Using SRG/eROSITA to predict soft proton induced ATHENA backgrounds

IF 2.7 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS
Emanuele Perinati, Michael J. Freyberg, Michael C. H. Yeung, Konrad Dennerl, Christian Pommranz, Bastian Heß, Sebastian Diebold, Chris Tenzer, Andrea Santangelo
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引用次数: 0

Abstract

Soft protons populating the space environment have affected the performance of the X-ray detectors on board Chandra and XMM-Newton, and they pose a threat for future high energy astrophysics missions with larger aperture, such as ATHENA. In this paper, we aim to predict the soft proton induced ATHENA backgrounds from the modelling of the orbital flux obtained using eROSITA on board SRG. To this end, we analysed the background measured by eROSITA and with the help of simulations we defined a range of values for the potential count-rate of quiet-time soft protons focused through the mirror shells. We used it to derive an estimate of the orbital soft proton flux, from which the induced background for the WFI and X-IFU detectors can be predicted, assuming ATHENA in the same L2-orbit as SRG. The scaling, based on the computed proton transmission yields of the optics and optical/thermal filters, indicates that the soft proton induced WFI and X-IFU backgrounds could be expected within the requirement. Regardless of where ATHENA will be placed (L1 or L2), our analysis also suggests that increasing somewhat the thickness of the WFI optical blocking filter, e.g. by \(\sim \)30%, would help to further reduce the soft proton flux onto the detector, which might be worth in case the planned magnetic diverters perform worse than expected due to soft proton neutralisation at the mirror level.

利用 SRG/eROSITA 预测软质子诱导的 ATHENA 背景
空间环境中充斥的软质子影响了钱德拉和 XMM-Newton 上 X 射线探测器的性能,并对 ATHENA 等未来具有更大孔径的高能天体物理学任务构成威胁。在本文中,我们的目的是通过使用 SRG 上的 eROSITA 获得的轨道通量建模来预测软质子诱导的 ATHENA 背景。为此,我们分析了 eROSITA 测得的背景,并在模拟的帮助下确定了通过镜壳聚焦的安静时软质子潜在计数率的取值范围。假定 ATHENA 与 SRG 处于相同的 L2 轨道上,我们利用它得出了轨道软质子通量的估计值,并据此预测了 WFI 和 X-IFU 探测器的诱导本底。根据光学和光学/热学滤波器的质子透射率计算得出的比例表明,软质子诱导的 WFI 和 X-IFU 背景预计不会超出要求。无论ATHENA将被放置在哪里(L1还是L2),我们的分析还表明,在一定程度上增加WFI光学阻挡滤波器的厚度,例如增加(\sim \)30%,将有助于进一步减少探测器上的软质子通量。
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来源期刊
Experimental Astronomy
Experimental Astronomy 地学天文-天文与天体物理
CiteScore
5.30
自引率
3.30%
发文量
57
审稿时长
6-12 weeks
期刊介绍: Many new instruments for observing astronomical objects at a variety of wavelengths have been and are continually being developed. Furthermore, a vast amount of effort is being put into the development of new techniques for data analysis in order to cope with great streams of data collected by these instruments. Experimental Astronomy acts as a medium for the publication of papers of contemporary scientific interest on astrophysical instrumentation and methods necessary for the conduct of astronomy at all wavelength fields. Experimental Astronomy publishes full-length articles, research letters and reviews on developments in detection techniques, instruments, and data analysis and image processing techniques. Occasional special issues are published, giving an in-depth presentation of the instrumentation and/or analysis connected with specific projects, such as satellite experiments or ground-based telescopes, or of specialized techniques.
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