The origin of accreted stellar halo populations in the milky way using apogee, gaia, and the eagle simulations

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dc.contributor.authorMackereth, J. Ted
dc.contributor.authorSchiavon, Ricardo P.
dc.contributor.authorPfeffer, Joel
dc.contributor.authorHayes, Christian R.
dc.contributor.authorBovy, Jo
dc.contributor.authorAnguiano, Borja
dc.contributor.authorPrieto, Carlos Allende
dc.contributor.authorHasselquist, Sten
dc.contributor.authorHoltzman, Jon
dc.contributor.authorJohnson, Jennifer A.
dc.contributor.authorMajewski, Steven R.
dc.contributor.authorO’Connell, Robert
dc.contributor.authorShetrone, Matthew
dc.contributor.authorTissera, Patricia B.
dc.contributor.authorFernandez-Trincado, J. G.
dc.date.accessioned2023-06-07T14:22:21Z
dc.date.available2023-06-07T14:22:21Z
dc.date.issued2019-01-21
dc.descriptionIndexación Scopuses
dc.description.abstractKinematics of halo stars. We show that ∼2/3 of nearby halo stars have high orbital eccentricities (e 0.8), and abundance patterns typical of massive Milky Way dwarf galaxy satellites today, characterized by relatively low [Fe/H], [Mg/Fe], [Al/Fe], and [Ni/Fe]. The trend followed by high-e stars in the [Mg/Fe]-[Fe/H] plane shows a change of slope at [Fe/H] ∼ -1.3, which is also typical of stellar populations from relatively massive dwarf galaxies. Low-e stars exhibit no such change of slope within the observed [Fe/H] range and show slightly higher abundances of Mg, Al, and Ni. Unlike their low-e counterparts, high-e stars show slightly retrograde motion, make higher vertical excursions, and reach larger apocentre radii. By comparing the position in [Mg/Fe]-[Fe/H] space of high-e stars with those of accreted galaxies from the EAGLE suite of cosmological simulations, we constrain the mass of the accreted satellite to be in the range 108.5≲ M ≲ 109M⊙ We show that the median orbital eccentricities of debris are largely unchanged since merger time, implying that this accretion event likely happened at z≲1.5. The exact nature of the low-e population is unclear, but we hypothesize that it is a combination of in situ star formation, high-|z| disc stars, lower mass accretion events, and contamination by the low-e tail of the high-e population. Finally, our results imply that the accretion history of the Milky Way was quite unusual.es
dc.identifier.citationMonthly Notices of the Royal Astronomical Society Volume 482, Issue 3, Pages 3426 - 3442 21 January 2019es
dc.identifier.doi10.1093/mnras/sty2955en
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/50409
dc.language.isoenes
dc.publisherMonthly Notices of the Royal Astronomical Societyes
dc.rights.licenseAttribution 4.0 International (CC BY 4.0)en
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en
dc.subjectGalaxyes
dc.subjectGalaxy: abundanceses
dc.subjectGalaxy: formationes
dc.subjectGalaxy: haloes
dc.subjectKinematics and dynamicses
dc.subjectStellar contentes
dc.titleThe origin of accreted stellar halo populations in the milky way using apogee, gaia, and the eagle simulationses
dc.typeArtículoes
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