Azimuthally averaged surface brightness profile of Abell 1795 from Chandra data with clump candidates included and excluded. The bottom panel shows the difference, where a slight decrement in the profile at the radius of the clump candidates becomes prominent when removing these sources. The best-fit power-law also becomes moderately steeper with the 24 clump candidates removed, with the best-fit α increasing from 4.18 ± 0.13 to 4.34 ± 0.09. This steepening, however, is attributed mainly to the relatively large difference between the last data points and the associated uncertainties.