Fig. 2
Representative spectra of Abell 426 (the Perseus cluster) (black) and the adopted background (gray) at 0.3−0.5r180 from MOS and PN fitted with Gaussians and continuum. Best-fit Gaussians corresponding to the Kα-lines of He-like and H-like Fe are plotted as bold lines: those for background lines are plotted as thin dashed lines.
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