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Context. The study of the galaxy stellar mass function (SMF) in relation tothe galaxy environment and the stellar mass density profile, rho(r), is apowerful tool to constrain models of galaxy evolution. Aims. We determine theSMF of the z=0.44 cluster of galaxies MACS J1206.2-0847 separately for passiveand star-forming (SF) galaxies, in different regions of the cluster, from thecenter out to approximately 2 virial radii. We also determine rho(r) to compareit to the number density and total mass density profiles. Methods. We use thedataset from the CLASH-VLT survey. Stellar masses are obtained by SED fittingon 5-band photometric data obtained at the Subaru telescope. We identify 1363cluster members down to a stellar mass of 10^9.5 Msolar. Results. The wholecluster SMF is well fitted by a double Schechter function. The SMFs of clusterSF and passive galaxies are statistically different. The SMF of the SF clustergalaxies does not depend on the environment. The SMF of the passive populationhas a significantly smaller slope (in absolute value) in the innermost (<0.50Mpc), highest density cluster region, than in more external, lower densityregions. The number ratio of giant/subgiant galaxies is maximum in thisinnermost region and minimum in the adjacent region, but then gently increasesagain toward the cluster outskirts. This is also reflected in a decreasingradial trend of the average stellar mass per cluster galaxy. On the other hand,the stellar mass fraction, i.e., the ratio of stellar to total cluster mass,does not show any significant radial trend. Conclusions. Our results appearconsistent with a scenario in which SF galaxies evolve into passive galaxiesdue to density-dependent environmental processes, and eventually get destroyedvery near the cluster center to become part of a diffuse intracluster medium.

CLASH-VLT: The stellar mass function and stellar mass density profile of the z=0.44 cluster of galaxies MACS J1206.2-0847