Revised Mass-to-Light Ratios For Nearby Galaxy Groups and Clusters
  We present a detailed investigation of the cluster stellar mass-to-light
(M*/L) ratio and cumulative stellar masses, derived on a galaxy-by-galaxy
basis, for 12 massive (M500 ~ 10^14 - 10^15 Msun), nearby clusters with
available optical imaging data from the Sloan Digital Sky Survey Data Release
10 and X-ray data from the Chandra X-ray Observatory. Our method involves a
statistical cluster membership using both photometric and spectroscopic
redshifts when available to maximize completeness whilst minimizing
contamination effects. We show that different methods of estimating the stellar
mass-to-light ratio from observed photometry result in systematic discrepancies
in the total stellar masses and average mass-to-light ratios of cluster
galaxies. Nonetheless, all conversion methodologies point to a lack of
correlation between M*/Li and total cluster mass, even though low-mass groups
contain relatively more blue galaxies. We also find no statistically
significant correlation between M*/Li and the fraction of blue galaxies. For
the mass range covered by our sample, the assumption of a Chabrier IMF yields
an integrated M*/Li = 1.7 +/- 0.2 Msun/Lsun, a lower value than used in most
similar studies, though consistent with the study of low-mass galaxy groups by
Leauthaud et al. (2012). A light (diet) Salpeter IMF would imply a ~60%
increase in M*/Li.
