Fig. 12
Simulation of 300 ks observation of the northern skirt of Abell 1795. Upper panel: surface brightness of the cluster. Green points are from Suzaku observation (Bautz et al. 2009). Grey points are from Swift XRT observation (already shown in Fig. 2). Black points would be the result of 300 ks observation. Lower panel: the surface brightness profile of the cluster as observed by Suzaku, with the same color code. XRT spatial bins in the simulation are chosen in order to have a minimum of 1000 source counts in the 0.7−2.0 keV band.
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