A_V for AGN versus A_V stellar population, for AGN with L_bol >  10⁴⁴ erg s⁻¹ and m444W < 28 (first and third rows from top, where we have limited the y axis to A_V = 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. A_V for the stellar population of systems selected as cLRDs is moderately small with respect to the full extent of the distribution, while A_V for the AGN is significantly skewed toward low values with respect to the global population.