Extended Data Figure 5: Weak emission lines at different energy resolutions.
From: Solar abundance ratios of the iron-peak elements in the Perseus cluster
a, SXS spectrum of the Perseus cluster around the Cr and Mn emission. The red line is the best-fitting model (model A1) with the Cr and Mn abundances set to zero. The bottom panel shows the ratio between the data and the model results. The error bars correspond to the 1σ confidence level. b, Simulated spectrum at the typical energy resolution of the XMM-Newton CCD data (MOS1 detector), assuming the best-fitting model for the SXS data and sufficiently long exposure time (4 Ms). This comparison demonstrates the robustness of our measurements of weak emission lines with high-resolution spectroscopy (see Methods for details).
