Star-formation efficiency and metal enrichment of the intracluster
  medium in local massive clusters of galaxies
  We have investigated the baryon-mass content in a subsample of 19 clusters of
galaxies extracted from the X-ray flux-limited sample HIFLUGCS according to
their positions in the sky. For these clusters, we measured total masses and
characteristic radii on the basis of a rich optical spectroscopic data set, the
physical properties of the intracluster medium (ICM) using XMM-Newton and ROSAT
X-ray data, and total (galaxy) stellar masses utilizing the SDSS DR7 multi-band
imaging. The observed (hot) gas-mass fractions are almost constant in this mass
range. We confirm that the stellar mass fraction decreases as the total mass
increases and shows (20+/-4)% scatter; in addition, we show that it decreases
as the central entropy increases. The latter behavior supports a twofold
interpretation where heating from merging quenches the star-formation activity
of galaxies in massive systems, and feedback from supernovae and/or radio
galaxies drives a significant amount of gas to the regions beyond r_{500} or,
alternatively, a substantially large amount of intracluster light (ICL) is
associated with galaxies in nonrelaxed systems. Furthermore, less massive
clusters are confirmed to host less gas per unit total mass; however, they
exhibit higher mass fractions in metals, so that their ICM is more metal-rich.
This again supports the interpretation that in the potential wells of low-mass
systems the star-formation efficiency of galaxies was high or, alternatively,
some gas is missing from the hot phase of the ICM. The former hypothesis is
preferred as the main driver of the mass-dependent metal enrichment since the
total mass-to-optical luminosity ratio increases as the total mass increases.
