Mapping the dynamics of a giant Ly α halo at z = 4.1 with MUSE: the energetics of a large-scale AGN-driven outflow around a massive, high-redshift galaxy
Mapping the dynamics of a giant Ly α halo at z = 4.1 with MUSE: the energetics of a large-scale AGN-driven outflow around a massive, high-redshift galaxy
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使用 MUSE 绘制 z = 4.1 处巨大 Ly α 晕的动力学图：围绕一个巨大、高红移星系的大规模活动星系核驱动外流的能量学
DOI：
10.1093/mnras/stv366
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发表时间：
2015
影响因子：
4.8
通讯作者：
B. Venemans
中科院分区：
文献类型：
--
作者：
M. Swinbank;J. Vernet;I. Smail;C. Breuck;R. Bacon;T. Contini;J. Richard;H. Rottgering;T. Urrutia;B. Venemans
我们提出了对 z = 4.1 射电星系 TN J1338-1942 周围约 150 kpc Lyalpha 晕的多单位光谱探测器 (MUSE) 积分场单位光谱观测。这项为期 9 小时的观测绘制了 Lyalpha 发射穿过光晕的完整二维运动学图，显示了投影中 150 kpc 上 Deltav ～ 700 km s-1 的速度梯度，并且还确定了与射电星系 Lyalpha 发射相关的两个吸收系统。两种吸收体都具有高覆盖率 (~1)，跨越整个光晕的~150 × 80 kpc2 范围。更强、更蓝移的吸收体（距系统 Deltav ～ -1200 km s-1）的动力学反映了底层晕发射的动力学，我们认为这种高柱材料（n(H I) ～ 1019.4 cm-2）（在 C IV 吸收中也可见）代表了由活跃星系核（AGN）或星系内恒星形成驱动的流出壳层。较弱（n(H I) ~ 1014 cm-2）和蓝移较小（Deltav ~ -500 km s-1）的吸收体最有可能代表流出壳层和 Lyalpha 晕之间空腔中的物质。我们估计壳层中的质量必须约为 1010 Ms，这是 z = 4 处星系中星际介质的很大一部分。这些相干结构的大尺度说明了 AGN 反馈对其周围物质的分布和能量学的潜在强大影响。事实上，在中央射电源附近发现的高速（~1000 km s-1）、群晕尺度（即>150 kpc）和质量负载风符合调用活动星系核驱动的流出来调节大质量星系中恒星形成和黑洞生长的模型的要求。
We present Multi Unit Spectroscopic Explorer (MUSE) integral field unit spectroscopic observations of the ˜150 kpc Lyalpha halo around the z = 4.1 radio galaxy TN J1338-1942. This 9-h observation maps the full two-dimensional kinematics of the Lyalpha emission across the halo, which shows a velocity gradient of Deltav ˜ 700 km s-1 across 150 kpc in projection, and also identified two absorption systems associated with the Lyalpha emission from the radio galaxy. Both absorbers have high covering fractions (˜1) spanning the full ˜150 × 80 kpc2 extent of the halo. The stronger and more blueshifted absorber (Deltav ˜ -1200 km s-1 from the systemic) has dynamics that mirror that of the underlying halo emission and we suggest that this high column material (n(H I) ˜ 1019.4 cm-2), which is also seen in C IV absorption, represents an outflowing shell that has been driven by the active galactic nuclei (AGN) or the star formation within the galaxy. The weaker (n(H I) ˜ 1014 cm-2) and less blueshifted (Deltav ˜ -500 km s-1) absorber most likely represents material in the cavity between the outflowing shell and the Lyalpha halo. We estimate that the mass in the shell must be ˜1010 Ms - a significant fraction of the interstellar medium from a galaxy at z = 4. The large scales of these coherent structures illustrate the potentially powerful influence of AGN feedback on the distribution and energetics of material in their surroundings. Indeed, the discovery of high-velocity (˜1000 km s-1), group-halo-scale (i.e. >150 kpc) and mass-loaded winds in the vicinity of the central radio source is in agreement with the requirements of models that invoke AGN-driven outflows to regulate star formation and black hole growth in massive galaxies.
影响因子：
4.8
作者：
M. Swinbank;J. Simpson;I. Smail;C. Harrison;J. Hodge;A. Karim;F. Walter;D. Alexander;N. Brandt;C. Breuck;E. D. Cunha;S. Chapman;K. Coppin;A. Danielson;H. Dannerbauer;Roberto Decarli Thomas Greve;R. Ivison;K. Knudsen;C. Lagos;E. Schinnerer;A. Thomson;J. Wardlow;A. Weiss;Paul van der Werf Icc;Durham;Heidelberg;Bonn;Penn State;Eső;Dalhousie;Hertfordshire;Vienna;Ucl;Ifa;Edinburgh;Chalmers;UC Irvine;Leiden
通讯作者：
M. Swinbank;J. Simpson;I. Smail;C. Harrison;J. Hodge;A. Karim;F. Walter;D. Alexander;N. Brandt;C. Breuck;E. D. Cunha;S. Chapman;K. Coppin;A. Danielson;H. Dannerbauer;Roberto Decarli Thomas Greve;R. Ivison;K. Knudsen;C. Lagos;E. Schinnerer;A. Thomson;J. Wardlow;A. Weiss;Paul van der Werf Icc;Durham;Heidelberg;Bonn;Penn State;Eső;Dalhousie;Hertfordshire;Vienna;Ucl;Ifa;Edinburgh;Chalmers;UC Irvine;Leiden