XRISM Resolve Simulations of 1E 0102.2-7219 and N132D

The Resolve calorimeter instrument on the JAXA X-ray Imaging and Spectroscopy Mission (XRISM) will provide spectra of extended sources with unprecedented resolution and sensitivity. I present spectral simulations of the brightest supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) N132D and the brightest SNR in the Small Magellanic Cloud (SMC) 1E 0102.2-7219 (hereafter E0102). Both of these sources will be valuable for the in-flight verification and calibration of the low energy response of the Resolve calorimeter and Xtend CCD instruments. The bright lines in the spectra of both objects have been well-characterized by the gratings instruments on XMM-Newton and Chandra. Our standard spectral model for E0102 (developed by the thermal SNRs working group of the International Astronomical Consortium for High Energy Calibration (IACHEC), see Plucinsky et al. 2017) has been used by all operational missions with response to low energy X-rays in order to improve their respective calibrations. The line-rich spectra of both of these objects will be useful for verifying the gain scale, spectral resolution, and effective area of the Resolve instrument derived from the ground calibration in the energy range from 0.5 to 3.0~keV. The Resolve calorimeter data promise new insights into the three dimensional structure of both of these remnants, as indicated by the tantalizing result from the Hitomi SXS spectra of a predominantly red-shifted Fe-K component in N132D (Hitomi Collaboration et al. 2017). The Resolve spectra will be superior to the gratings data for constraining the broadening of emission lines due to bulk velocities in the SNR and for thermal broadening to constrain the ion temperatures. The Resolve spectra will also provide the most sensitive data for detecting and characterizing fainter features in the spectrum such as those expected from a recombining plasma or charge exchange. Studies such as these will of course be done for the Galactic SNRs where the XARM angular resolution allows the emission from different regions to be spatially resolved.