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arXiv · 1111.0289

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

E. Freeland·K-V. Tran·T. Irwin·L. Giordano·A. Saintonge·A. Gonzalez·D. Zaritsky·D. Just
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Abstract

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.

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E. Freeland, K-V. Tran, T. Irwin, L. Giordano, A. Saintonge, A. Gonzalez, D. Zaritsky, D. Just. 2011-11-01. Detection of Outflowing and Extraplanar Gas in Disks in an Assembling Galaxy Cluster at z=0.37. https://doi.org/10.1088/2041-8205%2F742%2F2%2Fl34

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