so structure could be emphasized on different size scales (see Fig. \[image\]). Figure \[lobes\] shows the X-ray emission from the lobes of 3C452.

Finally, we made use of a radio map of 3C452 from the online 3CRR Atlas[^2], at a frequency of 1.4 GHz and with a resolution of 6 arcsec.

Spectroscopic Analysis
======================

In this section we discuss the two methods we used to extract spectra for the various components of the radio galaxy and its environment and then go on to discuss our results. Throughout the spectroscopic analysis, we used events in the energy range 0.3 – 8 keV.

Background methods {#background}
------------------

We used two approaches to determining the appropriate background for our spectra: local background regions and a full double-subtraction technique that takes account of the spatially variable particle background. Where possible we used a local background for simplicity. However, doing this for regions over which the particle background might be spatially variable leads to bias in the results, and so for larger regions we used closed-filter data with instrument modes matching our observations to constrain the particle background properties. In this situation, we used the method of Maurin [[et al.]{}]{} (in prep); which is described 