Stellar masses of SDSS-III/BOSS galaxies at z ∼ 0.5 and constraints to galaxy formation models

We calculate stellar masses for similar to 400 000 massive luminous galaxies at redshift similar to 0.2-0.7 using the first two years of data from the Baryon Oscillation Spectroscopic Survey (BOSS). Stellar masses are obtained by fitting model spectral energy distributions to u, g, r, i, z magnitudes, and simulations with mock galaxies are used to understand how well the templates recover the stellar mass. Accurate BOSS spectroscopic redshifts are used to constrain the fits. We find that the distribution of stellar masses in BOSS is narrow (delta log M similar to 0.5 dex) and peaks at about log M/M-circle dot similar to 11.3 (for a Kroupa initial stellar mass function), and that the mass sampling is uniform over the redshift range 0.2-0.6, in agreement with the intended BOSS target selection. The galaxy masses probed by BOSS extend over similar to 10(12) M-circle dot, providing unprecedented measurements of the high-mass end of the galaxy mass function. We find that the galaxy number density above similar to 2.5 x 10(11) M-circle dot agrees with previous determinations. We perform a comparison with semi-analytic galaxy formation models tailored to the BOSS target selection and volume, in order to contain incompleteness. The abundance of massive galaxies in the models compare fairly well with the BOSS data, but the models lack galaxies at the massive end. Moreover, no evolution with redshift is detected from similar to 0.6 to 0.4 in the data, whereas the abundance of massive galaxies in the models increases to redshift zero. Additionally, BOSS data display colour-magnitude (mass) relations similar to those found in the local Universe, where the most massive galaxies are the reddest. On the other hand, the model colours do not display a dependence on stellar mass, span a narrower range and are typically bluer than the observations. We argue that the lack of a colour-mass relation for massive galaxies in the models is mostly due to metallicity, which is too low in the models.