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IGRJ18410-0535 is a supergiant fast X-ray transients. This subclass ofsupergiant X-ray binaries typically undergoes few- hour-long outbursts reachingluminosities of 10^(36)-10^(37) erg/s, the occurrence of which has beenascribed to the combined effect of the intense magnetic field and rotation ofthe compact object hosted in them and/or the presence of dense structures("clumps") in the wind of their supergiant companion. IGR J18410-0535 wasobserved for 45 ks by XMM-Newton as part of a program designed to study thequiescent emission of supergiant fast X-ray transients and clarify the originof their peculiar X-ray variability. We carried out an in-depth spectral andtiming analysis of these XMM-Newton data. IGR J18410-0535 underwent a brightX-ray flare that started about 5 ks after the beginning of the observation andlasted for \sim15 ks. Thanks to the capabilities of the instruments on-boardXMM-Newton, the whole event could be followed in great detail. The results ofour analysis provide strong convincing evidence that the flare was produced bythe accretion of matter from a massive clump onto the compact object hosted inthis system. By assuming that the clump is spherical and moves at the samevelocity as the homogeneous stellar wind, we estimate a mass and radius of Mcl\simeq1.4\times10^(22) g and Rcl \simeq8\times10^(11) cm. These are inqualitative agreement with values expected from theoretical calculations. Wefound no evidence of pulsations at \sim4.7 s after investigating coherentmodulations in the range 3.5 ms-100 s. A reanalysis of the archival ASCA andSwift data of IGR J18410-0535, for which these pulsations were previouslydetected, revealed that they were likely to be due to a statistical fluctuationand an instrumental effect, respectively.

XMM-Newton observations of IGRJ18410-0535: The ingestion of a clump by a supergiant fast X-ray transient