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Fig. 5.


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Comparison between the LIR obtained by CIGALE from UV–IR SED modelling with and without using the MIPS 24 μm flux density for galaxies that are MIPS detected. Candidates of the final sample with a MIPS 24 μm detection are indicated by diamonds. Red circles indicate the candidates of the final sample for which the quenching is confirmed by spectroscopy.

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