快速射电暴-持续射电源系统III：PRS光度与FRB旋转测量之间的关系
Fast radio burst - persistent radio source systems III. The relation between PRS luminosity and FRB rotation measure
- INAF-Istituto di Radio Astronomia (IRA)（意大利国家天体物理研究所射电天文研究所）
- Centre for Radio Astronomy Techniques and Technologies (RATT), Department of Physics and Electronics, Rhodes University（罗德斯大学物理与电子学院射电天文技术与方法中心）
- South African Radio Astronomy Observatory（南非射电天文观测台）
- INAF-Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）
- Scuola Universitaria Superiore IUSS Pavia（帕维亚高等大学）
- INAF–Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano（意大利国家天体物理研究所米兰空间天体物理学与宇宙物理学研究所）
- Dipartimento di Fisica e Astronomia, Universitá di Bologna（博洛尼亚大学物理与天文学系）
- Dipartimento di Fisica, Università di Tr（特兰托大学物理系）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究分析50个FRB源，利用贝叶斯MCMC建模光度-RM关系，约束PRS星云尺寸约0.016 pc，发现显著内在离散性，支持高效粒子加速或快速膨胀的演化模型。
AI中文摘要：
快速射电暴（FRBs）是毫秒时标的河外射电瞬变源，其物理起源仍不确定。已知一小部分FRBs会重复爆发，其中一些与持续射电源（PRSs）相关联，这些PRSs被解释为围绕FRB源的同步辐射星云。在基于磁星的模型中，FRB的旋转测量（RM）预期与其相关PRS的光谱光度相关，从而为星云的物理性质和演化提供探针。我们研究了FRB RM与PRS光谱光度之间的关系，约束了PRS星云的特征尺寸，并利用该关系的内在离散性来探究FRB-PRS系统的演化情景。我们分析了50个已知RM的FRB源样本，包括PRS探测和光谱光度上限，使用贝叶斯MCMC框架联合处理探测和非探测事件。我们将光度-RM关系建模为$L_\nu \propto \zeta_e \gamma_c^2 R^2 {\rm RM}^\beta$，约束了特征星云尺寸$R$和RM缩放指数$\beta$。对于完整样本，在自由$\beta$下，我们得到$R = 0.016^{+0.115}_{-0.014}$ pc（1$\sigma$置信度），而将RM依赖固定为典型线性缩放（$\beta = 1$）时，得到$R = 0.008^{+0.058}_{-0.007}$ pc。数据略微倾向于超线性RM缩放，尽管推断的$\beta$值在2$\sigma$内仍与$\beta = 1$一致。我们发现光度-RM关系中存在显著的内在离散性，远大于先前基于确认PRS的估计。在演化模型中解释这种离散性，我们的结果倾向于涉及高效粒子加速和/或快速星云膨胀的情景。
英文摘要：
Fast radio bursts (FRBs) are millisecond-duration radio transients of extragalactic origin whose physical origin remains uncertain. A small fraction of FRBs are known to repeat, and some of them are associated with persistent radio sources (PRSs), interpreted as synchrotron-emitting nebulae surrounding the FRB source. In the context of magnetar-based models, the rotation measure (RM) of an FRB is expected to correlate with the spectral luminosity of its associated PRS, providing a probe of the physical properties and evolution of the nebula. We investigate the relation between FRB RM and PRS spectral luminosity, constrain the characteristic size of the PRS nebulae, and use the intrinsic scatter of the relation to investigate evolutionary scenarios for FRB--PRS systems. We analyse a sample of 50 FRB sources with known RM, including both PRS detections and spectral luminosity upper limits, using a Bayesian MCMC framework that jointly accounts for detections and non-detections. We model the luminosity--RM relation as $L_ν\propto ζ_e γ_c^2 R^2 {\rm RM}^β$, constraining the characteristic nebular size $R$ and the RM scaling index $β$. For the full sample, we obtain $R = 0.016^{+0.115}_{-0.014}$ pc at $1σ$ confidence for a free $β$, while fixing the RM dependence to the canonical linear scaling, $β= 1$, gives $R = 0.008^{+0.058}_{-0.007}$ pc. The data mildly favour super linear RM scalings, although the inferred values of $β$ remain consistent with $β= 1$ within $2σ$. We find a substantial intrinsic scatter in the luminosity--RM relation, significantly larger than previous estimates based on confirmed PRSs alone. Interpreting this scatter within evolutionary models, our results favour scenarios involving efficient particle acceleration and/or rapid nebular expansion.
