Shi Shao
The multiplicity and anisotropy of galactic satellite accretion
Shao, Shi; Cautun, Marius; Frenk, Carlos S.; Grand, Robert J.J.; Gómez, Facundo A.; Marinacci, Federico; Simpson, Christine M.
Authors
Marius Cautun
Carlos S. Frenk
Robert J.J. Grand
Facundo A. Gómez
Federico Marinacci
Christine M. Simpson
Abstract
We study the incidence of group and filamentary dwarf galaxy accretion into Milky Way (MW) mass haloes using two types of hydrodynamical simulations: EAGLE, which resolves a large cosmological volume, and the AURIGA suite, which are very high resolution zoom-in simulations of individual MW-sized haloes. The present-day 11 most massive satellites are predominantly (75%) accreted in single events, 14% in pairs and 6% in triplets, with higher group multiplicities being unlikely. Group accretion becomes more common for fainter satellites, with 60% of the top 50 satellites accreted singly, 12% in pairs, and 28% in richer groups. A group similar in stellar mass to the Large Magellanic Cloud (LMC) would bring on average 15 members with stellar mass larger than 104 M⊙ . Half of the top 11 satellites are accreted along the two richest filaments. The accretion of dwarf galaxies is highly anisotropic, taking place preferentially perpendicular to the halo minor axis, and, within this plane, preferentially along the halo major axis. The satellite entry points tend to be aligned with the present-day central galaxy disc and satellite plane, but to a lesser extent than with the halo shape. Dwarfs accreted in groups or along the richest filament have entry points that show an even larger degree of alignment with the host halo than the full satellite population. We also find that having most satellites accreted as a single group or along a single filament is unlikely to explain the MW disc of satellites.
Citation
Shao, S., Cautun, M., Frenk, C. S., Grand, R. J., Gómez, F. A., Marinacci, F., & Simpson, C. M. (2018). The multiplicity and anisotropy of galactic satellite accretion. Monthly Notices of the Royal Astronomical Society, 476(2), 1796-1810. https://doi.org/10.1093/mnras/sty343
Journal Article Type | Article |
---|---|
Online Publication Date | Feb 9, 2018 |
Publication Date | May 11, 2018 |
Deposit Date | Mar 6, 2018 |
Publicly Available Date | Mar 8, 2018 |
Journal | Monthly Notices of the Royal Astronomical Society |
Print ISSN | 0035-8711 |
Electronic ISSN | 1365-2966 |
Publisher | Royal Astronomical Society |
Peer Reviewed | Peer Reviewed |
Volume | 476 |
Issue | 2 |
Pages | 1796-1810 |
DOI | https://doi.org/10.1093/mnras/sty343 |
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Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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