FAR-INFRARED THERMAL EMISSION FROM THE INNER COOLING FLOW REGION OF NGC-1275

Measurements of the spatial distribution of 100 mu m emission are pres ented for NGC 1275, the central galaxy in the Perseus cluster. The emi ssion is clearly resolved on a kiloparsec level, and has the same flux density as seen by IRAS at an epoch when the nonthermal emission was a factor of 10 higher. This emission which traces the greater part of the luminosity of this galaxy, is thus identified as thermal emission from dust. The emission appears to be distributed more nearly like the low-velocity H alpha filaments in the core of this galaxy than the st arlight, extended nonthermal radio, X-ray emission, or high velocity g as. While the dust might be heated by a star-formation region that is fed by the cooling flow in this cluster, the intracluster gas also app ears to be energetically capable of this as well, in which case the du st would be, at least at the present time, the dominant cooling mechan ism for the hot gas. The large quantity of dust in NGC 1275 is unlikel y to have been created within the galaxy, or in the cooling flow, but was probably accreted from a recent galactic interloper.