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Low Surface Brightness Galaxies (LSBGs) are excellent probes of quenching andother environmental processes near massive galaxies. We study an extensivesample of LSBGs near massive hosts in the local universe that are distributedacross a diverse range of environments. The LSBGs with surface-brightness$\mu_{\rm eff,g}> $24.2 mag arcsec$^{-2}$ are drawn from the Dark Energy SurveyYear 3 catalog while the hosts with masses $9.0< log(M_{\star}/M_{\odot})<11.0$ comparable to the Milky Way and the Large Magellanic Cloud are selectedfrom the z0MGS sample. We study the projected radial density profiles of LSBGsas a function of their color and surface brightness around hosts in both therich Fornax-Eridanus cluster environment and the low-density field. We detectan overdensity with respect to the background density, out to 2.5 times thevirial radius for both hosts in the cluster environment and the isolated fieldgalaxies. When the LSBG sample is split by $g-i$ color or surface brightness$\mu_{\rm eff,g}$, we find the LSBGs closer to their hosts are significantlyredder and brighter, like their high surface-brightness counterparts. The LSBGsform a clear 'red sequence' in both the cluster and isolated environments thatis visible beyond the virial radius of the hosts. This suggests apre-processing of infalling LSBGs and a quenched backsplash population aroundboth host samples. However, the relative prominence of the 'blue cloud' featureimplies that pre-processing is ongoing near the isolated hosts compared to thecluster hosts.

Environmental Quenching of Low Surface Brightness Galaxies near Milky Way mass Hosts