Near-Infrared Spectrophotometry of the Radio Galaxy 4C 40.36 at z = 2.269
Near-Infrared Spectrophotometry of the Radio Galaxy 4C 40.36 at z = 2.269
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Radio Galaxy 4C 40.36 在 z = 2.269 处的近红外分光光度测定
DOI：
10.1086/310175
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发表时间：
1996
期刊：
影响因子：
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通讯作者：
T. Maihara
中科院分区：
文献类型：
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作者：
F. Iwamuro;S. Oya;H. Tsukamoto;T. Maihara
我们给出了高z射电星系4C40.36(z=2.269)的新的近红外光谱观测结果，包括J波段和H波段图像以及1.14-1.70λ/Δλm之间的低分辨率(μ~100)谱，我们探测到了明显强的[O III]λ4959/5007双线和其他相对较弱的发射线叠加在微弱的平坦连续体上。除了[Ne III]λ3869/[O II]λ3727比值较大外，测得的发射线比与典型的具有太阳金属丰度的窄线活动星系核基本一致，这可能是由于该天体中的Ne丰度过高造成的。由于恒星发射的J波段图像与射电轴线对齐，而主要由[O III]谱线发射(约73%)产生的H波段图像更对称，表明强氧谱线发射云的同心分布。基于这些形态特征和静止坐标系中紫外光光谱区域极其平坦的连续体，我们检验了两个模型，即极年轻星系模型(AGE=0.02-0.1Gyr)和散射活动星系核模型。
We present new near-infrared spectrophotometric observations of the high-z radio galaxy 4C 40.36 (z = 2.269) including J- and H-band images and a low-resolution (λ/Δλ ~ 100) spectrum between 1.14 and 1.70 μm. We have detected distinctively strong [O III] λ4959/5007 doublet and other relatively weak emission lines superposed on the faint flat continuum. The measured emission-line ratios are roughly consistent with the typical narrow-line AGN with the solar metal abundance, except for the large [Ne III] λ3869/[O II] λ3727 ratio that is probably caused by the overabundance of neon in this object. The J-band image attributable to stellar emission is aligned with the radio axis, while the H-band image mostly due to [O III] line emission (about 73%) is more symmetric, indicating a concentric distribution of strong oxygen line-emitting clouds. Based on these morphological features together with the extremely flat continuum over the UV-to-optical spectral region in the rest frame, we have examined two models, which are an extremely young galaxy model (age = 0.02-0.1 Gyr) as well as a scattered AGN model.