Some recent studies have examined the gamma-ray flux profile of our Galaxy to determine the signal of dark matter annihilation. However, the results are controversial and no confirmation is obtained. In this article, we study the radio flux density profile of the M31 galaxy and show that it could manifest a possible signal of dark matter annihilation. By comparing the likelihoods between the archival observed radio flux density profile data and the predicted radio flux density profile contributed by dark matter and stellar emission, we can constrain the relevant dark matter parameters. Specifically, for the thermal annihilation cross section via the $b\bar{b}$ channel, the best-fit value of dark matter mass is $\sim 30$ GeV, which is consistent with the results of many recent studies. We expect that this method would become another useful way to constrain dark matter, which is complementary to the traditional radio analyses and the other indirect detections.
MOMO VI: Multifrequency radio variability of the blazar OJ 287 from 2015-2022, absence of predicted 2021 precursor-flare activity, and a new binary interpretation of the 2016/2017 outburst
Confronting the Magnetar Interpretation of Fast Radio Bursts Through Their Host Galaxy Demographics
我们探讨的背景下，快速射电暴（FRB）的宿主星系的人口统计和偏移分布的提示磁星祖的情况。磁星是一种中子星，具有$10^{15}$ G量级的强磁场，衰变寿命短于$10^4$年。由于它们的寿命极短，磁星应该根据它们目前的恒星形成率（SFR）遵循星系的人口统计。此外，我们假设磁星应该遵循SFR配置文件内的星系，我们假设遵循指数配置文件。我们构建了一个简单的模型，假设这些事件跟踪SFR在所有星系的磁星的宿主星系，并将其与观察到的属性从一个样本的\nsecure \安全FRB主机。我们发现在$>95\%$ c. l.处观测到的SFR的分布与模型不一致。偏移分布与这种情况是一致的，然而，这可能是由于有限的样本大小和有限的估计FRB宿主星系的有效半径。尽管最近在银河系中发现了FRB与磁星的关联，但磁星可能不是宇宙中FRB的唯一来源，但任何其他成功的模型都必须考虑到SFR中FRB宿主的人口统计及其观测到的银河系中心偏移。
A Shock-based Interpretation of Radio and X-ray Emission in Active Galactic Nuclei
School of Physics and Astronomy, Yunnan University（云南大学物理与天文学院）；Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University（云南省天体粒子物理重点实验室）
Some possible interpretations from data of the CODALEMA experiment
安装在南赛射电天文台（法国）的CODALEMA实验的目的是研究$10^{16}-10^{18} eV$能量范围内的超高能宇宙射线的无线电探测。分布在0.25 km $^2$的区域内，原始设备同时使用粒子探测器阵列和短天线阵列，并进行集中采集。在考虑地磁场影响的情况下，给出了无线电能量观测量的新分析。自2011年以来，在初始配置周围1.5公里$^2$的区域内部署了由60个独立和自触发台站组成的新的无线电探测器阵列。这一新的发展导致了具体的限制，要讨论的方面，宇宙射线的识别和分析的波前。
Radio Emission with Dust: A Bow-Shock Interpretation for the TDE Candidate AT 2019avd
School of Astronomy and Space Sciences, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Department of Physics and Institute of Theoretical Physics, Nanjing Normal University（南京师范大学物理科学与技术学院/理论物理研究所）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Department of Space, Earth and Environment, Chalmers University of Technology（查尔姆斯理工大学地球与环境空间系）；INAF - Istituto di Radioastronomia（意大利国家天体物理研究所射电天文研究所）
The XMM-Newton X-ray Spectra of the Most X-ray Luminous Radio-quiet ROSAT Bright Survey-QSOs: A Reference Sample for the Interpretation of High-redshift QSO Spectra
