Erratum : Deep VLT spectroscopy of the vec {z}= 2.49 radio galaxy MRC 2104-242. Evidence for a metallicity gradient in its extended emission line region
Erratum : Deep VLT spectroscopy of the vec {z}= 2.49 radio galaxy MRC 2104-242. Evidence for a metallicity gradient in its extended emission line region
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勘误：vec {z}= 2.49 射电星系 MRC 2104-242 的深 VLT 光谱。
DOI：
10.1051/0004-6361:20010041
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发表时间：
2001
影响因子：
6.5
通讯作者：
C. Breuck
中科院分区：
文献类型：
--
作者：
R. Overzier;H. Rottgering;J. Kurk;C. Breuck
我们目前的光谱观测的休息帧紫外线辐射周围的射电星系MRC 2104-242在$z=2.49$，获得与VLT Antu上的FORS 1。晕的形态主要是由两个空间分辨区域。Ly α沿射电轴延伸沿着12。整个光谱是典型的高红移射电星系。最引人注目的空间变化是，N $\rm V $存在于与星系中心相关的区域的频谱中，该区域是无线电源所在的北方区域，而在南方区域则没有。假设气体被隐藏的类星体光电离，N $\rm V $发射的差异可以用晕内的金属丰度梯度来解释，北方区域的金属丰度为Z\approx1.5 Z_{\odot}$，南方区域为Z\leq0.4 Z_{\odot}$。这与气体与大规模冷却流有关或起源于两个或更多星系合并的碎片的情况一致。
We present spectroscopic observations of the rest-frame UV line emission around radio galaxy MRC 2104-242 at $z=2.49$, obtained with FORS1 on VLT Antu. The morphology of the halo is dominated by two spatially resolved regions. Ly α is extended by >12´´along the radio axis, C $\rm IV$ and He $\rm II$ are extended by ∼ 8´´. The overall spectrum is typical for that of high redshift radio galaxies. The most striking spatial variation is that N $\rm V $ is present in the spectrum of the region associated with the center of the galaxy hosting the radio source, the northern region, while absent in the southern region. Assuming that the gas is photoionized by a hidden quasar, the difference in N $\rm V $ emission can be explained by a metallicity gradient within the halo, with the northern region having a metallicity of $Z\approx1.5 Z_{\odot}$ and $Z\leq0.4 Z_{\odot}$ for the southern region. This is consistent with a scenario in which the gas is associated with a massive cooling flow or originates from the debris of the merging of two or more galaxies.