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Fig. 1.

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Evolution of CIGALE models with nebular parameters. This sample of models created by CIGALE is an extract of the entire and much larger one used for the SED fitting (88 × 106 models). Here, in addition to the nebular parameters given in the legend, we fix the SFH (delayed with τmain = 500 Myrs, and agemain = 100 Myrs), AV(ISM) = 0.3, Tdust = 40 K, the dust emissivity β = 2.0, and the redshift z = 0. However, to improve the visibility, we offset the spectra by δz = 0.1 on the X axis and 1 dex on the Y axis. The bottom spectra, with log10U = −2 are more representative of the IR spectra emitted by an HII-region dominated galaxy, with a strong [OIII]88.3 μm line (blue-shaded area) detected, for example, in Lyman break galaxies in the early Universe. The top spectra, with log10U = −4, resemble an IR spectra emitted by a PDR-dominated galaxy, with a strong [CII]157.6 μm line (red-shaded area), detected, for example, in DSFGs in the early Universe. A higher gas metallicity amplifies the strength of the metal lines.

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