We measure the r-band galaxy luminosity function ( LF ) across environments over the redshift range 0 < z < 0.107 using the SDSS .
We divide our sample into galaxies residing in large scale voids ( void galaxies ) and those residing in denser regions ( wall galaxies ) .
The best fitting Schechter parameters for void galaxies are : \log \Phi ^ { * } = -3.40 \pm 0.03 \log ( Mpc ^ { -3 } ) , M ^ { * } = -19.88 \pm 0.05 , and \alpha = -1.20 \pm 0.02 .
For wall galaxies , the best fitting parameters are : \log \Phi ^ { * } = -2.86 \pm 0.02 \log ( Mpc ^ { -3 } ) , M ^ { * } = -20.80 \pm 0.03 , and \alpha = -1.16 \pm 0.01 .
We find a shift in the characteristic magnitude , M ^ { * } , towards fainter magnitudes for void galaxies and find no significant difference between the faint-end slopes of the void and wall galaxy LFs .
We investigate how low surface brightness selections effects can affect the galaxy LF .
To attempt to examine a sample of galaxies that is relatively free of surface brightness selection effects , we compute the optical galaxy LF of galaxies detected by the blind H i survey , ALFALFA .
We find that the global LF of the ALFALFA sample is not well fit by a Schechter function , because of the presence of a wide dip in the LF around M _ { r } = -18 and an upturn at fainter magnitudes ( \alpha \sim - 1.47 ) .
We compare the H i selected r-band LF to various LFs of optically selected populations to determine where the H i selected optical LF obtains its shape .
We find that sample selection plays a large role in determining the shape of the LF .