-23
dc.identifier.citationG. A. Bragança, S. Daflon, T. Lanz, K. Cunha, T. Bensby, P. J. McMillan, C. D. Garmany, J. W. Glaspey, M. Borges Fernandes, M. S. Oey and I. Hubeny A&A, 625 (2019) A120en_US
dc.identifier.issn1432-0746
dc.identifier.doi10.1051/0004-6361/201834554
dc.identifier.urihttp://hdl.handle.net/10150/634032
dc.description.abstractContext. Elemental abundance gradients in galactic disks are important constraints for models of how spiral galaxies form and evolve. However, the abundance structure of the outer disk region of the Milky Way is poorly known, which hampers our understanding of the spiral galaxy that is closest to us and that can be studied in greatest detail. Young OB stars are good tracers of the present-day chemical abundance distribution of a stellar population and because of their high luminosities they can easily be observed at large distances, making them suitable to explore and map the abundance structure and gradients in the outer regions of the Galactic disk. Aims. Using a sample of 31 main-sequence OB stars located between galactocentric distances 8.4-15.6 kpc, we aim to probe the present-day radial abundance gradients of the Galactic disk. Methods. The analysis is based on high-resolution spectra obtained with the MIKE spectrograph on the Magellan Clay 6.5-m telescope on Las Campanas. We used a non-NLTE analysis in a self-consistent semi-automatic routine based on TLUSTY and SYNSPEC to determine atmospheric parameters and chemical abundances. Results. Stellar parameters (effective temperature, surface gravity, projected rotational velocity, microturbulence, and macroturbulence) and silicon and oxygen abundances are presented for 28 stars located beyond 9 kpc from the Galactic center plus three stars in the solar neighborhood. The stars of our sample are mostly on the main-sequence, with effective temperatures between 20800-31300 K, and surface gravities between 3.23-4.45 dex. The radial oxygen and silicon abundance gradients are negative and have slopes of -0.07 dex kpc(-1) and -0.09 dex kpc(-1), respectively, in the region 8.4 <= R-G <= 15.6 kpc. Conclusions. The obtained gradients are compatible with the present-day oxygen and silicon abundances measured in the solar neighborhood and are consistent with radial metallicity gradients predicted by chemodynamical models of Galaxy Evolution for a subsample of young stars located close to the Galactic plane.en_US
dc.description.sponsorshipCAPES; CNPq; Knut and Alice Wallenberg Foundation; US National Science Foundation [AST-0448900]; NSF [AST-907873]en_US
dc.language.isoenen_US
dc.publisherEDP SCIENCES S Aen_US
dc.rightsCopyright © ESO 2019.en_US
dc.subjectstars: abundancesen_US
dc.subjectstars: early-typeen_US
dc.titleRadial abundance gradients in the outer Galactic disk as traced by main-sequence OB starsen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTRONOMY & ASTROPHYSICSen_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.volume625
dc.source.beginpageA120
refterms.dateFOA2019-08-30T21:17:19Z


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