... IMF

Based on observations ESO/VLT service observations (65.N-0308 and 67.B-0197).

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... stars

We compute $N_{\rm O7V} = Q_0 / 10^{49.12} = L({\rm H}\alpha) / (1.36~ 10^{-12} \times 10^{49.12}$ taking the Lyman continuum flux Q₀ of an O7V star from Vacca et al. (1996) and assuming case B recombination for $T_{\rm e}=$ 10 000 K and $n_{\rm e} =$ 100 cm^-3.

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... emission

It can be seen that C  IV $\lambda$5808 is not formally detected in all regions with C  III $\lambda$5696 detections. However, in most of these cases (2 exceptions), C  IV $\lambda$5808 is weak, but likely present.

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... galaxies

The few remaining "candidate'' WR regions at high $L({\rm H}\alpha)$ are all located in NGC 4321, have formally a WR detection at $1.4 \la \sigma \la 2$, and appear as rather clear WR detections at visual inspection. The observations of NGC 4321 may be of less good quality due to limited seeing conditions.

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...

At Z=0.04 one has a reduction of $W({\rm WR})$ both in the early burst phase (ages $\la$ 3.5 Myr) at $\log W({\rm H}\beta)\ \ga 1.8$ Å and after $\ga$6 Myr ( $\log W({\rm H}\beta)\ \la$ 1.35), while in between the models predict that WC stars dominate the bump (cf. SV98, Figs. 2 and 11).

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...$<\log L_{\rm cont}> \sim \!36.8 \pm 0.4$

The model $L_{\rm cont}$ at young ages ($\la$1 Myr) is scaled to the observed value, implying a stellar mass of $\sim$ $5. (3.3) \times 10^4$ $M_{\odot }$ for a Salpeter IMF between 0.8 (2.) and 120 $M_{\odot }$. Accounting for somewhat older ages would yield a slightly larger mass.

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