Outflows from supermassive black holes (SMBHs) play an important role in the co-evolution of themselves, their host galaxies, and the larger scale environments. Such outflows are often characterized by emission and absorption lines in various bands and in a wide velocity range blueshifted from the systematic redshift of the host quasar. In this paper, we report a strong broad line region (BLR) outflow from the z ≈ 4.7 quasar BR 1202-0725 based on the high-resolution optical spectrum taken with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph installed on the 6.5 m Magellan/Clay telescope, obtained from the ‘Probing the He ii re-Ionization ERa via Absorbing C iv Historical Yield’ (HIERACHY) project. This rest-frame ultraviolet (UV) spectrum is characterized by a few significantly blueshifted broad emission lines from high ions; the most significant one is the C iv line at a velocity of $\sim -6500$ km s−1 relative to the H α emission line, which is among the highest velocity BLR outflows in observed quasars at z > 4. The measured properties of UV emission lines from different ions, except for O i and Ly α, also follow a clear trend that higher ions tend to be broader and outflow at higher average velocities. There are multiple C iv and Si iv absorbing components identified on the blue wings of the corresponding emission lines, which may be produced by either the outflow or the intervening absorbers.

中文翻译：

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通过吸收 C iv 历史产量 (HIERACHY) I 探测 He ii 再电离 ERa：来自 az ∼ 4.7 类星体的强烈流出

超大质量黑洞 (SMBH) 的流出物在自身、宿主星系和更大规模环境的共同演化中发挥着重要作用。这种流出的特征通常是不同波段的发射和吸收线，并且在较宽的速度范围内，从宿主类星体的系统红移蓝移。在本文中，我们根据安装在 6.5 m Magellan 上的 Magellan Inamori Kyocera Echelle (MIKE) 光谱仪拍摄的高分辨率光谱，报告了来自 z ≈ 4.7 类星体 BR 1202-0725 的强宽线区域 (BLR) 流出/粘土望远镜，从“通过吸收 C iv 历史产量探测 He ii 再电离 ERa”（HIERACHY）项目获得。这种静止帧紫外 (UV) 光谱的特点是高离子的一些显着蓝移的宽发射线；最重要的是 C iv 线，相对于 H α 发射线的速度为 $\sim -6500$ km s-1，这是观测到的类星体中在 z > 处的最高速度 BLR 流出之一。4. 除O i 和Ly α 外，不同离子的UV 发射谱线的测量特性也遵循明显的趋势，即较高的离子往往更宽，以较高的平均速度流出。在相应发射线的蓝色翼上识别出多个 C iv 和 Si iv 吸收组分，它们可能由流出或中间吸收体产生。除 O i 和 Ly α 外，还遵循一个明显的趋势，即更高的离子往往更宽，并以更高的平均速度流出。在相应发射线的蓝色翼上识别出多个 C iv 和 Si iv 吸收组分，它们可能由流出或中间吸收体产生。除 O i 和 Ly α 外，还遵循一个明显的趋势，即更高的离子往往更宽，并以更高的平均速度流出。在相应发射线的蓝色翼上识别出多个 C iv 和 Si iv 吸收组分，它们可能由流出或中间吸收体产生。