10 keV luminosity (ergs s$^{-1}$):   $(1.02\pm0.2)\times10^{44}$                            
  $\chi^2/$dof                                          1252/1058                                              

-3.0cm

    Region                                                                                          $\chi^2$/dof                                             
  ---------- ------------------------ ------------------------------------------------------- ------------------------ ------------------------------------- -----------
                   Photon Index        Normalization (photons keV$^{-1}$ cm$^{-2}$ s$^{-1}$)           T(keV)           Normalization ($10^{14}$ cm$^{-5}$)  
    Lobes     $1.71_{-0.17}^{+0.13}$           $5.76_{-1.54}^{+0.83} \times10^{-5}$            $1.36_{-0.17}^{+0.39}$   $5.98_{-2.77}^{+5.82}\times10^{-5}$   1229/1049
   Region 1             -                                        -                                 $1.18\pm0.11$        $1.01_{-0.25}^{+0.24}\times10^{-4}$   1146/1047
   Region 2             -                                        -                             $0.86_{-0.05}^{+0.13}$        $7.6\pm0.5\times10^{-5}$          862/623
   Region 3             -                                        -                             $1.72_{-0.49}^{+0.9}$        $4.56\pm1.23\times10^{-5}$          35/25

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### The lobes

To avoid having to mask out a large region, we extracted a spectrum for both the AGN and the lobes together and then fixed the parameters of the AGN model to the best-fitting values found in the analysis of the AGN spectrum (see previous section). We then added to the model a power law to model inverse-Compton emission from the lobes. In addition, we tried the fit both with and without an [*apec*]{} model intended to represent thermal emission from the regions in front of and behind the lobes in our extraction region. We found that the fit was marginally improved with the inclusion of an [*apec*]{} model with Galactic absorption and abundance fixed at 0.3 solar ($\chi^2/$dof was 1229/1049 with and 1241/1051 without the [*apec*]{} model) and so, given that we expect some thermal emission to be present 