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To better understand the formation of large, low surface brightness galaxies,we measure the correlation function between ultra-diffuse galaxy (UDG)candidates and Milky Way analogs (MWAs). We find that (1) the projected radialdistribution of UDG satellites (projected surface density $\proptor^{-0.84\pm0.06}$) is consistent with that of normal satellite galaxies, (2)the number of UDG satellites per MWA ($S_{\rm UDG}$) is $\sim 0.5\pm0.1$ overprojected radii from 20 to 250 kpc and $-17< M_r < -13.5$, (3) $S_{\rm UDG}$ isconsistent with a linear extrapolation of the relationship between the numberof UDGs per halo vs. halo mass obtained over galaxy group and cluster scales,(4) red UDG satellites dominate the population of UDG satellites ($\sim80$%),(5) over the range of satellite magnitudes studied, UDG satellites comprise$\sim$ 10% of the satellite galaxy population of MWAs, (6) a significantfraction of these ($\sim$13%) have estimated total masses $>$ 10$^{10.9}$M$_\odot$ or, equivalently, at least half the halo mass of the LMC, andpopulate a large fraction ($\sim$ 18%) of the expected subhalos down to thesemasses. All of these results suggest a close association between the overalllow mass galaxy population and UDGs, which we interpret as favoring modelswhere UDG formation principally occurs within the general context of low massgalaxy formation over models invoking more exotic physical processesspecifically invoked to form UDGs.

Systematically Measuring Ultra-Diffuse Galaxies (SMUDGes). IV. Ultra-Diffuse Satellites of Milky Way Analogs