  We study galaxy distributions with Sloan Digital Sky Survey SDSS DR14 data
and with simulations searching for variables that can constrain neutrino
masses. To be specific, we consider the scenario of three active neutrino
eigenstates with approximately the same mass, so $\sum m_\nu = 3 m_\nu$.
Fitting the predictions of the $\Lambda$CDM model to the Sachs-Wolfe effect,
$\sigma_8$, the galaxy power spectrum $P_\textrm{gal}(k)$, fluctuations of
galaxy counts in spheres of radii ranging from $16/h$ to $128/h$ Mpc, BAO
measurements, and $h = 0.678 \pm 0.009$, in various combinations, with free
spectral index $n$, and free galaxy bias and galaxy bias slope, we obtain
consistent measurements of $\sum m_\nu$. The results depend on $h$, so we have
presented confidence contours in the $(\sum m_\nu, h)$ plane. A global fit with
$h = 0.678 \pm 0.009$ obtains $\sum m_\nu = 0.719 \pm 0.312 \textrm{
(stat)}^{+0.055}_{-0.028}
  \textrm{ (syst)}$ eV, and the amplitude and spectral index of the power
spectrum of linear density fluctuations $P(k)$: $N^2 = (2.09 \pm 0.33) \times
10^{-10}$, and $n = 1.021 \pm 0.075$. The fit also returns the galaxy bias $b$
including its scale dependence.
