The clustering of galaxies in the SDSS-III Baryon Oscillation
  Spectroscopic Survey: single-probe measurements and the strong power of
  normalized growth rate on constraining dark energy
  We present measurements of the anisotropic galaxy clustering from the Data
Release 9 (DR9) CMASS sample of the SDSS-III Baryon Oscillation Spectroscopic
Survey (BOSS). We analyze the broad-range shape of the monopole and quadrupole
correlation functions to obtain constraints, at the effective redshift $z=0.57$
of the sample, on the Hubble expansion rate $H(z)$, the angular-diameter
distance $D_A(z)$, the normalized growth rate $f(z)\sigma_8(z)$, the physical
matter density $\Omega_m h^2$, and the biased amplitude of matter fluctuation
b\sigma_8(z). We obtain {$H(0.57)$, $D_A(0.57)$, $f(0.57)\sigma_8(0.57)$,
$\Omega_m h^2$, $b\sigma_8(0.57)$} = {$87.6_{-6.8}^{+6.7}$, $1396\pm73$,
$0.126_{-0.010}^{+0.008}$, $1.19\pm0.14$, $0.428\pm0.066$} and their covariance
matrix as well. The parameters which are not well constrained by our of galaxy
clustering analysis are marginalized over with wide flat priors. Since no
priors from other data sets (i.e., 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. We
show that the major power on constraining dark energy from the anisotropic
galaxy clustering signal, as compared to the angular-averaged one (monopole),
arises from including the normalized growth rate $f(z)\sigma_8(z)$. In the case
of the wCDM cosmological model our single-probe CMASS constraints, combined
with CMB (WMAP9+SPT), yield a value for the dark energy equation of state
parameter of $w=-0.90\pm0.11$. Therefore, it is important to include
$f(z)\sigma_8(z)$ while investigating the nature of dark energy with current
and upcoming large-scale galaxy surveys.
