近距离到远距离星系中的 X 射线风 (X-WING)。I. 对 z ∼ 0-4 范围内具有超快外流和暖吸收体的星系进行的遗留观测

Satoshi Yamada, Taiki Kawamuro, Misaki Mizumoto, Claudio Ricci, Shoji Ogawa, Hirofumi Noda, Yoshihiro Ueda, Teruaki Enoto, Mitsuru Kokubo, Takeo Minezaki, Hiroaki Sameshima, Takashi Horiuchi, Shoichiro Mizukoshi
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引用次数: 0

摘要

作为 "近距离到远距离星系中的 X 射线风(X-WING)"计划的首次调查,我们收集了一个数据集,其中包括 132 个活动星系核(AGN),其红移 z ∼ 0-4,其特征是蓝移吸收线表明存在 X 射线风。通过对以往研究的详尽回顾,我们汇编了 583 个 X 射线风的外流参数,包括外流速度(Vout)、电离参数(ξ)和氢柱密度等关键属性。通过利用 Vout 和 ξ 参数,我们将这些风系统地分为三类:超快外流风(UFO)、低电离参数 UFO 和暖吸收风(WAs)。令人震惊的是,外流参数中明显缺乏线性相关关系,而且其分布接近仪器探测极限。另一个值得注意的发现是在 Vout ∼ 10,000 km s-1 附近发现了一个速度差距。这种差距在通过≲2 keV波段内的吸收线探测到的风中尤为明显,表明低IP UFO和WA的起源不同。在涉及铁 xxv/Fe xxvi 线的情况下,差距可能是由于发射线/吸收线和铁 K 边之间的潜在混淆造成的,因此考虑了 UFO 和银河尺度 WAs 互不关联的可能性。对流出半径和尘埃升华半径的研究揭示了两者之间的区别:UFO似乎由无尘物质组成,而WA则可能由含尘气体组成。从 2024 年起,X 射线成像和光谱任务将缓解观测偏差,提供对已发现缺口真实性的见解,这是理解 UFO AGN 反馈的一个关键问题。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4
As an inaugural investigation under the X-ray Winds In Nearby-to-distant Galaxies (X-WING) program, we assembled a data set comprising 132 active galactic nuclei (AGNs) spanning redshifts z ∼ 0–4 characterized by blueshifted absorption lines indicative of X-ray winds. Through an exhaustive review of previous research, we compiled the outflow parameters for 583 X-ray winds, encompassing key attributes such as outflow velocities (V out), ionization parameters (ξ), and hydrogen column densities. By leveraging the parameters V out and ξ, we systematically categorized the winds into three distinct groups: ultrafast outflows (UFOs), low-ionization parameter (low-IP) UFOs, and warm absorbers (WAs). Strikingly, a discernible absence of linear correlations in the outflow parameters, coupled with distributions approaching instrumental detection limits, was observed. Another notable finding was the identification of a velocity gap around V out ∼ 10,000 km s−1. This gap was particularly evident in the winds detected via absorption lines within the ≲2 keV band, indicating disparate origins for low-IP UFOs and WAs. In cases involving Fe xxv/Fe xxvi lines, where the gap might be attributed to potential confusion between emission/absorption lines and the Fe K-edge, the possibility of UFOs and galactic-scale WAs being disconnected is considered. An examination of the outflow and dust sublimation radii revealed a distinction: UFOs appear to consist of dust-free material, whereas WAs likely comprise dusty gas. From 2024, the X-Ray Imaging and Spectroscopy Mission is poised to alleviate observational biases, providing insights into the authenticity of the identified gap, a pivotal question in comprehending AGN feedback from UFOs.
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