galaxies in this redshift range: the cumulative number density of ${\mathcal{M}_*}>10^{10}{\mathcal{M}_{\sun}}$ galaxies has increased by $\sim30$% since $z\sim0.6$ and the cumulative number density of ${\mathcal{M}_*}>10^{11}{\mathcal{M}_{\sun}}$ galaxies has changed by $<\pm10$% since $z\sim1$. Much stronger, differing evolution is found when the sample is divided into quiescent and star-forming galaxies, placing strong constraints on the rates of star formation quenching that builds up the quiescent population. In this paper, however, we consider only the global SMF and attempt to reconcile the relative lack of evolution in the SMF of galaxies with the strong evolution observed in the AGN population.

The distribution of specific accretion rates {#sec:accdist}
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To populate galaxies with AGNs we adopt measurements of the distribution of SMBH accretion rates for a given stellar mass and redshift from @Aird12. In @Aird12 we identified AGNs within the PRIMUS galaxy sample using hard (2–10 keV) X-ray observations of three of the PRIMUS fields. We then studied the probability of a galaxy hosting an AGN as a function of the stellar mass.

We used hard X-ray selection to identify AGNs because X-ray emission from a moderately luminous AGN ($L_\mathrm{2-10keV}\gtrsim10^{42}$ [$\mathrm{erg\;s^{-1}}$]{}) will dominate over other processes within the host galaxy (such as the combined 