THE KINEMATICS OF IONIZED GAS IN LYMAN-BREAK ANALOGS AT z ∼ 0.2
THE KINEMATICS OF IONIZED GAS IN LYMAN-BREAK ANALOGS AT z ∼ 0.2
复制标题
DOI：
10.1088/0004-637x/724/2/1373
复制
发表时间：
2010-09
期刊：
影响因子：
--
通讯作者：
T. Gonçalves;A. Basu-Zych;R. Overzier;D. C. Martin;D. Law;D. Schiminovich;T. Wyder;Ryan Mallery;R. Rich;T. Heckman
中科院分区：
文献类型：
--
作者：
T. Gonçalves;A. Basu-Zych;R. Overzier;D. C. Martin;D. Law;D. Schiminovich;T. Wyder;Ryan Mallery;R. Rich;T. Heckman
我们给出了在Keck/OSIRIS上观测到的19个“Lyman-Break类似物”的结果，其自适应光学辅助空间分辨率小于200pc。我们探测到卫星/同伴、漫射和速度切变，所有这些都具有高信噪比。这些星系沿着视线(∼70公里S−1)呈现出非常高的速度弥散，远远高于低红移宇宙中标准的恒星形成螺旋。我们人为地将我们的数据红移到z-∼2.2中，以便与对高z-Lyman-Break星系的观测进行直接比较，并在两个样本之间找到惊人的相似之处。这表明，要么是相似的物理过程导致了它们的观测特性，要么是因为根据现有数据，很难区分在低红移和高红移星暴星系中运行的不同机制。UV/光学连续谱中的形态与我们的运动测量分析之间的比较经常表明，这两种分析本身都不足以证实或完全排除最近合并事件的贡献。我们发现了运动学性质和恒星质量之间的关联，因为质量越大的星系显示出更强的盘状结构的证据。这表明恒星质量的积累与星系内形态和动力学亚结构的形成之间存在着一个共同的进化过程。
We present results for 19 “Lyman-break analogs” observed with Keck/OSIRIS with an adaptive-optics-assisted spatial resolution of less than 200 pc. We detect satellites/companions, diffuse emission, and velocity shear, all with high signal-to-noise ratios. These galaxies present remarkably high velocity dispersion along the line of sight (∼70 km s−1), much higher than standard star-forming spirals in the low-redshift universe. We artificially redshift our data to z ∼ 2.2 to allow for a direct comparison with observations of high-z Lyman-break galaxies and find striking similarities between both samples. This suggests that either similar physical processes are responsible for their observed properties, or, alternatively, that it is very difficult to distinguish between different mechanisms operating in the low- versus high-redshift starburst galaxies based on the available data. The comparison between morphologies in the UV/optical continuum and our kinemetry analysis often shows that neither is by itself sufficient to confirm or completely rule out the contribution from recent merger events. We find a correlation between the kinematic properties and stellar mass, in that more massive galaxies show stronger evidence for a disk-like structure. This suggests a co-evolutionary process between the stellar mass buildup and the formation of morphological and dynamical substructure within the galaxy.