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

Size distribution of galaxies in SDSS DR7: weak dependence on halo environment