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In this paper we identify and study the properties of low mass dwarfsatellites of a nearby Local Group analogue - the NGC-3175 galaxy group withthe goal of investigating the nature of the lowest mass galaxies and the`Missing Satellites' problem. Deep imaging of nearby groups such as NGC-3175are one of the only ways to probe these low mass galaxies which are importantfor problems in cosmology, dark matter and galaxy formation. We discover 553candidate dwarf galaxies in the group, the vast majority of which have neverbeen 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 detectgalaxies down to $\sim$23 mag (M$_{B} \sim$-7.7 mag) in the B band. In theabsence of spectroscopic information, dwarf members and likely backgroundgalaxies are separated using colour, morphology and surface brightnesscriteria. We compare the observed size, surface brightness and mass scalingrelations to literature data. The luminosity function with a faint end slope of$\alpha$ = -1.31, is steeper than that observed in the Local Group. Incomparison with simulations, we find that our observations are between a pure$\Lambda$CDM model and one involving baryonic effects, removing the apparentproblem of finding too few satellites as seen around the Milky Way.

Faint Satellite Population of the NGC-3175 Group - a Local Group Analogue