The Imprint of Clump Formation at High Redshift. II. The Chemistry of the Bulge

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dc.contributor.authorDebattista, Victor P.
dc.contributor.authorLiddicott, David J.
dc.contributor.authorGonzalez, Oscar A.
dc.contributor.authorBeraldo e Silva, Leandro
dc.contributor.authorAmarante, Joao A. S.
dc.contributor.authorLazar, Ilin
dc.contributor.authorZoccali, Manuela
dc.contributor.authorValenti, Elena
dc.contributor.authorFisher, Deanne B.
dc.contributor.authorKhachaturyants, Tigran
dc.contributor.authorNidever, David L.
dc.contributor.authorQuinn, Thomas R.
dc.contributor.authorDu, Min
dc.contributor.authorKassin, Susan
dc.date.accessioned2025-01-20T20:15:47Z
dc.date.available2025-01-20T20:15:47Z
dc.date.issued2023
dc.description.abstractIn Paper I, we showed that clumps in high-redshift galaxies, having a high star formation rate density (sigma(SFR)), produce disks with two tracks in the [Fe/H]-[alpha/Fe] chemical space, similar to that of the Milky Way's (MW's) thin+thick disks. Here we investigate the effect of clumps on the bulge's chemistry. The chemistry of the MW's bulge is comprised of a single track with two density peaks separated by a trough. We show that the bulge chemistry of an N-body + smoothed particle hydrodynamics clumpy simulation also has a single track. Star formation within the bulge is itself in the high-sigma(SFR) clumpy mode, which ensures that the bulge's chemical track follows that of the thick disk at low [Fe/H] and then extends to high [Fe/H], where it peaks. The peak at low metallicity instead is comprised of a mixture of in situ stars and stars accreted via clumps. As a result, the trough between the peaks occurs at the end of the thick disk track. We find that the high-metallicity peak dominates near the mid-plane and declines in relative importance with height, as in the MW. The bulge is already rapidly rotating by the end of the clump epoch, with higher rotation at low [alpha/Fe]. Thus clumpy star formation is able to simultaneously explain the chemodynamic trends of the MW's bulge, thin+thick disks, and the splash.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/acbb00
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/acbb00
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/92284
dc.identifier.wosidWOS:000964123700001
dc.issue.numero2
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleThe Imprint of Clump Formation at High Redshift. II. The Chemistry of the Bulge
dc.typeartículo
dc.volumen946
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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