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Fig. 6

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Iron emission lines and recombination emission lines of He- and H-like species in the eclipse spectrum of 4U 1538−52. Top panel: spectra and best-fit model (two absorbed power laws and six emission lines) in the 0.3−11.5 keV energy range obtained with PN (top) and MOS (light grey filled squared and dark grey cross) cameras. Bottom panels show the residuals. Second panel: without emission lines. Third panel: with iron and recombination of He- and H-like emission lines for the combined spectra.

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