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We have made observations of the active, cooling flow galaxy NGC 1275 with the University of Texas 2X10 bolometer on the Kuiper Airborne Observatory in order to determine the source of the far infrared flux. The data were calibrated with observations of asteroids. Our 100 micron flux from NGC 1275 is about 7.9 Jy which is consistent with the IRAS flux of 7.76 Jy. Since the non-thermal flux from the AGN is a factor of ten less than it was in the IRAS epoch the far IR flux is most likely dominated by thermal emission from dust. The far IR emission is resolved on a 30" scale and is inconsistent with the pointlike AGN and the starlight. Instead, the IR flux is spatially consistent with the line emission that is thought to represent recombining or reionized gas in the cooling flow. The morpholgy and temperature of the dust implied by the far IR flux suggest that much of the dust is captured from a recent merger and it may be heated by hot plasma from the cooling flow. This could mean the cooling timescale of the hot plasma in the NGC 1275 cooling flow is determined by the dust and not by the X-ray emission.
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