The new generation of X-ray polarisation detectors, the gas pixel detectors, which will be\nemployed by the future space missions IXPE and eXTP, allows for spatially resolved X-ray polarisation\nstudies. This will be of particular interest for X-ray synchrotron emission from extended sources like\nyoung supernova remnants and pulsar wind nebulae. Here we report on employing a polarisation\nstatistic that can be used to makes maps in the Stokes I, Q, and U parameters, a method that\nwe expand by correcting for the energy-dependent instrumental modulation factor, using optimal\nweighting of the signal. In order to explore the types of Stokes maps that can be obtained, we present\na Monte Carlo simulation program called xpolim, with which different polarisation weighting schemes\nare explored. We illustrate its use with simulations of polarisation maps of young supernova remnants,\nafter having described the general science case for polarisation studies of supernova remnants, and its\nconnection to magnetic-field turbulence. We use xpolim simulations to show that in general deep,\n~2 Ms observations are needed to recover polarisation signals, in particular for Cas A, for which in\nthe polarisation fraction may be as low as 5%.
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