  We provide constraints on the accuracy with which the neutrino mass fraction,
$f_{\nu}$, can be estimated when exploiting measurements of redshift-space
distortions, describing in particular how the error on neutrino mass depends on
three fundamental parameters of a characteristic galaxy redshift survey:
density, halo bias and volume. In doing this, we make use of a series of dark
matter halo catalogues extracted from the BASICC simulation. The mock data are
analysed via a Markov Chain Monte Carlo likelihood analysis. We find a fitting
function that well describes the dependence of the error on bias, density and
volume, showing a decrease in the error as the bias and volume increase, and a
decrease with density down to an almost constant value for high density values.
This fitting formula allows us to produce forecasts on the precision achievable
with future surveys on measurements of the neutrino mass fraction. For example,
a Euclid-like spectroscopic survey should be able to measure the neutrino mass
fraction with an accuracy of $\delta f_{\nu} \approx 6.7\times10^{-4}$, using
redshift-space clustering once all the other cosmological parameters are kept
fixed to the $\Lambda$CDM case.
