CTA Bridging Grant 2020

2020 年 CTA 过渡补助金

• 批准号: ST/V000284/1
• 负责人: Paula Chadwick
• 金额: $ 14.08万
• 依托单位: Durham University
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2020
• 资助国家: 英国
• 起止时间: 2020 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FV000284%2F1
• 关键词: CTA; Bridging; Grant; 2020

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 130 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. The northern array will consist of 4 LSTs and 25 MSTs. The southern array will add to its 4 LSTs and 25 MSTs an extensive array of 70 SSTs, to investigate the highest energy phenomena, visible mainly in the southern sky. We expect construction of the first telescopes on the CTA southern site to begin in 2021.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 has been recently selected along with the Italian ASTRI telescope structure, from the three competing SST designs, as the basis for the final SST design. During the 2020 funding period we will use the lessons learned from CHEC to design and produce a final production-ready camera for SST. This will involve making essential changes from the CHEC design to improve manufacturability, operation, maintenance and reliability, maximise performance, and cut costs. The research work to be undertaken in 2020 includes: mechanical design modifications, improvements to cooling, a new window and lid design, updated sensors, reduced power consumption, and improvements to electronics components. We will also prepare AIV facilities in preparation for production. This will be supported by ongoing camera software and simulations development. We will expand outreach activities to include a planetarium show and UK science meeting and enhance project management and product assurance in readiness for production.

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光彩要比10,000倍，因此需要大的镜子来收集它，并且因为闪光只能持续几十亿秒的二十亿秒，需要录制它们。 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乐器可以完成的工作的限制，因此，来自世界31个国家 /地区的1640个科学家和工程师都聚集在一起建造一种新的乐器-Cherenkov telescope Array（CTA）.CTA.CTA将极大地提高对当前工具的敏感性，并延伸了更高的gamma ray和更高值的能量范围。可以预测，已知的发射物体的目录将从现在已知的大约130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。北部阵列将由4个LST和25 MST组成。南部阵列将增加40个LST和25 MSTS的70 sST阵列，以调查最高的能量现象，主要在南部的天空中可见。我们预计，CTA南部遗址上首批望远镜的建设将于2021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。 CHEC最近与意大利Astri望远镜结构一起从三种竞争SST设计中选出，作为最终SST设计的基础。在2020年的资金期间，我们将使用从CHEC中学到的经验教训来设计并为SST制作最终的生产相机。这将涉及从CHEC设计进行基本的更改，以提高生产能力，操作，维护和可靠性，最大化性能和削减成本。 2020年将要进行的研究工作包括：机械设计修改，改进冷却，新窗口和盖子设计，更新的传感器，功耗减少以及对电子组件的改进。我们还将准备AIV设施为生产做准备。持续的相机软件和模拟开发将支持这一点。我们将扩大外展活动，包括一个天文馆表演和英国科学会议，并增强生产准备的项目管理和产品保证。

项目成果

Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation

切伦科夫望远镜阵列通过伽马射线传播探测宇宙学和基础物理的灵敏度

• DOI: 10.1088/1475-7516/2021/02/048
• 发表时间: 2021
• 期刊: Journal of Cosmology and Astroparticle Physics
• 影响因子: 6.4
• 作者: Abdalla, H.;Abe, H.;Acero, F.;Acharyya, A.;Adam, R.;Agudo, I.;Aguirre-Santaella, A.;Alfaro, R.;Alfaro, J.;Alispach, C.
• 通讯作者: Alispach, C.

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.

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.