In an earlier paper, we determined the morphological types of galaxies in the Coma Cluster using data from the HST/ACS Coma Cluster treasury survey. We found that of the 132 members, 51 are non dwarfs and 81 are dwarfs. We define dwarfs to have a absolute luminosity $M_{ F814W}\geq -18.5$ as in \cite{ 2012ApJ...746..136M}. In this paper, we determine the morphological types of these dwarf galaxies and make a detailed study of their properties. Using GALFIT, we determine the structural properties of our sample and with spectroscopic redshifts, we determined memberships and distances to identify dwarfs. A visual examination of the residual images reveals that our sample of 78 dwarf galaxies comprises of: dwarf lenticular (\textit{ dS0}) 22\%, dwarf Elliptical ($dE$) 69\%, dwarf spirals (\textit{ dSp}) 4\%, dwarf ring (\textit{ dring}) 1\%, dwarf barred spirals (\textit{ dSBp}) 3\% and dwarf irregular (\textit{ dIrr}) 1\% galaxies. We find that the bulge-disk decomposition (S\'ersic + exponential) fits are good only for the \textit{ dS0} galaxies. The remainder of the sample gives good fits only for single S\'ersic fits. The Colour Magnitude Relation (CMR) shows that the $dEs$ are redder and fainter than the rest of the sample (except one $dIrr$ galaxy). The Kormendy relation reveals that $dE$ galaxies have lower surface brightness than the rest of the sample. Our research leads us to the conclusion that dwarf galaxies appear to have a different formation and evolution process than non-dwarf galaxies.
Categories: astro-ph.GA