Exploring the Stellar Age Distribution of the Milky Way Bulge Using APOGEE

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dc.contributor.authorHasselquist, Sten
dc.contributor.authorZasowski, Gail
dc.contributor.authorFeuillet, Diane K.
dc.contributor.authorSchultheis, Mathias
dc.contributor.authorNataf, David M.
dc.contributor.authorAnguiano, Borja
dc.contributor.authorBeaton, Rachael L.
dc.contributor.authorBeers, Timothy C.
dc.contributor.authorCohen, Roger E.
dc.contributor.authorCunha, Katia
dc.contributor.authorFernandez-Trincado, Jose G.
dc.contributor.authorGarcia-Hernandez, D. A.
dc.contributor.authorGeisler, Doug
dc.contributor.authorHoltzman, Jon A.
dc.contributor.authorJohnson, Jennifer
dc.contributor.authorLane, Richard R.
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorBidin, Christian Moni
dc.contributor.authorNitschelm, Christian
dc.contributor.authorRoman-Lopes, Alexandre
dc.contributor.authorSchiavon, Ricardo
dc.contributor.authorSmith, Verne V.
dc.contributor.authorSobeck, Jennifer
dc.date.accessioned2025-01-23T19:48:17Z
dc.date.available2025-01-23T19:48:17Z
dc.date.issued2020
dc.description.abstractWe present stellar age distributions of the Milky Way bulge region using ages for similar to 6000 high-luminosity (log (g), metal-rich ([Fe/H] >= -0.5) bulge stars observed by the Apache Point Observatory Galactic Evolution Experiment. Ages are derived using The Cannon label-transfer method, trained on a sample of nearby luminous giants with precise parallaxes for which we obtain ages using a Bayesian isochrone-matching technique. We find that the metal-rich bulge is predominantly composed of old stars (>8 Gyr). We find evidence that the planar region of the bulge (vertical bar Z(GC)vertical bar <= 0.25 kpc) is enriched in metallicity, Z, at a faster rate (dZ/dt similar to 0.0034 Gyr(-1)) than regions farther from the plane (dZ/dt similar to 0.0013 Gyr(-1) at vertical bar Z(GC)vertical bar > 1.00 kpc). We identify a nonnegligible fraction of younger stars (age similar to 2-5 Gyr) at metallicities of +0.2 < [Fe/H] < +0.4. These stars are preferentially found in the plane (vertical bar Z(GC)vertical bar <= 0.25 kpc) and at R-cy approximate to 2-3 kpc, with kinematics that are more consistent with rotation than are the kinematics of older stars at the same metallicities. We do not measure a significant age difference between stars found inside and outside the bar. These findings show that the bulge experienced an initial starburst that was more intense close to the plane than far from the plane. Then, star formation continued at supersolar metallicities in a thin disk at 2 kpc less than or similar to R-cy less than or similar to 3 kpc until similar to 2 Gyr ago.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/abaeee
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/abaeee
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100434
dc.identifier.wosidWOS:000576322600001
dc.issue.numero2
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleExploring the Stellar Age Distribution of the Milky Way Bulge Using APOGEE
dc.typeartículo
dc.volumen901
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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