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Open AccessConference Report

The “Building Blocks” of Stellar Halos

1
Department of Physics & Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada
2
Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
*
Author to whom correspondence should be addressed.
Senior CIfAR fellow.
Academic Editors: Duncan A. Forbes and Ericson D. Lopez
Galaxies 2017, 5(3), 33; https://doi.org/10.3390/galaxies5030033
Received: 30 June 2017 / Revised: 27 July 2017 / Accepted: 28 July 2017 / Published: 2 August 2017
(This article belongs to the Special Issue On the Origin (and Evolution) of Baryonic Galaxy Halos)
The stellar halos of galaxies encode their accretion histories. In particular, the median metallicity of a halo is determined primarily by the mass of the most massive accreted object. We use hydrodynamical cosmological simulations from the apostle project to study the connection between the stellar mass, the metallicity distribution, and the stellar age distribution of a halo and the identity of its most massive progenitor. We find that the stellar populations in an accreted halo typically resemble the old stellar populations in a present-day dwarf galaxy with a stellar mass ∼0.2–0.5 dex greater than that of the stellar halo. This suggests that had they not been accreted, the primary progenitors of stellar halos would have evolved to resemble typical nearby dwarf irregulars. View Full-Text
Keywords: galaxy formation and evolution; stellar halo; numerical simulations galaxy formation and evolution; stellar halo; numerical simulations
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MDPI and ACS Style

Oman, K.A.; Starkenburg, E.; Navarro, J.F. The “Building Blocks” of Stellar Halos. Galaxies 2017, 5, 33. https://doi.org/10.3390/galaxies5030033

AMA Style

Oman KA, Starkenburg E, Navarro JF. The “Building Blocks” of Stellar Halos. Galaxies. 2017; 5(3):33. https://doi.org/10.3390/galaxies5030033

Chicago/Turabian Style

Oman, Kyle A.; Starkenburg, Else; Navarro, Julio F. 2017. "The “Building Blocks” of Stellar Halos" Galaxies 5, no. 3: 33. https://doi.org/10.3390/galaxies5030033

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