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A fraction of the XMM-Newton/EPIC FOV is obscured by the dysfunctional (i.e.bad) pixels. The fraction varies between different EPIC instruments in a givenobservation. These complications affect the analysis of extended X-ray sourcesobserved with XMM-Newton/EPIC and the consequent scientific interpretation ofthe results. For example, the accuracy of the widely used cosmological probe ofthe gas mass of clusters of galaxies depends on the accuracy of the procedureof removing the obscuration effect from the measured flux. The Science AnalysisSoftware (SAS) includes an option for recovering the lost fraction of the fluxmeasured by a primary instrument by utilising a supplementary image of the samesource. The correction may be accurate if the supplementary image is minimallyobscured at the locations of the bad pixels of the primary instrument. This canbe achieved e.g. by using the observation-based MOS2 image for correcting thepn flux, or by using a synthetic model image. By utilising a sample of 27galaxy cluster observations we evaluated the accuracy of the recovery methodbased on observed images, as implemented in SAS 18.0.0. We found that theaccuracy of the recovered total flux in the 0.5-7.0 keV band in the fullgeometric area within the central r = 6 arcmin is better than 0.1% on averagewhile in some individual cases the recovered flux may be uncertain by ~1%.

Accuracy of the recovered flux of extended sources obscured by bad pixels in the central EPIC FOV