Experimental Astronomy最新文献

High-Performance and Low-Noise Front-End Electronics for GRAPES-3 Muon Telescope 葡萄-3 μ子望远镜的高性能低噪声前端电子器件

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-07-09 DOI: 10.1007/s10686-023-09898-5

K. Ramesh, S. K. Gupta, B. Hariharan, Y. Hayashi, P. Jagadeesan, A. Jain, S. Kawakami, P. K. Mohanty, P. K. Nayak, A. Oshima, L. V. Reddy, M. Zuberi

{"title":"High-Performance and Low-Noise Front-End Electronics for GRAPES-3 Muon Telescope","authors":"K. Ramesh, S. K. Gupta, B. Hariharan, Y. Hayashi, P. Jagadeesan, A. Jain, S. Kawakami, P. K. Mohanty, P. K. Nayak, A. Oshima, L. V. Reddy, M. Zuberi","doi":"10.1007/s10686-023-09898-5","DOIUrl":"10.1007/s10686-023-09898-5","url":null,"abstract":"<div><p>Cosmic Ray Laboratory – TIFR, Ooty, India is operating the largest tracking muon telescope as a component of the GRAPES-3 (Gamma Ray Astronomy PeV EnergieS at phase – 3) experiment. The basic building blocks of the telescope are proportional counters (PRCs), a large number of which are fabricated in-house for the planned expansion of the existing muon telescope to double its area and enhance the solid angle coverage from 2.3 sr to 3.7 sr as well as achieving higher sensitivity for studying space weather and atmospheric phenomena, cosmic ray composition, etc. The existing muon telescope consists of 3712 PRCs, and after the planned expansion which requires an additional 3776 PRCs, the area of the telescope will increase from the present 560 m<span>(^{2})</span> to 1130 m<span>(^{2})</span>. Each of the PRCs will need to be individually equipped with front-end electronics for processing the output signals. The output pulses from PRCs are extremely feeble, and their charges are in the order of <span>(sim )</span>100 pC. The tiny signal has to be isolated from potential sources of noise before its processing. High-performance, ultra-low noise, and cost-effective electronics are designed, developed, and mass-produced in-house for about 8000 channels of PRCs. The quality of data is improved significantly by interfacing the new electronics with PRCs of the existing muon telescope due to improved signal-to-noise (S/N) ratio, and the data acquisition is made effective as a result of multifold improvement achieved by avoiding undesired interruptions in the data.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"31 - 47"},"PeriodicalIF":3.0,"publicationDate":"2023-07-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4389932","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}

引用次数: 1

On-ground calibration of low gain response for Gamma-Ray Detectors onboard the GECAM satellite GECAM卫星上伽玛射线探测器低增益响应的地面校准

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-07-07 DOI: 10.1007/s10686-023-09892-x

Chaoyang Li, Wenxi Peng, Yaqing Liu, Xingzhu Cui, Zhenghua An, Xinqiao Li, Shaolin Xiong, Dali Zhang, Ke Gong, Min Gao, Dongya Guo, Xiaohua Liang, Xiaojing Liu, Rui Qiao, Xilei Sun, Jinzhou Wang, Xiangyang Wen, Yanbing Xu, Sheng Yang, Fan Zhang, Xiaoyun Zhao, Juncheng Liang, Haoran Liu, Zhijie Yang, Xiaofei Lan

{"title":"On-ground calibration of low gain response for Gamma-Ray Detectors onboard the GECAM satellite","authors":"Chaoyang Li, Wenxi Peng, Yaqing Liu, Xingzhu Cui, Zhenghua An, Xinqiao Li, Shaolin Xiong, Dali Zhang, Ke Gong, Min Gao, Dongya Guo, Xiaohua Liang, Xiaojing Liu, Rui Qiao, Xilei Sun, Jinzhou Wang, Xiangyang Wen, Yanbing Xu, Sheng Yang, Fan Zhang, Xiaoyun Zhao, Juncheng Liang, Haoran Liu, Zhijie Yang, Xiaofei Lan","doi":"10.1007/s10686-023-09892-x","DOIUrl":"10.1007/s10686-023-09892-x","url":null,"abstract":"<div><p>The Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) consists of two small satellites operating in the same Earth orbit with opposite phases. Its scientific goal is to monitor the electromagnetic counterparts associated with Gravitational Wave events (GWE) and other cosmic high energy transient sources. As the main detector, the Gamma-Ray Detector (GRD) adopts LaBr<span>(_{3})</span>:Ce scintillator coupled with SiPM array. Each GRD has two output channels, i.e. high gain channel (8 <span>(sim )</span> 250 keV) and low gain channel (50 <span>(sim )</span> 6000 keV). In this paper, we present the low gain calibration results of GRDs with radioactive sources on ground, including the E-C relation, energy resolution, absolute detection efficiency and spatial response. Meanwhile, the consistency between the measurements and Geant4 simulation demonstrates the accuracy of the simulation code.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"49 - 60"},"PeriodicalIF":3.0,"publicationDate":"2023-07-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4624609","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}

引用次数: 1

Measuring the cosmic X-ray background accurately 精确测量宇宙x射线背景

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-07-06 DOI: 10.1007/s10686-023-09896-7

Hancheng Li, Roland Walter, Nicolas Produit, Fiona Hubert

引用次数: 0

Snapshot averaged Matrix Pencil Method (SAM) for direction of arrival estimation 快照平均矩阵铅笔法(SAM)的到达方向估计

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-06-28 DOI: 10.1007/s10686-023-09897-6

Harsha Avinash Tanti, Abhirup Datta, S. Ananthakrishnan

{"title":"Snapshot averaged Matrix Pencil Method (SAM) for direction of arrival estimation","authors":"Harsha Avinash Tanti, Abhirup Datta, S. Ananthakrishnan","doi":"10.1007/s10686-023-09897-6","DOIUrl":"10.1007/s10686-023-09897-6","url":null,"abstract":"<div><p>The estimation of the direction of electromagnetic (EM) waves from a radio source using electrically short antennas is one of the challenging problems in the field of radio astronomy. In this paper we have developed an algorithm which performs better in direction and polarization estimations than the existing algorithms. Our proposed algorithm Snapshot Averaged Matrix Pencil Method (SAM) is a modification to the existing Matrix Pencil Method (MPM) based Direction of Arrival (DoA) algorithm. In general, MPM estimates DoA of the incoherent EM waves in the spectra using unitary transformations and least square method (LSM). Our proposed SAM modification is made in context to the proposed Space Electric and Magnetic Sensor (SEAMS) mission to study the radio universe below 16 MHz. SAM introduces a snapshot averaging method to improve the incoherent frequency estimation thereby improving the accuracy of DoA estimation. It can also detect polarization to differentiate between Right Hand Circular Polarlization (RHCP), Right Hand Elliptical Polarlization (RHEP), Left Hand Circular Polarlization (LHCP), Left Hand Elliptical Polarlization (LHEP) and Linear Polarlization (LP). This paper discusses the formalism of SAM and shows the initial results of a scaled version of a DoA experiment at a resonant frequency of <span>(sim )</span>72 MHz.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"267 - 292"},"PeriodicalIF":3.0,"publicationDate":"2023-06-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-023-09897-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5084665","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}

引用次数: 0

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-06-24 DOI: 10.1007/s10686-023-09894-9

Ana I. Gómez de Castro, Noah Brosch, Daniela Bettoni, Leire Beitia-Antero, Paul Scowen, David Valls-Gabaud, Mikhail Sachkov

{"title":"The IAU recommended photometric system for ultraviolet astronomy","authors":"Ana I. Gómez de Castro, Noah Brosch, Daniela Bettoni, Leire Beitia-Antero, Paul Scowen, David Valls-Gabaud, Mikhail Sachkov","doi":"10.1007/s10686-023-09894-9","DOIUrl":"10.1007/s10686-023-09894-9","url":null,"abstract":"<div><p>In the current era when access to space is becoming easier and at a lower cost thanks to the standardised cubesat technology, numerous missions are expected to be launched to observe, particularly, at ultraviolet wavelengths. Given the reduced dimensions of the telescope that a cubesat can carry, most of these missions will be focused on photometric surveys of a reduced sample of targets of interest, and therefore each mission will define their own photometric bands according to their scientific objectives and orbital constraints. However, in order to provide a coherent view of the ultraviolet sky, the data should be post-processed under a common framework. In 2017, the IAU working group on ultraviolet astronomy identified the need to define such a common framework for the upcoming ultraviolet missions, and coordinated the definition of a standard set of photometric bands that could serve for homogenizing the current and future data. This paper presents the procedure adopted by the working group for the definition of the standard photometric system, that was approved by the IAU during the General Assembly Business Sessions held in August, 2021. The photometric system consists of seven bands, denoted as UV1-UV7, all included in the range 115 - 400 nm. Some of these bands are based on existing filters, while others have been defined as theoretical bands with constant throughput. This system is to be regarded as a set of synthetic bands for post-processing the data of any mission, and an example of its application to the SPARCS cubesat is also included. The photometric bands are publicly available and can be downloaded from https://www.nuva.eu/uv-photometry/.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"171 - 195"},"PeriodicalIF":3.0,"publicationDate":"2023-06-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-023-09894-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4936407","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}

引用次数: 0

Application of Infrared Thermal Imager to measure the temperature of Back-Up Structure of the TianMa radio telescope 红外热成像仪在天马射电望远镜备用结构温度测量中的应用

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-05-25 DOI: 10.1007/s10686-023-09895-8

Li Fu, Jiansen Tang, Rongbing Zhao, Yongbin Jiang, Jinqing Wang, Qinghui Liu, Zhiqiang Shen, Xu Wang, Haiming Liu

{"title":"Application of Infrared Thermal Imager to measure the temperature of Back-Up Structure of the TianMa radio telescope","authors":"Li Fu, Jiansen Tang, Rongbing Zhao, Yongbin Jiang, Jinqing Wang, Qinghui Liu, Zhiqiang Shen, Xu Wang, Haiming Liu","doi":"10.1007/s10686-023-09895-8","DOIUrl":"10.1007/s10686-023-09895-8","url":null,"abstract":"<div><p>Two infrared thermal imagers have been installed on the TianMa radio telescope (TMRT) to continuously monitor the temperature distributions of the back-up structure (BUS). In order to compensate the measurement error of the infrared thermal imager (ITI) for a BUS, a correction formula, as a function of measuring distance and viewing angle, is proposed. According to the relationship between the locations of the measurement points in the thermographic image and those in the actual structure, the 3D coordinates of the measurement points are determined by a finite element model of the BUS. Then, the measuring distances and viewing angles are calculated using 3D coordinates of the measurement points. The measurement accuracy of the ITI improves from ±2<span>(^{circ })</span>C to ±0.5<span>(^{circ })</span>C with the proposed formula. Additionally, based on the information of rotation angle and rotation speed of the elevation, the problem of the ITI moving with the elevation of the telescope in real time is solved. The temperature data at each elevation are recorded in excel documents respectively which are integrated into a document in chronological order through compiling program. Finally, the temperature of the measurement points at different altazimuthal positions is displayed as curves or contours. The thermal states of about 40% measuring points of the BUS are simultaneously monitored by the ITI, which provides accurate temperature distribution for the prediction of thermal deformations of the BUS.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"223 - 238"},"PeriodicalIF":3.0,"publicationDate":"2023-05-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4981005","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}

引用次数: 0

Radio astronomical images object detection and segmentation: a benchmark on deep learning methods 射电天文图像目标检测和分割:深度学习方法的基准

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-05-05 DOI: 10.1007/s10686-023-09893-w

Renato Sortino, Daniel Magro, Giuseppe Fiameni, Eva Sciacca, Simone Riggi, Andrea DeMarco, Concetto Spampinato, Andrew M. Hopkins, Filomena Bufano, Francesco Schillirò, Cristobal Bordiu, Carmelo Pino

{"title":"Radio astronomical images object detection and segmentation: a benchmark on deep learning methods","authors":"Renato Sortino, Daniel Magro, Giuseppe Fiameni, Eva Sciacca, Simone Riggi, Andrea DeMarco, Concetto Spampinato, Andrew M. Hopkins, Filomena Bufano, Francesco Schillirò, Cristobal Bordiu, Carmelo Pino","doi":"10.1007/s10686-023-09893-w","DOIUrl":"10.1007/s10686-023-09893-w","url":null,"abstract":"<div><p>In recent years, deep learning has been successfully applied in various scientific domains. Following these promising results and performances, it has recently also started being evaluated in the domain of radio astronomy. In particular, since radio astronomy is entering the Big Data era, with the advent of the largest telescope in the world - the Square Kilometre Array (SKA), the task of automatic object detection and instance segmentation is crucial for source finding and analysis. In this work, we explore the performance of the most affirmed deep learning approaches, applied to astronomical images obtained by radio interferometric instrumentation, to solve the task of automatic source detection. This is carried out by applying models designed to accomplish two different kinds of tasks: object detection and semantic segmentation. The goal is to provide an overview of existing techniques, in terms of prediction performance and computational efficiency, to scientists in the astrophysics community who would like to employ machine learning in their research.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"293 - 331"},"PeriodicalIF":3.0,"publicationDate":"2023-05-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4221746","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}

引用次数: 2

Study of solar flares and gamma-ray bursts using low-cost stratospheric balloon borne experiments 利用低成本平流层气球实验研究太阳耀斑和伽马射线暴

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-05-02 DOI: 10.1007/s10686-023-09899-4

Rupnath Sikdar, Sandip K. Chakrabarti, Debashis Bhowmick

引用次数: 0

Spectral performance of the Microchannel X-ray Telescope on board the SVOM mission SVOM任务上的微通道x射线望远镜的光谱性能

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-04-04 DOI: 10.1007/s10686-022-09886-1

B. Schneider, N. Renault-Tinacci, D. Götz, A. Meuris, P. Ferrando, V. Burwitz, E. Doumayrou, T. Lavanant, N. Meidinger, K. Mercier

{"title":"Spectral performance of the Microchannel X-ray Telescope on board the SVOM mission","authors":"B. Schneider, N. Renault-Tinacci, D. Götz, A. Meuris, P. Ferrando, V. Burwitz, E. Doumayrou, T. Lavanant, N. Meidinger, K. Mercier","doi":"10.1007/s10686-022-09886-1","DOIUrl":"10.1007/s10686-022-09886-1","url":null,"abstract":"<div><p>The Microchannel X-ray Telescope (MXT) is an innovative compact X-ray instrument on board the SVOM astronomical mission dedicated to the study of transient phenomena such as gamma-ray bursts. During 3 weeks, we have tested the MXT flight model at the Panter X-ray test facility under the nominal temperature and vacuum conditions that MXT will undergo in-flight. We collected data at series of characteristic energies probing the entire MXT energy range, from 0.28 keV up to 9 keV, for multiple source positions with the center of the point spread function (PSF) inside and outside the detector field of view (FOV). We stacked the data of the positions with the PSF outside the FOV to obtain a uniformly illuminated matrix and reduced all data sets using a dedicated pipeline. We determined the best spectral performance of MXT using an optimized data processing, especially for the energy calibration and the charge sharing effect induced by the pixel low energy thresholding. Our results demonstrate that MXT is compliant with the instrument requirement regarding the energy resolution (< 80 eV at 1.5 keV), the low and high energy threshold, and the accuracy of the energy calibration (± 20 eV). We also determined the charge transfer inefficiency (<span>(sim 10^{-5})</span>) of the detector and modeled its evolution with energy prior to the irradiation that MXT will undergo during its in-orbit lifetime. Finally, we measured the relation of the energy resolution as function of the photon energy. We determined an equivalent noise charge of <span>(4.9 pm 0.2 mathrm {e}^{-}_{text {rms}})</span> for the MXT detection chain and a Fano factor of 0.131 ± 0.003 in silicon at 208 K, in agreement with previous works. This campaign confirmed the promising scientific performance that MXT will be able to deliver during the mission lifetime.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"77 - 97"},"PeriodicalIF":3.0,"publicationDate":"2023-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4149135","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}

引用次数: 1

The Improved X-ray Detector (iXRD) on Sharjah-Sat-1, design principles, tests and ground calibration 沙迦- sat -1上的改进型x射线探测器(iXRD)，设计原理、测试和地面校准

IF 3 3区物理与天体物理

Experimental Astronomy Pub Date : 2023-03-08 DOI: 10.1007/s10686-023-09890-z

Emrah Kalemci, Ali M. Altıngün, Ayhan Bozkurt, Alim Rüstem Aslan, Refik Yalçın, Kaya Gökalp, Kaan Veziroğlu, Ilias Fernini, Antonios Manousakis, Ali Yaşar, Milad Diba, Boğaç Karabulut, Egemen Çatal, Onur Öztekin

{"title":"The Improved X-ray Detector (iXRD) on Sharjah-Sat-1, design principles, tests and ground calibration","authors":"Emrah Kalemci, Ali M. Altıngün, Ayhan Bozkurt, Alim Rüstem Aslan, Refik Yalçın, Kaya Gökalp, Kaan Veziroğlu, Ilias Fernini, Antonios Manousakis, Ali Yaşar, Milad Diba, Boğaç Karabulut, Egemen Çatal, Onur Öztekin","doi":"10.1007/s10686-023-09890-z","DOIUrl":"10.1007/s10686-023-09890-z","url":null,"abstract":"<div><p>The iXRD is the primary science payload on <i>Sharjah-Sat-1</i>, a 3U CubeSat expected to be launched in Q4, 2022. Its main scientific goal is monitoring bright hard X-ray sources and transients in 20 - 200 keV band. The iXRD consists of a CdZnTe crystal (6.45 cm<sup>2</sup> area, 5 mm thickness), a Tungsten collimator with square holes with an opening angle of 4.26<sup>∘</sup>, readout and control electronics and power supply circuitry, a back-shield and mechanical structures. Some of the design elements of iXRD have been inherited from the XRD on BeEagleSat with significant improvements in terms of collecting area, X-ray background and electronic noise. In this article, the design of the iXRD is discussed in detail taking into account mechanical, electronic, control software and data handling aspects. Its expected performance is determined after ground calibration. Depending on the pixel size, the energy resolution is 4 - 7 keV at 60 keV and the minimum detectable energy is 19 - 23 keV.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"99 - 116"},"PeriodicalIF":3.0,"publicationDate":"2023-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4352007","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}

引用次数: 1