Table 7: Some spectral properties derived from the observed stellar content (2nd column) and from the one with BSG, WR and whole population replaced with the one predicted by the fitted power-law IMF (3rd, 4th and 5th columns, respectively). Q(X) designates the photon rate able to ionize the ion "X'' population of a nebula. ^aThe 5th and 6th columns correspond to analytical models, whose total mass here reproduce the observed F439W luminosity. ^bBest-fit model of the canonical analysis.
BSG content Real IMF Real IMF^a 2.8 Myr^a,b

WR content Real Real IMF IMF^a 2.8 Myr^a,b

MS content Real Real Real IMF^a 2.8 Myr^a,b

$W({\rm H}\beta )$ (Å) 342 133 284 80 247

$Q({\rm H}^0)$ (10⁵⁰ s^-1) 2.14 2.16 1.39 0.54 1.60

$Q({\rm He}^0)/Q({\rm H}^0)$ 0.13 0.12 0.14 0.11 0.14

10⁸ $Q({\rm He}^+)/Q({\rm H}^0)$ 9.3 8.0 2.8 $\times$ 10⁴ 8.8 130

$Q({\rm O}^+)/Q({\rm H}^0)$ 0.020 0.020 0.024 0.011 0.017

**Table 7:** Some spectral properties derived from the observed stellar content (2nd column) and from the one with BSG, WR and whole population replaced with the one predicted by the fitted power-law IMF (3rd, 4th and 5th columns, respectively). Q(X) designates the photon rate able to ionize the ion "X'' population of a nebula. ^aThe 5th and 6th columns correspond to analytical models, whose total mass here reproduce the observed *F439W* luminosity. ^bBest-fit model of the canonical analysis.
BSG content	Real	IMF	Real	IMF^a	2.8 Myr^a,b
WR content	Real	Real	IMF	IMF^a	2.8 Myr^a,b
MS content	Real	Real	Real	IMF^a	2.8 Myr^a,b
$W({\rm H}\beta )$ (Å)	342	133	284	80	247
$Q({\rm H}^0)$ (10⁵⁰ s^-1)	2.14	2.16	1.39	0.54	1.60
$Q({\rm He}^0)/Q({\rm H}^0)$	0.13	0.12	0.14	0.11	0.14
10⁸ $Q({\rm He}^+)/Q({\rm H}^0)$	9.3	8.0	2.8 $\times$ 10⁴	8.8	130
$Q({\rm O}^+)/Q({\rm H}^0)$	0.020	0.020	0.024	0.011	0.017

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