  Low Surface Brightness Galaxies (LSBGs) are excellent probes of quenching and
other environmental processes near massive galaxies. We study an extensive
sample of LSBGs near massive hosts in the local universe that are distributed
across 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 Survey
Year 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 selected
from the z0MGS sample. We study the projected radial density profiles of LSBGs
as a function of their color and surface brightness around hosts in both the
rich Fornax-Eridanus cluster environment and the low-density field. We detect
an overdensity with respect to the background density, out to 2.5 times the
virial radius for both hosts in the cluster environment and the isolated field
galaxies. 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 significantly
redder and brighter, like their high surface-brightness counterparts. The LSBGs
form a clear 'red sequence' in both the cluster and isolated environments that
is visible beyond the virial radius of the hosts. This suggests a
pre-processing of infalling LSBGs and a quenched backsplash population around
both host samples. However, the relative prominence of the 'blue cloud' feature
implies that pre-processing is ongoing near the isolated hosts compared to the
cluster hosts.
