power law, with the column density fixed to the Galactic value and abundance fixed at solar. The two [*apec*]{} models account for the emission from the Galactic bubble and the power law accounts for the cosmic X-ray background. The temperatures were allowed to vary, as were the normalizations, but the power law index was fixed at $\Gamma = 1.41$ [@lwpdl02]. The normalizations were allowed to vary to help minimize intrumental differences between the MOS and PN cameras and to account for differences in the local X-ray background in different directions. Finally, a scaled version of this spectrum, with all parameters fixed, was used in fits to the spectra for each source region. Table \[background-fit\] shows the parameters of the best-fitting model for the background region we used. Our model is in agreement with the model of @lwpdl02.

12.5cm

12.5cm

Regions for spectral extraction {#spectralregion}
-------------------------------

We extracted spectra for the following regions:

1.  An inner region (radius 160 arcsec) surrounding the source (region 1 in Fig. \[image\])

2.  An outer annulus (radii between 160 and 320 arcsec: region 2 in Fig. \[image\])

3.  A region just outside the end of the E lobe (region 3 in Fig. \[image\])

4.  A 