(a) ﹩\Gamma _{s}﹩(0.5–2 keV) vs. ﹩M_{\mathrm{BH}\,}﹩. Observations from this paper (filled circles) fill in the low‐mass region of this diagram, and demonstrate that ﹩\Gamma _{s}﹩ is not determined by ﹩M_{\mathrm{BH}\,}﹩. For comparison we include the optically selected samples of Williams et al. (2004; open circles) and the PG quasars observed with XMM‐Newton from Porquet et al. (2004; open squares). NGC 4395 is plotted as an asterisk. (b) ﹩\Gamma _{s}﹩ vs. ﹩L_{0.5{\mbox{--}} 2\ \mathrm{keV}\,}﹩. (c) ﹩\Gamma _{s}﹩ vs. ﹩L_{\mathrm{bol}\,}/ L_{\mathrm{Edd}\,}﹩. We have estimated ﹩L_{\mathrm{bol}\,}/ L_{\mathrm{Edd}\,}﹩ from the optical luminosity alone, assuming ﹩L_{\mathrm{bol}\,}=9L_{5100\ \Å }﹩, in order to avoid potential secondary correlations between X‐ray luminosity and slope, introduced, for instance, by our increased sensitivity to soft sources.