to be $(1.55^{+0.24}_{-0.19})\times10^{44}$ ergs s$^{-1}$. We directly compared key parameters of both datasets (e.g. the absorbed column density) and found that there were no significant differences between the [*Chandra*]{} and [*XMM-Newton*]{} data. This suggests that there has been very little variability in the 6 years between the observations using [*Chandra*]{} and [*XMM-Newton*]{}.

Lobes
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Inverse-Compton emission from the lobes is clearly detected in our [*XMM-Newton*]{} data. Our flux density measurement ($40 \pm 4$ nJy at 1 keV) is in excellent agreement with the results from [*Chandra*]{} data: @itmismma02 give $41 \pm 15$ nJy while @chbw05 , in their analysis of the same data, quote $37 \pm 2$ nJy. Both previous analyses, like ours, fitted a combination of thermal and power-law models to the spectrum of the lobe region. The differences in the error bars presumably arises in part because Isobe [[et al.]{}]{} allowed the Galactic $N_{\rm H}$ to vary; we follow @chhbbw05 in keeping it fixed. Our measurement of the photon index of the power-law component is also very consistent with the results of @chbw05.

Environmental impact
--------------------

We can make a rough estimate of the work done by the lobes on the environment. Modelling the lobes as a cylinder 