A puzzling class of exotic objects, which have been known about for more than 30 years, is reaching a new era of understanding. We have discovered hundreds of Ultra Luminous X-ray sources (ULXs) - non-nuclear sources with X-ray luminosity in excess of the Eddington luminosity for "normal" size stellar Black Holes (BH) - and we are making progresses towards understanding their emission mechanisms. The current explanations imply either a peculiar state of accretion onto a stellar size BH or the presence of an intermediate mass BH, the long-sought link between stellar and supermassive BHs. Both models might co-exist and therefore studying this class of object will give insight into the realm of accretion in a variety of environments and at the same time find look-alikes of the primordial seed BHs that are thought to be at the origin of todays supermassive BHs at the centre of galaxies. The radio band has been exploited only scantily due to the relative faint fluxes of the sources, but we know a number of interesting sources exhibiting both extended emission (like bubbles and possibly jets) and cores, as well as observed transient behaviour. The new eras of the SKA will lead us to a major improvement of our insight of the extreme accretion within ULXs. We will both investigate in detail known sources and research new and fainter ones. When we have reached a thorough understanding of radio emission in ULX we could also use the SKA as a discovery instrument for new ULX candidates. The new array will give an enormous space to discovery: sources like the ones currently known will be detected in a snapshot up to 50 Mpc instead of at 5 Mpc with long, pointed observations.
Exploring the Magnetic Field Structure of the Milky Way with Pulsars in the SKA Era
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；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）
Exploring Galactic plasma with pulsars in the SKA era
INAF-Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；SETI Institute（SETI研究所）；Rochester Institute of Technology（罗切斯特理工学院）；Swinburne University of Technology（斯威本科技大学）；Moscow State University（莫斯科国立大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所）；California Institute of Technology（加州理工学院）；Carnegie Institution for Science（卡内基科学促进会）；University of Galway（高威大学）
Dual AGN and Multiple SMBH Systems in the Era of SKAO
University of the Witwatersrand（威特沃特斯兰德大学）；Tata Institute of Fundamental Research（塔塔基础研究所）；Institute of Astronomy Space and Earth Sciences（天体空间与地球科学研究所）；University of Oslo（奥斯陆大学）；Donostia International Physics Center（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊卡巴斯基克，巴斯克科学基金会）；University of Edinburgh（爱丁堡大学）；University of Geneva（日内瓦大学）
Probing Merger Shocks in Galaxy Clusters in the SKA Era
National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（国家射电天文中心，塔塔基础研究所）；Centre for Radio Astronomy Techniques and Technologies, Rhodes University（射电天文技术与方法中心，罗德斯大学）；Institute of Astronomy, National Tsing Hua University（天文研究所，国立清华大学）；Pole Scientific, University Catholic of Lyon（科学系，里昂天主教大学）；Department of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore（天文学、天体物理学与空间工程系，印度印度理工学院印多尔分校）
Exploring the Galactic plasma with pulsars in the SKA Era
SETI Institute（SETI研究所）；Rochester Institute of Technology（罗切斯特理工学院）；Swinburne University of Technology（斯威本科技大学）；Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav)（澳大利亚研究委员会引力波发现卓越中心（OzGrav））；Moscow State University（莫斯科国立大学）；ASTRON, Netherlands Institute for Radio Astronomy（荷兰射电天文研究所 ASTRON）；California Institute of Technology（加州理工学院）；University of Galway（高威大学）；Macquarie University（麦考瑞大学）；University of Central Florida（中佛罗里达大学）；Curtin University（科廷大学）；Observatoire de Paris（巴黎天文台）；Chinese Academy of Sciences（中国科学院）；University of Chinese Academy of Sciences（中国科学院大学）；University of Cape Town（开普敦大学）；The University of Manchester（曼彻斯特大学）
Radio sirens: inferring $H_0$ with binary black holes and neutral hydrogen in the era of the Einstein Telescope and the SKA Observatory
Marietta Blau Institute - Austrian Academy of Sciences（玛丽亚·布劳研究所 - 奥地利科学院）；INFN, Sezione di Roma（罗马国家核物理研究所）；Observatoire de la Côte d’Azur, Laboratoire Lagrange（蔚蓝海岸天文台，拉格朗日实验室）；Department of Physics & Astronomy, University of the Western Cape（西开普大学物理与天文学系）；INAF - Institute of Radioastronomy (IRA)（意大利国家天体物理研究所射电天文研究所）；Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN - Laboratori Nazionali del Gran Sasso (LNGS)（意大利国家核物理研究所格兰萨索国家实验室）；Dipartimento di Fisica, Università degli Studi di Cagliari（卡利亚里大学物理系）；INFN, Sezione di Cagliari（卡利亚里国家核物理研究所）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）
Testing Gravity with Binary Pulsars in the SKA Era
Peking University（北京大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Swinburne University of Technology（斯威本科技大学）；University of Cape Town（开普敦大学）；University of Bremen（不来梅大学）；University of Oldenburg（奥尔登堡大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；State Key Laboratory of Radio Astronomy and Technology（射电天文与技术国家重点实验室）；University of British Columbia（不列颠哥伦比亚大学）；The University of Manchester（曼彻斯特大学）
Testing Gravity with Binary Pulsars in the SKA Era
Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学柯利天体物理与天文研究所）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；INAF-Osservatorio Astronomico di Cagliari（意大利国家天体物理研究院卡利亚里天文台）；Center for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）；High Energy Physics, Cosmology & Astrophysics Theory (HEPCAT) Group, Department of Mathematics and Applied Mathematics, University of Cape Town（开普敦大学数学与应用数学系高能物理、宇宙学与天体物理理论组）；Center of Applied Space Technology and Microgravity (ZARM), University of Bremen（不来梅大学应用空间技术与微重力中心）；Lohrmann Observatory, Technische Universität Dresden（德累斯顿工业大学洛尔曼天文台）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；Institute of Physics, University of Oldenburg（奥尔登堡大学物理研究所）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）
Fast Luminous Blue Transients in the Reionization Era and Beyond
精确确定再电离时代和揭示非均匀再电离的性质是现代宇宙学的重要课题。现有的研究再电离的方法，使用宇宙微波背景，Ly $α$发射体，类星体，或伽马射线暴，在精度或事件率方面有困难。我们建议，最近发现的快速发光蓝瞬变（FLBTs）有可能作为一种新的探针的再电离。我们研究了FLBTs的可探测性在再电离的时代与即将到来的WFIRST宽视场仪器（WFI），使用来自星系观测的恒星形成率和FLBTs的事件率成比例的恒星形成率。我们发现，如果FLBTs的发生率为核心坍缩超新星发生率的1%，那么，在近红外波段以26.5等的极限星等和10天的周期进行巡天，每年每度$^2$ at $z>6$（$z>8$）可探测到2（0.3）个FLBTs。我们的结论是，WFIRST超新星深度巡天可以在不久的将来探测到再电离时期的$\sim20$ FLBT。
SKA-VLBI Probes of High-energy Emission Processes in Relativistic Jets
University of Manchester（曼彻斯特大学）；University of Bristol（布里斯托大学）；Max Planck Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；Joint Institute for VLBI ERIC（甚长基线干涉测量联合研究所）；University of Turku（图尔库大学）；Aalto University（阿尔托大学）
University of Hertfordshire（赫特福德大学）；Amity University Uttar Pradesh（北方阿美蒂大学）；The Inter-University Institute for Data Intensive Astronomy (IDIA)（数据密集型天文学跨大学研究所）；University of Cape Town（开普敦大学）；National Centre for Radio Astrophysics - Tata Institute of Fundamental Research（国家射电天文中心 - 塔塔基础研究所）；UM-DAE Centre for Excellence in Basic Sciences, University of Mumbai（孟买大学基础科学卓越中心）；NCU（尼古拉·哥白尼大学）；Catholic University of Lyon（里昂天主教大学）；University of Oslo（奥斯陆大学）；University of Tasmania（塔斯马尼亚大学）
Discovery of the luminous X-ray ignition eRASSt J234402.9$-$352640; I. Tidal disruption event or a rapid increase in accretion in an active galactic nucleus?
Western Sydney University（西悉尼大学）；College of Science, China Three Gorges University（三峡大学理学院）；Center for Astronomy and Space Sciences, China Three Gorges University（三峡大学天文与空间科学中心）；Institute for Applied Problems in Mechanics and Mathematics, National Academy of Sciences of Ukraine（乌克兰国家科学院应用力学与数学问题研究所）；International Centre for Radio Astronomy Research, Curtin University（科廷大学国际射电天文研究中心）；Dominion Radio Astrophysical Observatory, Herzberg Astronomy and Astrophysics, National Research Council Canada（加拿大国家研究委员会赫茨伯格天体物理学部 Dominion 射电天文台）；Dr. Karl Remeis Observatory, Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg（埃尔朗根-纽伦堡大学弗里德里希·亚历山大大学卡尔·雷梅斯天文台暨埃尔朗根高能粒子物理中心）
