Deep Synoptic Array science: Two fast radio burst sources in massive galaxy clusters
Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark H… 展开作者
Liam Connor, Vikram Ravi, Morgan Catha, Ge Chen, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Jack Sayers, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
The hot gas that constitutes the intracluster medium (ICM) has been studied at X-ray and millimeter/sub-millimeter wavelengths (Sunyaev-Zeldovich effect) for decades. Fast radio bursts (FRBs) offer an additional method of directly measuring the ICM and gas surrounding clusters, via observables such as dispersion measure (DM) and Faraday rotation measure (RM). We report the discovery of two FRB sources detected with the Deep Synoptic Array (DSA-110) whose host galaxies belong to massive galaxy clusters. In both cases, the FRBs exhibit excess extragalactic DM, some of which likely originates in the ICM of their respective clusters. FRB 20220914A resides in the galaxy cluster Abell 2310 at z=0.1125 with a projected offset from the cluster center of 520 kpc. The host of a second source, FRB 20220509G, is an elliptical galaxy at z=0.0894 that belongs to the galaxy cluster Abell 2311 at projected offset of 870 kpc. These sources represent the first time an FRB has been localized to a galaxy cluster. We combine our FRB data with archival X-ray, SZ, and optical observations of these clusters in order to infer properties of the ICM, including a measurement of gas temperature from DM and ySZ of 0.8-3.9 keV. We then compare our results to massive cluster halos from the IllustrisTNG simulation. Finally, we describe how large samples of localized FRBs from future surveys will constrain the ICM, particularly beyond the virial radius of clusters.
Deep Synoptic Array science: a 50 Mpc fast radio burst constrains the mass of the Milky Way circumgalactic medium
我们提出的深层天气阵列（DSA-110）的发现和干涉定位到目前为止，非重复FRB 20220319 D。FRB起源于一个年轻的、快速形成恒星的棒旋星系IRAS 02044 $+$ 7048，它的质量只有50 Mpc。虽然NE 2001和YMW 16模型的银河系星际介质（ISM）的DM的FRB 20220319 D的贡献超过其总观测DM，我们表明，在这些模型中的不确定性容纳的爆发河外起源。我们推导出一个保守的上限DM贡献的环银河系介质（CGM）的银河系：限制是28.7 pc cm $^{-3}$和47.3 pc cm $^{-3}$，这取决于两个恒星附近的天空FRB 20220319 D是用来估计ISM DM。这些极限都意味着银河系CGM的总质量是$<10^{11}M_{\odot}$，而银河系的重子质量是给定总晕质量的宇宙学平均值的$\lesssim60\%$。当遥远的球状星团M53中的双星DM被另外考虑时，可能会有更严格但不那么保守的约束。虽然我们的约束条件是敏感的CGM中可能的各向异性和假设的形式的径向密度分布，它们不受CGM的化学和热性质的不确定性。我们的研究结果强烈支持星系形成模拟通常预测的情况，其中反馈过程从像银河系这样的星系晕中驱逐重子物质。
Searches for inspiral gravitational waves associated with short gamma-ray bursts in LIGO's fifth and Virgo's first science run
两个致密物体的合并，比如两颗中子星或一颗中子星和一个黑洞，很可能是短伽马射线暴的起源。这些事件也是有希望的引力波来源，目前正在激发国际引力波探测器网络的相关搜索。在这里，我们描述了一个搜索的引力波从螺旋阶段的两个合并紧凑的对象，在巧合的短伽玛射线暴发生在LIGO的第五次科学运行和处女座的第一次科学运行。这次搜索包括22个GRB，这些GRB的数据来自LIGO/Virgo网络中的多个探测器。没有发现统计上显著的引力波候选者，参数检验表明在我们的伽玛暴样本中没有多余的弱引力波信号。90%~ C. L.在中子星-黑洞祖先模型假设下，我们的样本中伽玛暴的中位排斥距离为6.7 Mpc。
Modelling DSA, FAST and CRAFT surveys in a z-DM analysis and constraining a minimum FRB energy
International Centre for Radio Astronomy Research, Curtin University（国际射电天文研究中心，科廷大学）；Department of Astronomy and Astrophysics, University of California, Santa Cruz（天文学与天体物理学系，加州大学圣克鲁兹分校）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University（天体物理跨学科探索与研究中心（CIERA）及物理与天文学系，西北大学）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（天体物理学与超级计算中心，斯威本科技大学）；School of Mathematical and Physical Sciences, Macquarie University（数学与物理科学学院，麦考瑞大学）
The DSA/Chronoscope fast radio burst survey: forecasts and science overview
Harvard & Smithsonian（哈佛大学与史密森尼学会）；California Institute of Technology（加州理工学院）；The Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Cornell University（康奈尔大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；University of Arizona（亚利桑那大学）；Northwestern University（西北大学）；University of California, Berkeley（加州大学伯克利分校）；Massachusetts Institute of Technology（麻省理工学院）
Tracing the Host-Galaxy Environments of FRBs with a New Sample of Localized Sources Detected with the DSA-110
California Institute of Technology（加州理工学院）；Owens Valley Radio Observatory, California Institute of Technology（加州理工学院欧文斯谷射电天文台）；Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）
Optimal Pulsar Timing Array Strategies with the Deep Synoptic Array
New Mexico Institute of Mining and Technology（新墨西哥矿业理工学院）；National Radio Astronomy Observatory（国家射电天文台）；Oregon State University（俄勒冈州立大学）；Green Bank Observatory（格林班克天文台）；SETI Institute（SETI研究所）；University of Wisconsin-Milwaukee（威斯康星大学密尔沃基分校）；University of North Carolina, Chapel Hill（北卡罗来纳大学教堂山分校）；Newcastle University（纽卡斯尔大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Widener University（韦德纳大学）；Lafayette College（拉斐特学院）；Institute for Gravitational Wave Astr（引力波天体物理研究所）
SVOM/VT: Instrument Overview, Science Objectives, and First-Year Performance
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Xi’an Institute of Optics and Precision Mechanics, Chinese Academy of Sciences（中国科学院西安光学精密机械研究所）
Université Paris-Saclay（巴黎萨克雷大学）；Université Paris Cité（巴黎西岱大学）；CEA（法国原子能和替代能源委员会）；CNRS（法国国家科学研究中心）；AIM（天体物理与分子研究所）；CEA Paris-Saclay, Institut de Recherche sur les lois Fondamentales de l’Univers（巴黎萨克雷CEA基础定律研究所）；Aix Marseille Univ（艾克斯-马赛大学）；CNES（法国国家空间研究中心）；LAM（天体物理与分子实验室）；Sorbonne Université（索邦大学）；Institut d’Astrophysique de Paris（巴黎天体物理研究所）；IRAP（天体物理学研究）；Université de Toulouse（图卢兹大学）
