(Left) 0.5–2 keV X-ray image of NGC 6872 (see upper left panel of Figure 5 with X-ray point sources (ellipses as in Figure 5) and young star clusters (Xs) superposed. The X-ray image is background-subtracted, exposure corrected, and smoothed with a σ = 4″ Gaussian. (Right) 0.5–2 keV Chandra X-ray image of the core of the Pavo group, confirming the excess X-ray emission (trail), found in XMM-Newton images (Machacek et al. 2005b), between the dominant elliptical galaxy NGC 6876 and the spiral galaxy NGC 6872. The Chandra image has been background subtracted, exposure corrected, and smoothed with an 8″ Gaussian kernel.