Fig. 9
Determination of the star formation rate from this work is compared with that obtained by Brinchmann et al. (2004, multiplied by 1.5 to account for the change of IMF from Kroupa to Salpeter) (bottom panel) and with that obtained using the NUV magnitudes of Huang et al. (2012) (top panel). Blue dots represent galaxies with nuclear HII-like spectra, red dots are AGNs (or LINERs), green dots are nuclear passive spectra.
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