  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 Visible
Multi-Object Spectrograph at the Very Large Telescope (VIMOS@VLT) and the
AutoFiber 2 at the William Herschel Telescope (AF2@WHT), we obtained almost
1,430 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 and
NED spectroscopic information, result in 460 confirmed cluster members. This
dataset allows the study of the luminosity function (LF) of the cluster
galaxies covering three orders of magnitudes in luminosities. The total and
radial LFs are best modelled by a double Schechter function. The normalized LFs
show that their bright ($M_{r} \leq -21.5$) and faint ($M_{r}\geq -18.0$) ends
are independent of clustercentric distance and similar to the field LFs unlike
the intermediate luminosity range ($-21.5 \leq M_{r} \leq -18.0$). Similar
results 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, star
forming, non-virialized and recent-infall galaxies are well described by a
single Schechter function. These populations contribute to a small fraction of
the galaxy density in the innermost cluster region. However, in the outskirts
of the cluster, they have similar densities to red, passive, virialized and
early-infall members at the LF faint end. These results confirm a clear
dependence of the colour and star formation of Abell 85 members in the cluster
centric distance.
