Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton

| Summary:

[[{“value”:”Quantifying the connection between galaxies and their host dark matter halos
has been key for testing cosmological models on various scales. Below $M_star
sim 10^9,M_odot$, such studies have primarily relied on the satellite galaxy
population orbiting the Milky Way. Here we present new constraints on the
connection between satellite galaxies and their host dark matter subhalos using
the largest sample of satellite galaxies in the Local Volume ($D lesssim
12,mathrm{Mpc}$) to date. We use $250$ confirmed and $71$ candidate dwarf
satellites around 27 Milky Way (MW)-like hosts from the Exploration of Local
VolumE Satellites (ELVES) Survey and use the semi-analytical SatGen model for
predicting the population of dark matter subhalos expected in the same volume.
Through a Bayesian model comparison of the observed and the forward-modeled
satellite stellar mass functions (SSMF), we infer the satellite stellar-to-halo
mass relation. We find that the observed SSMF is best reproduced when subhalos
at the low mass end are populated by a relation of the form $M_star propto
M^alpha_mathrm{peak}$, with a moderate slope of $alpha_mathrm{const}=2.10
pm 0.01$ and a low scatter, constant as a function of the peak halo mass, of
$sigma_mathrm{const}=0.06^{+0.07}_{-0.05}$. A model with a steeper slope
($alpha_mathrm{grow}=2.39 pm 0.06$) and a scatter that grows with decreasing
$M_mathrm{peak}$ is also consistent with the observed SSMF but is not
required. Our new model for the satellite-subhalo connection, based on hundreds
of Local Volume satellite galaxies, is in line with what was previously derived
using only the Milky Way satellites.”}]] 

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