Detection of extended X-ray emission around the PeVatron microquasar V4641 Sgr with XRISM
Hiromasa Suzuki, Naomi Tsuji, Yoshiaki Kanemaru, Megumi Shidatsu, Laura Olivera-Nieto, Samar Safi-Harb, Shigeo S. Kimura, Eduardo de la Fuente, Sabrina Casanova… 展开作者
Hiromasa Suzuki, Naomi Tsuji, Yoshiaki Kanemaru, Megumi Shidatsu, Laura Olivera-Nieto, Samar Safi-Harb, Shigeo S. Kimura, Eduardo de la Fuente, Sabrina Casanova, Kaya Mori, Xiaojie Wang, Sei Kato, Dai Tateishi, Hideki Uchiyama, Takaaki Tanaka, Hiroyuki Uchida, Shun Inoue, Dezhi Huang, Marianne Lemoine-Goumard, Daiki Miura, Shoji Ogawa, Shogo B. Kobayashi, Chris Done, Maxime Parra, María Díaz Trigo, Teo Muñoz-Darias, Montserrat Armas Padilla, Ryota Tomaru, Yoshihiro Ueda
备注：
9 pages, 5 figures, accepted for publication in ApJL
A recent report on the detection of very-high-energy gamma rays from V4641 Sagittarii (V4641 Sgr) up to ~0.8 peta-electronvolt has made it the second confirmed "PeVatron" microquasar. Here we report on the observation of V4641 Sgr with X-Ray Imaging and Spectroscopy Mission (XRISM) in September 2024. Thanks to the large field of view and low background, the CCD imager Xtend successfully detected for the first time X-ray extended emission around V4641 Sgr with a significance of > 4.5 sigma and > 10 sigma based on our imaging and spectral analysis, respectively. The spatial extent is estimated to have a radius of $7 \pm 3$ arcmin ($13 \pm 5$ pc at a distance of 6.2 kpc) assuming a Gaussian-like radial distribution, which suggests that the particle acceleration site is within ~10 pc of the microquasar. If the X-ray morphology traces the diffusion of accelerated electrons, this spatial extent can be explained by either an enhanced magnetic field (~80 uG) or a suppressed diffusion coefficient (~$10^{27}$ cm$^2$ s$^{-1}$ at 100 TeV). The integrated X-ray flux, (4-6)$\times 10^{-12}$ erg s$^{-1}$ cm$^{-2}$ (2-10 keV), would require a magnetic field strength higher than the galactic mean (> 8 uG) if the diffuse X-ray emission originates from synchrotron radiation and the gamma-ray emission is predominantly hadronic. If the X-rays are of thermal origin, the measured extension, temperature, and plasma density can be explained by a jet with a luminosity of ~$2\times 10^{39}$ erg s$^{-1}$, which is comparable to the Eddington luminosity of this system.
Instituto Argentino de Radioastronomía (CCT La Plata, CONICET（阿根廷射电天文研究所）；CICPBA（拉普拉塔国立大学天文与地球物理学院）；UNLP)（巴塞罗那大学宇宙科学研究所）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata；Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB)
Microquasar Remnants as Pevatrons Illuminating the Galactic Cosmic Ray Knee
Key Laboratory of Particle Astrophysics and Experimental Physics Division and Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所粒子天体物理重点实验室及实验物理部计算中心）；TIANFU Cosmic Ray Research Center（天府宇宙线研究中心）；Department of Physics and Astronomy, University of Utah（犹他大学物理与天文系）
Microquasar Cygnus X-3 as the PeVatron powering the Cygnus Bubble
University of Science and Technology of China（中国科学技术大学）；Yerevan State University（埃里温国立大学）；TIANFU Cosmic Ray Research Center（天府宇宙线研究中心）；Max-Planck-Institut for Nuclear Physics（马克斯·普朗克核物理研究所）
Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；TIANFU Cosmic Ray Research Center（天府宇宙线研究中心）；Frontier Research Institute for Interdisciplinary Sciences, Tohoku University（东北大学前沿跨学科研究院）；Astronomical Institute, Tohoku University（东北大学天文研究所）；The Pennsylvania State University（宾夕法尼亚州立大学）；Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理研究所）
XMM-Newton Resolves Parsec-scale X-ray Jets in the PeVatron Microquasar V4641 Sgr
Institute for Cosmic Ray Research, The University of Tokyo（宇宙线研究所，东京大学）；Interdisciplinary Theoretical & Mathematical Science Center (iTHEMS), RIKEN（理化学研究所交叉理论与数学科学中心(iTHEMS)）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Como Lake Center for Astrophysics (CLAP), DiSAT, Università degli Studi dell’Insubria（因苏布里亚大学地球科学与技术系科莫湖天体物理中心）；Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学哥伦比亚天体物理学实验室）；The University of Miyazaki（宫崎大学）；Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所粒子天体物理重点实验室）；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）；Department of Physics and Astronomy, University of Manitoba（曼尼托巴大学物理与天文学系）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内库克天体物理研究所）
Magnetic rigidity reveals the PeVatron acceleration region in SS 433
School of Physics and Astronomy, Sun Yat-sen University（中山大学物理与天文学院）；State Key Laboratory of Radio Astronomy and Technology, Xinjiang Astronomical Observatory, CAS（中国科学院新疆天文台射电天文与技术国家重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学与空间科学学院）；Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（孔科利天文台，匈牙利研究与教育网络天文学与地球科学研究中心）；Xinjiang Key Laboratory of Radio Astrophysics, Xinjiang Astronomical Observatory, CAS（中国科学院新疆天文台射电天体物理学新疆重点实验室）
Two kinds of Galactic source populations could explain the cosmic-ray observation up to the "knee" region
Beihang University（北京航空航天大学）；Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；University of Chinese Academy of Sciences（中国科学院大学）
The unidentified PeV source LHAASO J2108+5157: A microquasar remnant?
Universidad de Jaén（哈恩大学）；Instituto Argentino de Radioastronomía (CCT La Plata, CONICET（阿根廷射电天文研究所）；CICPBA（拉普拉塔国立大学天文与地球科学学院）；UNLP)（巴塞罗那大学）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata；Universitat de Barcelona
XRISM spectroscopy of a crowded Galactic center region -- II. Narrow emission lines in the Black Hole candidate MAXI J1744-294/Swift J174540.2-290037
Ehime University（爱媛大学）；Columbia University（哥伦比亚大学）；Kyoto University（京都大学）；Osaka University（大阪大学）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；Massachusetts Institute of Technology（麻省理工学院）
Constraints on Hadronic Emission from Microquasars Detected by LHAASO
INAF Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切尔西天文台）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交大凌波书院）；Université Paris Cité, CNRS, AstroParticule et Cosmologie（巴黎西岱大学法国国家科学研究中心粒子与宇宙学实验室）
Revisiting the XMM-Newton Observations of the Galactic Microquasar SS 433: Implications for the Origin of the Ultrahigh-Energy Emission Detected by LHAASO
School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education（南京大学现代天体学与天体物理教育部重点实验室）；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）
Instituto Argentino de Radioastronomía (CCT La Plata, CONICET（阿根廷射电天文研究所）；CICPBA（拉普拉塔国立大学天文与地球物理科学学院）；UNLP)（巴塞罗那大学宇宙科学研究所量子天体物理系）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata；Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB)
Hadronic Emissions from the Microquasar V4641 Sgr, SS433, and its implications in the Diffuse Galactic Emission
Presidency University（总统大学）；Gran Sasso Science Institute（格兰萨索科学研究所）；INFN/Laboratori Nazionali del Gran Sasso（意大利国家核物理研究所/格兰萨索国家实验室）；Aryabhatta Research Institute of Observational Sciences (ARIES)（阿亚巴哈观测科学研究所）；University of Johannesburg（约翰内斯堡大学）；Central University of Kashmir（克什米尔中央大学）
Candidate X-ray Counterparts of Ultra-High-Energy Emission of the Galactic Microquasar V4641 Sgr Revealed by Einstein Probe
Nanjing University（南京大学）；Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education（南京大学现代天文与天体物理教育部重点实验室）；Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；State Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所粒子天体物理国家重点实验室）；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）
Particle acceleration and non-thermal broadband spectrum of extended shocked outflows in black hole binary V4641 Sgr - a galactic pevatron
Ioffe Institute（伊俄费研究所）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Space Research Institute (IKI)（太空研究所（IKI））；Rudolf Peierls Centre for Theoretical Physics, Department of Physics, University of Oxford（牛津大学物理系鲁道夫·派尔斯理论物理中心）
Large-scale radio bubbles around the black hole transient V4641 Sgr
Université Paris Cité（巴黎西岱大学）；Université Paris-Saclay（巴黎萨克雷大学）；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、分子与星际介质实验室）；University of Oxford（牛津大学）；University of Cape Town（开普敦大学）；Rhodes University（罗德岛大学）；South African Radio Astronomy Observatory（南非射电天文观测站）；INAF-Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Istituto Nazionale di Astrofisica（意大利国家天体物理研究所）；Osservatorio Astronomico di Brera（布雷拉天文台）
Leptonic and hadronic models of high-energy nebula around V4641 Sgr
Institut Polytechnique de Paris（巴黎理工学院）；Université de Paris Cite, CNRS, Astroparticule et Cosmologie（巴黎西岱大学、法国国家科学研究中心、亚原子粒子与宇宙学）；Laboratory of Astrophysics, Ecole Polytechnique Federale de Lausanne（洛桑联邦理工学院天体物理学实验室）；Institutt for fysikk, NTNU（挪威科技大学物理系）
An Ultrahigh-energy $γ$-ray Bubble Powered by a Super PeVatron
Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所）；University of Chinese Academy of Sciences（中国科学院大学）；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）；Dublin Institute for Advanced Studies（都柏林高等研究院）；State Key Laboratory of Particle Detection and Electronics（粒子探测与电子学国家重点实验室）；University of Science and Technology of China（中国科学技术大学）；Southwest Jiaotong University（西南交通大学）；Nanjing University（南京大学）；Guangzhou University（广州大学）；Hebei Normal University（河北师范大学）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Shanghai Jiao Tong University（上海交通大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Tibet University（西藏大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Sun Yat-sen University（中山大学）；Yunnan University（云南大学）；Shandong University（山东大学）；Tsinghua University（清华大学）；Zhengzhou University（郑州大学）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Sichuan University（四川大学）；Institute for Nuclear Research of Russian Academy of Sciences（俄罗斯科学院核物理研究所）；Peking University（北京大学）；Guangxi University（广西大学）；Mahidol University（玛希隆大学）；Nanchang University（南昌大学）；National Space Science Center, Chinese Academy of Sciences（中国科学院国家空间科学中心）
The Western Jet of SS 433/W50: Hard X-ray Emission, Spectral Evolution, and Comparison to the Eastern Jet
University of Manitoba（曼尼托巴大学）；Chinese Academy of Sciences（中国科学院）；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）；Columbia Astrophysics Laboratory（哥伦比亚天体物理实验室）；University of California San Diego（加州大学圣地亚哥分校）；Institute for Cosmic Ray Research, University of Tokyo（东京大学宇宙射线研究所）
利用 NuSTAR 和 XMM-Newton 观测，在 W50 西瓣检测到高达 30 keV 的硬非热 X 射线发射，源自“头部”区域，具有硬光子指数 1.55，并呈现远离 SS 433 的谱变陡，与东瓣对称，支持喷流驱动起源。
