Measuring neutrino mass imprinted on the anisotropic galaxy clustering
  The anisotropic galaxy clustering of large scale structure observed by the
Baryon Oscillation Spectroscopic Survey Data Release 11 is analyzed to probe
the sum of neutrino mass in the small $m_\nu < 1eV$ limit in which the early
broadband shape determined before the last scattering surface is immune from
the variation of $m_\nu$. The signature of $m_\nu$ is imprinted on the altered
shape of the power spectrum at later epoch, which provides an opportunity to
access the non--trivial $m_\nu$ through the measured anisotropic correlation
function in redshift space (hereafter RSD instead of Redshift Space
Distortion). The non--linear RSD corrections with massive neutrinos in the
quasi linear regime are approximately estimated using one-loop order terms
computed by tomographic linear solutions. We suggest a new approach to probe
$m_\nu$ simultaneously with all other distance measures and coherent growth
functions, exploiting this deformation of the early broadband shape of the
spectrum at later epoch. If the origin of cosmic acceleration is unknown,
$m_\nu$ is poorly determined after marginalising over all other observables.
However, we find that the measured distances and coherent growth functions are
minimally affected by the presence of mild neutrino mass. Although the standard
model of cosmic acceleration is assumed to be the cosmological constant, the
constraint on $m_\nu$ is little improved. Interestingly, the measured CMB
distance to the last scattering surface sharply slices the degeneracy between
the matter content and $m_\nu$, and the hidden $m_\nu$ is excavated to be
$m_\nu=0.19^{+0.28}_{-0.17} eV$ which is different from massless neutrino more
than 68% confidence.
