标题： 混乱中的和谐片段：对星系 RX J1301.9+2747 的 X 射线准周期爆发的进一步观察 显示英文标题

标题： Fragments of harmony amid apparent chaos: a closer look at the X-ray quasi-periodic eruptions of the galaxy RX J1301.9+2747

摘要： 准周期喷发（QPEs）是一种与低质量超大质量黑洞相关的极端X射线变化现象。最初在星系GSN 069的核区被发现，迄今为止已在另外五个星系中得到可靠的检测，其中包括RX J1301.9+2747。 当检测到时，QPE之外的发射（平静期）与吸积盘热辐射的高能尾部一致。 我们展示了RX J1301.9+2747在平静期和QPE期间的X射线和射电特性。 我们分析了2000年至2022年间五次XMM-Newton观测期间收集的X射线数据。 最后三次观测与卡尔·古斯塔夫·詹斯基大型阵列的射电观测协调进行。 我们还利用了1983年至2009年间的EXOSAT、ROSAT和Chandra存档观测数据。 XMM-Newton探测到了34次QPE，其中8次的幅度明显低于其他事件。 在QPE期间没有观察到相关联的射电/X射线变化。 就时间特性而言，RX J1301.9+2747中的QPE没有表现出在发现源GSN 069中观察到的显著规律性。 事实上，QPE之间没有明显的重复模式：它们峰值之间的平均时间间隔约为四个小时，但最短可至一小时，最长可达六小时。 然而，RX J1301.9+2747的QPE光谱特性与能量的关系非常类似于GSN 069和其他QPE源的特性。 RX J1301.9+2747的平静发射比GSN 069更复杂，因为它除了吸积盘的热辐射外，还需要一个软X射线过量类似成分。 其长期的X射线平静通量变化幅度较低且非严格单调，在$\sim 22$年内呈总体衰减趋势。 我们根据目前提出的关于QPE物理起源的一些想法和模型讨论了我们的观测结果。 显示英文摘要

摘要： Quasi-periodic eruptions (QPEs) are an extreme X-ray variability phenomenon associated with low-mass supermassive black holes. First discovered in the nucleus of the galaxy GSN 069, they have been so far securely detected in five other galaxies, including RX J1301.9+2747. When detected, the out-of-QPE emission (quiescence) is consistent with the high-energy tail of thermal emission from an accretion disk. We present the X-ray and radio properties of RX J1301.9+2747, both in quiescence and during QPEs. We analyse X-ray data taken during five XMM-Newton observations between 2000 and 2022. The last three observations were taken in coordination with radio observations with the Karl G. Jansky Very Large Array. We also make use of EXOSAT, ROSAT, and Chandra archival observations taken between 1983 and 2009. XMM-Newton detected 34 QPEs of which 8 have significantly lower amplitudes than the others. No correlated radio/X-ray variability was observed during QPEs. In terms of timing properties, the QPEs in RX J1301.9+2747 do not exhibit the striking regularity observed in the discovery source GSN 069. In fact there is no clear repetition pattern between QPEs: the average time separation between their peaks is about four hours, but it can be as short as one, and as long as six hours. The QPE spectral properties of RX J1301.9+2747 as a function of energy are however very similar to those of GSN 069 and of other QPE sources. The quiescent emission of RX J1301.9+2747 is more complex than that of GSN 069, as it requires a soft X-ray excess-like component in addition to the thermal emission from the accretion disk. Its long-term X-ray quiescent flux variations are of low-amplitude and not strictly monotonic, with a general decay over $\sim 22$ years. We discuss our observational results in terms of some of the ideas and models that have been proposed so far for the physical origin of QPEs.