发表机构
INAF-IAPS; Lomonosov Moscow State University/Sternberg Astronomical Institute; Space Research Institute of the Russian Academy of Sciences; Lomonosov Moscow State University Branch in the City of Sarov; University of Chicago（意大利国家天体物理研究所; 莫斯科罗蒙诺索夫国立大学/斯登伯格天文研究所; 俄罗斯科学院空间研究所; 莫斯科罗蒙诺索夫国立大学萨罗夫分校; 芝加哥大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文利用多卫星X射线观测和整体运动康普顿化模型，通过光谱标度技术首次估算准周期爆发源RX J1301.9+2747的黑洞质量，结果为4×10^5至7×10^6太阳质量，与时间分析及其他方法测量一致。
AI 中文摘要
我们利用ASCA、ROSAT、XMM-Newton和NICER的观测数据，对RX J1301.9+2747中活跃吸积的超大质量黑洞（SMBH）的X射线发射进行了光谱和时间分析，该源具有显著的准周期爆发（QPEs）。NICER在2024年探测到该源重新出现的QPE活动。我们应用第一性原理模型——整体运动康普顿化，详细研究了该源在QPE爆发期间X射线光谱的形成。我们发现光子指数Γ随质量吸积率Ṁ增加而增大，在爆发峰值期间高Ṁ值下指数饱和于Γ_sat=2.7±0.1。基于推导出的Γ-Ṁ相关性，我们首次应用标度技术来测量RX J1301.9+2747中的黑洞质量。根据AGN统一模型假设，采用HLX--1 ESO 243--49、OJ 287和1H 0707--495作为参考标度源，在倾角范围0°至70°内，该源的SMBH质量估计在4×10^5 M_⊙至7×10^6 M_⊙之间，这一范围被认为是合理的。我们还通过时间分析估算了RX J1301.9+2747中的黑洞质量，其中从准周期振荡频率ν~10^-4 Hz估算的康普顿云大小约为10^11 cm，表明RX J1301.9+2747中的SMBH质量量级为10^6 M_⊙。总体而言，通过标度方法获得的该源黑洞质量与此前使用其他方法的测量结果一致。
英文摘要
We present a spectral and timing analysis of X-ray emission from the actively accreting supermassive black hole (SMBH) in RX~J1301.9+2747 with prominent quasi-periodic eruptions (QPEs) using {\it ASCA, ROSAT, XMM-Newton}, and {\it NICER} observations. {\it NICER} detected renewed QPE activity from this source in 2024. We examined in detail the X-ray spectrum formation in this source during QPE outbursts applying the first-principal model, Bulk Motion Comptonization. We find an increase of the photon index $Γ$ with a mass accretion rate $\dot M$, the index saturation at $Γ_{sat}=2.7\pm 0.1$ at high $\dot M$ value during outburst peaks. Based on the derived $Γ-\dot M$ correlation, we apply the scaling technique for the first time to measure the black hole mass in RX~J1301.9+2747. The SMBH mass in this source was estimated to be between $4\times 10^5$ M$_ {\odot}$ and $7\times 10^6$ M$_ {\odot}$ for the inclination range from 0$^{\circ}$ to 70$^{\circ}$, which is adopted as a plausible range based on the AGN unified model assumption, applying HLX--1~ESO 243--49, OJ~287, and 1H~0707--495 as reference scaling sources. We also estimate a BH mass in RX~J1301.9+2747 applying a timing analysis, in which the Compton cloud size to be $\sim 10^{11}$ cm, estimated from the quasi-periodic oscillation frequency, $ν\sim 10^{-4}$ Hz, indicates SMBH mass in RX~J1301.9+2747 is of order of $10^6$ M$_{\odot}$. Overall, the BH mass obtained by the scaling method in this source is consistent with previous measurements using other methods.
Comments19 pages, 9 figures
