The clustering of galaxies in the SDSS-III Baryon Oscillation
  Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy
  clustering
  With the largest spectroscopic galaxy survey volume drawn from the SDSS-III
Baryon Oscillation Spectroscopic Survey (BOSS), we can extract cosmological
constraints from the measurements of redshift and geometric distortions at
quasi-linear scales (e.g. above 50 $h^{-1}$Mpc). We analyze the broad-range
shape of the monopole and quadrupole correlation functions of the BOSS Data
Release 12 (DR12) CMASS galaxy sample, at the effective redshift $z=0.59$, to
obtain constraints on the Hubble expansion rate $H(z)$, the angular-diameter
distance $D_A(z)$, the normalized growth rate $f(z)\sigma_8(z)$, and the
physical matter density $\Omega_mh^2$. We obtain robust measurements by
including a polynomial as the model for the systematic errors, and find it
works very well against the systematic effects, e.g., ones induced by stars and
seeing. We provide accurate measurements $\{D_A(0.59)r_{s,fid}/r_s$ $\rm Mpc$,
$H(0.59)r_s/r_{s,fid}$ $km s^{-1} Mpc^{-1}$, $f(0.59)\sigma_8(0.59)$, $\Omega_m
h^2\}$ = $\{1427\pm26$, $97.3\pm3.3$, $0.488 \pm 0.060$, $0.135\pm0.016\}$,
where $r_s$ is the comoving sound horizon at the drag epoch and
$r_{s,fid}=147.66$ Mpc is the sound scale of the fiducial cosmology used in
this study. The parameters which are not well constrained by our galaxy
clustering analysis are marginalized over with wide flat priors. Since no
priors from other data sets, e.g., cosmic microwave background (CMB), are
adopted and no dark energy models are assumed, our results from BOSS CMASS
galaxy clustering alone may be combined with other data sets, i.e., CMB, SNe,
lensing or other galaxy clustering data to constrain the parameters of a given
cosmological model. The uncertainty on the dark energy equation of state
parameter, $w$, from CMB+CMASS is about 8 per cent. The uncertainty on the
curvature fraction, $\Omega_k$, is 0.3 per cent. We do not find deviation from
flat $\Lambda$CDM.
