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Fig. 11


Left: comparison of additional observables with model predictions for cB58 adopting the Calzetti attenuation law. Shown is the logarithmic ratio of the model prediction with respect to the observable quantity for LIR, the flux in the Hα, Hβ, [O ii] λ3727, and [O iii] λλ4959,5007 lines, as well as the Hα equivalent width. The observed values are from this paper (LIR), and from Teplitz et al. (2000). Although other emission lines have been detected in this galaxy, we do not include them here because the information they provide is basically redundant. Error bars indicate the 68% confidence interval predicted by the models; the typical observational errors, not included here, are shown with the black dotted error bars. Colors correspond to models with different SFHs (green: exponentially declining, and yellow: delayed SFHs; both for subsolar metallicity, 1/5 Z. Black: SFR = const.; red: exponentially rising; both for solar metallicity). Results for the SMC law are similar and equally reproduce the observables. Right: same as left panel for the Cosmic Eye adopting the Calzetti attenuation law. Sources of the observational data are described in the text. Blue points show the predictions for models with exponentially declining SFHs and higher extinction to nebular emission (i.e. E(B − V) = 0.44  × E(B − V)neb). Red and black dashed symbols show the same for the rising and constant SFR models, respectively.

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