Open Access

Fig. A.1.


Optical to radio Spectral Energy Distributions for the 35 galaxies detected in the GOODS-ALMA survey. If the studied galaxy has also been detected with Hershel, we fit the SED using the CIGALE code, otherwise we use the dust spectral energy distribution library presented in Schreiber et al. (2018b). The solid black line represents the best fit, which can be decomposed into the IR dust contribution (brown line), a stellar component uncorrected for dust attenuation (dark blue line), synchrotron emission (purple line) and the AGN contribution (orange line). In addition, we show the best fit of a modified black body, with β = 1.5 (light blue line). The corrected UV emission is also shown in green. The bottom panel shows the residuals: (observation – model)/observation.

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