Very high energy particle acceleration powered by the jets of the microquasar SS 433
HAWC Collaboration, 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… 展开作者
HAWC Collaboration, 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, E. G. Pérez-Pérez, J. Pretz, 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
备注：
Preprint version of Nature paper. Contacts: S. BenZvi, B. Dingus, K. Fang, C.D. Rho , H. Zhang, H. Zhou
SS 433是一个双星系统，其中包含一颗超巨星，这颗超巨星的洛希瓣溢出，物质吸积到一个紧凑的物体（黑洞或中子星）上。两股整体速度为$\sim0.26c$的电离物质喷流从双星中垂直于视线延伸出来，并终止于W 50内部，这是一个被喷流扭曲的超新星遗迹。SS 433与其他微类星体的不同之处在于，它的吸积被认为是超爱丁顿的，系统的光度是$\sim10^{40}$ erg s $^{-1}$。喷流终止的W50的波瓣，距离中心源约40 pc，预计会加速带电粒子，并且确实观察到与磁场中的电子同步辐射一致的无线电和X射线发射。在更高的能量（>100 GeV），来自SS 433周围X射线热点的$γ$射线的粒子通量被报道为通量上限。在这种能量状态下，还不清楚发射是由通过逆康普顿散射与来自宇宙微波背景的光子相互作用的电子主导，还是由与周围气体相互作用的质子主导。在这里，我们报告TeV $γ$射线观测的SS 433/W 50系统的叶空间分辨。TeV辐射定位于叶瓣中的结构，远离形成喷流的系统中心。我们已经测量到至少25 TeV的光子能量，由于观测几何的原因，这些光子能量肯定不是多普勒增强的。我们的结论是，从无线电到TeV的能量的发射是一致的一个单一的电子人口的能量扩展到至少数百TeV的磁场中的$\sim16$ ~微高斯。
英文摘要：
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 (>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.
ALMA Observations of DEM L241/LMC P3 in the Large Magellanic Cloud: Evidence for the Formation of Cool Molecular Jets Driven by a Microquasar
Nagoya University（名古屋大学）；Gifu University（岐阜大学）；Institute for Advanced Study, Gifu University（岐阜大学高等研究院）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究所）；Institute for Advanced Research, Nagoya University（名古屋大学高等研究院）；Western Sydney University（西悉尼大学）
Microquasar remnants as reservoirs of PeV cosmic rays
Instituto Argentino de Radioastronomía (CCT La Plata, CONICET（阿根廷射电天文研究所）；CICPBA（拉普拉塔国立大学天文学与地球物理学学院）；UNLP)（巴塞罗那大学量子物理与天体物理系、宇宙科学研究所）；Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata；Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB)
Revisiting the XMM-Newton Observations of the Galactic Microquasar SS 433: Implications for the Origin of the Ultrahigh-Energy Emission Detected by LHAASO
School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education（南京大学现代天体学与天体物理教育部重点实验室）；Tianfu Cosmic Ray Research Center（天府宇宙线研究中心）
Investigation of the Microquasar SS 433 with VERITAS
DePauw University（迪保大学）；Temple University（天普大学）；University of Utah（犹他大学）；University College Dublin（都柏林大学学院）；University of California, Los Angeles（加州大学洛杉矶分校）；California Polytechnic State University（加州州立理工大学）；Washington University（华盛顿大学）；Santa Cruz Institute for Particle Physics（圣克鲁兹粒子物理研究所）；University of California, Santa Cruz（加州大学圣克鲁兹分校）
