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Fig. 13.

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AV for AGN versus AV stellar population, for AGN with Lbol >  1044 erg s−1 and m444W < 28 (first and third rows from top, where we have limited the y axis to AV = 50) and for systems selected as cLRDs (second and fourth rows from top). We only show SMC-like dust for the sEdd and overm models. AV for the stellar population of systems selected as cLRDs is moderately small with respect to the full extent of the distribution, while AV for the AGN is significantly skewed toward low values with respect to the global population.

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