  We present the identification and analysis of an X-ray selected AGN sample
that lie within the local ($z < 0.35$) galaxy population. From a parent sample
of 22,079 MPA-JHU (based on SDSS DR8) galaxies, we identified 917 galaxies with
central, excess X-ray emission (from 3XMM-DR7) likely originating from an AGN.
We measured the host galaxies' star formation rates and classified them as
either star-forming or quiescent based on their position relative to main
sequence of star formation. Only 72% of the X-ray selected sample were
identified as AGN using BPT selection; this technique is much less effective in
quiescent hosts, only identifying 50% of the X-ray AGN. We also calculated the
growth rates of the black holes powering these AGN in terms of their specific
accretion rate ($\propto \mathrm{L_X/M_*}$) and found quiescent galaxies, on
average, accrete at a lower rate than star-forming galaxies. Finally, we
measured the sensitivity function of 3XMM so we could correct for observational
bias and construct probability distributions as a function of accretion rate.
AGN were found in galaxies across the full range of star formation rates
($\log_{10} \mathrm{SFR/M_\odot\ yr^{-1}} = -3\ \mathrm{to}\ 2$) in both
star-forming and quiescent galaxies. The incidence of AGN was enhanced by a
factor 2 (at a 3.5$\sigma$ significance) in star-forming galaxies compared to
quiescent galaxies of equivalent stellar mass and redshift, but we also found a
significant population of AGN hosted by quiescent galaxies.
