Context: Observations of transient emission from extreme accretion events onto supermassive black holes can reveal conditions in the center of galaxies and the black hole itself. Most recently, they have been suggested to be emitters of high-energy neutrinos. If it is suddenly rejuvenated accretion or a tidal disruption event (TDE) is not clear in most cases. Aims: We expanded on existing samples of infrared flares to compile the largest and most complete list available. A large sample size is necessary to provide high enough statistics for far away and faint objects to estimate their rate. Our catalog is large enough to facilitate a preliminary study of the rate evolution with redshift for the first time. Methods: We compiled a sample of 40 million galaxies, and, using a custom, publicly available pipeline, analyzed the WISE light curves for these 40 million objects using the Bayesian Blocks algorithm. We selected promising candidates for dust echos of transient accretion events and inferred the luminosity, extension, and temperature of the hot dust by fitting a blackbody spectrum. Results: We established a clean sample of 823 dust-echo-like infrared flares, of which we can estimate the dust properties for 568. After removing 70 objects with possible contribution by synchrotron emission, the luminosity, extension, and temperature are consistent with dust echos. Estimating the dust extension from the light curve shape revealed that the duration of the incident flare is broadly compatible with the duration of TDEs. The resulting rate per galaxy is consistent with the latest measurements of infrared-detected TDEs and appears to decline at increasing redshift. Conclusions: Although systematic uncertainties may impact the calculation of the rate evolution, this catalog will enable further research in phenomena related to dust-echos from TDEs and extreme accretion flares.
PeV extended emission around Galactic PeVatrons and echos of their flares
Université Paris Cité（巴黎西岱大学）；CNRS, Astroparticule et Cosmologie（法国国家科学研究中心，亚原子粒子与宇宙学）；Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne（洛桑联邦理工学院天体物理实验室）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）
Testing the Association of Supermassive Black Hole Infrared Flares and High-energy Neutrinos
MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院）；Department of Astronomy and Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学）；Center for Computational Astrophysics, Flatiron Institute（西蒙斯基金会平顿研究所计算天体物理中心）；Department of Physics, Norwegian University of Science and Technology（挪威科技大学）
The Demographics of Sagittarius A* X-ray Flares over 25 Years with Chandra
McGill University（麦吉尔大学）；Trottier Space Institute（特罗蒂尔太空研究所）；Villanova University（维拉诺瓦大学）；Washington University in St. Louis（圣路易斯华盛顿大学）；University of Maryland（马里兰大学）
SRON Space Research Organization Netherlands（荷兰空间研究所）；University of Ferrara（费拉拉大学）；INAF-OAS Bologna（意大利国家天体物理研究所博洛尼亚天文台）；ESTEC, ESA（欧洲空间研究和技术中心）；INAF-IAPS Roma（意大利国家天体物理研究所罗马天文物理研究所）
Low-angular-momentum accretion shocks can power weak-to-moderate X-ray flares from SgrA*
International Center for Theoretical Sciences, Tata Institute of Fundamental Research（塔塔基础研究所国际理论科学中心）；Center for Theoretical Physics, Polish Academy of Sciences（波兰科学院理论物理中心）；Department of Theoretical Physics and Astrophysics, Masaryk University（马萨里克大学理论与天体物理学系）；McGill University（麦吉尔大学）；Trottier Space Institute（特罗蒂尔太空研究所）
Repeating flares, X-ray outbursts and delayed infrared emission: A comprehensive compilation of optical tidal disruption events
Institute of Astrophysics, FORTH（FORTH天体物理研究所）；Department of Physics, University of Crete（克里特大学物理系）；NASA Marshall Space Flight Center（美国宇航局马歇尔太空飞行中心）；Institutt for Fysikk, Norwegian University of Science and Technology（挪威科技大学物理系）；Instituto de Astronomía, Universidad Nacional Autónoma de México Campus Ensenada（墨西哥国立自治大学恩塞纳达天文研究所）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；Astronomical Observatory, University of Warsaw（华沙大学天文台）；Astrophysics Division, National Centre for Nuclear Research（国家核研究中心天体物理部）；Astronomical Institute, University of Wrocław（弗罗茨瓦夫大学天文研究所）
