Monte carlo design studies for the cherenkov telescope array
Monte carlo design studies for the cherenkov telescope array
复制标题
DOI：
10.1016/j.astropartphys.2012.10.002
复制
发表时间：
2012-10
影响因子：
3.5
通讯作者：
K. Bernlöhr;A. Barnacka;Y. Becherini;O. B. Bigas;E. Carmona;P. Colin;G. Decerprit;F. D. Pierro;F. Dubois;C. Farnier;S. Funk;G. Hermann;J. Hinton;T. Humensky;B. Kh'elifi;T. Kihm;N. Komin;J. Lenain;G. Maier;D. Mazin;D. Mazin;M. C. Medina;A. Moralejo;S. Nolan;S. Ohm;E. O. Wilhelmi;R. Parsons;M. Arribas;G. Pedaletti;S. Pita;H. Prokoph;C. Rulten;U. Schwanke;M. Shayduk;V. Stamatescu;P. Vallania;S. Vorobiov;R. Wischnewski;T. Yoshikoshi;A. Zech
中科院分区：
文献类型：
--
作者：
K. Bernlöhr;A. Barnacka;Y. Becherini;O. B. Bigas;E. Carmona;P. Colin;G. Decerprit;F. D. Pierro;F. Dubois;C. Farnier;S. Funk;G. Hermann;J. Hinton;T. Humensky;B. Kh'elifi;T. Kihm;N. Komin;J. Lenain;G. Maier;D. Mazin;D. Mazin;M. C. Medina;A. Moralejo;S. Nolan;S. Ohm;E. O. Wilhelmi;R. Parsons;M. Arribas;G. Pedaletti;S. Pita;H. Prokoph;C. Rulten;U. Schwanke;M. Shayduk;V. Stamatescu;P. Vallania;S. Vorobiov;R. Wischnewski;T. Yoshikoshi;A. Zech
切伦科夫望远镜阵列（CTA）计划作为未来的甚高能伽马射线天文学仪器，具有四个数量级的宽能量范围，与目前的仪器相比，灵敏度提高了约一个数量级。蒙特卡罗模拟是CTA设计中的重要工具。这些模拟的最终目标是为给定的物理目标和灵敏度目标找到最具成本效益的解决方案，或者为给定的成本找到最适合不同类型CTA目标的解决方案。除了不确定的组件成本估计，在这个过程中的主要问题是依赖于大量的配置参数，无论是在规格的个别望远镜类型和阵列布局。这是解决了一个巨大的阵列，旨在作为一个超集的许多不同的现实阵列布局的模拟，也通过模拟不同的望远镜参数的阵列子集。不同的分析方法-在使用当前的安装和扩展（或专门开发）CTA -被应用到模拟数据集，以获得CTA的预期灵敏度。在本文中，我们描述了这种迭代方法的现状，以优化CTA的设计和布局。
The Cherenkov Telescopes Array (CTA) is planned as the future instrument for very-high-energy (VHE) gamma-ray astronomy with a wide energy range of four orders of magnitude and an improvement in sensitivity compared to current instruments of about an order of magnitude. Monte Carlo simulations are a crucial tool in the design of CTA. The ultimate goal of these simulations is to find the most cost-effective solution for given physics goals and thus sensitivity goals or to find, for a given cost, the solution best suited for different types of targets with CTA. Apart from uncertain component cost estimates, the main problem in this procedure is the dependence on a huge number of configuration parameters, both in specifications of individual telescope types and in the array layout. This is addressed by simulation of a huge array intended as a superset of many different realistic array layouts, and also by simulation of array subsets for different telescope parameters. Different analysis methods – in use with current installations and extended (or developed specifically) for CTA – are applied to the simulated data sets for deriving the expected sensitivity of CTA. In this paper we describe the current status of this iterative approach to optimize the CTA design and layout.