Experimental Astronomy最新文献

{"title":"The real-time trigger software of the follow-up X-ray telescope on board the EP satellite","authors":"Xiaofan Zhao,&nbsp;Hanyu Ban,&nbsp;Hongbo Cai,&nbsp;Jingjing Xu,&nbsp;Fei Li,&nbsp;Zijian Zhao,&nbsp;Ye Zhang,&nbsp;Weiwei Cui,&nbsp;Hao Wang,&nbsp;Laidan Luo,&nbsp;Wei Li,&nbsp;Yong Chen","doi":"10.1007/s10686-025-10006-y","DOIUrl":"10.1007/s10686-025-10006-y","url":null,"abstract":"<div><p>The Follow-up X-ray Telescope (FXT) is a primary scientific instrument on board the Einstein Probe (EP) astronomical satellite, which was launched in January 2024. FXT consists of two nested Wolter I-type telescopes (FXT-A and FXT-B) with a focal length of 1600 mm. The focal plane detector utilizes a PNCCD with a resolution of 384<span>(times )</span>384 pixels. One of the key functions of FXT is to perform the real-time triggering and localization of transients and burst sources. We have developed specialized real-time trigger software that operates within the Payload Data Processing Unit of EP. This onboard software can effectively search for and locate sources, while transmitting source information in real time via the Beidou short message unit and the Very High Frequency (VHF) unit. This paper provides a comprehensive description of the design and development of the onboard software, covering software requirements, module design, and workflow. Additionally, the paper introduces both ground-based and in-orbit testing of this software, and the test results demonstrate that the software meets all design requirements.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144140125","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"AlMn-Al dual TES bolometer development for CMB telescopes","authors":"Jiamin Sun,&nbsp;Lin Zhu,&nbsp;Ye Chai,&nbsp;He Gao,&nbsp;Zhouhui Liu,&nbsp;Shibo Shu,&nbsp;Yaqiong Li,&nbsp;Yifei Zhang,&nbsp;Zhengwei Li,&nbsp;Yudong Gu,&nbsp;Mengqi Jiang,&nbsp;Qinglei Xiu,&nbsp;Zhijia Sun,&nbsp;Daikang Yan,&nbsp;Congzhan Liu","doi":"10.1007/s10686-025-10005-z","DOIUrl":"10.1007/s10686-025-10005-z","url":null,"abstract":"<div><p>Transition-edge sensor (TES) as a type of low-temperature superconducting bolometers offers excellent signal-to-noise-ratio, and is one of the most up-to-date technologies used for cosmic microwave background (CMB) observations. The Ali CMB polarization telescope (AliCPT) project in China uses TES bolometers as the focal plane detector through an international collaborative effort. To increase collecting efficiency of the telescope, and include bolometers of different frequency bands, large-scale production of TES bolometer arrays needs to be accomplished in the future. In this work, we developed single pixel TES bolometers, the saturation power and noise equivalent power (NEP) of which satisfy the requirements of 90 GHz and 150 GHz CMB applications. Each of the bolometers consist of a 1200 ppm AlMn alloy TES for CMB science observation and an Al TES for laboratory optical tests. Dark characterization is applied on these bolometers. Their heat capacities are in the range of 0.7<span>(sim )</span>1.6 pJ/K and the NEP values are below 30 aW/<span>(sqrt{Hz})</span>. The T<span>(_{c})</span> values are about 360 mK and can be adjusted to about 410 mK by additional annealing.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143949636","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Pre-flight calibration of the optics assembly for CATCH’s first pathfinder","authors":"Jingyu Xiao,&nbsp;Yiming Huang,&nbsp;Zijian Zhao,&nbsp;Yusa Wang,&nbsp;Qian-Qing Yin,&nbsp;Chen Zhang,&nbsp;Dongjie Hou,&nbsp;Yuxuan Zhu,&nbsp;Yifan Zhang,&nbsp;Donghua Zhao,&nbsp;Sheng Yang,&nbsp;Lingling Men,&nbsp;Ge Jin,&nbsp;Lian Tao,&nbsp;Shuang-Nan Zhang,&nbsp;Wen Chen,&nbsp;Yanfeng Dai,&nbsp;Min Gao,&nbsp;Huilin He,&nbsp;Guoli Huang,&nbsp;Zhengwei Li,&nbsp;Xiaojing Liu,&nbsp;Panping Li,&nbsp;Yajun Li,&nbsp;Ruican Ma,&nbsp;Liqiang Qi,&nbsp;Xiangyang Wen,&nbsp;Shaolin Xiong,&nbsp;Yibo Xu,&nbsp;Liyuan Xiong,&nbsp;Yong Yang,&nbsp;Juan Zhang,&nbsp;Aimei Zhang,&nbsp;Heng Zhou,&nbsp;Shujie Zhao,&nbsp;Kang Zhao,&nbsp;Qingchang Zhao","doi":"10.1007/s10686-025-10001-3","DOIUrl":"10.1007/s10686-025-10001-3","url":null,"abstract":"<div><p>The first pathfinder of the CATCH mission, CATCH-1, was launched in June 2024. It is equipped with a light-weight, narrow-field optimized Lobster Eye X-ray Optics. By sacrificing a portion of the field of view to achieve a large effective area, the telescope’s sensitivity is enhanced. This paper presents the equipment and procedures employed for calibrating the optics assembly. A comprehensive on-ground calibration for the Lobster Eye X-ray Optics is conducted before its launch using multi-target X-ray sources and the pnCCD Color X-Ray Camera in the 100 m X-Ray Test Facility. The results are derived from calibration measurements taken before and after the mechanical testing and mainly include measurements of the focal length, point spread function, angular resolution, and the effective area for incident X-rays at 0.28 keV, 0.93 keV, 1.49 keV, 2.98 keV, and 4.51 keV. The results indicate that the mirror’s performance remains stable and no observable variation before and after the mechanical testing. At 0.93 keV, the mirror’s angular resolution is <span>(6.11^{prime })</span> (FWHM), and the effective area is 40.75 <span>(textrm{cm}^{2})</span>, meeting the expected performance of CATCH-1 X-ray optics.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143918915","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Optimization of deep learning method on track reconstruction for X-ray polarimetry with gas pixel detectors","authors":"Yang Jiao,&nbsp;Weichun Jiang,&nbsp;Jiechen Jiang,&nbsp;Huilin He,&nbsp;Hua Feng,&nbsp;Xiaohua Liu,&nbsp;Hong Li,&nbsp;Liming Song,&nbsp;Yuanyuan Du,&nbsp;Liang Sun,&nbsp;Xiaojing Liu,&nbsp;Qiong Wu,&nbsp;Jiawei Yang,&nbsp;Zipeng Song,&nbsp;Hangyu Chen,&nbsp;Yongqi Zhao,&nbsp;Yupeng Xu,&nbsp;Congzhan Liu,&nbsp;Shuangnan Zhang","doi":"10.1007/s10686-025-10003-1","DOIUrl":"10.1007/s10686-025-10003-1","url":null,"abstract":"<div><p>The reconstruction of the photoelectron tracks in X-ray polarimetric detectors based on Gas Pixel Detectors (GPD) is crucial for polarization detection. In addition to traditional moment analysis methods, the convolutional neural network (CNN) is also a noteworthy approach. However, most existing CNN methods for polarization detection have only been effectively validated on simulated data, and the few methods validated on experimental data have not yielded satisfactory results. We have improved the CNN algorithm for reconstructing the emission direction of photoelectron tracks in X-ray polarimetric detectors. We tested this algorithm using calibration data from the detectors of the PolarLight mission and the Polarimetry Focusing Array (PFA) onboard the enhanced X-ray Timing and Polarimetry (eXTP) mission. The results indicate that the optimized deep learning model increased the modulation factor by approximately 0.02 over the 2-8 keV energy range and only introduced a small systematic error. This can enhance the sensitivity of polarization detector in the low-energy range. Additionally, the computational resources required for the model are much lower than the previous CNN models.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143918914","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"An optimization framework for wide-field small aperture telescope arrays used in sky surveys","authors":"Wennan Xiang,&nbsp;Peng Jia,&nbsp;Zhengyang Li,&nbsp;Jifeng Liu,&nbsp;Zhenyu Ying,&nbsp;Zeyu Bai","doi":"10.1007/s10686-025-10004-0","DOIUrl":"10.1007/s10686-025-10004-0","url":null,"abstract":"<div><p>For time-domain astronomy, it is crucial to frequently image celestial objects at specific depths within a predetermined cadence. To fulfill these scientific demands, scientists globally have started or planned the development of non-interferometric telescope arrays in recent years. Due to the numerous parameters involved in configuring these arrays, there is a need for an automated optimization framework that selects parameter sets to satisfy scientific needs while minimizing costs. In this paper, we introduce such a framework, which integrates optical design software, an exposure time calculator, and an optimization algorithm, to balance the observation capabilities and the cost of optical telescope arrays. Neural networks are utilized to speed up results retrieval of the system with different configurations. We use the SiTian project as a case study to demonstrate the framework’s effectiveness, showing that this approach can aid scientists in selecting optimal parameter sets. The code for this framework is published in the China Virtual Observatory PaperData Repository, enabling users to optimize parameters for various non-interferometric telescope array projects.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143913918","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cross-calibration of GRID via correlative spectral analysis of GRBs","authors":"Zirui Yang,&nbsp;Chenyu Wang,&nbsp;Hanwen Lin,&nbsp;Xiaofan Pan,&nbsp;Qize Liu,&nbsp;Xutao Zheng,&nbsp;Huaizhong Gao,&nbsp;Longhao Li,&nbsp;Qidong Wang,&nbsp;Jianping Cheng,&nbsp;Zhi Zeng,&nbsp;Ming Zeng,&nbsp;Hua Feng,&nbsp;Binbin Zhang,&nbsp;Zhonghai Wang,&nbsp;Rong Zhou,&nbsp;Yuanyuan Liu,&nbsp;Lin Lin,&nbsp;Jiayong Zhong,&nbsp;Jianyong Jiang,&nbsp;Wentao Han,&nbsp;Yang Tian,&nbsp;Benda Xu","doi":"10.1007/s10686-025-10002-2","DOIUrl":"10.1007/s10686-025-10002-2","url":null,"abstract":"<div><p>Gamma-ray bursts (GRBs) are among the most energetic phenomena in the universe, and their observation has significantly advanced with the development of space-based gamma-ray telescopes. The Gamma-Ray Integrated Detectors (GRID) mission has initiated a nanosatellite constellation capable of all-sky GRB monitoring, deploying 12 detector payloads in low Earth orbit and collecting its first batch of scientific data. For GRB analysis, dedicated detector response matrices (DRMs) were individually constructed for each detector using Monte Carlo simulations and ground calibration. To further validate detector performance under real operational conditions, cross-calibration with existing space missions offers a robust validation. Herein, cross-calibration between the GRID detectors and the Fermi’s Gamma-ray Burst Monitor (GBM) was performed through joint spectral analysis. The excellent agreement between the instruments validates the accuracy of GRID’s DRMs and the reliability of its scientific data. For nanosatellite constellations like GRID, cross-calibration through orbital observations involving multiple distributed detector payloads is a crucial tool for ensuring uniformity and verifying overall performance of such systems.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-10002-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143908731","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Ground-breaking exoplanet science with the ANDES spectrograph at the ELT","authors":"Enric Palle,&nbsp;Katia Biazzo,&nbsp;Emeline Bolmont,&nbsp;Paul Mollière,&nbsp;Katja Poppenhaeger,&nbsp;Jayne Birkby,&nbsp;Matteo Brogi,&nbsp;Gael Chauvin,&nbsp;Andrea Chiavassa,&nbsp;Jens Hoeijmakers,&nbsp;Emmanuel Lellouch,&nbsp;Christophe Lovis,&nbsp;Roberto Maiolino,&nbsp;Lisa Nortmann,&nbsp;Hannu Parviainen,&nbsp;Lorenzo Pino,&nbsp;Martin Turbet,&nbsp;Jesse Weder,&nbsp;Simon Albrecht,&nbsp;Simone Antoniucci,&nbsp;Susana C. Barros,&nbsp;Andre Beaudoin,&nbsp;Bjorn Benneke,&nbsp;Isabelle Boisse,&nbsp;Aldo S. Bonomo,&nbsp;Francesco Borsa,&nbsp;Alexis Brandeker,&nbsp;Wolfgang Brandner,&nbsp;Lars A. Buchhave,&nbsp;Anne-Laure Cheffot,&nbsp;Robin Deborde,&nbsp;Florian Debras,&nbsp;Rene Doyon,&nbsp;Paolo Di Marcantonio,&nbsp;Paolo Giacobbe,&nbsp;Jonay I. González Hernández,&nbsp;Ravit Helled,&nbsp;Laura Kreidberg,&nbsp;Pedro Machado,&nbsp;Jesus Maldonado,&nbsp;Alessandro Marconi,&nbsp;B. L. Canto Martins,&nbsp;Adriano Miceli,&nbsp;Christoph Mordasini,&nbsp;Mamadou N’Diaye,&nbsp;Andrzej Niedzielski,&nbsp;Brunella Nisini,&nbsp;Livia Origlia,&nbsp;Celine Peroux,&nbsp;Alexander G. M. Pietrow,&nbsp;Enrico Pinna,&nbsp;Emily Rauscher,&nbsp;Sabine Reffert,&nbsp;Cristina Rodríguez-López,&nbsp;Philippe Rousselot,&nbsp;Nicoletta Sanna,&nbsp;Nuno C. Santos,&nbsp;Adrien Simonnin,&nbsp;Alejandro Suárez Mascareño,&nbsp;Alessio Zanutta,&nbsp;Maria Rosa Zapatero-Osorio,&nbsp;Mathias Zechmeister","doi":"10.1007/s10686-025-10000-4","DOIUrl":"10.1007/s10686-025-10000-4","url":null,"abstract":"<div><p>In the past decade the study of exoplanet atmospheres at high-spectral resolution, via transmission/emission spectroscopy and cross-correlation techniques for atomic/molecular mapping, has become a powerful and consolidated methodology. The current limitation is the signal-to-noise ratio that one can obtain during a planetary transit, which is in turn ultimately limited by telescope size. This limitation will be overcome by ANDES, an optical and near-infrared high-resolution spectrograph for the Extremely Large Telescope, which is currently in Phase B development. ANDES will be a powerful transformational instrument for exoplanet science. It will enable the study of giant planet atmospheres, allowing not only an exquisite determination of atmospheric composition, but also the study of isotopic compositions, dynamics and weather patterns, mapping the planetary atmospheres and probing atmospheric formation and evolution models. The unprecedented angular resolution of ANDES, will also allow us to explore the initial conditions in which planets form in proto-planetary disks. The main science case of ANDES, however, is the study of small, rocky exoplanet atmospheres, including the potential for biomarker detections, and the ability to reach this science case is driving its instrumental design. Here we discuss our simulations and the observing strategies to achieve this specific science goal. Since ANDES will be operational at the same time as NASA’s JWST and ESA’s ARIEL missions, it will provide enormous synergies in the characterization of planetary atmospheres at high and low spectral resolution. Moreover, ANDES will be able to probe for the first time the atmospheres of several giant and small planets in reflected light. In particular, we show how ANDES will be able to unlock the reflected light atmospheric signal of a golden sample of nearby non-transiting habitable zone earth-sized planets within a few tenths of nights, a scientific objective that no other currently approved astronomical facility will be able to reach.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-10000-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143908666","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"De-jittering Ariel: An optimized algorithm","authors":"Andrea Bocchieri,&nbsp;Lorenzo V. Mugnai,&nbsp;Enzo Pascale,&nbsp;Andreas Papageorgiou,&nbsp;Angèle Syty,&nbsp;Angelos Tsiaras,&nbsp;Paul Eccleston,&nbsp;Giorgio Savini,&nbsp;Giovanna Tinetti,&nbsp;Renaud Broquet,&nbsp;Patrick Chapman,&nbsp;Gianfranco Sechi","doi":"10.1007/s10686-025-09999-3","DOIUrl":"10.1007/s10686-025-09999-3","url":null,"abstract":"<div><p>The European Space Agency’s <i>Ariel</i> mission, scheduled for launch in 2029, aims to conduct the first large-scale survey of atmospheric spectra of transiting exoplanets. <i>Ariel</i> achieves the high photometric stability on transit timescales required to detect the spectroscopic signatures of chemical elements with a payload design optimized for transit photometry that either eliminates known systematics or allows for their removal during data processing without significantly degrading or biasing the detection. Jitter in the spacecraft’s line of sight is a source of disturbance when measuring the spectra of exoplanet atmospheres. We describe an improved algorithm for de-jittering <i>Ariel</i> observations simulated in the time domain. We opt for an approach based on the spatial information on the Point Spread Function (PSF) distortion from jitter to detrend the optical signals. The jitter model is based on representative simulations from Airbus Defence and Space, the prime contractor for the <i>Ariel</i> service module. We investigate the precision and biases of the retrieved atmospheric spectra from the jitter-detrended observations. At long wavelengths, the photometric stability of the <i>Ariel</i> spectrometer is already dominated by photon noise. Our algorithm effectively de-jitters both photometric and spectroscopic data, ensuring that the performance remains photon noise-limited across the entire <i>Ariel</i> spectrum, fully compliant with mission requirements. This work contributes to the development of the data reduction pipeline for <i>Ariel</i>, aligning with its scientific goals, and may also benefit other astronomical telescopes and instrumentation.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-09999-3.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143908665","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"An acoustic levitator design for suspending cosmic dust analogues and aerosol particles in light scattering experiments","authors":"A. Colin,&nbsp;O. Muñoz,&nbsp;F. J. García-Izquierdo,&nbsp;E. Frattin,&nbsp;J. Martikainen,&nbsp;Z. Gray,&nbsp;J. L. Ramos,&nbsp;J. Jiménez,&nbsp;A. Tobaruela,&nbsp;J. M. Gómez-López,&nbsp;I. Bustamante,&nbsp;J. C. Gómez,&nbsp;F. Moreno,&nbsp;A. Marzo","doi":"10.1007/s10686-025-09994-8","DOIUrl":"10.1007/s10686-025-09994-8","url":null,"abstract":"<div><p>We present a design of an acoustic levitator composed of 35 ultrasonic transducers operating at 40 <i>kHz</i> configured to form a spherical cavity. The acoustic radiation force measured experimentally in the center of the cavity is <span>({{varvec{F}}}_{rad}approx 9.6 mN)</span>, enough for levitating spheres as well as irregular particles of different materials of up to ~ 50 <i>mg</i>. Levitation tests have been performed with particles of different geometries and compositions, including liquid droplets and minerals relevant in studies of atmospheric aerosol and cosmic dust. This device has been deployed in the center of a polar nephelometer set-up to conduct studies of light scattering by irregular solid particles and liquid droplets. Test experiments have been carried out using a 1.5 <i>mm</i> diameter NBK- 7 glass sphere, for which three elements of the scattering matrix have been measured as functions of the scattering angle using a 647 <i>nm</i> diode laser. Mie theory calculations of the scattering matrix elements at this wavelength agree well with the measurements, demonstrating the functionality of the whole device.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-09994-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143856494","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Research on the proton-induced radiation damage of pixelated CdZnTe detectors for space applications","authors":"Hao Chang,&nbsp;Ming Zeng,&nbsp;Di Wang,&nbsp;Hua Feng,&nbsp;Yang Tian,&nbsp;Ge Ma,&nbsp;Xiaofan Pan,&nbsp;Chen Li,&nbsp;Zhongming Wang,&nbsp;Xin Zhuo,&nbsp;Xutao Zheng,&nbsp;Yulan Li","doi":"10.1007/s10686-025-09998-4","DOIUrl":"10.1007/s10686-025-09998-4","url":null,"abstract":"<div><p>High-performance pixelated CZT detectors that achieve 3D position sensitivity are promising candidates for use in Compton imaging telescopes. We proposed to use pixelated CZT detectors in the MeV Astrophysical Spectroscopic Surveyor (MASS), which is a large area Compton telescope. Nevertheless, the presence of high-energy protons in space can lead to radiation damage in pixelated CZT detectors, causing their performance to degrade gradually. Using non-ionizing energy loss (NIEL), this study develops a method that quantitatively evaluates the radiation damage of detectors in space. To verify the method, this study irradiated two <span>(2times 2times 1text { cm}^3)</span> pixelated CZT detectors with 100 MeV protons at fluences ranging from <span>(3times 10^7text { p}^+/text {cm}^2)</span> to <span>( 3times 10^9text { p}^+/text {cm}^2)</span> under two bias sets. When the proton fluence reaches <span>(3 times 10^9 text { p}^+/text {cm}^2)</span>, the energy resolution of the detectors significantly deteriorates to <span>(3.8%)</span> at 511 keV (FWHM/E), even after post-correction. Finally, this study provides engineering considerations for their application in space.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-04-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143856493","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}