Size distribution of galaxies in SDSS DR7: weak dependence on halo
  environment
  Using a sample of galaxies selected from the Sloan Digital Sky Survey Data
Release 7 (SDSS DR7) and a catalog of bulge-disk decompositions, we study how
the size distribution of galaxies depends on the intrinsic properties of
galaxies, such as concentration, morphology, specific star formation rate
(sSFR), and bulge fraction, and on the large-scale environments in the context
of central/satellite decomposition, halo environment, the cosmic web: \cluster,
\filament, \sheet ~and \void, as well as galaxy number density. We find that
there is a strong dependence of the luminosity- or mass-size relation on the
galaxy concentration, morphology, sSFR, and bulge fraction. Compared with
late-type (spiral) galaxies, there is a clear trend of smaller sizes and
steeper slope for early-type (elliptical) galaxies. Similarly, galaxies with
high bulge fraction have smaller sizes and steeper slope than those with low
bulge fraction. Fitting formula of the average luminosity- and mass-size
relations are provided for galaxies of these different intrinsic properties.
Examining galaxies in terms of their large scale environments, we find that the
mass-size relation has some weak dependence on the halo mass and
central/satellite segregation for galaxies within mass range $9.0\le \log
M_{\ast} \le 10.5$, where satellites or galaxies in more massive halos have
slightly smaller sizes than their counterparts. While the cosmic web and local
number density dependence of the mass-size relation is almost negligible.
