All Tables

Table 3: Results of the canonical analytical modeling of the cluster, for the two metallicities Z=0.004 and Z=0.008. Single values correspond to the best fits. Parenthesized ranges correspond to theapproximate 3 $\sigma$ ranges.
Table 5: Numerical results of the star-by-star analysis of the cluster. The parenthesized age ranges indicate the 90% confidence limits.
Table 6: WR line strengths, observed/predicted in the dereddened CAHA spectrum.
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.
Table 1: Journal of Observations.
Table 2: Observed and model colors with filter F547M as the zero point. The observed colors are here corrected for foreground Galactic extinction. The three models (a), (b) and (c) shown here stand for $m_{\rm up}=120$ $M_{\odot }$ , Z=0.004, and respectively, $\alpha =1$ , 1 and 2.35 and $\tau =2$ , 3 and 4 Myr. We also show the three tested extinction laws in the form $f(\lambda )=A(\lambda )/E_{B-V}$ . The color differences $\Delta (M_y-M_\lambda )$ between the observations and a given model were to be well fit by a function of the form $a+E_{B-V}f(\lambda )$ for the tested extinction law to be accepted.
Table 4: Positions, reddened absolute magnitudes, E_B-V coefficients, and initial masses of the brightest stars of NGC 588. The extinction is discussed in Sect. 6.3.2, and the initial masses, in Sect. 6.4. ^aValues eventually set to 0.11.