MAGIC observations of the diffuse $γ$-ray emission in the vicinity of the Galactic Centre
MAGIC Collaboration, V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, D. Baack, A. Babić, B. Banerjee, U. Barres de Almeida, J. A. Barrio, J. Becerr… 展开作者
MAGIC Collaboration, V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, D. Baack, A. Babić, B. Banerjee, U. Barres de Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, L. Bellizzi, E. Bernardini, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, Ž. Bošnjak, G. Busetto, R. Carosi, G. Ceribella, Y. Chai, A. Chilingaryan, S. Cikota, S. M. Colak, U. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, V. D'Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, D. Depaoli, F. Di Pierro, L. Di Venere, E. Do Souto Espiñeira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, A. Fernández-Barral, G. Ferrara, D. Fidalgo, L. Foffano, M. V. Fonseca, L. Font, C. Fruck, S. Fukami, R. J. García López, M. Garczarczyk, S. Gasparyan, M. Gaug, N. Giglietto, F. Giordano, N. Godinović, D. Green, D. Guberman, D. Hadasch, A. Hahn, J. Herrera, J. Hoang, D. Hrupec, M. Hütten, T. Inada, S. Inoue, K. Ishio, Y. Iwamura, L. Jouvin, D. Kerszberg, H. Kubo, J. Kushida, A. Lamastra, D. Lelas, F. Leone, E. Lindfors, S. Lombardi, F. Longo, M. López, R. López-Coto, A. López-Oramas, S. Loporchio, B. Machado de Oliveira Fraga, C. Maggio, P. Majumdar, M. Makariev, M. Mallamaci, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, S. Masuda, D. Mazin, S. Mićanović, D. Miceli, M. Minev, J. M. Miranda, R. Mirzoyan, E. Molina, A. Moralejo, D. Morcuende, V. Moreno, E. Moretti, P. Munar-Adrover, V. Neustroev, C. Nigro, K. Nilsson, D. Ninci, K. Nishijima, K. Noda, L. Nogués, M. Nöthe, S. Nozaki, S. Paiano, J. Palacio, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, P. Peñil, M. Peresano, M. Persic, P. G. Prada Moroni, E. Prandini, I. Puljak, W. Rhode, M. Ribó, J. Rico, C. Righi, A. Rugliancich, L. Saha, N. Sahakyan, T. Saito, S. Sakurai, K. Satalecka, K. Schmidt, T. Schweizer, J. Sitarek, I. Šnidarić, D. Sobczynska, A. Somero, A. Stamerra, D. Strom, M. Strzys, Y. Suda, T. Surić, M. Takahashi, F. Tavecchio, P. Temnikov, T. Terzić, M. Teshima, N. Torres-Albà, L. Tosti, S. Tsujimoto, V. Vagelli, J. van Scherpenberg, G. Vanzo, M. Vazquez Acosta, C. F. Vigorito, V. Vitale, I. Vovk, M. Will, D. Zarić
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10 pages, 10 figures. Accepted for publication by A&A. Corresponding authors: Christian Fruck (fruck@mpp.mpg.de), Ievgen Vovk (vovk@icrr.u-tokyo.ac.jp), Yuki Iwamura (iwamura@icrr.u-tokyo.ac.jp) and Marcel Strzys (strzys@icrr.u-tokyo.ac.jp)
Aims: $γ$ rays can be used as a tracer in the search of sources of Galactic cosmic rays (CRs). We present deep observations of the Galactic Centre (GC) region with the MAGIC telescopes, which we use for inferring the underlying CR distribution. Methods: We observed the GC region for ${\approx}100$ hours with the MAGIC telescopes from 2012 to 2017, at high zenith angles (58-70~deg). This implies a larger energy threshold, but also an increased effective collection area compared to low zenith observations. Using new software, we derive instrument response and background models, enabling us to study the diffuse emission in the region. We use pre-existing data of the gas distribution in the GC region to derive the underlying distribution of CRs. Results: We obtain a significant detection for all four model components used to fit our data (Sgr~A*, ``Arc'', G0.9+0.1, and an extended component for the Galactic Ridge). We find that the diffuse component is best described as a power-law with index 2 and an exponential cut-off at around 20~TeV with the significance of the cut-off being only 2~$σ$. The derived cosmic-ray profile hints to a peak at the GC position, with a measured profile index of $1.2 \pm 0.3$, supporting the hypothesis of a CR accelerator at the GC. We argue that the measurements of this profile are presently limited by our knowledge of the gas distribution in the GC vicinity.
Modelling the thermal X-ray emission around the Galactic centre from colliding Wolf-Rayet winds
我们计算的热X射线发射的流体动力学模拟的30个沃尔夫-拉叶（WR）星轨道内的Sgr A $^*$秒差距，解释钱德拉X射线观测的目的是在这个地区。该模型很好地再现了观测的光谱形状，表明冲击WR风是这种热辐射的主要来源。模型X射线通量与Sgr A $^*$流出的强度相关，该流出将Sgr A $^*$附近的热气清除。适度的外流最符合目前的观测结果，尽管这个超大质量黑洞（SMBH）的外流在$\sim$ 100年前就结束了。
Probing the sensitivity of CTAO-N LSTs observations at large zenith angles to the multi-TeV gamma-ray emission from the inner 10 parsecs of the Galactic Center
Probing fundamental physics with ALMA2040 mm-wavelength observations of neutron stars
Shanghai Astronomical Observatory, CAS（中国科学院上海天文台）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Universit‘a di Napoli “Federico II”（那不勒斯费德里科二世大学）；State University of New York at Oswego（纽约州立大学奥斯威戈分校）；National Astronomical Research Institute of Thailand (Public Organization)（泰国国家天文研究所）；University of Michigan（密歇根大学）；Peking University（北京大学）；Institut de Radioastronomie Millimétrique (IRAM)（毫米波射电天文研究所）；Julius-Maximilians-Universität Würzburg（维尔茨堡朱利叶斯-马克西米利安大学）
