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Fig. 10


Top: observed and model SED for cB58. Although not a good fit, the best match to the full, global SED is found with templates from M10. We can see that the template does not match the photometry in the NUV-blue as it does not describe a population as young as is cB58’s and misses the IR peak by a factor of ~2.5. The FIR fit is obtained with a template among the brightest and warmest from CE01 that matches the IR peak very well. Bottom: SED fits to the stellar part of cB58. The red line shows the best-fit for declining SFHs, including nebular emission, and assuming the SMC extinction law. Green shows the fit neglecting nebular emission and assuming the Calzetti law (best fit among the Calzetti-based solutions). We can see that for the Calzetti law the fitted SED falls out of the 1σ uncertainty of the g-band photometry as noticed in Wuyts et al. (2012) and Siana et al. (2008). In this a case, UV slopes derived from SED fits can vary substantially depending on the extinction law used, especially around the 1300−1800 Å interval.

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