Using a new spectroscopic sample and methods accounting for spectroscoic sampling fractions that vary in magnitude and surface brightness , we present R-band galaxy luminosity functions ( GLFs ) for six nearby galaxy clusters with redshifts 4000 < cz < 20000 km/s and velocity dispersions 700 < \sigma < 1250 km/s .
In the case of the nearest cluster , Abell 1060 , our sample extends to M _ { R } = -14 ( 7 magnitudes below M ^ { * } ) , making this the deepest spectroscopic determination of the cluster GLF to date .
Our methods also yield composite GLFs for cluster and field galaxies to M _ { R } = -17 ( M ^ { * } +4 ) , including the GLFs of subsamples of star forming and quiescent galaxies .
The composite GLFs are consistent with Schechter functions ( M ^ { * } _ { R } = -21.14 ^ { +0.17 } _ { -0.17 } , \alpha = -1.21 ^ { +0.08 } _ { -0.07 } for the clusters , M ^ { * } _ { R } = -21.15 ^ { +0.16 } _ { -0.16 } , \alpha = -1.28 ^ { +0.12 } _ { -0.11 } for the field ) .
All six cluster samples are individually consistent with the composite GLF down to their respective absolute magnitude limits , but the GLF of the quiescent population in clusters is not universal .
There are also significant variations in the GLF of quiescent galaxies between the field and clusters that can be described as a steepening of the faint end slope .
The overall GLF in clusters is consistent with that of field galaxies , except for the most luminous tip , which is enhanced in clusters versus the field .
The star formation properties of giant galaxies are more strongly correlated with the environment than those of fainter galaxies .