Fig. 6.
Residuals of the best fit to the time-averaged RGS spectrum (in the observed frame) of NGC 3783 in 2000–2001 around the O VII RRC (left panels) and O VII He-like triplets (right panels). The upper and lower panels show residuals of the best fit with and without the broad (FWHM ∼ 21000 km s−1) PION emission component (the third component in Table 4), respectively.
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