Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM
A recent report on the detection of very-high-energy gamma rays from V4641 Sagittarii (V4641 Sgr) up to ≈0.8 PeV 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 2024 September. Thanks to t...
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| author | 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 Maria Díaz Trigo Teo Muñoz-Darias Montserrat Armas Padilla Ryota Tomaru Yoshihiro Ueda |
| author_facet | 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 Maria Díaz Trigo Teo Muñoz-Darias Montserrat Armas Padilla Ryota Tomaru Yoshihiro Ueda |
| author_sort | Hiromasa Suzuki |
| collection | DOAJ |
| description | A recent report on the detection of very-high-energy gamma rays from V4641 Sagittarii (V4641 Sgr) up to ≈0.8 PeV 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 2024 September. 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 σ and >10 σ based on our imaging and spectral analysis, respectively. The spatial extent is estimated to have a radius of 7′ ± 3′ (13 ± 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 μ G) or a suppressed diffusion coefficient (∼10 ^27 cm ^2 s ^−1 at 100 TeV). The integrated X-ray flux, (4–6) × 10 ^−12 erg s ^−1 cm ^−2 (2–10 keV), would require a magnetic field strength higher than the Galactic mean (≳8 μ G) 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 × 10 ^39 erg s ^−1 , which is comparable to the Eddington luminosity of this system. |
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| spelling | doaj-art-ab6a235999a14d59add92bc2e33b0ade2025-08-20T01:53:25ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019782L2010.3847/2041-8213/ad9d11Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISMHiromasa Suzuki0https://orcid.org/0000-0002-8152-6172Naomi Tsuji1https://orcid.org/0000-0001-7209-9204Yoshiaki Kanemaru2https://orcid.org/0000-0002-4541-1044Megumi Shidatsu3https://orcid.org/0000-0001-8195-6546Laura Olivera-Nieto4https://orcid.org/0000-0002-9105-0518Samar Safi-Harb5https://orcid.org/0000-0001-6189-7665Shigeo S. Kimura6https://orcid.org/0000-0003-2579-7266Eduardo de la Fuente7https://orcid.org/0000-0001-9643-4134Sabrina Casanova8https://orcid.org/0000-0002-6144-9122Kaya Mori9https://orcid.org/0000-0002-9709-5389Xiaojie Wang10https://orcid.org/0000-0001-6798-353XSei Kato11https://orcid.org/0000-0003-2251-2544Dai Tateishi12https://orcid.org/0000-0003-0248-4064Hideki Uchiyama13https://orcid.org/0000-0003-4580-4021Takaaki Tanaka14https://orcid.org/0000-0002-4383-0368Hiroyuki Uchida15https://orcid.org/0000-0003-1518-2188Shun Inoue16https://orcid.org/0000-0003-3085-304XDezhi Huang17https://orcid.org/0000-0002-5447-1786Marianne Lemoine-Goumard18https://orcid.org/0000-0002-4462-3686Daiki Miura19https://orcid.org/0009-0009-0439-1866Shoji Ogawa20https://orcid.org/0000-0002-5701-0811Shogo B. Kobayashi21https://orcid.org/0000-0001-7773-9266Chris Done22https://orcid.org/0000-0002-1065-7239Maxime Parra23https://orcid.org/0009-0003-8610-853XMaria Díaz Trigo24https://orcid.org/0000-0001-7796-4279Teo Muñoz-Darias25https://orcid.org/0000-0002-3348-4035Montserrat Armas Padilla26https://orcid.org/0000-0002-4344-7334Ryota Tomaru27https://orcid.org/0000-0002-6797-2539Yoshihiro Ueda28https://orcid.org/0000-0001-7821-6715Institute of Space and Astronautical Science (ISAS) , Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, JapanFaculty of Science, Kanagawa University , 3-27-1 Rokukakubashi, Kanagawa-ku, Yokohama-shi, Kanagawa 221-8686, Japan; Interdisciplinary Theoretical & Mathematical Science Program (iTHEMS) , RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, JapanInstitute of Space and Astronautical Science (ISAS) , Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, JapanDepartment of Physics, Ehime University , 2-5 Bunkyocho, Matsuyama, Ehime 790-8577, JapanMax-Planck-Institut für Kernphysik , P.O. Box 103980, D-69029 Heidelberg, GermanyDepartment of Physics and Astronomy, University of Manitoba , Winnipeg, MB R3T 2N2, CanadaFrontier Research Institute for Interdisciplinary Sciences, Tohoku University , Sendai 980-8578, Japan; Astronomical Institute, Graduate School of Science, Tohoku University , Sendai 980-8578, JapanDepartamento de Física, CUCEI, Universidad de Guadalajara , Blvd. Marcelino García Barragan 1420, Olímpica, 44430, Guadalajara, Jalisco, MexicoInstytut Fizyki Ja̧drowej PAN , ul. Radzikowskiego 152, 31-342 Kraków, PolandColumbia Astrophysics Laboratory, Columbia University , 538 West 120th Street, New York, NY 10027, USADepartment of Physics, Michigan Technological University , Houghton, MI, USAInstitute for Cosmic Ray Research, University of Tokyo , Kashiwa 277-8582, JapanDepartment of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanFaculty of Education, Shizuoka University , 836 Ohya, Suruga-ku, Shizuoka, Shizuoka 422-8529, JapanKonan University , Department of Physics, 8-9-1 Okamoto, Higashinada, Kobe, Hyogo, 658-8501, JapanDepartment of Physics, Graduate School of Science, Kyoto University , Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, JapanDepartment of Physics, Graduate School of Science, Kyoto University , Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, JapanDepartment of Physics, University of Maryland , College Park, MD, USAUniversité Bordeaux , CNRS, CENBG, UMR 5797, F-33170 Gradignan, FranceInstitute of Space and Astronautical Science (ISAS) , Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, Japan; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanInstitute of Space and Astronautical Science (ISAS) , Japan Aerospace Exploration Agency (JAXA), Kanagawa 252-5210, JapanDepartment of Physics, Tokyo University of Science , 1-3 Kagurazaka, Shinjuku-ku, Tokyo 162-8601, JapanCentre for Extragalactic Astronomy, Department of Physics, University of Durham , South Road, Durham DH1 3LE, UKUniversité Grenoble Alpes , CNRS, IPAG, F-38000 Grenoble, France; Dipartimento di Matematica e Fisica, Universitá degli Studi RomaTre , Via della Vasca Navale 84, I-00146 Roma, ItalyESO , Karl-Schwarzschild-Strasse 2, 85748, Garching bei München, GermanyInstituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna , E-38206 La Laguna, Tenerife, SpainInstituto de Astrofísica de Canarias , E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna , E-38206 La Laguna, Tenerife, SpainDepartment of Earth and Space Science, Graduate School of Science, Osaka University , 1-1 Machikaneyama, Toyonaka, Osaka 560-0043, JapanDepartment of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, JapanA recent report on the detection of very-high-energy gamma rays from V4641 Sagittarii (V4641 Sgr) up to ≈0.8 PeV 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 2024 September. 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 σ and >10 σ based on our imaging and spectral analysis, respectively. The spatial extent is estimated to have a radius of 7′ ± 3′ (13 ± 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 μ G) or a suppressed diffusion coefficient (∼10 ^27 cm ^2 s ^−1 at 100 TeV). The integrated X-ray flux, (4–6) × 10 ^−12 erg s ^−1 cm ^−2 (2–10 keV), would require a magnetic field strength higher than the Galactic mean (≳8 μ G) 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 × 10 ^39 erg s ^−1 , which is comparable to the Eddington luminosity of this system.https://doi.org/10.3847/2041-8213/ad9d11Low-mass x-ray binary starsGamma-ray sourcesRadio jetsNon-thermal radiation sources |
| spellingShingle | 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 Maria Díaz Trigo Teo Muñoz-Darias Montserrat Armas Padilla Ryota Tomaru Yoshihiro Ueda Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM The Astrophysical Journal Letters Low-mass x-ray binary stars Gamma-ray sources Radio jets Non-thermal radiation sources |
| title | Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM |
| title_full | Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM |
| title_fullStr | Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM |
| title_full_unstemmed | Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM |
| title_short | Detection of Extended X-Ray Emission around the PeVatron Microquasar V4641 Sgr with XRISM |
| title_sort | detection of extended x ray emission around the pevatron microquasar v4641 sgr with xrism |
| topic | Low-mass x-ray binary stars Gamma-ray sources Radio jets Non-thermal radiation sources |
| url | https://doi.org/10.3847/2041-8213/ad9d11 |
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