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Fig. C.4.
Match of the atlas by Kennicutt (1992) to our classes using the E-step. See Sect. 7.2. The strong discrepancies in the fits for some classes (dI, Im, SO, Sb:) are due to very strong and thin emission lines in the Kennicutt (1992) spectra. The fits are strongly improved when these spectra are smoothed to reduce the noise.
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