Multi-frequency studies of galaxies and groups: I. Environmental effect
  on galaxy stellar mass and morphology
  To understand the role of the environment in galaxy formation, evolution, and
present-day properties, it is essential to study the multi-frequency behavior
of different galaxy populations under various environmental conditions. We
crossmatch the SDSS DR10 group catalog with GAMA Data Release 2 and Wide-field
Survey Explorer (WISE) data to construct a catalog of 1651 groups and 11436
galaxies containing photometric information in 15 different wavebands ranging
from ultraviolet (0.152 {\mu}m) to mid-infrared (22 {\mu}m). We perform the
spectral energy distribution (SED) fitting of galaxies using the MAGPHYS code
and estimate the rest frame luminosities and stellar masses. We use the 1/Vmax
method to estimate the galaxy stellar mass and luminosity functions, and the
luminosity density field of galaxies to define the large scale environment of
galaxies. The stellar mass functions of both central and satellite galaxies in
groups are different in low and high density large scale environments.
Satellite galaxies in high density environments have a steeper low mass end
slope compared to low density environments, independently of the galaxy
morphology. Central galaxies in low density environments have a steeper low
mass end slope but the difference disappears for fixed galaxy morphology. The
characteristic stellar mass of satellite galaxies is higher in high density
environments and the difference exists only for galaxies with elliptical
morphologies. Galaxy formation in groups is more efficient in high density
large scale environments. Groups in high density environments have higher
abundances of satellite galaxies, irrespective of the satellite galaxy
morphology. The elliptical satellite galaxies are generally more massive in
high density environments. The stellar masses of spiral satellite galaxies show
no dependence on the large scale environment.
