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Faint dwarf satellite galaxies are important as tracers of small-scalestructure, but remain poorly characterized outside the Local Group, due to thedifficulty of identifying them consistently at larger distances. We review arecently proposed method for estimating the average satellite population arounda given sample of nearby bright galaxies, using a combination of size andmagnitude cuts (to select low-redshift dwarf galaxies preferentially) andclustering measurements (to estimate the fraction of true satellites in the cutsample). We test this method using the high-precision photometric redshiftcatalog of the COSMOS survey, exploring the effect of specific cuts on theclustering signal. The most effective of the size-magnitude cuts consideredrecover the clustering signal around low-redshift primaries (z < 0.15) withabout two-thirds of the signal and 80\%\ of the signal-to-noise ratioobtainable using the full COSMOS photometric redshifts. These cuts are alsofairly efficient, with more than one third of the selected objects beingclustered satellites. We conclude that structural selection represents a usefultool in characterizing dwarf populations to fainter magnitudes and/or overlarger areas than are feasible with spectroscopic surveys.} In reviewing thelow-redshift content of the COSMOS field, we also note the existence of severaldozen objects that appear resolved or partially resolved in the HST imaging,and are confirmed to be local (at distances of $\sim$250 Mpc or less) by theirphotometric or spectroscopic redshifts. This underlines the potential forfuture space-based surveys to reveal local populations of intrinsically faintgalaxies through imaging alone.

Quantifying the abundance of faint, low-redshift satellite galaxies in the COSMOS survey