H-ATLAS: The Far-Infrared properties of galaxies in and around the Coma
  Cluster
  We describe a far infrared survey of the Coma cluster and the galaxy filament
it 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 SDSS
spectroscopic survey ($m_{r} \le 17.8)$ is used to define an area (within the
Virial radius) and redshift selected ($4268 < v < 9700$ km s$^{-1}$) sample of
744 Coma cluster galaxies - the Coma Cluster Catalogue (CCC). For comparison we
also define a sample of 951 galaxies in the connecting filament - the Coma
Filament Catalogue (CFC). The optical positions and parameters are used to
define appropriate apertures to measure each galaxy's far infrared emission. We
have detected 99 of 744 (13\%) and 422 of 951 (44\%) of the cluster and
filament galaxies in the SPIRE 250$\mu$m band. We consider the relative
detection rates of galaxies of different morphological types finding that it is
only the S0/Sa population that shows clear differences between the cluster and
filament. We find no differences between the dust masses and temperatures of
cluster and filament galaxies with the exception of early type galaxy dust
temperatures, which are significantly hotter in the cluster than in the
filament (X-ray heating?). From a chemical evolution model we find no evidence
for different evolutionary processes (gas loss or infall) between galaxies in
the cluster and filament.
