Very high energy particle acceleration powered by the jets of the microquasar SS 433
Creators: name: HAWC Collaboration
name: Abeysekara, A. U.
name: Albert, A.
name: Alfaro, R.
name: Alvarez, C.
name: Álvarez, J. D.
name: Arceo, R.
name: Arteaga-Velázquez, J. C.
name: Rojas, D. Avila
name: Solares, H. A. Ayala
name: Belmont-Moreno, E.
name: BenZvi, S. Y.
name: Brisbois, C.
name: Caballero-Mora, K. S.
name: Capistrán, T.
name: Carramiñana, A.
name: Casanova, S.
name: Castillo, M.
name: Cotti, U.
name: Cotzomi, J.
name: de León, S. Coutiño
name: De León, C.
name: De la Fuente, E.
name: Díaz-Vélez, J. C.
name: Dichiara, S.
name: Dingus, B. L.
name: DuVernois, M. A.
name: Ellsworth, R. W.
name: Engel, K.
name: Espinoza, C.
name: Fang, K.
name: Fleischhack, H.
name: Fraija, N.
name: Galván-Gámez, A.
name: García-González, J. A.
name: Garfias, F.
name: Muñoz, A. González
name: González, M. M.
name: Goodman, J. A.
name: Hampel-Arias, Z.
name: Harding, J. P.
name: Hernandez, S.
name: Hinton, J.
name: Hona, B.
name: Hueyotl-Zahuantitla, F.
name: Hui, C. M.
name: Hüntemeyer, P.
name: Iriarte, A.
name: Jardin-Blicq, A.
name: Joshi, V.
name: Kaufmann, S.
name: Kar, P.
name: Kunde, G. J.
name: Lauer, R. J.
name: Lee, W. H.
name: Vargas, H. León
name: Li, H.
name: Linnemann, J. T.
name: Longinotti, A. L.
name: Luis-Raya, G.
name: López-Coto, R.
name: Malone, K.
name: Marinelli, S. S.
name: Martinez, O.
name: Martinez-Castellanos, I.
name: Martínez-Castro, J.
name: Matthews, J. A.
name: Miranda-Romagnoli, P.
name: Moreno, E.
name: Mostafá, M.
name: Nayerhoda, A.
name: Nellen, L.
name: Newbold, M.
name: Nisa, M. U.
name: Noriega-Papaqui, R.
name: Pérez-Pérez, E. G.
name: Pretz, J.
name: Ren, Z.
name: Rho, C. D.
name: Rivière, C.
name: Rosa-González, D.
name: Rosenberg, M.
name: Ruiz-Velasco, E.
name: Greus, F. Salesa
name: Sandoval, A.
name: Schneider, M.
name: Schoorlemmer, H.
name: Arroyo, M. Seglar
name: Sinnis, G.
name: Smith, A. J.
name: Springer, R. W.
name: Surajbali, P.
name: Taboada, I.
name: Tibolla, O.
name: Tollefson, K.
name: Torres, I.
name: Vianello, G.
name: Villaseñor, L.
name: Weisgarber, T.
name: Werner, F.
name: Westerhoff, S.
name: Wood, J.
name: Yapici, T.
name: Yodh, G.
name: Zepeda, A.
name: Zhang, H.
name: Zhou, H.
Publisher: name: arXiv
Year: 2018
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: 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). Two jets of ionized matter with a bulk velocity of $\sim0.26c$ extend from the binary, perpendicular to the line of sight, and terminate inside W50, a supernova remnant that is being distorted by the jets. SS 433 differs from other microquasars in that the accretion is believed to be super-Eddington, and the luminosity of the system is $\sim10^{40}$ erg s$^{-1}$. The lobes of W50 in which the jets terminate, about 40 pc 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. At higher energies (&gt;100 GeV), the particle fluxes of $γ$ rays from X-ray hotspots around SS 433 have been reported as flux upper limits. 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 interacting with the ambient gas. Here we report TeV $γ$-ray observations of the SS 433/W50 system where the lobes are spatially resolved. The TeV emission is localized to structures in the lobes, far from the center of the system where the jets are formed. We have measured photon energies of at least 25 TeV, and these are certainly not Doppler boosted, because of the viewing geometry. We conclude that the emission from radio to TeV energies is consistent with a single population of electrons with energies extending to at least hundreds of TeV in a magnetic field of $\sim16$~micro-Gauss.
description: Preprint version of Nature paper. Contacts: S. BenZvi, B. Dingus, K. Fang, C.D. Rho , H. Zhang, H. Zhou