Geert Raaijmakers, Samaya Nissanke, Francois Foucart, Mansi M. Kasliwal, Mattia Bulla, Rodrigo Fernandez, Amelia Henkel, Tanja Hinderer, Kenta Hotokezaka, Kamilė Lukošiūtė, Tejaswi Venumadhav, Sarah Antier, Michael W. Coughlin, Tim Dietrich, Thomas D. P. Edwards
In recent years, there have been significant advances in multi-messenger astronomy due to the discovery of the first, and so far only confirmed, gravitational wave event with a simultaneous electromagnetic (EM) counterpart, as well as improvements in numerical simulations, gravitational wave (GW) detectors, and transient astronomy. This has led to the exciting possibility of performing joint analyses of the GW and EM data, providing additional constraints on fundamental properties of the binary progenitor and merger remnant. Here, we present a new Bayesian framework that allows inference of these properties, while taking into account the systematic modeling uncertainties that arise when mapping from GW binary progenitor properties to photometric light curves. We extend the relative binning method presented in Zackay et al. (2018) to include extrinsic GW parameters for fast analysis of the GW signal. The focus of our EM framework is on light curves arising from r-process nucleosynthesis in the ejected material during and after merger, the so called kilonova, and particularly on black hole - neutron star systems. As a case study, we examine the recent detection of GW190425, where the primary object is consistent with being either a black hole (BH) or a neutron star (NS). We show quantitatively how improved mapping between binary progenitor and outflow properties, and/or an increase in EM data quantity and quality are required in order to break degeneracies in the fundamental source parameters.
Detecting electromagnetic counterparts to LIGO/Virgo/KAGRA gravitational wave events with DECam: Neutron Star Mergers
Carnegie Mellon University（卡内基梅隆大学）；University of Chicago（芝加哥大学）；University of Ferrara（费拉拉大学）；INFN, Sezione di Ferrara（意大利国家核物理研究所费拉拉分部）；INAF, Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Universität Potsdam（波茨坦大学）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；Utrecht University（乌得勒支大学）；Nikhef（荷兰国家核物理与粒子物理研究所）；California Institute of Technology（加州理工学院）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）
nmma: An extended Bayesian framework for Nuclear Multimessenger Astronomy in the Era of Next-Generation Detectors
Universität Potsdam（波茨坦大学）；Universiteit Utrecht（乌得勒支大学）；Nikhef（尼赫夫国家粒子物理研究所）；University of Ferrara（费拉拉大学）；INFN, Sezione di Ferrara（意大利国家核物理学院费拉拉分部）；INAF, Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；U. Minnesota（明尼苏达大学）；Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））
A first-principles binary neutron star merger model of GW170817, GRB170817A, and AT2017gfo
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Frontier Research Institute for Interdisciplinary Sciences, Tohoku University（东北大学前沿跨学科研究院）；Astronomical Institute, Graduate School of Science, Tohoku University（东北大学理学研究科天文学研究所）；Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics（理论物理学京都研究所引力物理与量子信息研究中心）；Department of Physics, Toho University（东海大学物理学部）
Joint Electromagnetic and Gravitational Wave Inference of Binary Neutron Star Merger GW170817 Using Forward-Modeling Ejecta Predictions
Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；Rochester Institute of Technology（罗切斯特理工学院）；The University of Arizona（亚利桑那大学）；The University of New Mexico（新墨西哥大学）；The George Washington University（乔治华盛顿大学）
Constraints on the dense matter equation of state and neutron star properties from NICER's mass-radius estimate of PSR J0740+6620 and multimessenger observations
Insights from GRBs for optical follow-up of gravitational wave counterparts
Deutsches Elektronen-Synchrotron DESY（德国电子同步加速器）；Deutsches Zentrum für Astrophysik DZA（德国天体物理中心）；Institut für Physik und Astronomie, Universität Potsdam（波恩大学物理与天文研究所）；Department of Astrophysics/IMAPP, Radboud University（拉德堡德大学天体物理学/IMAPP系）；Department of Physics, University of Warwick（华威大学物理系）；GRAPPA Institute, Anton Pannekoek Institute for Astronomy and Institute of High-Energy PhysicsUniversity of Amsterdam（阿姆斯特丹大学GRAPPA研究所、安东·潘内科克天文学研究所和高能物理研究所）；Nikhef（荷兰国家核子和粒子物理研究所）；School of Physics, University College Dublin（都柏林大学学院物理学院）；Cerro Tololo Inter-American Observatory/NSF NOIRLab（塞罗托洛洛美洲际天文台/美国国家科学基金会NOIR实验室）
Fast Radio Bursts from Monster Shocks and Flares of Inspiraling Binary Neutron Stars: A Kinetic Model for Double Pulsar
Astronomical Institute of the Czech Academy of Sciences（捷克科学院天文研究所）；University of Potsdam（波茨坦大学）；Deutsches Elektronen-Synchrotron DESY（德国电子同步加速器）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学、法国国家科学研究中心、天体物理学与行星学研究所）
