SIMBAD references

We explore the distribution of R_MS ≡ 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 L_X = 2 x 10⁴³ erg s^–1 to investigate whether the R_MS distribution changes as a function of AGN power. Our main results suggest that, when the R_MS 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. L_X > 2 x 10⁴³ erg s^–1) display a narrower R_MS distribution that is shifted to higher values compared to their lower L_X 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 L_X AGNs. Despite this, the mean SFRs (as opposed to R_MS) measured from these distributions are consistent with the previously observed flat relationship between SFR and L_X. Our results suggest that the typical star-forming properties of AGN hosts change with L_X, and that more powerful AGNs typically reside in more MS-like star-forming galaxies compared to lower L_X AGNs.