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Ultra-High-Energy Gamma-Ray Bubble around Microquasar V4641 Sgr

Fuente: arXiv
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Hauptverfasser: Alfaro, R., Alvarez, C., Arteaga-Velázquez, J. C., Rojas, D. Avila, Solares, H. A. Ayala, Babu, R., Belmont-Moreno, E., Caballero-Mora, K. S., Capistrán, T., Carramiñana, A., Casanova, S., Cotti, U., Cotzomi, J., de León, S. Coutiño, De la Fuente, E., Depaoli, D., Di Lalla, N., Hernandez, R. Diaz, Dingus, B. L., DuVernois, M. A., Durocher, M., Díaz-Vélez, J. C., Engel, K., Espinoza, C., Fan, K. L., Fang, K., Fraija, N., Fraija, S., García-González, J. A., Garfias, F., Muñoz, A. Gonzalez, González, M. M., Goodman, J. A., Groetsch, S., Harding, J. P., Herzog, I., Hinton, J., Huang, D., Hueyotl-Zahuantitla, F., Hüntemeyer, P., Iriarte, A., Joshi, V., Kaufmann, S., Kieda, D., de León, C., Lee, J., Vargas, H. León, Linnemann, J. T., Longinotti, A. L., Luis-Raya, G., Malone, K., Martinez, O., Martínez-Castro, J., Matthews, J. A., Miranda-Romagnoli, P., Morales-Soto, J. A., Moreno, E., Mostafá, M., Nayerhoda, A., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Olivera-Nieto, L., Omodei, N., Osorio, M., Araujo, Y. Pérez, Pérez-Pérez, E. G., Rho, C. D., Rosa-González, 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., Ureña-Mena, F., Varela, E., Villaseñor, L., Wang, X., Watson, I. J., Willox, E., Yun-Cárcamo, S., Zhou, H.
Format: Preprint
Veröffentlicht: 2024
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High Energy Astrophysical Phenomena
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author Alfaro, R.
Alvarez, C.
Arteaga-Velázquez, J. C.
Rojas, D. Avila
Solares, H. A. Ayala
Babu, R.
Belmont-Moreno, E.
Caballero-Mora, K. S.
Capistrán, T.
Carramiñana, A.
Casanova, S.
Cotti, U.
Cotzomi, J.
de León, S. Coutiño
De la Fuente, E.
Depaoli, D.
Di Lalla, N.
Hernandez, R. Diaz
Dingus, B. L.
DuVernois, M. A.
Durocher, M.
Díaz-Vélez, J. C.
Engel, K.
Espinoza, C.
Fan, K. L.
Fang, K.
Fraija, N.
Fraija, S.
García-González, J. A.
Garfias, F.
Muñoz, A. Gonzalez
González, M. M.
Goodman, J. A.
Groetsch, S.
Harding, J. P.
Herzog, I.
Hinton, J.
Huang, D.
Hueyotl-Zahuantitla, F.
Hüntemeyer, P.
Iriarte, A.
Joshi, V.
Kaufmann, S.
Kieda, D.
de León, C.
Lee, J.
Vargas, H. León
Linnemann, J. T.
Longinotti, A. L.
Luis-Raya, G.
Malone, K.
Martinez, O.
Martínez-Castro, J.
Matthews, J. A.
Miranda-Romagnoli, P.
Morales-Soto, J. A.
Moreno, E.
Mostafá, M.
Nayerhoda, A.
Nellen, L.
Newbold, M.
Nisa, M. U.
Noriega-Papaqui, R.
Olivera-Nieto, L.
Omodei, N.
Osorio, M.
Araujo, Y. Pérez
Pérez-Pérez, E. G.
Rho, C. D.
Rosa-González, 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.
Ureña-Mena, F.
Varela, E.
Villaseñor, L.
Wang, X.
Watson, I. J.
Willox, E.
Yun-Cárcamo, S.
Zhou, H.
author_facet Alfaro, R.
Alvarez, C.
Arteaga-Velázquez, J. C.
Rojas, D. Avila
Solares, H. A. Ayala
Babu, R.
Belmont-Moreno, E.
Caballero-Mora, K. S.
Capistrán, T.
Carramiñana, A.
Casanova, S.
Cotti, U.
Cotzomi, J.
de León, S. Coutiño
De la Fuente, E.
Depaoli, D.
Di Lalla, N.
Hernandez, R. Diaz
Dingus, B. L.
DuVernois, M. A.
Durocher, M.
Díaz-Vélez, J. C.
Engel, K.
Espinoza, C.
Fan, K. L.
Fang, K.
Fraija, N.
Fraija, S.
García-González, J. A.
Garfias, F.
Muñoz, A. Gonzalez
González, M. M.
Goodman, J. A.
Groetsch, S.
Harding, J. P.
Herzog, I.
Hinton, J.
Huang, D.
Hueyotl-Zahuantitla, F.
Hüntemeyer, P.
Iriarte, A.
Joshi, V.
Kaufmann, S.
Kieda, D.
de León, C.
Lee, J.
Vargas, H. León
Linnemann, J. T.
Longinotti, A. L.
Luis-Raya, G.
Malone, K.
Martinez, O.
Martínez-Castro, J.
Matthews, J. A.
Miranda-Romagnoli, P.
Morales-Soto, J. A.
Moreno, E.
Mostafá, M.
Nayerhoda, A.
Nellen, L.
Newbold, M.
Nisa, M. U.
Noriega-Papaqui, R.
Olivera-Nieto, L.
Omodei, N.
Osorio, M.
Araujo, Y. Pérez
Pérez-Pérez, E. G.
Rho, C. D.
Rosa-González, 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.
Ureña-Mena, F.
Varela, E.
Villaseñor, L.
Wang, X.
Watson, I. J.
Willox, E.
Yun-Cárcamo, S.
Zhou, H.
contents 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 of the spatial morphology of a microquasar, SS 433, to TeV gamma rays \cite{abeysekara2018very} localizes the acceleration of electrons at shocks in the jet far from the black hole \cite{hess2024ss433}. Here we report TeV gamma-ray emission from another microquasar, V4641~Sgr, which reveals particle acceleration at similar distances from the black hole as SS~433. Additionally, the gamma-ray spectrum of V4641 is among the hardest TeV spectra observed from any known gamma-ray source and is detected up to 200 TeV. Gamma rays are produced by particles, either electrons or hadrons, of higher energies. Because 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 hadrons. This observation suggests that large-scale jets from microquasars could be more common than previously expected and that microquasars could be a significant source of Galactic cosmic rays. high energy gamma-rays also provide unique constraints on the acceleration mechanisms of extra-Galactic cosmic rays postulated to be produced by the supermassive black holes and relativistic jets of quasars. The distance to quasars limits imaging studies due to insufficient angular resolution of gamma-rays and due to attenuation of the highest energy gamma-rays by the extragalactic background light.
format Preprint
id arxiv_https___arxiv_org_abs_2410_16117
institution arXiv
publishDate 2024
record_format arxiv
spellingShingle Ultra-High-Energy Gamma-Ray Bubble around Microquasar V4641 Sgr
Alfaro, R.
Alvarez, C.
Arteaga-Velázquez, J. C.
Rojas, D. Avila
Solares, H. A. Ayala
Babu, R.
Belmont-Moreno, E.
Caballero-Mora, K. S.
Capistrán, T.
Carramiñana, A.
Casanova, S.
Cotti, U.
Cotzomi, J.
de León, S. Coutiño
De la Fuente, E.
Depaoli, D.
Di Lalla, N.
Hernandez, R. Diaz
Dingus, B. L.
DuVernois, M. A.
Durocher, M.
Díaz-Vélez, J. C.
Engel, K.
Espinoza, C.
Fan, K. L.
Fang, K.
Fraija, N.
Fraija, S.
García-González, J. A.
Garfias, F.
Muñoz, A. Gonzalez
González, M. M.
Goodman, J. A.
Groetsch, S.
Harding, J. P.
Herzog, I.
Hinton, J.
Huang, D.
Hueyotl-Zahuantitla, F.
Hüntemeyer, P.
Iriarte, A.
Joshi, V.
Kaufmann, S.
Kieda, D.
de León, C.
Lee, J.
Vargas, H. León
Linnemann, J. T.
Longinotti, A. L.
Luis-Raya, G.
Malone, K.
Martinez, O.
Martínez-Castro, J.
Matthews, J. A.
Miranda-Romagnoli, P.
Morales-Soto, J. A.
Moreno, E.
Mostafá, M.
Nayerhoda, A.
Nellen, L.
Newbold, M.
Nisa, M. U.
Noriega-Papaqui, R.
Olivera-Nieto, L.
Omodei, N.
Osorio, M.
Araujo, Y. Pérez
Pérez-Pérez, E. G.
Rho, C. D.
Rosa-González, 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.
Ureña-Mena, F.
Varela, E.
Villaseñor, L.
Wang, X.
Watson, I. J.
Willox, E.
Yun-Cárcamo, S.
Zhou, H.
High Energy Astrophysical Phenomena
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 of the spatial morphology of a microquasar, SS 433, to TeV gamma rays \cite{abeysekara2018very} localizes the acceleration of electrons at shocks in the jet far from the black hole \cite{hess2024ss433}. Here we report TeV gamma-ray emission from another microquasar, V4641~Sgr, which reveals particle acceleration at similar distances from the black hole as SS~433. Additionally, the gamma-ray spectrum of V4641 is among the hardest TeV spectra observed from any known gamma-ray source and is detected up to 200 TeV. Gamma rays are produced by particles, either electrons or hadrons, of higher energies. Because 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 hadrons. This observation suggests that large-scale jets from microquasars could be more common than previously expected and that microquasars could be a significant source of Galactic cosmic rays. high energy gamma-rays also provide unique constraints on the acceleration mechanisms of extra-Galactic cosmic rays postulated to be produced by the supermassive black holes and relativistic jets of quasars. The distance to quasars limits imaging studies due to insufficient angular resolution of gamma-rays and due to attenuation of the highest energy gamma-rays by the extragalactic background light.
title Ultra-High-Energy Gamma-Ray Bubble around Microquasar V4641 Sgr
topic High Energy Astrophysical Phenomena
url https://arxiv.org/abs/2410.16117

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