![Caption of the figure: The spectroscopic LF of A85 (gray shadow), blue and red diamonds show the LF of blue and red galaxies of A85. The full lines correspond to the Schecter function fits. The histograms are the LF of field red and blue galaxies (Blanton Caption of the figure: The spectroscopic LF of A85 (gray shadow), blue and red diamonds show the LF of blue and red galaxies of A85. The full lines correspond to the Schecter function fits. The histograms are the LF of field red and blue galaxies (Blanton](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/resultados135_147.jpg?itok=jF-LLy33)
We present a new deep determination of the spectroscopic LF within the virial radius of the nearby and massive Abell 85 (A85) cluster down to the dwarf regime (M*+6) using VLT/VIMOS spectra for ~2000 galaxies with m r ≤ 21 mag and <μ e,r > ≤ 24 mag arcsec -2. The resulting LF from 438 cluster members is best modeled by a double Schechter function due to the presence of a statistically significant upturn at the faint-end. The amplitude of this upturn (α f = -1.58 +0.19 -0.15), however, is much smaller than that of the SDSS composite photometric cluster LF by Popesso et al. (2006, α f ~-2)
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