Internal kinematics of groups of galaxies in the Sloan Digital Sky
  Survey data release 7
  We present measurements of the velocity dispersion profile (VDP) for galaxy
groups in the final data release of the Sloan Digital Sky Survey (SDSS). For
groups of given mass we estimate the redshift-space cross-correlation function
(CCF) with respect to a reference galaxy sample, xi(r_p, pi), the projected
CCF, w_p(r_p), and the real-space CCF, xi(r). The VDP is then extracted from
the redshift distortion in xi(r_p, pi), by comparing xi(r_p, pi) with xi(r). We
find that the velocity dispersion (VD) within virial radius (R_200) shows a
roughly flat profile, with a slight increase at radii below ~0.3 R_200 for high
mass systems. The average VD within the virial radius, sigma_v, is a strongly
increasing function of central galaxy mass. We apply the same methodology to
N-body simulations with the concordance Lambda cold dark matter cosmology but
different values of the density fluctuation parameter sigma_8, and we compare
the results to the SDSS results. We show that the sigma_v-M_* relation from the
data provides stringent constraints on both sigma_8 and sigma_ms, the
dispersion in log M_* of central galaxies at fixed halo mass. Our best-fitting
model suggests sigma_8 = 0.86 +/- 0.03 and sigma_ms = 0.16 +/- 0.03. The
slightly higher value of sigma_8 compared to the WMAP7 result might be due to a
smaller matter density parameter assumed in our simulations. Our VD
measurements also provide a direct measure of the dark matter halo mass for
central galaxies of different luminosities and masses, in good agreement with
the results obtained by Mandelbaum et al. (2006) from stacking the
gravitational lensing signals of the SDSS galaxies.
