The rate of tidal disruption flares (TDFs) per mass of the disrupting black hole encodes information on the present-day mass function (PDMF) of stars in the clusters surrounding super massive black holes. We explore how the shape of the TDF rate with black hole mass can constrain the PDMF, with only weak dependence on black hole spin. We show that existing data can marginally constrain the minimum and maximum masses of stars in the cluster, and the high-mass end of the PDMF slope, as well as the overall TDF rate. With of order 100 TDFs expected to be identified with the Zwicky Transient Facility, the overall rate can be highly constrained, but still with only marginal constraints on the PDMF. However, if less than of order 10% of the TDFs expected to be found by LSST over a decade (of order 1000 TDFs) are identified, then precise and accurate estimates can be made for the minimum stellar mass (within a factor of two) and the average slope of the high-mass PDMF (to within ~10%) in nuclear star clusters. This technique could be adapted in the future to probe, in addition to the PDMF, the local black hole mass function and possibly the massive black hole binary population.
Constraining high-energy neutrinos from tidal disruption events with IceCube high-energy starting events
Fermi National Accelerator Laboratory（费米国家加速器实验室）；University of Chicago（芝加哥大学）；The Pennsylvania State University（宾夕法尼亚州立大学）；Yukawa Institute for Theoretical Physics（汤川理论物理研究所）
Wandering intermediate-mass black holes and off-nuclear tidal disruption events from early star clusters
Carnegie Mellon University（卡内基梅隆大学）；Massachusetts Institute of Technology（麻省理工学院）；Philipps Universität Marburg（马尔堡菲利普斯大学）；Rutgers, The State University of New Jersey（罗格斯大学）；Flatiron Institute（平顿研究所）；The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI)（宇宙物理与数学研究 Kavli 研究所）
Can tidal disruption event models reliably measure black hole masses?
Queen’s University Belfast（贝尔法斯特女王大学）；University of Birmingham（伯明翰大学）；University of Cambridge（剑桥大学）；The Observatories of the Carnegie Institute for Science（卡内基科学研究所天文台）；University of California, Davis（加州大学戴维斯分校）；University of California, Berkeley（加州大学伯克利分校）；University of Maryland, College Park（马里兰大学帕克分校）
TDEs on FIRE: Illuminating the Cosmic Evolution of Tidal Disruption Rates
The University of Hong Kong（香港大学）；Tata Institute of Fundamental Research（塔塔基础研究所）；The Hong Kong Institute for Astronomy and Astrophysics, The University of Hong Kong（香港大学天文及天体物理研究所）；The Chinese University of Hong Kong（香港中文大学）
Constraining Black Hole Natal Kicks with Astrometric Microlensing
多项证据表明，中子星在由坍缩恒星的残余物形成时会受到巨大的撞击。然而，黑洞（BH）是否受到出生踢的证据并不清楚，依赖于对BH X射线双星和大质量失控和逃逸恒星的分析的弱约束。在这里，我们第一次表明，最近的微透镜检测提供了一种新的方法来测量BHS在出生时收到的踢。当黑洞通过光度和天体测量微透镜被识别，并且透镜恒星有已知的距离和自行时，黑洞的质量、距离和自行就可以确定。我们研究了在超新星爆发过程中被破坏的偏心双星的逃逸速度，发现特殊的速度与BH出生时的反冲强烈相关，通常在20%以内，即使出生时的反冲小于轨道速度。因此，通过测量黑洞或其他致密天体的特殊速度，我们实际上是测量了该天体受到的出生反冲。我们专注于MOA-2011-BLG-191/OGLE-2011-BLG-0462，这是一个通过微透镜检测到的孤立的单个BH，并考虑了一系列可能的形成场景，包括其形成于超新星事件期间双星的破坏。我们确定MOA-2011-BLG-191/OGLE-2011-BLG-0462具有与厚盘人口一致的银河系轨道，但如果它是在运动学薄盘中形成的，它会收到出生踢$\lesssim$ 100 km s $^{-1}$。
No evidence for a supermassive black hole binary in GSN 069
Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交大李政道研究所）；School of Physics & Astronomy, Shanghai Jiao-Tong University（上海交通大学物理与天文学院）；Institute for Astronomy, School of Physics, Zhejiang University（浙江大学物理学院天体物理研究所）；Center for Cosmology and Computational Astrophysics, Institute for Advanced Study in Physics, Zhejiang University（浙江大学物理学高等研究院宇宙学与计算天体物理中心）；Department of Astronomy, University of Science and Technology of China（中国科学技术大学天文系）
California Institute of Technology（加州理工学院）；Massachusetts Institute of Technology（麻省理工学院）；Center for Astrophysics, Harvard and Smithsonian（哈佛史密松天体物理中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文研究所）；Institute for Astronomy, University of Hawaii（夏威夷大学天体物理研究所）
