WISSH类星体项目XIII：宇宙正午时期超快宽吸收线外流的多历元研究
The WISSH quasars project XIII. A multi-epoch study of ultra-fast broad absorption line outflows at cosmic noon
- INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica（意大利国家天体物理研究所空间天体物理与宇宙学研究所）
- INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）
- Center for General Education, Shinshu University（信州大学通识教育中心）
- INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天体物理与空间科学观测站）
- Dipartimento di Fisica “G. Occhialini”, Università degli Studi di Milano-Bicocca（米兰比可卡大学G. Occhialini物理系）
- INAF - Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）
- Dipartimento di Fisica（比萨大学）
- Università di Pisa（意大利国家天体物理研究所阿尔切特里天文台）
- INAF - Osservatorio Astrofisico di Arcetri
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究对WISSH样本中三个高红移类星体的超快宽吸收线外流进行多历元分析，发现其速度高达0.2c且显著变化，动能功率可达热光度的25%，足以影响宿主星系。
AI中文摘要：
超快宽吸收线外流（uBAL，速度约为0.1-0.2倍光速）代表了类星体驱动风中最极端的表现形式之一。我们旨在通过在不同历元和多种离子物种下的特征描述来研究uBAL的变异性。主要目标是约束其物理性质、位置和动能功率，以评估它们对相应类星体宿主星系的潜在影响。我们对来自WISSH样本的三个超亮类星体（即WISSH53、WISSH56和WISSH71）进行了多历元分析，它们的红移分别为z=3.628、4.101和3.567。分析中使用了新的和存档的光谱，覆盖了观测参考系中长达约23年的监测数据。我们用高斯分量对与CIV跃迁相关的吸收进行了建模，并考虑了覆盖因子变化。还进行了多离子轮廓（PV、Lyalpha、NV、SiIV）的保守分析，采用与CIV相同的uBAL速度。我们推导了离子柱密度以及电离参数，从而能够估计外流距离和动能功率的下限和上限。三个源中的CIV uBAL表现出高达约0.2倍光速的速度，并在不同历元间显示出显著变异性，这可能是由电离状态变化和/或横向气体运动驱动的。对多个吸收槽的分析突出了导致变异性的主要机制，并能够推导出外流物理和能量性质的稳健下限和上限。外流距离被约束在从宽线区（BLR）半径（约1秒差距）到几百秒差距的范围内，单个吸收槽的动能功率在最极端情况下可达类星体热光度的大约25%。我们的结果表明，像uBAL这样的极端外流能够注入足够的动能来影响宿主介质。
英文摘要：
Ultra-fast broad absorption line outflows (uBAL, ~0.1-0.2c) represent some of the most extreme manifestations of quasar-driven winds. We aim to investigate the variability of uBALs through their characterisation across different epochs and multiple ionic species. The main goal is to constrain their physical properties, locations, and kinetic powers to evaluate their potential impact on the respective quasar host galaxies. We performed a multi-epoch analysis of three hyper-luminous quasars from the WISSH sample, namely WISSH53, WISSH56, and WISSH71, at redshifts z=3.628, 4.101, and 3.567, respectively. New and archival spectra, spanning up to ~23 years of monitoring in the observed frame, were used in the analysis. We modeled absorption associated with the CIV transition with Gaussian components, accounting for covering factor variations. A conservative analysis of multi-ion profiles (PV, Lyalpha, NV, SiIV) was also performed, considering the same uBAL velocity as CIV. We derived ionic column density, as well as ionisation parameters, which allowed us to estimate lower and upper limits on distances and kinetic powers of the outflows. The CIV uBALs in the three sources exhibit velocities up to ~0.2c and show significant variability across epochs, likely driven by changes in ionisation state and/or transverse gas motion. The analysis of the multiple troughs highlights the dominant mechanisms causing variability and enables the derivation of robust lower and upper limits of the physical and energetic properties of the outflows. Outflow distances are constrained from the broad line region (BLR) radius (~1 pc) up to a few hundred parsecs, and kinetic powers of individual troughs reach up to ~25% of the quasar bolometric luminosity, in the most extreme cases. Our results demonstrate that extreme outflows such as the uBALs are able to inject sufficient kinetic energy to affect the host medium.
