发表机构
University of Turku; Jagiellonian University; Indian Institute of Science Education and Research (IISER) Mohali; Tata Institute of Fundamental Research; Aryabhatta Research Institute of Observational Sciences (ARIES); Nordic Optical Telescope; Radio Astronomy Laboratory of Crimean Astrophysical Observatory; University of the National Education Commission（图尔库大学; 雅盖隆大学; 印度科学教育研究所（莫哈利）; 塔塔基础研究所; 阿耶波多观测科学研究所以; 北欧光学望远镜; 克里米亚天体物理台射电天文实验室; 国家教育委员会大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过宽波段观测研究 blazar OJ 287 2022年10月的耀发，确认其为潮汐耀发，结合进动率测得主黑洞质量为(18.35±0.05)×10⁹M☉，验证了双黑洞系统质量的前期测定。
AI 中文摘要
明亮的 blazar OJ~287 已展现出一系列耀发，这些耀发可由准开普勒轨道模型很好地解释，且与次级天体撞击主黑洞的吸积盘相关。该轨道必须发生进动才能产生正确的耀发序列，我们通过进动率计算出主黑洞质量 $M_{BH} = (18.35\pm0.05) \times 10^9 M_{\odot}$。研究人员已识别出两种耀发：撞击产生的直接耀发，以及吸积流增加进入喷流引发的潮汐耀发。由于两种耀发均可独立确定进动率和主黑洞质量，2022年10月的潮汐耀发被建议用于开展密集观测 campaign。本文描述了这些宽波段观测结果，表明2022年10月的耀发符合潮汐耀发的预期，从而支持了此前对 OJ 287 双黑洞系统质量的测定。此外，主黑洞质量也可通过次级指标推导，如与氢线强度及黑洞质量的相关性；这类研究要求质量高于 $M_{BH} \sim 10^{10} M_{\odot}$，但未给出更精确的数值。
英文摘要
The bright blazar OJ~287 has demonstrated a sequence of flares, which are well explained by a quasi-Keplerian orbit model. The flares are associated with the impact of the secondary on the accretion disk of the primary. The orbit must precess in order to produce the correct sequence of flares, and from the precession rate we calculate the mass of the primary. This precession rate gives the mass of the primary $M_{BH} = (18.35\pm0.05) \times 10^9 M_{\odot}$. Two kinds of flares have been identified: direct flares from the impacts, and tidal flares arising from an increased accretion flow into the jet. The precession rate and the primary black hole mass may be independently determined from both sets of flares; the tidal flare of October 2022 was recommended for an intense campaign for this reason. This paper describes these observations over a wide spectral range. We show that the October 2022 flare fits the expectations for a tidal flare and thus supports the earlier determination of the mass of the binary black hole system in OJ 287. The mass of the primary may also be deduced from secondary indicators such as the correlation with the hydrogen line strength and the black hole mass. These studies require that the mass is above $M_{BH} \sim 10^{10} M_{\odot}$, but do not specify the value more exactly.
Comments21 pages, 10 figures, 1 table
