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 \times 10 ^ { -4 } , using redshift-space clustering once all the other cosmological parameters are kept fixed to the \Lambda CDM case .