UK participation in the pre-production phase of CTA extension 2022

英国参与 2022 年 CTA 延期的预制作阶段

• 批准号: ST/X001741/1
• 负责人: Jonathan Lapington
• 金额: $ 19.27万
• 依托单位: University of Leicester
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2022
• 资助国家: 英国
• 起止时间: 2022 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FX001741%2F1
• 关键词: UK; participation; pre; production; phase

The Universe is full of particles with energies so great that they are travelling at very close to the speed of light. They affect the Universe in many ways, influencing the life cycles of stars and the evolution of galaxies. These particles are hard to trace but can reveal their presence by producing gamma rays. Like their lower-energy cousins, X-rays, gamma rays do not penetrate the Earth's atmosphere and usually satellite-based telescopes are used to detect them. However, at very high energies (VHE) there are so few gamma rays that detecting them using spacecraft becomes impossible. Luckily, it is possible to observe them from the ground via the flashes of blue light, Cherenkov radiation, produced when they interact in the atmosphere. The glow from Cherenkov radiation in the atmosphere is 10,000 times fainter than starlight, so large mirrors are required to collect it, and because the flashes last only a few billionths of a second, ultra-fast cameras are needed to record them. We know from current ground-based gamma-ray telescopes such as HESS that there is a wealth of phenomena to be studied. VHE gamma ray telescopes have detected the remains of supernova explosions, binary star systems, highly energetic jets produced by black holes in distant galaxies, star formation regions, and many other objects. These observations can help us to understand not only what is going on inside these objects, but also answer fundamental physics questions relating to the nature of Dark Matter and of space-time itself. However, we have reached the limit of what can be done with current instruments, and so over 1640 scientists and engineers from 31 countries around the world have come together to build a new instrument - the Cherenkov Telescope Array (CTA).CTA will offer a dramatic increase in sensitivity over current instruments and extend the energy range of the gamma rays observed to both lower and higher values. It is predicted that the catalogue of known VHE emitting objects will expand from the roughly 200 known now to over 1000, and we can expect many new discoveries in key areas of astrophysics and fundamental physics. To achieve the energy coverage of CTA, telescopes of three different sizes are needed: Small (~4 m diameter), Medium (12 m) and Large (23 m) Sized Telescopes (SSTs, MSTs and LSTs, respectively). CTA will have arrays in the northern and southern hemispheres. Both arrays will include LSTs and MSTs, and the SSTs will be situated only in the souths as these are designed to investigate the highest energy phenomena, which are visible mainlyin the southern sky. We expect construction of the first telescopes on the CTA southern site to begin in 2024.There are currently 12 UK universities and Laboratories involved in CTA. The four UK groups developing the hardware are concentrating their efforts on the construction of the SSTs for which we previously developed the Compact High Energy Camera (CHEC). CHEC was selected along with the Italian ASTRI telescope structure, from the three competing SST designs, as the basis for the final SST design. During the 2022 funding period we will complete:1. Manufacture, assembly and test of the MCAM, a mechanical model to validate the mechanical design and test assembly procedures.2. Manufacture, assembly and test of the QCAM, a full camera build but using a backplane with full functionality in only one quadrant (full back plane delayed by long FPGA lead time) and populated with 8 camera modules (comprising a 64-pixel SiPM tile, FEE, and TM). 3. Additional testing on single camera modules (comprising a 64-pixel SiPM tile, FEE, and TM) at Leicester, MPIK, and Erlangen to accelerate sensor and electronics subsystems verification.4. Preparation of camera documentation for the following:a) SST internal Product Review (PR) in September 2022, which we will use as a dry run for the CDR.b) CDR, currently scheduled for July 2023.

宇宙到处都是能量如此之大的颗粒，以至于它们非常接近光速。它们在许多方面影响宇宙，影响恒星的生命周期和星系的演变。这些颗粒很难追踪，但可以通过产生伽马射线来揭示其存在。像它们的低能量表亲一样，X射线，伽玛射线也不会穿透地球大气，通常使用基于卫星的望远镜来检测它们。但是，在非常高的能量（VHE）下，使用航天器检测到它们的伽马射线很少。幸运的是，可以通过蓝光，切伦科夫辐射在大气中相互作用时从地面上观察它们。大气中Cherenkov辐射的辉光比星光的淡淡10,000倍，因此需要大的镜子来收集它，并且因为闪光仅持续数十亿秒，需要超快速的摄像头来记录它们。我们从当前基于地面的伽马射线望远镜（例如Hess）中知道，需要研究大量现象。 Vhe伽马射线望远镜已经检测到超新星爆炸，二进制恒星系统，遥远星系中的黑洞产生的高能喷射，恒星形成区域和许多其他物体。这些观察结果可以帮助我们不仅了解这些物体内部发生的事情，还可以回答与暗物质本身和时空本身有关的基本物理问题。但是，我们已经达到了当前工具可以完成的工作的极限，因此，来自世界31个国家 /地区的1640多个科学家和工程师都聚集在一起建造一种新的乐器-Cherenkov望远镜阵列（CTA）。对电流仪器的灵敏度显着提高，并将观察到的伽马射线的能量范围扩展到较低和更高的值。可以预测，已知的发射物体的目录将从现在已知的大约200个扩展到1000多个，我们可以期望天体物理学和基本物理学的关键领域有许多新发现。为了达到CTA的能量覆盖率，需要三种不同尺寸的望远镜：小（〜4 m直径），中（12 m）和大型（23 m）大小的望远镜（分别为SSTS，MSTS和LST）。 CTA将在北半球和南半球有阵列。两个阵列都将包括LST和MST，SST仅位于南部，因为这些阵列旨在研究最高的能量现象，这些现象主要可见。我们预计，CTA南部现场的第一批望远镜建设将于2024年开始。目前，有12所英国大学和实验室参与CTA。开发硬件的四个英国群体将他们的精力集中在我们以前开发的紧凑型高能相机（CHEC）的SST上的构建上。从三个竞争的SST设计中选择了CHEC与意大利Astri望远镜结构一起选择，作为最终SST设计的基础。在2022年的资金期间，我们将完成：1。 MCAM的制造，组装和测试，MCAM是一种机械模型，旨在验证机械设计和测试组装程序。2。 QCAM的制造，组装和测试，一个完整的相机构建，但仅在一个象限中具有完整功能的背板（由长FPGA延迟延迟FPGA提前时间），并带有8个相机模块（包括64像素SIPM SIPM Tile，费用和TM）。 3。在莱斯特，MPIK和ERLANGEN上进行单相机模块的其他测试（包括64像素SIPM Tile，Fee和TM），以加速传感器和电子子系统验证4。准备以下摄像机文档：a）2022年9月的SST内部产品评论（PR），我们将用作目前定于2023年7月的CDR.B）CDR的干式运行。

项目成果

The Cherenkov Telescope Array: layout, design and performance

切伦科夫望远镜阵列：布局、设计和性能

• 发表时间: 2022
• 期刊: Proceedings of Science
• 作者: Abdalla H.

The Small-Sized Telescopes for the Southern Site of the Cherenkov Telescope Array

切伦科夫望远镜阵列南站的小型望远镜

• 发表时间: 2022
• 期刊: Proceedings of the 37th International Cosmic Ray Conference
• 作者: Tagliaferri Gianpiero;Antonelli Angelo;Arnesen Tora;Aschersleben Jann;Attina' Primo;Balbo Matteo;Bang Sunghyun;Barcelo Miquel;Baryshev Andrey;Bellassai Giancarlo;et al.;Adams Colin B. et al.;H. Abe et al.;H. Abe et al.;H. Abe et al.;B. Mode et al.;H. Abe et al.;R. Lopez-Coto et al.;R. White et al.
• 通讯作者: R. White et al.

HAWC J2227+610: A potential PeVatron candidate for the CTA in the northern hemisphere

HAWC J2227 610：北半球 CTA 的潜在 PeVatron 候选者

• 发表时间: 2021
• 期刊: arXiv
• 作者: Abdalla, H.

Sensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud

切伦科夫望远镜阵列对大麦哲伦星云 TeV 光子发射的灵敏度

• DOI: 10.1093/mnras/stad1576
• 发表时间: 2023
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Acharyya, A;Adam, R;Aguasca-Cabot, A;Agudo, I;Aguirre-Santaella, A;Alfaro, J;Aloisio, R;Alves Batista, R;Amato, E;Angüner, E O
• 通讯作者: Angüner, E O

Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre

切伦科夫望远镜阵列对来自银河系中心的暗物质信号的灵敏度

• DOI: 10.1088/1475-7516/2021/01/057
• 发表时间: 2021
• 期刊: Journal of Cosmology and Astroparticle Physics
• 影响因子: 6.4
• 作者: Tagliaferri Gianpiero;Antonelli Angelo;Arnesen Tora;Aschersleben Jann;Attina' Primo;Balbo Matteo;Bang Sunghyun;Barcelo Miquel;Baryshev Andrey;Bellassai Giancarlo;et al.;Adams Colin B. et al.;H. Abe et al.;H. Abe et al.;H. Abe et al.;B. Mode et al.;H. Abe et al.;R. Lopez-Coto et al.;R. White et al.;Y. Ohtani et al.;Y. Kobayashi et al.;O. Blanch et al.;D. Ribeiro et al.;C. Alispach et al.;L. Foffano et al.;H. Abe et al.;A. Okumura;R. Zanin et al.;Colin B. Adams et al.;Colin B. Adams et al.;Adams Colin B. et al.;Adams C.B et al.;Acharyya A et al.
• 通讯作者: Acharyya A et al.