The Cryogenic Anticoincidence Detector for the NewAthena X-IFU Instrument: A Program Overview

IF 1.9 Q3 PHYSICS, CONDENSED MATTER Condensed Matter Pub Date : 2023-12-13 DOI:10.3390/condmat8040108
C. Macculi, A. Argan, M. D’Andrea, S. Lotti, G. Minervini, Luigi Piro, L. Ferrari Barusso, Corrado Boragno, E. Celasco, Giovanni Gallucci, Flavio Gatti, Daniele Grosso, M. Rigano, F. Chiarello, Guido Torrioli, Mauro Fiorini, M. Uslenghi, D. Brienza, E. Cavazzuti, S. Puccetti, Angela Volpe, P. Bastia
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Abstract

Athena (advanced telescope for high-energy astrophysics) is an ESA large-class mission, at present under a re-definition “design-to-cost” phase, planned for a prospective launch at L1 orbit in the second half of the 2030s. It will be an observatory alternatively focusing on two complementary instruments: the X-IFU (X-ray Integral Field Unit), a TES (TransitionEdge Sensor)-based kilo-pixel array which is able to perform simultaneous high-grade energy spectroscopy (~3 eV@7 keV) and imaging over 4′ FoV (field of view), and the WFI (Wide Field Imager), which has good energy spectral resolution (~170 eV@7 keV) and imaging on wide 40′ × 40′ FoV. Athena will be a truly transformational observatory, operating in conjunction with other large observatories across the electromagnetic spectrum available in the 2030s like ALMA, ELT, JWST, SKA, CTA, etc., and in multi-messenger synergies with facilities like LIGO A+, Advanced Virgo+, LISA, IceCube and KM3NeT. The Italian team is involved in both instruments. It has the co-PIship of the cryogenic instrument for which it has to deliver the TES-based Cryogenic AntiCoincidence detector (CryoAC) necessary to guarantee the X-IFU sensitivity, degraded by a primary particle background of both solar and galactic cosmic ray (GCR) origins, and by secondary electrons produced by primaries interacting with the materials surrounding the main detector. The outcome of Geant4 studies shows the necessity for adopting both active and passive techniques to guarantee the residual particle background at 5 × 10−3 cts cm−2 s−1 keV−1 level in 2–10 keV scientific bandwidth. The CryoAC is a four-pixel detector made of Si-suspended absorbers sensed by Ir/Au TESes placed at <1 mm below the main detector. After a brief overview of the Athena mission, we will report on the particle background reduction techniques highlighting the impact of the Geant4 simulation on the X-IFU focal plane assembly design, then hold a broader discussion on the CryoAC program in terms of detection chain system requirements, test, design concept against trade-off studies and programmatic.
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用于 NewAthena X-IFU 仪器的低温反碰撞探测器:项目概述
雅典娜(高能天体物理学高级望远镜)是欧空局的一项大型飞行任务,目前正处于重新定义的 "按成本设计 "阶段,计划于 2030 年代后半期发射到 L1 轨道。它将是一个观测站,重点放在两个互补的仪器上:X-IFU(X 射线积分场单元)是一个基于 TES(过渡边缘传感器)的千像素阵列,能够同时进行高能量光谱分析(~3 eV@7 keV)和 4′FoV (视场)成像;WFI(宽视场成像仪)具有良好的能谱分辨率(~170 eV@7 keV)和 40′×40′FoV 宽视场成像。雅典娜天文台将是一个真正的变革性天文台,它将与 2030 年代的其他大型电磁波谱天文台(如 ALMA、ELT、JWST、SKA、CTA 等)一起运行,并与 LIGO A+、Advanced Virgo+、LISA、IceCube 和 KM3NeT 等设施发挥多信使协同作用。意大利团队参与了这两个仪器的工作。它是低温仪器的共同首席科学家,必须为该仪器提供必要的基于 TES 的低温反碰撞探测器(CryoAC),以保证 X-IFU 的灵敏度,这种灵敏度因太阳和银河宇宙射线(GCR)来源的原初粒子背景以及原初粒子与主探测器周围材料相互作用产生的次级电子而降低。Geant4 的研究结果表明,有必要同时采用主动和被动技术,以确保在 2-10 千伏科学带宽内将残余粒子背景保持在 5 × 10-3 cts cm-2 s-1 keV-1 的水平。CryoAC 是一个由悬浮硅吸收器组成的四像素探测器,由放置在主探测器下方 <1 毫米处的铱/金 TES 感应。在简要概述雅典娜任务之后,我们将报告粒子本底降低技术,重点介绍 Geant4 仿真对 X-IFU 焦平面组件设计的影响,然后从探测链系统要求、测试、设计概念与权衡研究和计划方面对 CryoAC 计划进行更广泛的讨论。
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来源期刊
Condensed Matter
Condensed Matter PHYSICS, CONDENSED MATTER-
CiteScore
2.90
自引率
11.80%
发文量
58
审稿时长
10 weeks
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