Probing extreme environments with the Cherenkov Telescope Array
C. Boisson, A. M. Brown, A. Burtovoi, M. Cerruti, M. Chernyakova, T. Hassan, J. -P. Lenain, M. Manganaro, P. Romano, H. Sol, F. Tavecchio, S. Vercellone, L. Zam… 展开作者
C. Boisson, A. M. Brown, A. Burtovoi, M. Cerruti, M. Chernyakova, T. Hassan, J. -P. Lenain, M. Manganaro, P. Romano, H. Sol, F. Tavecchio, S. Vercellone, L. Zampieri, R. Zanin, A. Zech, I. Agudo, R. Alves Batista, E. O. Anguner, L. A. Antonelli, M. Backes, C. Balazs, J. Becerra González, C. Bigongiari, E. Bissaldi, J. Bolmont, P. Bordas, Ž. Bošnjak, M. Böttcher, M. Burton, F. Cangemi, P. Caraveo, M. Cardillo, S. Caroff, A. Carosi, S. Casanova, S. Chaty, J. L. Contreras, J. G. Coelho, G. Cotter, A. D'Aì, F. D'Ammando, E. M. de Gouveia Dal Pino, D. de Martino, C. Delgado, D. della Volpe, A. Djannati-Ataï, R. C. Dos Anjos, E. de Oña Wilhelmi, V. Dwarkadas, G. Emery, E. Fedorova, S. Fegan, M. D. Filipovic, G. Galanti, D. Gasparrini, G. Ghirlanda, P. Goldoni, J. Granot, J. G. Green, M. Heller, B. Hnatyk, R. Hnatyk, D. Horan, T. Hovatta, S. Inoue, M. Jamrozy, B. Khélifi, N. Komin, K. Kohri, A. Lamastra, N. La Palombara, E. Lindfors, I. Liodakis, S. Lombardi, F. Longo, F. Lucarelli, P. L. Luque-Escamilla, J. Marti, M. Martinez, D. Mazin, J. D. Mbarubucyeye, S. Menchiari, L. Mohrmann, T. Montaruli, A. Moralejo Olaizola, D. Morcuende, G. Morlino, A. Morselli, C. G. Mundell, T. Murach, A. Nagai, A. Nayerhoda, J. Niemiec, M. Nikolajuk, B. Olmi, M. Orienti, J. M. Paredes, G. Pareschi, A. Pe'er, G. Pühlhofer, M. Punch, O. Reimer, M. Ribó, F. Rieger, G. Rodriguez, J. Rodriguez, G. Romeo, M. Roncadelli, G. Rowell, B. Rudak, I. Sadeh, F. Salesa Greus, U. Sawangwit, F. Schüssler, O. Sergijenko, R. C. Shellard, F. G. Saturni, A. Stamerra, Th. Stolarczyk, G. Tagliaferri, V. Testa, L. Tibaldo, S. Ventura, A. Viana, J. Vink, V. Vitale, S. Vorobiov, A. Wierzcholska, M. Zacharias, D. Zavrtanik
备注：
Submitted as input to ASTRONET Science Vision and Infrastructure roadmap on behalf of the CTA consortium
The physics of the non-thermal Universe provides information on the acceleration mechanisms in extreme environments, such as black holes and relativistic jets, neutron stars, supernovae or clusters of galaxies. In the presence of magnetic fields, particles can be accelerated towards relativistic energies. As a consequence, radiation along the entire electromagnetic spectrum can be observed, and extreme environments are also the most likely sources of multi-messenger emission. The most energetic part of the electromagnetic spectrum corresponds to the very-high-energy (VHE, E>100 GeV) gamma-ray regime, which can be extensively studied with ground based Imaging Atmospheric Cherenkov Telescopes (IACTs). The results obtained by the current generation of IACTs, such as H.E.S.S., MAGIC, and VERITAS, demonstrate the crucial importance of the VHE band in understanding the non-thermal emission of extreme environments in our Universe. In some objects, the energy output in gamma rays can even outshine the rest of the broadband spectrum. The Cherenkov Telescope Array (CTA) is the next generation of IACTs, which, with cutting edge technology and a strategic configuration of ~100 telescopes distributed in two observing sites, in the northern and southern hemispheres, will reach better sensitivity, angular and energy resolution, and broader energy coverage than currently operational IACTs. With CTA we can probe the most extreme environments and considerably boost our knowledge of the non-thermal Universe.
Impact of Laser Guide Star facilities on neighbouring telescopes: The case of GTC, TMT, VLT and ELT lasers and the Cherenkov Telescope Array
强大的激光导星（LGS）系统是下一代超大型望远镜的标准配置。然而，现代地球天文学已经经历了一个集中在少数具有特殊天空质量的地点的过程，导致这些地点变得越来越拥挤。因此，未来的LGS系统会遇到周围天文设施的环境，其中一些观测具有大视场。我们推导出公式来计算LGS光对邻近望远镜的相机的影响以及激光穿过相机视场发生的概率，并将其应用于下一个非常高能量伽马射线天文台“切伦科夫望远镜阵列”（CTA）的具体情况。它的南部将建在智利Cerro Armazones的山谷中，靠近“甚大望远镜”（VLT）和“欧洲极大望远镜”（ELT），而它的北部将位于La Palma加那利岛的“Observatorio del Roque de los Muchachos”，它也是“加那利群岛大望远镜”（GTC）的所在地，并作为“三十米望远镜”（TMT）的可选站点，两者都采用LGS系统。虽然在CTA望远镜的视场中找到人造恒星不会对观测造成很大的干扰，但穿过CTA望远镜视场的激光束可能是关键。我们发现ELT激光器没有预期的冲突，但是，1%（3%）的银河系外和1%（5%）的银河系观测与CTA可能会受到GTC（TMT）LGS激光器的影响，除非激光跟踪控制系统的增强版本得到实施。
Design and Realization of the LST Main Structure for the Cherenkov Telescope Array
Max Planck Institut für Physik（马克斯·普朗克物理研究所）；Laboratoire d'Annecy de Physique des Particules (LAPP)（阿讷西粒子物理实验室）；Institut de Física d'Altes Energies (IFAE)（高能物理研究所）；Universidad de Jaén（哈恩大学）
Neutrino Telescope Array Letter of Intent: A Large Array of High Resolution Imaging Atmospheric Cherenkov and Fluorescence Detectors for Survey of Air-showers from Cosmic Tau Neutrinos in the PeV-EeV Energy Range
本意向书（LoI）描述了中微子望远镜阵列（NTA）项目的大纲和计划。高能中微子为强子加速提供了独特而无可争辩的证据。最近，冰立方已经报道了超过预期的来自大气秒的天文中微子候选者，但受到水切伦科夫探测方法的限制。下一代高能中微子望远镜应该能够为宇宙高能中微子建立无可争辩的证据。它不仅应该有数量级的更大的灵敏度，而且还应该有足够的指向精度来探测已知或未知的天文物体，而不会受到大气层的影响。拟议的装置是一个大型阵列的成像大气切伦科夫和荧光探测器的复眼站，具有宽视场和精细的观测能力，从PeV-EeV能量范围的宇宙τ中微子的空气簇射。这套先进的光学复杂系统主要是在全天空巡天高分辨率空气簇射探测器（Ashra）的基础上发展起来的，并采用τ簇射掠地方法对PeV-EeV τ中微子进行巡天。在标准GRB中微子注量的条件下，它可以对PeV-EeV τ中微子进行宽（30 ° x 360 °）和深（~400 Mpc）的巡天观测，而且在基本无背景的条件下，它的指向精度优于0.2 °。通过在宽视场中对掠地τ阵雨进行先进成像，我们的目标是明确发现和识别天文τ中微子源，为天体物理强子模型提供不可逃避的证据，以加速和/或在精确确定的方向上传播极高能量的质子。
