Fig. A.2.
Ratio of the combined RXTE-PCA spectra to our best-fit model for epoch II. Features on a 1–2% level are visible below 7 keV, the existence of which is not confirmed by the Suzaku-XIS spectra (see Fig. 2). Similar features have been seen in combined PCA spectra of the Crab pulsar (Fig. 8, García et al. 2014) or of GRO J1008−57 (Fig. 3, Kühnel et al. 2016).
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