Fig. 5
Efficiency of our source detection algorithm in the innermost annulus (0–5 arcmin) of the simulated soft band XMM observations, as a function of the input source count-rate (or equivalently, flux for a typical AGN spectrum and a galactic hydrogen column density fixed to 2.6 × 1020 cm-2). The exposure time differs from one curve to the other, but not the background rate.
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