Deep SCUBA observations of NGC 1275 at 450 \mum and 850 \mum along with the application of deconvolution algorithms have permitted us to separate the strong core emission in this galaxy from the fainter extended emission around it .
The core has a steep spectral index and is likely due primarily to the AGN .
The faint emission has a positive spectral index and is clearly due to extended dust in a patchy distribution out to a radius of \sim 20 kpc from the nucleus .
These observations have now revealed that a large quantity of dust , \sim 6 \times 10 ^ { 7 } M _ { \odot } , 2 orders of magnitude larger than that inferred from previous optical absorption measurements , exists in this galaxy .
We estimate the temperature of this dust to be \sim 20 K ( using an emissivity index of \beta = 1.3 ) and the gas/dust ratio to be 360 .
These values are typical of spiral galaxies .
The dust emission correlates spatially with the hot X - ray emitting gas which may be due to collisional heating of broadly distributed dust by electrons .
Since the destruction timescale is short , the dust can not be replenished by stellar mass loss and must be externally supplied , either via the infalling galaxy or the cooling flow itself .