Calibration of segmented BGO scintillation detectors for space-based gamma-ray polarimeter

IF 2.2 3区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Experimental Astronomy Pub Date : 2025-02-01 DOI:10.1007/s10686-025-09977-9

A. Mkrtchyan, A. Pozanenko, P. Minaev, A. Strizhak, A. Ivashkin, A. Baranov, S. Musin

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Abstract

In the gamma range, polarization detection is particularly difficult. For example, the registration of linear polarization can help in determining the structure of the magnetic field in a jet when generating radiation in gamma-ray bursts. The measurement of linear polarization in the 511 keV line associated with the annihilation of electrons and positrons may be an indicator of the asymmetry of the distribution of radioactive nickel in the scattering shell of Supernovae. The principle of detecting the polarization of gamma radiation is based on the anisotropy of Compton scattering. This property can be used in the development of polarimeters, which are a segmented scintillation detector. The paper presents polarization calibrations for 3 BGO detectors, which are a simplified prototype of a segmented gamma-ray spectrometer (SGS) being developed for the Chibis-AI microsatellite. The complete assembly of the SGS detector consists of 32 BGO bars. Polarization calibrations of the SGS prototype in the 511 keV line were carried out at the experimental facility at the Institute for Nuclear Research of the Russian Academy of Sciences using the isotope \(^{22}\text {Na}\). Also, for comparison, a simulation of the registration of linear polarization was carried out using the Geant4 software package. The experimental results agree withing \(2\sigma \) of simulations.

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天基伽玛射线偏振计中分段BGO闪烁探测器的标定

在伽马范围内，偏振探测是特别困难的。例如，线极化的登记可以帮助确定在伽马射线爆发中产生辐射时射流中的磁场结构。与电子和正电子湮灭有关的511 keV线的线极化测量可能是放射性镍在超新星散射壳中分布不对称的一个指示。探测伽马辐射偏振的原理是基于康普顿散射的各向异性。这一特性可用于偏振仪的研制，偏振仪是一种分段闪烁探测器。本文介绍了3个BGO探测器的偏振校准，这些探测器是为赤壁星- ai微卫星开发的分段伽玛射线光谱仪（SGS）的简化原型。SGS探测器的完整组件由32个BGO棒组成。在俄罗斯科学院核研究所的实验设施中，使用同位素\(^{22}\text {Na}\)对SGS原型机的511 keV线进行了偏振校准。为了比较，利用Geant4软件包对线极化配准进行了仿真。实验结果与\(2\sigma \)模拟结果一致。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

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来源期刊

Experimental Astronomy 地学天文-天文与天体物理

CiteScore

5.30

自引率

3.30%

发文量

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.