在z=0.37的聚集星系团中探测面外气体和面外气体
Detection of Outflowing and Extraplanar Gas in Disks in an Assembling Galaxy Cluster at z=0.37
摘要：
我们检测到电离气体的特性，指示风在三个磁盘为主的星系，在z=0.37，将合并形成一个后发座星系团的一个超级集团的成员。这三个星系都是红外发光的（L_IR > 4 x 10^{10} L_sun，SFR >8 M_sun/年），位于星系群的X射线核心之外。我们发现，最红外发光的星系具有强烈的蓝移和红移的发射线，速度为~ +/-200 km/s和第三，蓝移（~ 900 km/s）的组成部分。这个星系的线宽（Hb，[OIII]5007，[NII]，Ha）对应的速度为100-1000 km/s。我们在三个SFR > 8M_sun/年的星系中的两个星系中探测到了面外气体，它们的方向近似于边向，并且在星盘外有IFU spaxels。IFU图显示面外气体延伸到r_h ~ 10 kpc，[NII]和Ha线宽对应于盘内~200-400 km/s的速度，盘上减小到~50-150 km/s。多波长观测表明，辐射主要是由恒星形成。包括最红外发光的星系，我们发现，18%的超群成员的SFR > 8 M_sun每年显示电离气体的特征，指示外流。这是一个下限，因为表明气体在剩余的适度倾斜的星系中流出，需要旋转和湍流运动对发射线的贡献的非平凡解耦。在这些风中，每个星系每年的电离气体质量损失约为0.1 M太阳，尽管风可能会夹带大量的中性和分子气体。
英文摘要：
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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