CHIME/FRB/Pulsar discovery of a nearby long period radio transient with a timing glitch
Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda … 展开作者
Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
备注：
V3: Typos fixed. V2:The previous submission was delayed due to other commitments of the lead author. Because of that, this new version of the paper has a) more data, b) baseband/raw volatage data, d) more analysis on the timing and polarisation, c) reformatted. This publication has been accepted to Astrophysical Journal Letters
We present the discovery of a 421 s long period radio transient (LPT) using the CHIME telescope, CHIME J0630+25. The source is localized to RA=06:30:38.4$\pm1'$ Dec=25:26:24$\pm1'$ using voltage data acquired with the CHIME baseband system. A timing analysis shows that a model including a glitch is preferred over a non-glitch model with $dF/F=1.3\times10^{-6}$, consistent with other glitching neutron stars. The timing model suggests a surface magnetic field of $\sim1.5\times10^{15}$ G and a characteristic age of $\sim1.28\times10^{6}$ yrs. A separate line of evidence to support a strong local magnetic field is an abnormally high rotation measure of $RM=-347.8(6) \mathrm{rad\, m^{-2}}$ relative to CHIME J0630+25's modest dispersion measure of 22(1) pc cm$^{-2}$, implying a dense local magneto-ionic structure. As a result, we believe that CHIME J0630+25 is a magnetized, slowly spinning, isolated neutron star. This marks CHIME J0630+25 as the longest period neutron star and the second long period neutron star with an inferred magnetar-like field. Based on dispersion measure models and comparison with pulsars with distance measurements, CHIME J0630+25 is located at a nearby distance of 170$^{+310}_{-100}$ pc (95.4\%), making it an ideal candidate for follow-up studies.
A series of unfortunate events: CHIME/FRB misclassification of a Galactic pulsar as a periodic fast radio burst
McGill University（麦吉尔大学）；Trottier Space Institute, McGill University（麦克唐纳空间研究所，麦吉尔大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Indian Institute of Technology Kanpur（坎普尔印度理工学院）；Universidad de Chile（智利大学）；Cornell Center for Astrophysics and Planetary Science, Cornell University（康奈尔大学天体物理学与行星科学中心，康奈尔大学）；University of British Columbia（不列颠哥伦比亚大学）；West Virginia University（西弗吉尼亚大学）；Center for Gravitational Waves and Cosmology, West Virginia University（引力波与宇宙学中心，西弗吉尼亚大学）
Nine New Repeating Fast Radio Burst Sources from CHIME/FRB
我们报告的发现和分析的爆发，从九个新的重复快速射电暴（FRB）源发现使用加拿大氢强度测绘实验（CHIME）望远镜。这些源跨越195至1380 pc cm $^{-3}$的色散测量（DM）范围。我们检测到两个爆发从三个新的来源，三个爆发从四个新的来源，四个爆发从一个新的来源，和五个爆发从一个新的来源。我们确定所有来源的天空坐标与$\sim$ 10 $^\prime$的不确定性。我们检测法拉第旋转措施的两个来源，值$-20(1)$和$-499.8(7)$ rad m $^{-2}$，这是大大低于RM从FRB 121102发出的突发。我们发现，DM分布的我们的事件，结合其他九个重复发现的CHIME/FRB，是无法区分的，迄今为止非重复CHIME/FRB事件。然而，如前所述，爆发宽度在统计上明显大于迄今为止非重复的CHIME/FRB事件，进一步支持了固有不同的发射机制和/或局部环境的概念。这些结果与以前的工作是一致的，虽然现在来自18个重复源CHIME/FRB在其第一年的操作中发现。我们确定候选星系，可能包含FRB 190303.J1353+48（DM = 222.4 pc cm $^{-3}$）。
Radio Monitoring Campaign of Active Repeater FRB 20220912A with CHIME
McGill University（麦吉尔大学）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；Massachusetts Institute of Technology（麻省理工学院）；Tel Aviv University（特拉维夫大学）；National Research Council of Canada, Herzberg Astronomy and Astrophysics（加拿大国家研究委员会赫茨伯格天文学与天体物理学研究所）；University of British Columbia（不列颠哥伦比亚大学）
Extreme-Value Distribution Analysis of the Second CHIME/FRB Catalog: Assessing the Rarity of the One-off FRB 20250316A
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；School of Astronomy and Space Sciences, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）
Constraints on the Physical Association between ICECAT1 Neutrinos and Fast Radio Bursts Using the Second CHIME/FRB Catalogue
The University of Tokyo（东京大学）；National Astronomical Observatory of Japan（日本国立天文台）；Mizusawa VLBI Observatory, National Astronomical Observatory of Japan（水泽甚长基线干涉测量观测站，日本国立天文台）；Department of Physics, National Chung Hsing University（国立中兴大学物理学系）；SOKENDAI（综合研究大学院大学）；Tohoku University（东北大学）；Frontier Research Institute for Interdisciplinary Sciences, Tohoku University（东北大学跨学科前沿研究院）；Astronomical Institute, Graduate School of Science, Tohoku University（东北大学理学研究科天文学研究所）
LOFAR constraints on the repetition & environments of CHIME FRBs
ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内科克天体物理研究所）；Max Planck Institute for Radio Astronomy, University of Bonn（波恩大学马克斯·普朗克射电天文研究所）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔太空研究所）；Department of Physics, McGill University（麦吉尔大学物理系）；Laboratoire d’Astrophysique de Marseille, Aix-Marseille University, CNRS, CNES（马赛大学CNRS/CNES天体物理学实验室）
Searching for Gamma Ray Bursts associated with CHIME Fast Radio bursts
Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；School of Astronomy and Space Sciences, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）；State Key Laboratory of Radio Astronomy and Technology, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台射电天文与技术国家重点实验室）；South-Western Institute for Astronomy Research, Yunnan University（云南大学西南天文研究所）
Discovery of 30 Repeating Fast Radio Burst Sources and Uniform Population Statistics of 80 Repeating Sources from CHIME/FRB
McGill University（麦吉尔大学）；University of Amsterdam（阿姆斯特丹大学）；California Institute of Technology（加州理工学院）；Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）
CHIME/FRB Detection of Eight New Repeating Fast Radio Burst Sources
我们报告发现的八个重复的快速射电暴（FRB）源使用加拿大氢强度测绘实验（CHIME）望远镜。这些源跨越103.5至1281 pc cm $^{-3}$的色散测量（DM）范围。它们显示出不同程度的活动：六个源被检测到两次，另一个三次，一个十次。这八个重复的FRB可能表示不频繁重复源的分布的亮端和/或高速率端。对于所有的源，我们确定天空坐标与$\sim$ 10 $^\prime$的不确定性。FRB 180916.J0158+65的爆发平均DM = $349.2 \pm 0.3$ pc cm $^{-3}$，并且DM超出模拟的银河系最大值（低至$\sim$ 20 pc cm $^{-3}$）;该源的法拉第旋转测量值（RM）为$-114.6 \pm 0.6$ rad m $^{-2}$，远低于FRB 121102的测量值。FRB 181030.J1054+73的中继器DM最低，为$103.5 \pm 0.3$ pc cm $^{-3}$，DM超出$\sim$ 70 pc cm $^{-3}$。这两个来源是有趣的目标，多波长的后续行动，由于其明显的接近。我们的中继器样本的DM分布在统计上与前12个没有重复的CHIME/FRB源的DM分布没有区别。我们发现，与4 $σ$的意义，重复突发一般比那些没有重复的CHIME/FRB突发，这表明不同的发射机制。我们的重复事件显示出复杂的形态，让人想起前两…
Probing the maximum energy of fast radio bursts using thousands of sources from the Second CHIME/FRB Catalog
McGill University（麦吉尔大学）；Trottier Space Institute, McGill University（特罗蒂尔空间研究所，麦吉尔大学）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内科克天文学研究所）；ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所 ASTRON）；School of Physics and Astronomy, Tel Aviv University（特拉维夫大学物理与天文学学院）；MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理学与空间研究研究所）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理系）
Constraining the Fast Radio Burst (FRB) properties using the joint distributions of dispersion measure and fluence of the events detected at Parkes, ASKAP, CHIME and UTMOST
