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We use the Hubble Space Telescope to obtain WFC3/F390W imaging of thesupergroup SG1120-1202 at z=0.37, mapping the UV emission of 138spectroscopically confirmed members. We measure total (F390W-F814W) colors andvisually classify the UV morphology of individual galaxies as "clumpy" or"smooth." Approximately 30% of the members have pockets of UV emission (clumpy)and we identify for the first time in the group environment galaxies with UVmorphologies similar to the jellyfish galaxies observed in massive clusters. Westack the clumpy UV members and measure a shallow internal color gradient,which indicates unobscured star formation is occurring throughout thesegalaxies. We also stack the four galaxy groups and measure a strong trend ofdecreasing UV emission with decreasing projected group distance ($R_{proj}$).We find that the strong correlation between decreasing UV emission andincreasing stellar mass can fully account for the observed trend in(F390W-F814W) - $R_{proj}$, i.e., mass-quenching is the dominant mechanism forextinguishing UV emission in group galaxies. Our extensive multi-wavelengthanalysis of SG1120-1202 indicates that stellar mass is the primary predictor ofUV emission, but that the increasing fraction of massive (red/smooth) galaxiesat $R_{proj}$ < 2$R_{200}$ and existence of jellyfish candidates is due to thegroup environment.

SG1120-1202: Mass-Quenching as Tracked by UV Emission in the Group Environment at z=0.37