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We compare the environmental and star formation properties of far-infrareddetected and non--far-infrared detected galaxies out to $z \sim0.5$. Usingoptical spectroscopy and photometry from the Galaxy And Mass Assembly (GAMA)and Sloan Digital Sky Survey (SDSS), with far-infrared observations from the{\em Herschel}-ATLAS Science Demonstration Phase (SDP), we apply the techniqueof Voronoi Tessellations to analyse the environmental densities of individualgalaxies. Applying statistical analyses to colour, $r-$band magnitude andredshift-matched samples, we show there to be a significant difference at the3.5$\sigma$ level between the normalized environmental densities of these twopopulations. This is such that infrared emission (a tracer of star formationactivity) favours underdense regions compared to those inhabited by exclusivelyoptically observed galaxies selected to be of the same $r-$band magnitude,colour and redshift. Thus more highly star-forming galaxies are found to residein the most underdense environments, confirming previous studies that haveproposed such a correlation. However, the degeneracy between redshift andfar-infrared luminosity in our flux-density limited sample means that we areunable to make a stronger statement in this respect. We then apply our methodto synthetic light cones generated from semi-analytic models, finding that overthe whole redshift distribution the same correlations between star-formationrate and environmental density are found.

{\em Herschel}-ATLAS/GAMA: The Environmental Density of Far-Infrared Bright Galaxies at $z \leq 0.5$