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.
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