  In this paper we identify and study the properties of low mass dwarf
satellites of a nearby Local Group analogue - the NGC-3175 galaxy group with
the goal of investigating the nature of the lowest mass galaxies and the
`Missing Satellites' problem. Deep imaging of nearby groups such as NGC-3175
are one of the only ways to probe these low mass galaxies which are important
for problems in cosmology, dark matter and galaxy formation. We discover 553
candidate dwarf galaxies in the group, the vast majority of which have never
been studied before. We obtained R and B band imaging, with the ESO 2.2m,
around the central $\sim$500kpc region of NGC-3175, allowing us to detect
galaxies down to $\sim$23 mag (M$_{B} \sim$-7.7 mag) in the B band. In the
absence of spectroscopic information, dwarf members and likely background
galaxies are separated using colour, morphology and surface brightness
criteria. We compare the observed size, surface brightness and mass scaling
relations to literature data. The luminosity function with a faint end slope of
$\alpha$ = -1.31, is steeper than that observed in the Local Group. In
comparison with simulations, we find that our observations are between a pure
$\Lambda$CDM model and one involving baryonic effects, removing the apparent
problem of finding too few satellites as seen around the Milky Way.
