Authors
Abstract
We develop a comprehensive and flexible model for the connection between satellite galaxies and dark matter subhalos in dark matter-only zoom-in simulations of Milky Way (MW)-mass host halos. We systematically identify the physical and numerical uncertainties in the galaxy-halo connection and simulations underlying our method, including (i) the influence of host halo properties; (ii) the relationship between satellite luminosities and subhalo properties, including the effects of reionization; (iii) the relationship between satellite and subhalo locations; (iv) the relationship between satellite sizes and subhalo properties, including the effects of tidal stripping; (v) satellite and subhalo disruption due to baryonic effects; and (vi) artificial subhalo disruption and orphan satellites. To illustrate our approach, we fit this model to the luminosity distribution of both classical MW satellites and those discovered in the Sloan Digital Sky Survey by performing realistic mock observations that depend on the luminosity, size, and distance of our predicted satellites, and we infer the total satellite population that will be probed by upcoming surveys. We argue that galaxy size and surface brightness modeling will play a key role in interpreting current and future observations, as the expected number of observable satellites depends sensitively on their surface brightness distribution.Details
| Publication | The Astrophysical Journal, Volume 873, Issue 1, article id. 34, |
| Publication Date | March 2019 |
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| arXiv | arXiv:1809.05542 |
| Bibcode | 2019ApJ...873...34N |
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| E-Print Comment(s) | 21 pages, 10 figures. Updated to published version. Code available at https://github.com/eonadler/subhalo_satellite_connection; ApJ 873, 34 (2019); doi:10.3847/1538-4357/ab040e |