Bulge Classification using MaNGA

Numerous studies have demonstrated strong correlations between the galaxy bulges and other host galaxy properties suggest that understanding bulge evolutions is a crucial for any complete theory for galaxy evolution. Galaxy bulges come in two flavours; rotations supported Pseudo bulges and dispersion-supported Classical bulges. These bulge types have distinct properties like galaxy Sersic index and their position in the Kormendy relation, which have been traditionally used for the classification of galaxy bulges. However, these properties are secondary as they do not probe the galaxy bulges directly. We have performed the photometric and kinematic classification of ~2300 galaxies from the Mapping of Nearby Galaxies at the Apache point observatory (MaNGA) survey. We have defined classical and pseudo bulge host (CBH & PBH) galaxies using Sloan Digital Sky Survey (SDSS) r-band photometric data we formed Kormendy relation of slope 2.17, offset of 17.53 and a scatter of 1.06 within the ellipticals classified by PyMorph and Deep Learning. We use Simard 2011 derived bulge properties to separate classical and pseudo bulges by their distance from the derived Kormendy relation. We use this to investigate the performance of traditional classification techniques to disentangle Pseudo-bulge and Classical bulge host galaxies. Utilizing a classification based on galaxy kinematics, we study the disk signatures in the formation of S0 galaxies