... galaxies

The catalog is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/397/527

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...

For comparison with SFR indicators used for "normal'' galaxies we also indicate the mass conversion factor $c_{\rm M}$ expressing the relative masses between our model IMF and a "standard'' Salpeter IMF with $M_{\rm low}$  =  0.1 and $M_{\rm up}$  =  100 $M_{\odot }$ used frequently throughout the literature. $c_{\rm M}$ is given by $c_{\rm M} = \int_{0.1}^{100} M \Phi(M) {\rm d}m / \int_{M_{\rm low}}^{M_{\rm up}} M \Phi(M) {\rm d}m$.

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... models

f₁₆₄₀ and the corresponding $Q({\rm He^+})$ are reduced by $\sim$9, 4, and 30% for IMFs A, B, and C respectively.

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...$M_{\rm up}$

IMFs A and B yield Lyman-break amplitudes differing by less than $\sim$0.1 dex.

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... ZAMS

The results discussed below are fairly insensitive to the exact (low) metallicity adopted for these quantities.

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... optical

The well known absence of H  II regions with very large H$\beta$ equivalent widths could be taken as an indications for such a scenario.

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