A SINFONI integral field spectroscopy survey for galaxy counterparts to damped Lyman α systems - IV. Masses and gas flows
A SINFONI integral field spectroscopy survey for galaxy counterparts to damped Lyman α systems - IV. Masses and gas flows
复制标题
针对阻尼莱曼 α 系统的星系量的 SINFONI 积分场光谱调查 - IV。
DOI：
10.1093/mnras/stt1760
复制
发表时间：
2013
影响因子：
4.8
通讯作者：
Usa
中科院分区：
文献类型：
--
作者：
C. Péroux;N. Bouché;V. Kulkarni;D. B. L. D. D. Marseille;France Laboratoire d'Astrophysique de Toulouse;France Univ. of South Carolina;U. Chicago;Usa
典型星系的环星系介质（CGM）对于我们理解气体进出星系的循环至关重要。探测CGM的一种方法是研究星系周围的气体，通过它们在背景类星体光谱中产生的吸收线来探测。在这里，我们提出了中等分辨率和新的类似于0.4角秒分辨率（类似于3千秒差距，z类似于1）的三维观测与超大型望远镜/摄谱仪积分场观测在近红外的星系负责高N（H i）类星体吸收。这些数据使我们能够详细地确定物体的运动学：发现四个z类似于1的物体如预期的那样从倾斜盘得到旋转支持，而第五个z类似于2的系统是分散主导的。其中两个系统有相互作用和合并的迹象。此外，我们使用几个指标（单位面积的星星形成，发射和吸收运动学的比较，参数的基础上的倾斜度和方向的吸收体的类星体视线和金属的分布），以确定方向的气体流入和流出这些星系。在某些情况下，我们的观测结果与吸收中看到的气体是一致的，这是由于物质与它们的晕共转。在朝向Q1009-0026和Q2222-0946的吸收星系的情况下，这些指示器指向存在吸收追踪的外流。
The circumgalactic medium (CGM) of typical galaxies is crucial to our understanding of the cycling of gas into, through and out of galaxies. One way to probe the CGM is to study gas around galaxies detected via the absorption lines they produce in the spectra of background quasars. Here, we present medium resolution and new similar to 0.4-arcsec resolution (similar to 3 kpc at z similar to 1) 3D observations with Very Large Telescope/Spectrograph for Integral Field Observations in the Near Infrared of galaxies responsible for high-N(H i) quasar absorbers. These data allow us to determine in details the kinematics of the objects: the four z similar to 1 objects are found to be rotation supported as expected from inclined discs, while the fifth z similar to 2 system is dispersion dominated. Two of the systems show sign of interactions and merging. In addition, we use several indicators (star formation per unit area, a comparison of emission and absorption kinematics, arguments based on the inclination and the orientation of the absorber to the quasar line of sight and the distribution of metals) to determine the direction of the gas flows in and out of these galaxies. In some cases, our observations are consistent with the gas seen in absorption being due to material corotating with their haloes. In the case of absorbing galaxies towards Q1009-0026 and Q2222-0946, these indicators point towards the presence of an outflow traced in absorption.