a narrow-line radio galaxy and the unification angle for these objects is of that order (e.g. @b89; @hwb98). Investigating different projection angles in the range $0^\circ < \theta < 45^\circ$, we find that although an increase in $\theta$ means a drop in internal pressure, as expected, it tends to increase the ratio between the internal and external pressures, up to a value of 3.2 at $\theta = 45^\circ$: so if anything the expected shock would be stronger, and our conclusions about the source dynamics are unchanged by plausible projection factors.

We discuss the implications of these results in Section \[discussion\].

Discussion
==========

AGN
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The model that best fits our [*XMM-Newton*]{} data gives us an unabsorbed 0.5-10 keV luminosity for all components of the model of $(1.44^{+0.08}_{-0.07})\times10^{44}$ ergs s$^{-1}$. This is not directly comparable to the results of the [*Chandra*]{} analysis presented by @itmismma02 and @ewhkb06, since they used a slightly different model. To make a direct comparison and search for any evidence of AGN variability, we used the same extraction regions that we used for the AGN spectrum on the [*Chandra*]{} data used by @itmismma02 and @ewhkb06. We found the unabsorbed 0.5-10 keV luminosity for the [*Chandra*]{} AGN spectrum 