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Abridged - We quantify the effect of the galaxy group environment (for 12.5 <log(M_group/Msun) < 14.0) on the star formation rates of the(morphologically-selected) population of disk-dominated local Universe spiralgalaxies (z < 0.13) with stellar masses log(M*/Msun) > 9.5. Within thispopulation, we find that, while a small minority of group satellites arestrongly quenched, the group centrals, and the large majority of satellitesexhibit levels of SFR indistinguishable from ungrouped "field" galaxies of thesame M*, albeit with a higher scatter, and for all M*. Modelling these results,we deduce that disk-dominated satellites continue to be characterized by arapid cycling of gas into and out of their ISM at rates similar to thoseoperating prior to infall, with the on-going fuelling likely sourced from thegroup intrahalo medium (IHM) on Mpc scales, rather than from thecircum-galactic medium on 100kpc scales. Consequently, the color-densityrelation of the galaxy population as a whole would appear to be primarily dueto a change in the mix of disk- and spheroid-dominated morphologies in thedenser group environment compared to the field, rather than to a reducedpropensity of the IHM in higher mass structures to cool and accrete ontogalaxies. We also suggest that the inferred substantial accretion of IHM gas bysatellite disk-dominated galaxies will lead to a progressive reduction in theirspecific angular momentum, thereby representing an efficient secular mechanismto transform morphology from star-forming disk-dominated types to more passivespheroid-dominated types.

the astronomical journal

Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies in the  Local Universe I. - The Effect of the Group Environment on Star Formation in  Spiral Galaxies