The mini-array of ASTRI SST-2M telescopes, precursors for the Cherenkov Telescope Array

14th International Conference on Topics in Astroparticle and Underground Physics

物理学;天文学

Pareschi, Giovanni^1 ; Bonnoli, Giacomo^2 ; Vercellone, Stefano^3

INAF-Osservatorio Astronomico di Brera, Via Brera 28, Milano

I-20121, Italy^1

INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46, Merate (LC)

I-23807, Italy^2

INAF-IASF Palermo, Via Ugo La Malfa 153, Palermo

I-90146, Italy^3

关键词: Angular resolution;    Cherenkov telescope arrays;    Entire system;    Large field of views;    Performance improvements;    Point sources;    Secondary mirror;    Technological aspects;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/718/5/052028/pdf
DOI  :  10.1088/1742-6596/718/5/052028

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

In the framework of the Cherenkov Telescope Array (CTA) Observatory, the Italian National Institute of Astrophysics (INAF) has recently inaugurated in Sicily (Italy), at the Serra La Nave astronomical site on the slopes of Mount Etna, a large field of view (FoV, ∼ 9.6°) dual-mirror prototype (ASTRI SST-2M) of the CTA small size class of telescopes (SST). The CTA plans to install about 70 SST in the southern site to allow the study of the gamma rays from a few TeV up to hundreds of TeV. The ASTRI SST-2M telescope prototype has been developed following an end-to-end approach, since it includes the entire system of structure, mirrors optics (primary and secondary mirrors), camera, and control/acquisition software. A remarkable performance improvement could come from the operation of the ASTRI mini-array, led by INAF in synergy with the Universidade de Sao Paulo (Brazil) and the North-West University (South Africa). The ASTRI mini-array will be composed of nine ASTRI SST-2M units and it is proposed as a precursor and initial seed of the CTA to be installed at the final CTA southern site. Apart from the assessment of a number of technological aspects related to the CTA, the ASTRI mini-array will, if compared for instance to H.E.S.S., extend the point source sensitivity up to ∼ 100 TeV, also improving it above 5-10 TeV. Moreover, the unprecedented width of the FoV, with its homogeneous acceptance and angular resolution, will significantly contribute to the achievement of original results during the early CTA science phase.