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首页> 外文期刊>The Astrophysical journal >A Molecular Einstein Ring At Z = 4.12: Imaging The Dynamics Of A Quasar Host Galaxy Through A Cosmic Lens
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A Molecular Einstein Ring At Z = 4.12: Imaging The Dynamics Of A Quasar Host Galaxy Through A Cosmic Lens

机译：Z = 4.12时的分子爱因斯坦环：通过宇宙透镜成像类星体宿主星系的动力学

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摘要

We present high-resolution (0.3") Very Large Array imaging of the molecular gas in the host galaxy of the high-redshift quasar PSS J2322+1944 (z = 4.12). These observations confirm that the molecular gas (CO) in the host galaxy of this quasar is lensed into a full Einstein ring and reveal the internal gas dynamics in this system. The ring has a diameter of ～ 1.5" and thus is sampled over ～20 resolution elements by our observations. Through a model-based lens inversion, we recover the velocity gradient of the molecular reservoir in the quasar host galaxy of PSS J2322+ 1944. The Einstein ring lens configuration enables us to zoom in on the emission and to resolve scales down to approx< 1 kpc. From the model-reconstructed source, we find that the molecular gas is distributed on a scale of 5 kpc and has a total massof M(H_2)= 1.7 × 10~(10)M_☉. A basic estimate of the dynamical mass gives M_(dyn) = 4.4 × 10~(10) sin~(-2) i M_☉, that is, only ～2.5 times the molecular gas mass and ～30 times the black hole mass (assuming that the dynamical structure is highly inclined). The lens configuration also allows us to tie the optical emission to the molecular gas emission, which suggests that the active galactic nucleus does reside within, but not close to the center of, the molecular reservoir. Together with the (at least partially) disturbed structure of the CO, this suggests that the system is interacting. Such interaction, possibly caused by a major "wet" merger, may be responsible for both feeding the quasar and fueling the massive starburst of 680 M_☉ yr~(-1) in this system, in agreement with recently suggested scenarios of quasar activity and galaxy assembly in the early universe.
机译：我们提供了高分辨率（0.3“）超大阵列成像，显示了高红移类星体PSS J2322 + 1944（z = 4.12）的宿主星系中的分子气体。这些观察结果证实了宿主中的分子气体（CO）该类星体的星系被透镜化成一个完整的爱因斯坦环，并揭示了该系统的内部气体动力学。该环的直径约为〜1.5“，因此根据我们的观测被采样到了约20个分辨率以上的元素。通过基于模型的透镜反演，我们恢复了PSS J2322 + 1944的准星系星系中分子储层的速度梯度。爱因斯坦环形透镜配置使我们能够放大发射并分辨出大约小于1 kpc的尺度。从模型重建的源头，我们发现分子气体以5 kpc的规模分布，总质量为M（H_2）= 1.7×10〜（10）M_☉。动力学质量的基本估计为M_（dyn）= 4.4×10〜（10）sin〜（-2）iM_☉，即分子气体质量的约2.5倍和黑洞质量的30倍（假设动力学结构高度倾斜）。透镜的配置还使我们能够将光发射与分子气体发射联系起来，这表明活跃的银河核确实存在于分子库的内部，但并不接近中心。连同CO的（至少部分）受干扰的结构一起，这表明系统正在相互作用。这种相互作用可能是由一次重大的“湿”合并引起的，可能与该类星体活动和新出现的场景一致，既为该类星体提供了能量，又为该系统中的680M_☉yr〜（-1）的大规模星爆提供了燃料。早期宇宙中的星系集合。

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