The contribution of N-rich stars to the Galactic stellar halo using APOGEE red giants

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dc.contributor.authorHorta, Danny
dc.contributor.authorMackereth, J. Ted
dc.contributor.authorSchiavon, Ricardo P.
dc.contributor.authorHasselquist, Sten
dc.contributor.authorBovy, Jo
dc.contributor.authorPrieto, Carlos Allende
dc.contributor.authorBeers, Timothy C.
dc.contributor.authorCunha, Katia
dc.contributor.authorGarcia-Hernandez, D. A.
dc.contributor.authorKisku, Shobhit S.
dc.contributor.authorLane, Richard R.
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorMason, Andrew C.
dc.contributor.authorNataf, David M.
dc.contributor.authorRoman-Lopes, Alexandre
dc.contributor.authorSchultheis, Mathias
dc.date.accessioned2025-01-20T23:55:05Z
dc.date.available2025-01-20T23:55:05Z
dc.date.issued2021
dc.description.abstractThe contribution of dissolved globular clusters (GCs) to the stellar content of the Galactic halo is a key constraint on models for GC formation and destruction, and the mass assembly history of the Milky Way. Earlier results from APOGEE pointed to a large contribution of destroyed GCs to the stellar content of the inner halo, by as much as 25 per cent, which is an order of magnitude larger than previous estimates for more distant regions of the halo. We set out to measure the ratio between nitrogen-rich (N-rich) and normal halo field stars, as a function of distance, by performing density modelling of halo field populations in APOGEE DR16. Our results show that at 1.5 kpc from the Galactic Centre, N-rich stars contribute a much higher 16.81(-7.0)(+10.0) per cent fraction to the total stellar halo mass budget than the 2.7(-0.8)(-1.0) per cent ratio contributed at 10 kpc. Under the assumption that N-rich stars are former GC members that now reside in the stellar halo field, and assuming the ratio between first and second population GC stars being 1:2, we estimate a total contribution from disrupted GC stars of the order of 27.5(-11.5)(+15.4) per cent at r = 1.5 kpc and 4.2(-1:3)(+1.5) per cent at r = 10 kpc. Furthermore, since our methodology requires fitting a density model to the stellar halo, we integrate such density within a spherical shell from 1.5 to 15 kpc in radius, and find a total stellar mass arising from dissolved and/or evaporated GCs of M-GC(total) = 9.6-2.6(+4.0) x 10(7) M-circle dot.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/staa3598
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/staa3598
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/95070
dc.identifier.wosidWOS:000606297700080
dc.issue.numero4
dc.language.isoen
dc.pagina.final5478
dc.pagina.inicio5462
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectGalaxy: evolution
dc.subjectGalaxy: formation
dc.subjectglobular clusters: general
dc.subjectGalaxy: halo
dc.titleThe contribution of N-rich stars to the Galactic stellar halo using APOGEE red giants
dc.typeartículo
dc.volumen500
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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