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Fig. 4


Spectral model with fado of the “composite” galaxy (cf. Fig. 2) 2MASX J15452094+0812244. The meaning of the diagrams is identical to that in Fig. 3 except for panel b), which facilitates visual inspection of the quality of kinematical fitting of stellar absorption features within five selected spectral intervals. Additionally, we exclude from panels c) and d) the vertical bars estimated ±1σ uncertainties for the luminosity and mass contribution of individual SSPs, in order to facilitate visual inspection. It can be seen that emission lines in this system are weak (EW(Hα)≤ 9 Å) and the nebular continuum is almost negligible throughout the considered spectral range.

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