Relative distribution of dark matter and stellar mass in three massive
  galaxy clusters
  This work observationally addresses the relative distribution of total and
optically luminous matter in galaxy clusters by computing the radial profile of
the stellar-to-total mass ratio. We adopt state-of-the-art accurate lensing
masses free from assumptions about the mass radial profile and we use extremely
deep multicolor wide--field optical images to distinguish star formation from
stellar mass, to properly calculate the mass in galaxies of low mass, those
outside the red sequence, and to allow a contribution from galaxies of low mass
that is clustercentric dependent. We pay special attention to issues and
contributions that are usually underrated, yet are major sources of
uncertainty, and we present an approach that allows us to account for all of
them. Here we present the results for three very massive clusters at
$z\sim0.45$, MACSJ1206.2-0847, MACSJ0329.6-0211, and RXJ1347.5-1145. We find
that stellar mass and total matter are closely distributed on scales from about
150 kpc to 2.5 Mpc: the stellar-to-total mass ratio is radially constant. We
find that the characteristic mass stays constant across clustercentric radii
and clusters, but that the less-massive end of the galaxy mass function is
dependent on the environment.
