The first galaxies with nuclear activity were studied in detail by Seyfert in the 1940's (Seyfert 1943). Now, over 50 years later, their numbers have increased by several orders of magnitude, revealing a rich diversity. In their attempt to reach a physical understanding of active galaxies, people have proposed unified schemes (e.g. Barthel 1989), which combine several apparently different classes into one, depending on the orientation of a central symmetry axis. A dusty torus causes anisotropy at wavelengths were the dust is optically thick, but is transparent to hard X-rays and radio emission. This easily explains many differences between Seyfert 1 and Seyfert 2 galaxies, and also between radio galaxies and radio quasars. However, there are many open questions, e.g. the presence and nature of type 2 radio-quiet quasars, the absence of broad emission lines in some objects (e.g. Hill et al. 1996). In this paper I will study one specific problem, that of the 25 µm peakers. These are broad-line radio galaxies (BLRGs) which have a clear peak in their spectral energy distribution around 25 µm, whereas all other radio-loud AGN have this peak at longer wavelengths (60–100 µm).