The clustering of galaxies in the SDSS-III Baryon Oscillation
  Spectroscopic Survey: modeling of the luminosity and colour dependence in the
  Data Release 10
  We investigate the luminosity and colour dependence of clustering of CMASS
galaxies in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic
Survey Tenth Data Release. The halo occupation distribution framework is
adopted to model the projected two-point correlation function measurements on
small and intermediate scales (from $0.02$ to $60\,h^{-1}{\rm {Mpc}}$) and to
interpret the observed trends and infer the connection of galaxies to dark
matter halos. We find that luminous red galaxies reside in massive halos of
mass $M{\sim}10^{13}$--$10^{14}\,h^{-1}{\rm M_\odot}$ and more luminous
galaxies are more clustered and hosted by more massive halos. The strong
small-scale clustering requires a fraction of these galaxies to be satellites
in massive halos, with the fraction at the level of 5--8 per cent and
decreasing with luminosity. The characteristic mass of a halo hosting on
average one satellite galaxy above a luminosity threshold is about a factor
$8.7$ larger than that of a halo hosting a central galaxy above the same
threshold. At a fixed luminosity, progressively redder galaxies are more
strongly clustered on small scales, which can be explained by having a larger
fraction of these galaxies in the form of satellites in massive halos. Our
clustering measurements on scales below $0.4\,h^{-1}{\rm {Mpc}}$ allow us to
study the small-scale spatial distribution of satellites inside halos. While
the clustering of luminosity-threshold samples can be well described by a
Navarro-Frenk-White (NFW) profile, that of the reddest galaxies prefers a
steeper or more concentrated profile. Finally, we also use galaxy samples of
constant number density at different redshifts to study the evolution of
luminous galaxies, and find the clustering to be consistent with passive
evolution in the redshift range of $0.5 \lesssim z \lesssim 0.6$.
