发表机构
Institute for Astronomy Astrophysics Space Applications and Remote Sensing (IAASARS), National Observatory of Athens; Department of Astronomy, University of Geneva; Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales（雅典国家天文台天文学、天体物理学、空间应用与遥感研究所; 日内瓦大学天文学系; 迭戈帕塔莱斯大学工程与科学学院天体物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过22年多历元X射线和光学观测，揭示了I型类星体2MASS J14302580+4159572中瞬态电离吸收体的兴起与衰退，表明其由热驱动外流引起，并影响窄线区电离状态。
AI 中文摘要
电离物质的外流，通常被称为暖吸收体（WAs），在邻近的赛弗特星系中很常见，但在遥远且能量更高的类星体（QSOs）中则较为稀少。我们展示了红移$z=0.35$的偶然发现的I型类星体2MASS J14302580+4159572的多历元X射线和光学观测，揭示了在22年时间尺度上一次罕见的瞬态电离吸收体的兴起与衰退。发现观测是在2002年至2005年间用XMM-Newton获得的。前两次观测显示出典型的未被遮蔽的I型类星体的普通X射线光谱，而2005年的观测则揭示了在$\sim3\\,\mathrm{keV}$以下光谱的显著抑制。光谱分析表明，这一事件是由一个中等电离吸收体产生的，其柱密度$N_{\rm H}\simeq5\times10^{22}\\\\,\mathrm{cm^{-2}}$，电离参数$\log\xi\simeq1.4$。对跨越22年的XMM-Newton、NuSTAR和Swift/XRT观测的联合分析表明，该吸收体在2023--2024年Swift/XRT数据中减弱之前，保持了近18年的稳定。在此期间，内在的3--10 keV连续谱保持非常稳定，表明观测到的变率是由视线方向电离吸收的变化驱动的，而非内在光度波动。我们将该事件解释为位于宽线区（BLR）之外、亚秒差距到秒差距尺度上的热驱动电离外流，其密度约为$10^{6}\\,\mathrm{cm^{-3}}$。支持这一情景的是，高电离[O\\\\,III] $\lambda4363$发射线与X射线吸收同步变化，表明该外流在十年时间尺度上逐渐改变了内窄线区（NLR）的电离状态。这些观测提供了对类星体暖吸收体长期演化及其对环核环境影响的罕见视角。
英文摘要
Outflows of ionised material, often dubbed warm absorbers (WAs), are common in nearby Seyferts but sparse in distant and more energetic quasars (QSOs). We present multi-epoch X-ray and optical observations of the serendipitously identified type-I QSO 2MASS J14302580+4159572 at a redshift of $z=0.35$, revealing the rare rise and decline of a transient ionised absorber over a 22-year timescale. The discovery observations were obtained with XMM-Newton between 2002 and 2005. The first two observations show unremarkable X-ray spectra typical of unobscured type-I QSOs, whereas the 2005 observation reveals a pronounced suppression of the spectrum below $\sim3\,\mathrm{keV}$. Spectral analysis shows that this event is produced by a moderately ionised absorber with column density $N_{\rm H}\simeq5\times10^{22}\,\mathrm{cm^{-2}}$ and ionisation parameter $\logξ\simeq1.4$. Joint analysis of XMM-Newton, NuSTAR, and Swift/XRT observations spanning 22 years indicates that the absorber remained stable for nearly 18 years before weakening in the 2023--2024 Swift/XRT data. Throughout this period, the intrinsic 3--10 keV continuum remained remarkably stable, indicating that the observed variability is driven by changes in line-of-sight ionised absorption rather than intrinsic luminosity fluctuations. We interpret the event as a thermally driven ionised outflow located outside the broad-line region (BLR), at sub-parsec to parsec scales, with a density of order $10^{6}\,\mathrm{cm^{-3}}$. Supporting this scenario, the high-ionisation [O\,III] $\lambda4363$ emission line varies in tandem with the X-ray absorption, suggesting that the outflow progressively modifies the ionisation state of the inner narrow-line region (NLR) on decadal timescales. These observations provide a rare view of the long-term evolution of a quasar warm absorber and its impact on the circumnuclear environment.
