  Far-infrared photometry of broad-line radio galaxies shows this class of AGN
to consist of many hot and some cool infrared emitters, with peaks in their
spectral energy distributions around 25 micron or longward of 60 micron,
respectively. Quantitative analysis indicates that this distribution relates to
a substantial dispersion in the strength of the cool dust component: broad-line
radio galaxies are relatively poor in large-scale dust. Possibly they have
undergone a different merger evolution, or are relatively old AGN.
