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We describe a far infrared survey of the Coma cluster and the galaxy filamentit resides within. Our survey covers an area of $\sim$150 deg$^2$ observed by$Herschel$ H-ATLAS in five bands at 100, 160, 250, 350 and 500$\mu$m. The SDSSspectroscopic survey ($m_{r} \le 17.8)$ is used to define an area (within theVirial radius) and redshift selected ($4268 < v < 9700$ km s$^{-1}$) sample of744 Coma cluster galaxies - the Coma Cluster Catalogue (CCC). For comparison wealso define a sample of 951 galaxies in the connecting filament - the ComaFilament Catalogue (CFC). The optical positions and parameters are used todefine appropriate apertures to measure each galaxy's far infrared emission. Wehave detected 99 of 744 (13\%) and 422 of 951 (44\%) of the cluster andfilament galaxies in the SPIRE 250$\mu$m band. We consider the relativedetection rates of galaxies of different morphological types finding that it isonly the S0/Sa population that shows clear differences between the cluster andfilament. We find no differences between the dust masses and temperatures ofcluster and filament galaxies with the exception of early type galaxy dusttemperatures, which are significantly hotter in the cluster than in thefilament (X-ray heating?). From a chemical evolution model we find no evidencefor different evolutionary processes (gas loss or infall) between galaxies inthe cluster and filament.

H-ATLAS: The Far-Infrared properties of galaxies in and around the Coma Cluster