Ultra-high-energy gamma-ray bubble around microquasar V4641 Sgr

• 成果类型: Article
• 署名作者: Alfaro, R.; Alvarez, C.; Arteaga-Velazquez, J. C.; Rojas, D. Avila; Solares, H. A. Ayala; Babu, R.; Belmont-Moreno, E.; Caballero-Mora, K. S.; Capistran, T.; Carraminana, A.; Casanova, S.; Cotti, U.; Cotzomi, J.; de Leon, S. Coutino; De la Fuente, E.; Depaoli, D.; Di Lalla, N.; Diaz Hernandez, R.; Dingus, B. L.; DuVernois, M. A.; Durocher, M.; Diaz-Velez, J. C.; Engel, K.; Espinoza, C.; Fan, K. L.; Fang, K.; Fraija, N.; Fraija, S.; Garcia-Gonzalez, J. A.; Garcias, F.; Gonzalez Munoz, A.; Gonzalez, M. M.; Goodman, J. A.; Groetsch, S.; Harding, J. P.; Herzog, I; Hinton, J.; Huang, D.; Hueyotl-Zahuantitla, F.; Huntemeyer, P.; Iriarte, A.; Joshi, V; Kaufmann, S.; Kieda, D.; de Leon, C.; Lee, J.; Leon Vargas, H.; Linnemann, J. T.; Longinotti, A. L.; Luis-Raya, G.; Malone, K.; Martinez, O.; Martinez-Castro, J.; Matthews, J. A.; Miranda-Romagnoli, P.; Morales-Soto, J. A.; Moreno, E.; Mostafa, M.; Nayerhoda, A.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Olivera-Nieto, L.; Omodei, N.; Osorio, M.; Perez Araujo, Y.; Perez-Perez, E. G.; Rho, C. D.; Rosa-Gonzalez, D.; Ruiz-Velasco, E.; Salazar, H.; Salazar-Gallegos, D.; Sandoval, A.; Schneider, M.; Serna-Franco, J.; Smith, A. J.; Son, Y.; Springer, R. W.; Tibolla, O.; Tollefson, K.; Torres, I; Torres-Escobedo, R.; Turner, R.; Urena-Mena, F.; Varela, E.; Villasenor, L.; Wang, X.; Watson, I. J.; Willox, E.; Yun-Carcamo, S.; Zhou, H.
• 署名单位: Universidad Nacional Autonoma de Mexico; Universidad Autonoma de Chiapas; Universidad Michoacana de San Nicolas de Hidalgo; Pennsylvania Commonwealth System of Higher Education (PCSHE); Pennsylvania State University; Pennsylvania State University - University Park; Michigan Technological University; Universidad Nacional Autonoma de Mexico; Instituto Nacional de Astrofisica, Optica y Electronica; Polish Academy of Sciences; Institute of Nuclear Physics - Polish Academy of Sciences; Benemerita Universidad Autonoma de Puebla; University of Wisconsin System; University of Wisconsin Madison; Universidad de Guadalajara; Max Planck Society; Stanford University; United States Department of Energy (DOE); Los Alamos National Laboratory; University System of Maryland; University of Maryland College Park; Tecnologico de Monterrey; Michigan State University; University of Erlangen Nuremberg; Utah System of Higher Education; University of Utah; University of Seoul; United States Department of Energy (DOE); Los Alamos National Laboratory; Instituto Politecnico Nacional - Mexico; University of New Mexico; Universidad Autonoma del Estado de Hidalgo; Pennsylvania Commonwealth System of Higher Education (PCSHE); Temple University; Universidad Nacional Autonoma de Mexico; Sungkyunkwan University (SKKU); Shanghai Jiao Tong University
• 刊物名称: Nature
• ISSN/ISSBN: 0028-5221
• DOI: 10.1038/s41586-024-07995-9
• 发表日期: 2024-10-17
• 页码: 557-+
• 关键词: black-hole; molecular clouds; crab-nebula; cosmic-rays; jets; catalog; outburst; binaries; galaxy; scale

摘要

Microquasars are laboratories for the study of jets of relativistic particles produced by accretion onto a spinning black hole. Microquasars are near enough to allow detailed imaging of spatial features across the multiwavelength spectrum. The recent extension measurement of the spatial morphology of a microquasar, SS433, to TeV gamma rays(1) localizes the acceleration of electrons at shocks in the jet far from the black hole(2). V4641Sagittarii (V4641Sgr) is a similar binary system with a black hole and B-type main-sequence companion star and has an orbit period of 2.8days (refs.(3,4)). It stands out for its super-Eddington accretion(5) and for its radio jet, which is one of the fastest superluminal jets in the Milky Way. Previous observations of V4641Sgr did not report gamma-ray emission(6). Here we report TeV gamma-ray emission from V4641Sgr that reveals particle acceleration at similar distances from the black hole as SS433. Furthermore, the gamma-ray spectrum of V4641Sgr is among the hardest TeV spectra observed from any known gamma-ray source and is detected above 200TeV. Gamma rays are produced by particles, either electrons or protons, of higher energies. Because energetic electrons lose energy more quickly the higher their energy, such a spectrum either very strongly constrains the electron-production mechanism or points to the acceleration of high-energy protons. This suggests that large-scale jets from microquasars could be more common than previously expected and that they could be a notable source of galactic cosmic rays(7-9).