Gas depletion in cluster galaxies depends strongly on their internal
  structure
  We analyze galaxies in 300 nearby groups and clusters identified in the Sloan
Digital Sky Survey using a photometric gas mass indicator that is useful for
estimating the degree to which the interstellar medium of a cluster galaxy has
been depleted. We study the radial dependence of inferred gas mass fractions
for galaxies of different stellar masses and stellar surface densities. At
fixed clustercentric distance and at fixed stellar mass, lower density galaxies
are more strongly depleted of their gas than higher density galaxies. An
analysis of depletion trends in the two-dimensional plane of stellar mass $M_*$
and stellar mass surface density $\mu_*$ reveals that gas depletion at fixed
clustercentric radius is much more sensitive to the density of a galaxy than to
its mass. We suggest that low density galaxies are more easily depleted of
their gas, because they are more easily affected by ram-pressure and/or tidal
forces. We also look at the dependence of our gas fraction/radius relations on
the velocity dispersion of the cluster, finding no clear systematic trend.
