Fig. B.9.
See text for a general description of the figure. NGC 4736: both [S II] and [O I] lines are unblended in the HST/STIS spectrum and they clearly present narrow profiles. In the Hα − [N II] lines a broad component is visible, as already reported by Constantin et al. (2015). For the Palomar spectrum, a narrow component is sufficient for fitting all the emission lines considered in our study.
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