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Compact groups of galaxies provide insight into the role of low-mass, denseenvironments in galaxy evolution because the low velocity dispersions and closeproximity of galaxy members result in frequent interactions that take placeover extended timescales. We expand the census of star formation in compactgroup galaxies by \citet{tzanavaris10} and collaborators with Swift UVOT,Spitzer IRAC and MIPS 24 \micron\ photometry of a sample of 183 galaxies in 46compact groups. After correcting luminosities for the contribution from oldstellar populations, we estimate the dust-unobscured star formation rate(SFR$_{\mathrm{UV}}$) using the UVOT uvw2photometry. Similarly, we use the MIPS24 \micron\ photometry to estimate the component of the SFR that is obscured bydust (SFR$_{\mathrm{IR}}$). We find that galaxies which are MIR-active(MIR-"red"), also have bluer UV colours, higher specific star formation rates,and tend to lie in H~{\sc i}-rich groups, while galaxies that are MIR-inactive(MIR-"blue") have redder UV colours, lower specific star formation rates, andtend to lie in H~{\sc i}-poor groups. We find the SFRs to be continuouslydistributed with a peak at about 1 M$_{\odot}$ yr$^{-1}$, indicating this mightbe the most common value in compact groups. In contrast, the specific starformation rate distribution is bimodal, and there is a clear distinctionbetween star-forming and quiescent galaxies. Overall, our results suggest thatthe specific star formation rate is the best tracer of gas depletion and galaxyevolution in compact groups.

The Ultraviolet and Infrared Star Formation Rates of Compact Group Galaxies: An Expanded Sample