Table 4: X-ray fluxes and luminosities.

Source		 $F_{\rm0.2-2~keV}$ $L_{\rm0.3-2~keV}$   $F_{\rm 2-10~keV}$ $L_{\rm 2-10~keV}$   $L_{\rm bol}/L_{\rm Edd}^b$
  $[{\rm erg~cm^{-2}~s^{-1}}]$ $[{\rm 10^{42}~erg~s^{-1}}]$ % $L_{\rm PL}^a$   $[{\rm erg~cm^{-2}~s^{-1}}]$ $[{\rm 10^{42}~erg~s^{-1}}]$ % $L_{\rm PL}^a$    
NGC 1692 $2.7\times10^{-13}$ 0.9 55%   $0.9\times10^{-13}$ 0.2 39%   $1\times 10^{-5}$

PKS 0625-35		 $4.7\times10^{-12}$ 78.2 98%   $2.6\times10^{-12}$ 18.7 100%   $2\times10^{-3}$

3C 88		 $1.4\times10^{-13}$ 0.4 34%   $2.8\times10^{-13}$ 0.5 99%   $2\times10^{-4}$

3C 444		 $6.8\times10^{-13}$ 63.0 50%   $5.1\times10^{-13}$ 33.1 78%   $3\times 10^{-3}$
a Percentage of the soft (hard) X-ray luminosity associated with the power-law component. b Eddington ratio $L_{\rm bol}/L_{\rm Edd}$, where $L_{\rm bol}$ was obtained by multiplying the 2-10 keV X-ray luminosity, associated with the power law, by a factor 20 (see text for details).

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