  We detect ionized gas characteristics indicative of winds in three
disk-dominated galaxies that are members of a super-group at z=0.37 that will
merge to form a Coma-mass cluster. All three galaxies are IR-luminous (L_IR > 4
x 10^{10} L_sun, SFR >8 M_sun per year) and lie outside the X-ray cores of the
galaxy groups. We find that the most IR-luminous galaxy has strong blue and
redshifted 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 gas
in two of three galaxies with SFR > 8 M_sun per year whose orientations are
approximately edge-on and which have IFU spaxels off the stellar disk. IFU maps
reveal that the extraplanar gas extends to r_h ~ 10 kpc; [NII] and Ha
line-widths correspond to velocities of ~200-400 km/s in the disk and decrease
to ~50-150 km/s above the disk. Multi-wavelength observations indicate that the
emission is dominated by star formation. Including the most IR-luminous galaxy
we find that 18% of supergroup members with SFR > 8 M_sun per year show ionized
gas characteristics indicative of outflows. This is a lower limit as showing
that gas is outflowing in the remaining, moderately inclined, galaxies requires
a non-trivial decoupling of contributions to the emission lines from rotational
and turbulent motion. Ionized gas mass loss in these winds is ~0.1 M_sun per
year for each galaxy, although the winds are likely to entrain significantly
larger amounts of mass in neutral and molecular gas.
