Fig. 12.
Hα – luminosity relation of SF dwarfs, expressed as the logarithm of Hα luminosity (erg s−1) as a function of the sech absolute magnitude. The previous linear trend is confirmed (Cedres et al. 2009; Iglesias-Paramo et al. 2002) by the following fit in NIR (Eq. (6), plotted as a dashed line). The cross in the upper left shows typical uncertainties in the two parameters.
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