S20B0104abst
S20B0104
The satellite systems of the Milky Way and Andromeda have proved extremely fruitful testing grounds for our concordance cosmology model. However, to fully understand small-scale structure, it is crucial to characterize a statistical sample of satellite systems around other MW-like galaxies. We have developed and tested machinery to use surface brightness fluctuations (SBF) to obtain distances to low mass satellites, allowing us to characterize satellite systems much more efficiently than previously possible and roughly double the number of systems that have been surveyed out to βΌ half their virial radius. We see hints that all of the satellite systems are more centrally concentrated than expected from simulations of MW-mass hosts. However, to robustly characterize the radial distribution of satellites, it is important to survey satellite systems over the full virial volume of the host. We propose to use HSC to complete the survey of satellites of the nearby MW-like spiral M51 out to its virial radius. Using the depth and image quality of HSC, we will measure SBF distances and classify each detected dwarf as a satellite of M51 or a background contaminant. This will let us measure the full radial distribution to the virial radius to conclusively evaluate how centrally concentrated the satellites are.
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