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 \leq \log M _ { \ast } \leq 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 .