The Fate of Stellar Mass Loss in Central Cluster Galaxies
  Star formation within the central galaxies of galaxy clusters is often
interpreted as being fueled by cooling of the hot intracluster medium. However,
the star-forming gas is dusty, and Spitzer spectra show that the dust
properties are similar to those in more normal star-forming environments, in
which the dust has come from the winds of dying stars. Here we consider whether
the primary source of the star-forming gas in central cluster galaxies could be
normal stellar mass loss. We show that the overall stellar mass-loss rate in a
large central galaxy (~4-8 solar masses per year) is at least as large as the
observed star-formation rates in all but the most extreme cases and must be
included in any assessment of the gas-mass budget of a central cluster galaxy.
We also present arguments suggesting that the gas shed by stars in galaxy
clusters with high core pressures and short central cooling times may remain
cool and distinct from its hot surroundings, thereby preserving the dust within
it.
