The intergalactic medium (IGM) plays an important role in the formation and evolution of galaxies. Recent developments in upcoming radio telescopes are starting to open up the possibility of making a first direct detection of the 21 cm signal of neutral hydrogen (HI) from the warm gas of the IGM in large-scale filaments. The cosmological hydrodynamical EAGLE simulation is used to estimate the typical IGM filament signal. Assuming the same average signal for all filaments, a prediction is made for the detectability of such a signal with the upcoming mid-frequency array of the Square Kilometer Array (SKA1-mid) or the future upgrade to SKA2. The signal-to-noise (S/N) then only depends on the size and orientation of each filament. With filament spines inferred from existing galaxy surveys as a proxy for typical real filaments, we find hundreds of filaments in the region of the sky accessible to the SKA that can be detected. Once the various phases of the SKA telescope become operational, their own surveys will be able to find the galaxies required to infer the position of even more filaments within the survey area. We find that in 120 h, SKA1-mid/SKA2 will detect HI emission from the strongest filaments in the field with a S/N of the order of 10 to $\sim$150 for the most pessimistic model considered here. Some of the brighter filaments can be detected with an integration time of a few minutes with SKA1-mid and a few seconds with SKA2. Therefore, SKA2 will be capable of not only detecting but also mapping a large part of the IGM in these filaments.
Study of Polarized Emission in Radio Halos and Filaments in the SKA Telescopes Era
Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；Sapienza—University of Rome（罗马第一大学）；University of Bologna（博洛尼亚大学）；Université Côte d'Azur（蔚蓝海岸大学）；University of Cagliari（卡利亚里大学）
The Large-Scale Structure of the Universe through the SKA lenses
University of Bologna（博洛尼亚大学）；Manipal Academy of Higher Education（马尼拉高等教育学院）；University of Hamburg（汉堡大学）；MIT Art, Design and Technology University（麻省理工学院艺术、设计与技术大学）；Tata Institute of Fundamental Research（塔塔基础研究所）；University of Tartu（塔尔图大学）；National Astronomical Observatory of Japan（日本国立天文台）
Square Kilometer Array Synergies for the Epoch of Reionization and Cosmic Dawn
National Centre for Radio Astrophysics, Tata Institute of Fundamental Research（塔塔基础研究院射电天体物理国家中心）；Jadavpur University（贾达普大学）；University of Toronto（多伦多大学）；University of Cambridge（剑桥大学）；Kavli Institute for Cosmology（卡弗里宇宙学研究所）；Stockholm University（斯德哥尔摩大学）；University of Groningen（格罗宁根大学）；Université Paris-Saclay（巴黎萨克雷大学）；CNRS, Institut d'Astrophysique Spatiale（法国国家科学研究中心空间天体物理研究所）；University of Vienna（维也纳大学）；Indian Institute of Technology Indore（印度理工学院印多尔分校）；University of Catania（卡塔尼亚大学）；The University of Tokyo（东京大学）；The Open University of Israel（以色列开放大学）；Australian National University（澳大利亚国立大学）；National Astronomical Observatory of Japan（日本国立天文台）；Uppsala University（乌普萨拉大学）
Probing ionized bubbles around luminous sources during reionization with SKA 21-cm observations
Jadavpur University（贾达普大学）；Indian Institute of Technology Indore（印度印多尔理工学院）；The Open University of Israel（以色列开放大学）；Indian Institute of Technology Madras（印度马德拉斯理工学院）
A stochastic forward model for the intergalactic dispersion-measure distribution of Fast Radio Bursts
University of Cape Town（开普敦大学）；African Institute for Mathematical Sciences（非洲数学科学研究所）；National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）；Universidade Federal de Ouro Preto（欧罗普雷图联邦大学）；INAF – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；IFPU – Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Universidade Federal do Espírito Santo（圣埃斯皮里图联邦大学）
LIMFAST. V. Probing Reionization with the Synergy Between 21 cm and Photometric Galaxy Surveys
Northwestern University（西北大学）；University of Pennsylvania（宾夕法尼亚大学）；California Institute of Technology（加州理工学院）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；University of California, Los Angeles（加利福尼亚大学洛杉矶分校）
Detecting the signature of helium reionization through 3HeII 3.46cm line-intensity mapping
Heidelberg University（海德堡大学）；Universität Bonn, Argelander-Institut für Astronomie（波恩大学阿根兰德天文学研究所）；SISSA, International School for Advanced Studies（国际高等研究院）；Università di Trieste（的里雅斯特大学）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学 Kavli 宇宙粒子与天体物理学研究所）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学）；INAF – Astronomical Observatory of Trieste（意大利国家天体物理研究所的里雅斯特天文台）
