2019
DOI: 10.1093/mnras/stz1852
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The distinct stellar metallicity populations of simulated Local Group dwarfs

Abstract: ABSTRACT A number of Local Group dwarf galaxies are known to have two spatially segregated stellar metallicity populations, a centrally concentrated metal-rich population, and a more extended metal-poor population. In this work we discuss mechanisms that lead to the formation of two spatially segregated metallicity populations. Using a set of high-resolution hydrodynamical simulations of Local Group-like environments, we select a sample of satellite and field gal… Show more

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Cited by 38 publications
(47 citation statements)
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“…is smaller in satellites, likely due to tidal stripping (Genina et al 2018(Genina et al , 2019. At the lowest stellar masses, Genina et al (2019) find that most multiple populations in dSphs are primarily formed due to mergers.…”
Section: H E M O Dy Na M I C P O P U L At I O N S T H Ro U G H O U mentioning
confidence: 84%
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“…is smaller in satellites, likely due to tidal stripping (Genina et al 2018(Genina et al , 2019. At the lowest stellar masses, Genina et al (2019) find that most multiple populations in dSphs are primarily formed due to mergers.…”
Section: H E M O Dy Na M I C P O P U L At I O N S T H Ro U G H O U mentioning
confidence: 84%
“…is smaller in satellites, likely due to tidal stripping (Genina et al 2018(Genina et al , 2019. At the lowest stellar masses, Genina et al (2019) find that most multiple populations in dSphs are primarily formed due to mergers. Observations of prolate rotation may be evidence for past mergers (Amorisco et al 2014;Kacharov et al 2017) and the two populations in UMi could be evidence for a late-time merger.…”
Section: H E M O Dy Na M I C P O P U L At I O N S T H Ro U G H O U mentioning
confidence: 84%
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“…Some of these differences could indicate an ancient merger, which would have dispersed the old stellar component and allowed the enriched gas to sink further in before forming stars (Benítez-Llambay et al 2016;Genina et al 2019). This would provide a plausible explanation for the radial offset between the original distribution of Fornax GCs and the present-day distributions of its stars.…”
Section: Discussionmentioning
confidence: 99%