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We present a new deep spectroscopic catalogue for Abell 85, within 3.0$\times$ 2.6 Mpc$^2$ and down to $M_{r} \sim M_{r}^* +6$. Using the VisibleMulti-Object Spectrograph at the Very Large Telescope (VIMOS@VLT) and theAutoFiber 2 at the William Herschel Telescope (AF2@WHT), we obtained almost1,430 new redshifts for galaxies with $m_r \leq 21$ mag and $\langle \mu_{e,r}\rangle \leq 24$ mag arcsec$^{-2}$. These redshifts, together with SDSS-DR6 andNED spectroscopic information, result in 460 confirmed cluster members. Thisdataset allows the study of the luminosity function (LF) of the clustergalaxies covering three orders of magnitudes in luminosities. The total andradial LFs are best modelled by a double Schechter function. The normalized LFsshow that their bright ($M_{r} \leq -21.5$) and faint ($M_{r}\geq -18.0$) endsare independent of clustercentric distance and similar to the field LFs unlikethe intermediate luminosity range ($-21.5 \leq M_{r} \leq -18.0$). Similarresults are found for the LFs of the dominant types of galaxies: red, passive,virialized and early-infall members. On the contrary, the LFs of blue, starforming, non-virialized and recent-infall galaxies are well described by asingle Schechter function. These populations contribute to a small fraction ofthe galaxy density in the innermost cluster region. However, in the outskirtsof the cluster, they have similar densities to red, passive, virialized andearly-infall members at the LF faint end. These results confirm a cleardependence of the colour and star formation of Abell 85 members in the clustercentric distance.

Deep spectroscopy of nearby galaxy clusters: I. Spectroscopic luminosity function of Abell 85