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 \times 10 ^ { 10 } \mathrm { L } _ { \odot } ,~ { } \mathrm { SFR } > 8 \mathrm { M } _ { % \odot } \mathrm { yr } ^ { -1 } ) 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 \sim \pm 200 \mathrm { ~ { } km s } ^ { -1 } and a third , blueshifted ( \sim 900 \mathrm { ~ { } km s } ^ { -1 } ) component .
This galaxy ’ s line-widths ( H \beta , [ OIII ] \lambda 5007 , [ NII ] , H \alpha ) correspond to velocities of 100 - 1000 \mathrm { ~ { } km s } ^ { -1 } .
We detect extraplanar gas in two of three galaxies with SFR > 8 \mathrm { M } _ { \odot } \mathrm { yr } ^ { -1 } 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 } \sim 10 kpc ; [ NII ] and H \alpha line-widths correspond to velocities of \sim 200 - 400 \mathrm { ~ { } km s } ^ { -1 } in the disk and decrease to \sim 50 - 150 \mathrm { ~ { } km s } ^ { -1 } 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 \mathrm { M } _ { \odot } \mathrm { yr } ^ { -1 } 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 \sim 0.1 \mathrm { M } _ { \odot } \mathrm { yr } ^ { -1 } for each galaxy , although the winds are likely to entrain significantly larger amounts of mass in neutral and molecular gas .