Oxygen abundances in the Galactic bulge

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dc.contributor.authorZoccali, M.
dc.contributor.authorLecureur, A.
dc.contributor.authorBarbuy, B.
dc.contributor.authorHill, V.
dc.contributor.authorRenzini, A.
dc.contributor.authorMinniti, D.
dc.contributor.authorMomany, Y.
dc.contributor.authorGomez, A.
dc.contributor.authorOrtolani, S.
dc.date.accessioned2025-01-21T01:05:54Z
dc.date.available2025-01-21T01:05:54Z
dc.date.issued2006
dc.description.abstractAims. We spectroscopically characterize the Galactic Bulge to infer its star formation timescale, compared to the other Galactic components, through the chemical signature on its individual stars.
dc.description.abstractMethods. We derived iron and oxygen abundances for 50 K giants in four fields towards the Galactic bulge. High resolution (R = 45 000) spectra for the target stars were collected with FLAMES-UVES at the VLT.
dc.description.abstractResults. Oxygen, as measured from the forbidden line at 6300 angstrom, shows a well-defined trend with [Fe/H], with [O/Fe] higher in bulge stars than in thick disk ones, which were known to be more oxygen enhanced than thin disk stars.
dc.description.abstractConclusions. These results support a scenario in which the bulge formed before and more rapidly than the disk, and therefore the MW bulge can be regarded as a prototypical old spheroid, with a formation history similar to that of early-type (elliptical) galaxies.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361:20065659
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361:20065659
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/96044
dc.identifier.wosidWOS:000240495300001
dc.issue.numero1
dc.language.isoen
dc.pagina.finalL4
dc.pagina.inicioL1
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectgalaxy : bulge
dc.subjectstars : abundances
dc.subjectstars : atmospheres
dc.titleOxygen abundances in the Galactic bulge
dc.typeartículo
dc.volumen457
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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