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Methods.There are no experimental data about the background experienced bymicrocalorimeters in the L2 orbit, and thus the particle background levels werecalculated by means of Monte Carlo simulations: we considered the originaldesign configuration and an improved configuration aimed to reduce theunrejected background, and tested them in the L2 orbit and in the low Earthorbit, comparing the results with experimental data reported by other X-rayinstruments.To show the results obtainable with the improved configuration wesimulated the observation of a faint, high-redshift, point source (F[0.5-10keV]~6.4E-16 erg cm-2 s-1, z=3.7), and of a hot galaxy cluster at R200(Sb[0.5-2 keV]=8.61E-16 erg cm-2 s-1 arcmin-2,T=6.6 keV). Results.First weconfirm that implementing an active cryogenic anticoincidence reduces theparticle background by an order of magnitude and brings it close to therequired level.The implementation and test of several design solutions canreduce the particle background level by a further factor of 6 with respect tothe original configuration.The best background level achievable in the L2 orbitwith the implementation of ad-hoc passive shielding for secondary particles issimilar to that measured in the more favorable LEO environment without thepassive shielding, allowing us to exploit the advantages of the L2 orbit.Wedefine a reference model for the diffuse background and collect all theavailable information on its variation with epoch and pointing direction.Withthis background level the ATHENA mission with the X-IFU instrument is able todetect ~4100 new obscured AGNs with F>6.4E-16 erg cm-2 s-1 during three years,to characterize cluster of galaxies with Sb(0.5-2 keV)>9.4E-16 erg cm-2 s-1sr-1 on timescales of 50 ks (500 ks) with errors <40% (<12%) onmetallicity,<16% (4.8%) on temperature,2.6% (0.72%) on the gas density, andseveral single-element abundances.

In-orbit background of X-ray microcalorimeters and its effects on observations