  We explore the distribution of RMS=SFR/SFR_MS (where SFR_MS is the star
formation rate of "Main Sequence" star-forming galaxies) for AGN hosts at z=1.
We split our sample into two bins of X-ray luminosity divided at Lx=2x10^43erg
s-1 to investigate whether the RMS distribution changes as a function of AGN
power. Our main results suggest that, when the RMS distribution of AGN hosts is
modelled as a log-normal distribution (i.e. the same shape as that of MS
galaxies), galaxies hosting more powerful X-ray AGNs (i.e. Lx>2x10^43erg s-1)
display a narrower RMS distribution that is shifted to higher values compared
to their lower Lx counterparts. In addition, we find that more powerful X-ray
AGNs have SFRs that are more consistent with that of MS galaxies compared to
lower Lx AGNs. Despite this, the mean SFRs (as opposed to RMS) measured from
these distributions are consistent with the previously observed flat
relationship between SFR and Lx. Our results suggest that the typical
star-forming properties of AGN hosts change with Lx , and that more powerful
AGNs typically reside in more MS-like star-forming galaxies compared to lower
Lx AGNs.
