We present our discovery and analysis of dwarf galaxies in the NGC 3585 galaxy group by the KMTNet Supernova Program .
Using deep stack images reaching \simeq 28 mag arcsec ^ { -2 } in BVI , we discovered 46 dwarf galaxy candidates distributed in a 7 square degree field .
The dwarf galaxy candidates exhibit central surface brightness as faint as \mu _ { 0 ,V } = 26.2 mag arcsec ^ { -2 } , with effective radii larger than 150 pc and total absolute magnitudes brighter than M _ { V } \approx - 10 mag , if at the distance of NGC 3585 .
The dwarf galaxy surface number density decreases with projected distance from NGC 3585 .
We estimate the background contamination to be about 20 % based both on the number density profile and on diffuse galaxy counts in a control field . The dwarf galaxy colors and Sérsic structural parameters are consistent with those found for other dwarf galaxies .
Unusually , there is no indication of a change of color or brightness in the dwarf galaxy candidates with projected distance from the group center .
Approximately 20 % of them contain an unresolved nucleus .
The nucleated fraction is larger for brighter ( and redder ) galaxies but is independent of distance from the group center .
We identify four ultra-diffuse galaxy candidates , all near the group center .
We interpret these spatial properties as suggesting that the NGC 3585 group might be dynamically younger than the typical group .
The galaxy luminosity function of the NGC 3585 group has a faint-end slope of \alpha \approx - 1.39 , which is roughly consistent with the slopes found for other nearby groups .
The possible dependence of the slope on global group properties is still unclear , and continues to motivate our homogeneous deep survey of dozens of nearby groups .