Very-high-energy particle acceleration powered by the jets of the microquasar SS 433

A. U. Abeysekara; A. Albert; R. Alfaro; C. Alvarez; J. D. Álvarez; R. Arceo; J. C. Arteaga-Velázquez; D. Avila Rojas; H. A. Ayala Solares; E. Belmont-Moreno; S. Y. BenZvi; C. Brisbois; K. S. Caballero-Mora; T. Capistrán; A. Carramiñana; S. Casanova; M. Castillo; U. Cotti; J. Cotzomi; S. Coutiño de León; C. De León; E. De la Fuente; J. C. Díaz-Vélez; S. Dichiara; B. L. Dingus; M. A. DuVernois; R. W. Ellsworth; K. Engel; C. Espinoza; K. Fang; H. Fleischhack; N. Fraija; A. Galván-Gámez; J. A. García-González; F. Garfias; A. González-Muñoz; M. M. González; J. A. Goodman; Z. Hampel-Arias; J. P. Harding; S. Hernandez; J. Hinton; B. Hona; F. Hueyotl-Zahuantitla; C. M. Hui; P. Hüntemeyer; A. Iriarte; A. Jardin-Blicq; V. Joshi; S. Kaufmann; P. Kar; G. J. Kunde; R. J. Lauer; W. H. Lee; H. León Vargas; H. Li; J. T. Linnemann; A. L. Longinotti; G. Luis-Raya; R. López-Coto; K. Malone; S. S. Marinelli; O. Martinez; I. Martinez-Castellanos; J. Martínez-Castro; J. A. Matthews; P. Miranda-Romagnoli; E. Moreno; M. Mostafá; A. Nayerhoda; L. Nellen; M. Newbold; M. U. Nisa; R. Noriega-Papaqui; J. Pretz; E. G. Pérez-Pérez; Z. Ren; C. D. Rho; C. Rivière; D. Rosa-González; M. Rosenberg; E. Ruiz-Velasco; F. Salesa Greus; A. Sandoval; M. Schneider; H. Schoorlemmer; M. Seglar Arroyo; G. Sinnis; A. J. Smith; R. W. Springer; P. Surajbali; I. Taboada; O. Tibolla; K. Tollefson; I. Torres; G. Vianello; L. Villaseñor; T. Weisgarber; F. Werner; S. Westerhoff; J. Wood; T. Yapici; G. Yodh; A. Zepeda; H. Zhang; H. Zhou

doi:10.1038/s41586-018-0565-5

Very-high-energy particle acceleration powered by the jets of the microquasar SS 433

A. U. Abeysekara, A. Albert, R. Alfaro, C. Alvarez, J. D. Álvarez, R. Arceo, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, E. Belmont-Moreno, S. Y. BenZvi, C. Brisbois, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, M. Castillo, U. Cotti, J. Cotzomi, S. Coutiño de LeónC. De León, E. De la Fuente, J. C. Díaz-Vélez, S. Dichiara, B. L. Dingus, M. A. DuVernois, R. W. Ellsworth, K. Engel, C. Espinoza, K. Fang, H. Fleischhack, N. Fraija, A. Galván-Gámez, J. A. García-González, F. Garfias, A. González-Muñoz, M. M. González, J. A. Goodman, Z. Hampel-Arias, J. P. Harding, S. Hernandez, J. Hinton, B. Hona, F. Hueyotl-Zahuantitla, C. M. Hui, P. Hüntemeyer, A. Iriarte, A. Jardin-Blicq, V. Joshi, S. Kaufmann, P. Kar, G. J. Kunde, R. J. Lauer, W. H. Lee, H. León Vargas, H. Li, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, R. López-Coto, K. Malone, S. S. Marinelli, O. Martinez, I. Martinez-Castellanos, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, J. Pretz, E. G. Pérez-Pérez, Z. Ren, C. D. Rho, C. Rivière, D. Rosa-González, M. Rosenberg, E. Ruiz-Velasco, F. Salesa Greus, A. Sandoval, M. Schneider, H. Schoorlemmer, M. Seglar Arroyo, G. Sinnis, A. J. Smith, R. W. Springer, P. Surajbali, I. Taboada, O. Tibolla, K. Tollefson, I. Torres, G. Vianello, L. Villaseñor, T. Weisgarber, F. Werner, S. Westerhoff, J. Wood, T. Yapici, G. Yodh, A. Zepeda, H. Zhang, H. Zhou

Centro de Investigación en Computación (CIC)

Producción científica: Contribución a una revista › Artículo › revisión exhaustiva

86 Citas (Scopus)

Resumen

SS 433 is a binary system containing a supergiant star that is overflowing its Roche lobe with matter accreting onto a compact object (either a black hole or neutron star)^1–3. Two jets of ionized matter with a bulk velocity of approximately 0.26c (where c is the speed of light in vacuum) extend from the binary, perpendicular to the line of sight, and terminate inside W50, a supernova remnant that is being distorted by the jets^2,4–8. SS 433 differs from other microquasars (small-scale versions of quasars that are present within our own Galaxy) in that the accretion is believed to be super-Eddington^9–11, and the luminosity of the system is about 10⁴⁰ ergs per second^2,9,12,13. The lobes of W50 in which the jets terminate, about 40 parsecs from the central source, are expected to accelerate charged particles, and indeed radio and X-ray emission consistent with electron synchrotron emission in a magnetic field have been observed^14–16. At higher energies (greater than 100 gigaelectronvolts), the particle fluxes of γ-rays from X-ray hotspots around SS 433 have been reported as flux upper limits^6,17–20. In this energy regime, it has been unclear whether the emission is dominated by electrons that are interacting with photons from the cosmic microwave background through inverse-Compton scattering or by protons that are interacting with the ambient gas. Here we report teraelectronvolt γ-ray observations of the SS 433/W50 system that spatially resolve the lobes. The teraelectronvolt emission is localized to structures in the lobes, far from the centre of the system where the jets are formed. We have measured photon energies of at least 25 teraelectronvolts, and these are certainly not Doppler-boosted, because of the viewing geometry. We conclude that the emission—from radio to teraelectronvolt energies—is consistent with a single population of electrons with energies extending to at least hundreds of teraelectronvolts in a magnetic field of about 16 microgauss.

Idioma original	Inglés
Páginas (desde-hasta)	82-85
Número de páginas	4
Publicación	Nature
Volumen	562
N.º	7725
DOI	https://doi.org/10.1038/s41586-018-0565-5
Estado	Publicada - 4 oct. 2018

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Abeysekara, A. U., Albert, A., Alfaro, R., Alvarez, C., Álvarez, J. D., Arceo, R., Arteaga-Velázquez, J. C., Avila Rojas, D., Ayala Solares, H. A., Belmont-Moreno, E., BenZvi, S. Y., Brisbois, C., Caballero-Mora, K. S., Capistrán, T., Carramiñana, A., Casanova, S., Castillo, M., Cotti, U., Cotzomi, J., ... Zhou, H. (2018). Very-high-energy particle acceleration powered by the jets of the microquasar SS 433. Nature, 562(7725), 82-85. https://doi.org/10.1038/s41586-018-0565-5

@article{2d93fbcf87e349d08450f9659effa5e8,

title = "Very-high-energy particle acceleration powered by the jets of the microquasar SS 433",

abstract = "SS 433 is a binary system containing a supergiant star that is overflowing its Roche lobe with matter accreting onto a compact object (either a black hole or neutron star)1–3. Two jets of ionized matter with a bulk velocity of approximately 0.26c (where c is the speed of light in vacuum) extend from the binary, perpendicular to the line of sight, and terminate inside W50, a supernova remnant that is being distorted by the jets2,4–8. SS 433 differs from other microquasars (small-scale versions of quasars that are present within our own Galaxy) in that the accretion is believed to be super-Eddington9–11, and the luminosity of the system is about 1040 ergs per second2,9,12,13. The lobes of W50 in which the jets terminate, about 40 parsecs from the central source, are expected to accelerate charged particles, and indeed radio and X-ray emission consistent with electron synchrotron emission in a magnetic field have been observed14–16. At higher energies (greater than 100 gigaelectronvolts), the particle fluxes of γ-rays from X-ray hotspots around SS 433 have been reported as flux upper limits6,17–20. In this energy regime, it has been unclear whether the emission is dominated by electrons that are interacting with photons from the cosmic microwave background through inverse-Compton scattering or by protons that are interacting with the ambient gas. Here we report teraelectronvolt γ-ray observations of the SS 433/W50 system that spatially resolve the lobes. The teraelectronvolt emission is localized to structures in the lobes, far from the centre of the system where the jets are formed. We have measured photon energies of at least 25 teraelectronvolts, and these are certainly not Doppler-boosted, because of the viewing geometry. We conclude that the emission—from radio to teraelectronvolt energies—is consistent with a single population of electrons with energies extending to at least hundreds of teraelectronvolts in a magnetic field of about 16 microgauss.",

author = "Abeysekara, {A. U.} and A. Albert and R. Alfaro and C. Alvarez and {\'A}lvarez, {J. D.} and R. Arceo and Arteaga-Vel{\'a}zquez, {J. C.} and {Avila Rojas}, D. and {Ayala Solares}, {H. A.} and E. Belmont-Moreno and BenZvi, {S. Y.} and C. Brisbois and Caballero-Mora, {K. S.} and T. Capistr{\'a}n and A. Carrami{\~n}ana and S. Casanova and M. Castillo and U. Cotti and J. Cotzomi and {Couti{\~n}o de Le{\'o}n}, S. and {De Le{\'o}n}, C. and {De la Fuente}, E. and D{\'i}az-V{\'e}lez, {J. C.} and S. Dichiara and Dingus, {B. L.} and DuVernois, {M. A.} and Ellsworth, {R. W.} and K. Engel and C. Espinoza and K. Fang and H. Fleischhack and N. Fraija and A. Galv{\'a}n-G{\'a}mez and Garc{\'i}a-Gonz{\'a}lez, {J. A.} and F. Garfias and A. Gonz{\'a}lez-Mu{\~n}oz and Gonz{\'a}lez, {M. M.} and Goodman, {J. A.} and Z. Hampel-Arias and Harding, {J. P.} and S. Hernandez and J. Hinton and B. Hona and F. Hueyotl-Zahuantitla and Hui, {C. M.} and P. H{\"u}ntemeyer and A. Iriarte and A. Jardin-Blicq and V. Joshi and S. Kaufmann and P. Kar and Kunde, {G. J.} and Lauer, {R. J.} and Lee, {W. H.} and {Le{\'o}n Vargas}, H. and H. Li and Linnemann, {J. T.} and Longinotti, {A. L.} and G. Luis-Raya and R. L{\'o}pez-Coto and K. Malone and Marinelli, {S. S.} and O. Martinez and I. Martinez-Castellanos and J. Mart{\'i}nez-Castro and Matthews, {J. A.} and P. Miranda-Romagnoli and E. Moreno and M. Mostaf{\'a} and A. Nayerhoda and L. Nellen and M. Newbold and Nisa, {M. U.} and R. Noriega-Papaqui and J. Pretz and P{\'e}rez-P{\'e}rez, {E. G.} and Z. Ren and Rho, {C. D.} and C. Rivi{\`e}re and D. Rosa-Gonz{\'a}lez and M. Rosenberg and E. Ruiz-Velasco and {Salesa Greus}, F. and A. Sandoval and M. Schneider and H. Schoorlemmer and {Seglar Arroyo}, M. and G. Sinnis and Smith, {A. J.} and Springer, {R. W.} and P. Surajbali and I. Taboada and O. Tibolla and K. Tollefson and I. Torres and G. Vianello and L. Villase{\~n}or and T. Weisgarber and F. Werner and S. Westerhoff and J. Wood and T. Yapici and G. Yodh and A. Zepeda and H. Zhang and H. Zhou",

note = "Publisher Copyright: {\textcopyright} 2018, Springer Nature Limited.",

year = "2018",

month = oct,

day = "4",

doi = "10.1038/s41586-018-0565-5",

language = "Ingl{\'e}s",

volume = "562",

pages = "82--85",

journal = "Nature",

issn = "0028-0836",

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Abeysekara, AU, Albert, A, Alfaro, R, Alvarez, C, Álvarez, JD, Arceo, R, Arteaga-Velázquez, JC, Avila Rojas, D, Ayala Solares, HA, Belmont-Moreno, E, BenZvi, SY, Brisbois, C, Caballero-Mora, KS, Capistrán, T, Carramiñana, A, Casanova, S, Castillo, M, Cotti, U, Cotzomi, J, Coutiño de León, S, De León, C, De la Fuente, E, Díaz-Vélez, JC, Dichiara, S, Dingus, BL, DuVernois, MA, Ellsworth, RW, Engel, K, Espinoza, C, Fang, K, Fleischhack, H, Fraija, N, Galván-Gámez, A, García-González, JA, Garfias, F, González-Muñoz, A, González, MM, Goodman, JA, Hampel-Arias, Z, Harding, JP, Hernandez, S, Hinton, J, Hona, B, Hueyotl-Zahuantitla, F, Hui, CM, Hüntemeyer, P, Iriarte, A, Jardin-Blicq, A, Joshi, V, Kaufmann, S, Kar, P, Kunde, GJ, Lauer, RJ, Lee, WH, León Vargas, H, Li, H, Linnemann, JT, Longinotti, AL, Luis-Raya, G, López-Coto, R, Malone, K, Marinelli, SS, Martinez, O, Martinez-Castellanos, I, Martínez-Castro, J, Matthews, JA, Miranda-Romagnoli, P, Moreno, E, Mostafá, M, Nayerhoda, A, Nellen, L, Newbold, M, Nisa, MU, Noriega-Papaqui, R, Pretz, J, Pérez-Pérez, EG, Ren, Z, Rho, CD, Rivière, C, Rosa-González, D, Rosenberg, M, Ruiz-Velasco, E, Salesa Greus, F, Sandoval, A, Schneider, M, Schoorlemmer, H, Seglar Arroyo, M, Sinnis, G, Smith, AJ, Springer, RW, Surajbali, P, Taboada, I, Tibolla, O, Tollefson, K, Torres, I, Vianello, G, Villaseñor, L, Weisgarber, T, Werner, F, Westerhoff, S, Wood, J, Yapici, T, Yodh, G, Zepeda, A, Zhang, H & Zhou, H 2018, 'Very-high-energy particle acceleration powered by the jets of the microquasar SS 433', Nature, vol. 562, n.º 7725, pp. 82-85. https://doi.org/10.1038/s41586-018-0565-5

TY - JOUR

T1 - Very-high-energy particle acceleration powered by the jets of the microquasar SS 433

AU - Abeysekara, A. U.

AU - Albert, A.

AU - Alfaro, R.

AU - Alvarez, C.

AU - Álvarez, J. D.

AU - Arceo, R.

AU - Arteaga-Velázquez, J. C.

AU - Avila Rojas, D.

AU - Ayala Solares, H. A.

AU - Belmont-Moreno, E.

AU - BenZvi, S. Y.

AU - Brisbois, C.

AU - Caballero-Mora, K. S.

AU - Capistrán, T.

AU - Carramiñana, A.

AU - Casanova, S.

AU - Castillo, M.

AU - Cotti, U.

AU - Cotzomi, J.

AU - Coutiño de León, S.

AU - De León, C.

AU - De la Fuente, E.

AU - Díaz-Vélez, J. C.

AU - Dichiara, S.

AU - Dingus, B. L.

AU - DuVernois, M. A.

AU - Ellsworth, R. W.

AU - Engel, K.

AU - Espinoza, C.

AU - Fang, K.

AU - Fleischhack, H.

AU - Fraija, N.

AU - Galván-Gámez, A.

AU - García-González, J. A.

AU - Garfias, F.

AU - González-Muñoz, A.

AU - González, M. M.

AU - Goodman, J. A.

AU - Hampel-Arias, Z.

AU - Harding, J. P.

AU - Hernandez, S.

AU - Hinton, J.

AU - Hona, B.

AU - Hueyotl-Zahuantitla, F.

AU - Hui, C. M.

AU - Hüntemeyer, P.

AU - Iriarte, A.

AU - Jardin-Blicq, A.

AU - Joshi, V.

AU - Kaufmann, S.

AU - Kar, P.

AU - Kunde, G. J.

AU - Lauer, R. J.

AU - Lee, W. H.

AU - León Vargas, H.

AU - Li, H.

AU - Linnemann, J. T.

AU - Longinotti, A. L.

AU - Luis-Raya, G.

AU - López-Coto, R.

AU - Malone, K.

AU - Marinelli, S. S.

AU - Martinez, O.

AU - Martinez-Castellanos, I.

AU - Martínez-Castro, J.

AU - Matthews, J. A.

AU - Miranda-Romagnoli, P.

AU - Moreno, E.

AU - Mostafá, M.

AU - Nayerhoda, A.

AU - Nellen, L.

AU - Newbold, M.

AU - Nisa, M. U.

AU - Noriega-Papaqui, R.

AU - Pretz, J.

AU - Pérez-Pérez, E. G.

AU - Ren, Z.

AU - Rho, C. D.

AU - Rivière, C.

AU - Rosa-González, D.

AU - Rosenberg, M.

AU - Ruiz-Velasco, E.

AU - Salesa Greus, F.

AU - Sandoval, A.

AU - Schneider, M.

AU - Schoorlemmer, H.

AU - Seglar Arroyo, M.

AU - Sinnis, G.

AU - Smith, A. J.

AU - Springer, R. W.

AU - Surajbali, P.

AU - Taboada, I.

AU - Tibolla, O.

AU - Tollefson, K.

AU - Torres, I.

AU - Vianello, G.

AU - Villaseñor, L.

AU - Weisgarber, T.

AU - Werner, F.

AU - Westerhoff, S.

AU - Wood, J.

AU - Yapici, T.

AU - Yodh, G.

AU - Zepeda, A.

AU - Zhang, H.

AU - Zhou, H.

PY - 2018/10/4

Y1 - 2018/10/4

N2 - SS 433 is a binary system containing a supergiant star that is overflowing its Roche lobe with matter accreting onto a compact object (either a black hole or neutron star)1–3. Two jets of ionized matter with a bulk velocity of approximately 0.26c (where c is the speed of light in vacuum) extend from the binary, perpendicular to the line of sight, and terminate inside W50, a supernova remnant that is being distorted by the jets2,4–8. SS 433 differs from other microquasars (small-scale versions of quasars that are present within our own Galaxy) in that the accretion is believed to be super-Eddington9–11, and the luminosity of the system is about 1040 ergs per second2,9,12,13. The lobes of W50 in which the jets terminate, about 40 parsecs from the central source, are expected to accelerate charged particles, and indeed radio and X-ray emission consistent with electron synchrotron emission in a magnetic field have been observed14–16. At higher energies (greater than 100 gigaelectronvolts), the particle fluxes of γ-rays from X-ray hotspots around SS 433 have been reported as flux upper limits6,17–20. In this energy regime, it has been unclear whether the emission is dominated by electrons that are interacting with photons from the cosmic microwave background through inverse-Compton scattering or by protons that are interacting with the ambient gas. Here we report teraelectronvolt γ-ray observations of the SS 433/W50 system that spatially resolve the lobes. The teraelectronvolt emission is localized to structures in the lobes, far from the centre of the system where the jets are formed. We have measured photon energies of at least 25 teraelectronvolts, and these are certainly not Doppler-boosted, because of the viewing geometry. We conclude that the emission—from radio to teraelectronvolt energies—is consistent with a single population of electrons with energies extending to at least hundreds of teraelectronvolts in a magnetic field of about 16 microgauss.

AB - SS 433 is a binary system containing a supergiant star that is overflowing its Roche lobe with matter accreting onto a compact object (either a black hole or neutron star)1–3. Two jets of ionized matter with a bulk velocity of approximately 0.26c (where c is the speed of light in vacuum) extend from the binary, perpendicular to the line of sight, and terminate inside W50, a supernova remnant that is being distorted by the jets2,4–8. SS 433 differs from other microquasars (small-scale versions of quasars that are present within our own Galaxy) in that the accretion is believed to be super-Eddington9–11, and the luminosity of the system is about 1040 ergs per second2,9,12,13. The lobes of W50 in which the jets terminate, about 40 parsecs from the central source, are expected to accelerate charged particles, and indeed radio and X-ray emission consistent with electron synchrotron emission in a magnetic field have been observed14–16. At higher energies (greater than 100 gigaelectronvolts), the particle fluxes of γ-rays from X-ray hotspots around SS 433 have been reported as flux upper limits6,17–20. In this energy regime, it has been unclear whether the emission is dominated by electrons that are interacting with photons from the cosmic microwave background through inverse-Compton scattering or by protons that are interacting with the ambient gas. Here we report teraelectronvolt γ-ray observations of the SS 433/W50 system that spatially resolve the lobes. The teraelectronvolt emission is localized to structures in the lobes, far from the centre of the system where the jets are formed. We have measured photon energies of at least 25 teraelectronvolts, and these are certainly not Doppler-boosted, because of the viewing geometry. We conclude that the emission—from radio to teraelectronvolt energies—is consistent with a single population of electrons with energies extending to at least hundreds of teraelectronvolts in a magnetic field of about 16 microgauss.

UR - http://www.scopus.com/inward/record.url?scp=85054326784&partnerID=8YFLogxK

U2 - 10.1038/s41586-018-0565-5

DO - 10.1038/s41586-018-0565-5

M3 - Artículo

C2 - 30283106

SN - 0028-0836

VL - 562

SP - 82

EP - 85

JO - Nature

JF - Nature

IS - 7725

ER -

Very-high-energy particle acceleration powered by the jets of the microquasar SS 433

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