Resolving acceleration to very high energies along the Jet of Centaurus A
The H. E. S. S. Collaboration, :, H. Abdalla, R. Adam, F. Aharonian, F. Ait Benkhali, E. O. Angüner, M. Arakawa, C. Arcaro, C. Armand, H. Ashkar, M. Backes, V. … 展开作者
The H. E. S. S. Collaboration, :, H. Abdalla, R. Adam, F. Aharonian, F. Ait Benkhali, E. O. Angüner, M. Arakawa, C. Arcaro, C. Armand, H. Ashkar, M. Backes, V. Barbosa Martins, M. Barnard, Y. Becherini, D. Berge, K. Bernlöhr, R. Blackwell, M. Böttcher, C. Boisson, J. Bolmont, S. Bonnefoy, J. Bregeon, M. Breuhaus, F. Brun, P. Brun, M. Bryan, M. Büchele, T. Bulik, T. Bylund, M. Capasso, S. Caroff, A. Carosi, S. Casanova, M. Cerruti, T. Chand, S. Chandra, A. Chen, S. Colafrancesco, M. Curyło, I. D. Davids, C. Deil, J. Devin, P. deWilt, L. Dirson, A. Djannati-Ataï, A. Dmytriiev, A. Donath, V. Doroshenko, L. O'C. Drury, J. Dyks, K. Egberts, G. Emery, J. -P. Ernenwein, S. Eschbach, K. Feijen, S. Fegan, A. Fiasson, G. Fontaine, S. Funk, M. Füßling, S. Gabici, Y. A. Gallant, F. Gaté, G. Giavitto, D. Glawion, J. F. Glicenstein, D. Gottschall, M. -H. Grondin, J. Hahn, M. Haupt, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, C. Hoischen, T. L. Holch, M. Holler, D. Horns, D. Huber, H. Iwasaki, M. Jamrozy, D. Jankowsky, F. Jankowsky, A. Jardin-Blicq, I. Jung-Richardt, M. A. Kastendieck, K. Katarzyński, M. Katsuragawa, U. Katz, D. Khangulyan, B. Khélifi, J. King, S. Klepser, W. Kluźniak, N. Komin, K. Kosack, D. Kostunin, M. Kraus, G. Lamanna, J. Lau, A. Lemière, M. Lemoine-Goumard, J. -P. Lenain, E. Leser, C. Levy, T. Lohse, I. Lypova, J. Mackey, J. Majumdar, D. Malyshev, V. Marandon, A. Marcowith, A. Mares, C. Mariaud, G. Martí-Devesa, R. Marx, G. Maurin, P. J. Meintjes, A. M. W. Mitchell, R. Moderski, M. Mohamed, L. Mohrmann, C. Moore, E. Moulin, J. Muller, T. Murach, S. Nakashima, M. de Naurois, H. Ndiyavala, F. Niederwanger, J. Niemiec, L. Oakes, P. O'Brien, H. Odaka, S. Ohm, E. de Ona Wilhelmi, M. Ostrowski, I. Oya, M. Panter, R. D. Parsons, C. Perennes, P. -O. Petrucci, B. Peyaud, Q. Piel, S. Pita, V. Poireau, A. Priyana Noel, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, S. Raab, R. Rauth, A. Reimer, O. Reimer, Q. Remy, M. Renaud, F. Rieger, L. Rinchiuso, C. Romoli, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, S. Saito, D. A. Sanchez, A. Santangelo, M. Sasaki, R. Schlickeiser, F. Schüssler, A. Schulz, H. M. Schutte, U. Schwanke, S. Schwemmer, M. Seglar-Arroyo, M. Senniappan, A. S. Seyffert, N. Shafi, K. Shiningayamwe, R. Simoni, A. Sinha, H. Sol, A. Specovius, M. Spir-Jacob, Ł. Stawarz, R. Steenkamp, C. Stegmann, C. Steppa, T. Takahashi, T. Tavernier, A. M. Taylor, R. Terrier, D. Tiziani, M. Tluczykont, C. Trichard, M. Tsirou, N. Tsuji, R. Tuffs, Y. Uchiyama, D. J. van der Walt, C. van Eldik, C. van Rensburg, B. van Soelen, G. Vasileiadis, J. Veh, C. Venter, P. Vincent, J. Vink, F. Voisin, H. J. Völk, T. Vuillaume, Z. Wadiasingh, S. J. Wagner, R. White, A. Wierzcholska, R. Yang, H. Yonedak, M. Zacharias, R. Zanin, A. A. Zdziarski, A. Zech, A. Ziegler, J. Zorn, N. Żywucka
The nearby radio galaxy Centaurus A belongs to a class of Active Galaxies that are very luminous at radio wavelengths. The majority of these galaxies show collimated relativistic outflows known as jets, that extend over hundreds of thousands of parsecs for the most powerful sources. Accretion of matter onto the central super-massive black hole is believed to fuel these jets and power their emission, with the radio emission being related to the synchrotron radiation of relativistic electrons in magnetic fields. The origin of the extended X-ray emission seen in the kiloparsec-scale jets from these sources is still a matter of debate, although Cen A's X-ray emission has been suggested to originate in electron synchrotron processes. The other possible explanation is Inverse Compton (IC) scattering with CMB soft photons. Synchrotron radiation needs ultra-relativistic electrons ($\sim50$ TeV), and given their short cooling times, requires some continuous re-acceleration mechanism to be active. IC scattering, on the other hand, does not require very energetic electrons, but requires jets that stay highly relativistic on large scales ($\geq$1 Mpc) and that remain well-aligned with the line of sight. Some recent evidence disfavours inverse Compton-CMB models, although other evidence seems to be compatible with them. In principle, the detection of extended gamma-ray emission, directly probing the presence of ultra-relativistic electrons, could distinguish between these options, but instruments have hitherto been unable to resolve the relevant structures. At GeV energies there is also an unusual spectral hardening in Cen A, whose explanation is unclear. Here we report observations of Cen A at TeV energies that resolve its large-scale jet. We interpret the data as evidence for the acceleration of ultra-relativistic electrons in the jet, and favour the synchrotron explanation for the X-rays.
Mass entrainment and turbulence-driven acceleration of ultra-high energy cosmic rays in Centaurus A
对FR I射电星系半人马座A在射电、X射线和伽马射线波段的观测提供了轻子加速到几TeV的证据，以及强子加速到几十EeV的线索。综合现有的观测约束的物理条件和粒子含量的喷流，内叶和巨大的半人马座A的瓣，我们的目标是评估其作为一个超高能宇宙射线源的可行性。我们应用了几种确定喷流功率的方法，并证实了各种功率估计值~ 1 x 10^43 erg s^-1的一致性。采用标度关系的基础上，以前的结果为3C 31，我们估计粒子数密度的射流，包括通过X射线观测可用的无线电。我们的模型与喷流相容，喷流通过热气体的外部卷吸作用吸收约3 x 10^21 g/s的物质，通过含喷流恒星的内部卷吸作用吸收约7 x 10^22 g/s的物质。这导致辐射粒子和磁场产生的内部波瓣压力与我们推导出的外部压力之间的不平衡。基于对其他FR I源外部环境的了解，我们估计巨瓣中的热压力为1.5 x 10^-12达因·厘米^-2，由此我们推导出温度的下限约为1.6 x 10^8 K。利用动力学和浮力参数，我们推断~ 440-645百万年和~ 560百万年分别为巨型裂片的声音交叉和浮力年龄，与它们的光谱年龄不一致。我们重新调查粒子加速的可行性，通过随机过程中的叶片，把新的约束的能量和湍流输入的叶片。相同的“非常热”的温度，允许夹带计算和丢失的压力之间的自洽性，也允许随机UHECR加速模型的工作。
Probing anisotropic particle acceleration and limb-brightening in Centaurus A's jet
University of Würzburg（维尔茨堡大学）；Goethe Universität Frankfurt（法兰克福歌德大学）；Shanghai Jiao Tong University（上海交通大学）；Radboud University（拉德堡德大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）
Far-infrared synchrotron properties of the inner lobes of the radio galaxy Centaurus A revealed with the Herschel observatory
Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA)（宇宙科学研究所）；Department of Physics and Astronomy, Kwansei Gakuin University（关西学院大学物理与天文学系）；Division of Liberal Arts, Kogakuin University of Technology & Engineering（工机大学人文教育部）；National Astronomical Observatory of Japan（日本国立天文台）；Advanced Research Laboratories, Tokyo City University（东京都市大学先进研究实验室）；Department of Physics, Saitama University（埼玉大学物理学系）
Resolving the temporal evolution of M87 jet with $\lesssim0.1$-arcsec Chandra observations
Université Laval（拉瓦尔大学）；Center for Astrophysics — Harvard & Smithsonian（哈佛-史密森天体物理中心）；ICRAR, University of Western Australia（西澳大利亚大学 ICRAR）；Department of Physics, University of Maryland Baltimore County（马里兰大学巴尔的摩分校物理系）
利用 13 年 Chandra/HRC-I 数据，通过点扩散函数反卷积实现亚角秒级 X 射线分辨，揭示了 M87 喷流中 HST-1 的双成分结构及下游结的复杂形态，并发现 X 射线整体流量下降高达 84%，符合同步辐射冷却模型。
Resolving the Galactic Center Region's Gamma-Ray Emission and Searching for its Neutrino Counterpart with HAWC and IceCube
Instituto de Física, Universidad Nacional Autónoma de México（墨西哥国立自治大学物理研究所）；Universidad de Costa Rica（哥斯达黎加大学）；Universidad Michoacana de San Nicolás de Hidalgo（米却肯圣尼古拉斯德伊达尔戈大学）；Department of Physics and Astronomy, Michigan State University（密歇根州立大学物理与天文学系）；Temple University（天普大学）；Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文研究所）；Universidad Autónoma de Chiapas（恰帕斯自治大学）；Instituto Nacional de Astrofísica, Óptica y Electrónica（国家天体物理学、光学和电子研究所）；Institute of Nuclear Physics Polish Academy of Sciences（波兰科学院核物理研究所）
The High Energy X-ray Probe (HEX-P): resolving the nature of Sgr A* flares, compact object binaries and diffuse X-ray emission in the Galactic Center and beyond
High-energy neutrino signatures of embedded GRB jets in AGN disks: a dynamic jet-propagation framework
Institute of Astrophysics, Central China Normal University（华中师范大学天体物理研究所）；Laboratory for Compact Object Astrophysics and Astronomical Technology, Central China Normal University（华中师范大学致密天体天体物理学与天文技术实验室）
