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We detect ionized gas characteristics indicative of winds in threedisk-dominated galaxies that are members of a super-group at z=0.37 that willmerge to form a Coma-mass cluster. All three galaxies are IR-luminous (L_IR > 4x 10^{10} L_sun, SFR >8 M_sun per year) and lie outside the X-ray cores of thegalaxy groups. We find that the most IR-luminous galaxy has strong blue andredshifted emission lines with velocities of ~ +/-200 km/s and a third,blueshifted (~ 900 km/s) component. This galaxy's line-widths (Hb, [OIII]5007,[NII], Ha) correspond to velocities of 100-1000 km/s. We detect extraplanar gasin two of three galaxies with SFR > 8 M_sun per year whose orientations areapproximately edge-on and which have IFU spaxels off the stellar disk. IFU mapsreveal that the extraplanar gas extends to r_h ~ 10 kpc; [NII] and Haline-widths correspond to velocities of ~200-400 km/s in the disk and decreaseto ~50-150 km/s above the disk. Multi-wavelength observations indicate that theemission is dominated by star formation. Including the most IR-luminous galaxywe find that 18% of supergroup members with SFR > 8 M_sun per year show ionizedgas characteristics indicative of outflows. This is a lower limit as showingthat gas is outflowing in the remaining, moderately inclined, galaxies requiresa non-trivial decoupling of contributions to the emission lines from rotationaland turbulent motion. Ionized gas mass loss in these winds is ~0.1 M_sun peryear for each galaxy, although the winds are likely to entrain significantlylarger amounts of mass in neutral and molecular gas.

Detection of Outflowing and Extraplanar Gas in Disks in an Assembling Galaxy Cluster at z=0.37