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We use the Herschel ATLAS (H-ATLAS) Phase I data to study the conditionalluminosity function of far-IR (250 um) selected galaxies in optically-selectedgalaxy groups from the GAMA spectroscopic survey, as well as environmentaleffects on the far-IR-to-optical colour. We applied two methods, which gaveconsistent results for the far-IR conditional luminosity functions. The directmatching method matches H-ATLAS sources to GAMA/SDSS galaxies, then links theoptical counterparts to GAMA groups. The stacking method counts the number offar-IR sources within the projected radii of GAMA groups, subtracting the localbackground. We investigated the dependence of the far-IR (250 um) luminosityfunction on group mass in the range 10d12 < M_h < 10d14Msun/h and on redshiftin the range 0 < z < 0.4, using a sample of 3000 groups containing H-ATLASsources with GAMA redshifts over an area of 126 sq. deg. We find that thecharacteristic 250 um luminosity, L^*(250), increases with group mass up to M_h~ 10d13Msun/h, but is roughly constant above this, while it increases withredshift at high group masses, but less so at low masses. We also find that thegroup far-IR luminosity-to-mass ratio L(250)/M_h increases with redshift and ishigher in low-mass groups. We estimate that around 70% of the 250 um luminositydensity in the local universe is contributed by groups with M_h > 10d12Msun/h.We also find that the far-IR-to-optical colours of H-ATLAS galaxies areindependent of group mass over the range 10d12 < M_h <10d14Msun/h in the localuniverse. We also compare our observational results with recent semi-analyticalmodels, and find that none of these galaxy formation model can reproduce theconditional far-IR luminosity functions of galaxy groups.

Herschel-ATLAS/GAMA:How does the far-IR luminosity function depend on galaxy group properties?