The Milky Way tomography with APOGEE: intrinsic density distribution and structure of mono-abundance populations

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dc.contributor.authorLian, Jianhui
dc.contributor.authorZasowski, Gail
dc.contributor.authorMackereth, Ted
dc.contributor.authorImig, Julie
dc.contributor.authorHoltzman, Jon A.
dc.contributor.authorBeaton, Rachael L.
dc.contributor.authorBird, Jonathan C.
dc.contributor.authorCunha, Katia
dc.contributor.authorFernandez-Trincado, Jose G.
dc.contributor.authorHorta, Danny
dc.contributor.authorLane, Richard R.
dc.contributor.authorMasters, Karen L.
dc.contributor.authorNitschelm, Christian
dc.contributor.authorRoman-Lopes, A.
dc.date.accessioned2025-01-20T21:06:57Z
dc.date.available2025-01-20T21:06:57Z
dc.date.issued2022
dc.description.abstractThe spatial distribution of mono-abundance populations (MAPs, selected in [Fe/H] and [Mg/Fe]) reflect the chemical and structural evolution in a galaxy and impose strong constraints on galaxy formation models. In this paper, we use APOGEE data to derive the intrinsic density distribution of MAPs in the Milky Way, after carefully considering the survey selection function. We find that a single exponential profile is not a sufficient description of the Milky Way's disc. Both the individual MAPs and the integrated disc exhibit a broken radial density distribution; densities are relatively constant with radius in the inner Galaxy and rapidly decrease beyond the break radius. We fit the intrinsic density distribution as a function of radius and vertical height with a 2D density model that considers both a broken radial profile and radial variation of scale height (i.e. flaring). There is a large variety of structural parameters between different MAPs, indicative of strong structure evolution of the Milky Way. One surprising result is that high-alpha MAPs show the strongest flaring. The young, solar-abundance MAPs present the shortest scale height and least flaring, suggesting recent and ongoing star formation confined to the disc plane. Finally we derive the intrinsic density distribution and corresponding structural parameters of the chemically defined thin and thick discs. The chemical thick and thin discs have local surface mass densities of 5.62 +/- 0.08 and 15.69 +/- 0.32 M(circle dot)pc(-2), respectively, suggesting a massive thick disc with a local surface mass density ratio between thick to thin disc of 36 per cent.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stac1151
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stac1151
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93382
dc.identifier.wosidWOS:000796696600010
dc.issue.numero3
dc.language.isoen
dc.pagina.final4151
dc.pagina.inicio4130
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectgalaxy: abundances
dc.subjectgalaxy: disc
dc.subjectgalaxy: evolution
dc.subjectgalaxy: fundamental parameters
dc.subjectgalaxy: stellar content
dc.subjectgalaxy: structure
dc.titleThe Milky Way tomography with APOGEE: intrinsic density distribution and structure of mono-abundance populations
dc.typeartículo
dc.volumen513
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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