Detection of extended X-ray emission around the PeVatron microquasar V4641 Sgr with XRISM
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2024
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| author | Suzuki, Hiromasa Tsuji, Naomi Kanemaru, Yoshiaki Shidatsu, Megumi Olivera-Nieto, Laura Safi-Harb, Samar Kimura, Shigeo S. de la Fuente, Eduardo Casanova, Sabrina Mori, Kaya Wang, Xiaojie Kato, Sei Tateishi, Dai Uchiyama, Hideki Tanaka, Takaaki Uchida, Hiroyuki Inoue, Shun Huang, Dezhi Lemoine-Goumard, Marianne Miura, Daiki Ogawa, Shoji Kobayashi, Shogo B. Done, Chris Parra, Maxime Trigo, María Díaz Muñoz-Darias, Teo Padilla, Montserrat Armas Tomaru, Ryota Ueda, Yoshihiro |
| author_facet | Suzuki, Hiromasa Tsuji, Naomi Kanemaru, Yoshiaki Shidatsu, Megumi Olivera-Nieto, Laura Safi-Harb, Samar Kimura, Shigeo S. de la Fuente, Eduardo Casanova, Sabrina Mori, Kaya Wang, Xiaojie Kato, Sei Tateishi, Dai Uchiyama, Hideki Tanaka, Takaaki Uchida, Hiroyuki Inoue, Shun Huang, Dezhi Lemoine-Goumard, Marianne Miura, Daiki Ogawa, Shoji Kobayashi, Shogo B. Done, Chris Parra, Maxime Trigo, María Díaz Muñoz-Darias, Teo Padilla, Montserrat Armas Tomaru, Ryota Ueda, Yoshihiro |
| contents | 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_08089 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Detection of extended X-ray emission around the PeVatron microquasar V4641 Sgr with XRISM Suzuki, Hiromasa Tsuji, Naomi Kanemaru, Yoshiaki Shidatsu, Megumi Olivera-Nieto, Laura Safi-Harb, Samar Kimura, Shigeo S. de la Fuente, Eduardo Casanova, Sabrina Mori, Kaya Wang, Xiaojie Kato, Sei Tateishi, Dai Uchiyama, Hideki Tanaka, Takaaki Uchida, Hiroyuki Inoue, Shun Huang, Dezhi Lemoine-Goumard, Marianne Miura, Daiki Ogawa, Shoji Kobayashi, Shogo B. Done, Chris Parra, Maxime Trigo, María Díaz Muñoz-Darias, Teo Padilla, Montserrat Armas Tomaru, Ryota Ueda, Yoshihiro High Energy Astrophysical Phenomena 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. |
| title | Detection of extended X-ray emission around the PeVatron microquasar V4641 Sgr with XRISM |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2412.08089 |