From observations with IRAS and ISOPHOT I find that there is a number of BLRGs with a peak in their SED at 25µm. Not all BLRGs show this behaviour, which deviates from the typical SED for NLRGs and QSRs. The peaker sample is compared with a sample of NLRGs and BLRGs which have a peak at 60–100 µm. I find no excess of hot dust in the 25 µm peakers, but a lack of cold dust, which is the dust heated by (hot) stars. This might be related to the evolutionary state of the object, being an older NLRG in which the extended dust has been depleted by star-formation and the nuclear dust torus is smaller. The fact that two classes of BLRG seem to exist is not contradicting the unification schemes, however, it adds an important new dimension.
Finally, the name 25 µm peaker should be abandoned as soon as possible, as it is misleading, but so far I have not found a good alternative.