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The HARPS/HARPS-N Data Reduction Software (DRS) relies on thecross-correlation between the observed spectra and a suitable stellar mask tocompute a cross-correlation function (CCF) to be used both for the radialvelocity (RV) computation and as an indicator of stellar lines asymmetry,induced for example by the stellar activity. Unfortunately the M2 maskcurrently used by the HARPS/HARPS-N DRS for M-type stars results in heavilydistorted CCFs. We created several new stellar masks in order to decrease theerrors in the RVs and to improve the reliability of the activity indicators asthe bisector's span. We obtained very good results with a stellar mask createdfrom the theoretical line list provided by the VALD3 database for an earlyM-type star (T$_{\mathrm{eff}}$=3500~K and $\log{g}=4.5$). The CCF's shape andrelative activity indicators improved and the RV time-series allowed us torecover known exoplanets with periods and amplitudes compatible with theresults obtained with HARPS-TERRA.

Stellar masks and bisector's shape for M-type stars observed in the GAPS Programme with HARPS-N at TNG