Caption: Simulations of the Phoenix cluster for a region of 50 arc second size adopting the XMM-Newton/RGS best-fit model plus the AGN and the cool (< 2 keV) gas (see Pinto et al. 2018 for spectral parameters). Cosmic X-ray background and particle background are accounted for. The strongest transitions are labelled in the observed frame (we adopt z = 0.596 and turbulence broadening = 250 km/s). We use the response matrix of Hitomi/SXS as a proxy for XRISM.

Additional comments: The X-IFU response used is XIFU_CC_BASELINECONF_2018_10_10. For XRISM, the response used is an old Hitomi response from just before the launch, i.e. 2015 (gate valve open of course).

Reference: Pinto, C., Bambic, C.J., Sanders, J. S., et al., 2018, MNRAS, 480, 4113. Data was provided by Ciro on October 23rd, 2019.

Creation date: 24/10/2019. Version #: 3.

Credits: X-IFU Consortium. Copyrights: ©DB/X-IFU.