{"title":"Mission analysis, design and operations plan of India’s first polarimetry satellite: X-ray Polarimetry Satellite (XPoSat)","authors":"Himani Saini, K. V. Madhu, Ritu Karidhal","doi":"10.1007/s10686-025-09988-6","DOIUrl":"10.1007/s10686-025-09988-6","url":null,"abstract":"<div><p><b>X</b>-ray <b>Po</b>larimeter <b>Sat</b>ellite (XPoSat) is India’s first landmark mission dedicated to X-ray polarimetry, with the aim of measuring and studying X-rays emitted by bright astronomical objects such as black hole X-ray binaries, pulsar wind nebulae, and accretion-powered pulsars. Polar Satellite Launch Vehicle-C58 (PSLV-C58) launched the XPoSat mission on 1st January 2024, equipped with two significant, scientific instruments: XSPECT (X-ray Spectroscopy and Timing) and POLIX (POLarimeter Instrument in X-rays). With the launch of XPoSat, a new and important fourth dimension of polarization has been added. POLIX became the first in the world to provide measurements of polarization in <b>8–30</b> kilo electron Volt (keV) energy band. XSPECT is a spectroscopy payload responsible for providing timing and spectral information in 0.8–15 keV energy band of X-ray emissions from about 54 potential identified cosmic X-ray sources. Astronomical sources emitting X-rays are sites of strong gravity, and strong magnetic fields and have a variety of geometries for scattering, which are expected to give rise to polarization signatures in these sources. This article provides a comprehensive overview from mission specifications to mission design, mission planning, mission analysis, and mission operations aspects of spacecraft configuration, operations, and on-orbit operations of XPoSat mission with the science brought by the first-time flown payload in high energy bands, which will allow astronomers to explore materials under intense magnetic and gravitational fields. The challenges involved in planning and executing the mission operations with critical scenarios have also been highlighted.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143489496","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}
Guofu Liao, Congzhan Liu, Zhengwei Li, Daikang Yan, Xiangxiang Ren, Yongjie Zhang, Laiyu Zhang, Yu Xu, Shibo Shu, He Gao, Yifei Zhang, Xuefeng Lu, Xufang Li, He Xu, Di Wu
{"title":"The Sliding Flux Ramp Demodulation algorithm with high sampling rate in Microwave SQUID Multiplexer","authors":"Guofu Liao, Congzhan Liu, Zhengwei Li, Daikang Yan, Xiangxiang Ren, Yongjie Zhang, Laiyu Zhang, Yu Xu, Shibo Shu, He Gao, Yifei Zhang, Xuefeng Lu, Xufang Li, He Xu, Di Wu","doi":"10.1007/s10686-025-09986-8","DOIUrl":"10.1007/s10686-025-09986-8","url":null,"abstract":"<div><p>Microwave SQUID Multiplexing (<span>(mu )</span>MUX) is a widely used technique in the low-temperature detectors community as it offers a high capacity for reading large-scale Transition-Edge Sensor (TES) arrays. This paper proposes a Sliding Flux Ramp Demodulation (SFRD) algorithm for <span>(mu )</span>MUX readout system. It can achieve a sampling rate in the order of MHz while maintaining a multiplexing ratio of about one thousand. Advancing of this large array readout technique makes it possible to observe scientific objects with improved time resolution and event count rate. This will be highly helpful for TES calorimeters in X-ray applications, such as X-ray astrophysics missions.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423113","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}
Jiang He, Jian-Chao Sun, Yong-Wei Dong, Bo-Bing Wu, Shi-Jie Zheng, Lu Li, Jiang-Tao Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, Rui-Jie Wang, Juan Zhang, Li Zhang, Shuang-Nan Zhang, Xiao-Yun Zhao, Xing-Guang Liu
{"title":"SVOM-GRM trigger performance study and verification","authors":"Jiang He, Jian-Chao Sun, Yong-Wei Dong, Bo-Bing Wu, Shi-Jie Zheng, Lu Li, Jiang-Tao Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, Rui-Jie Wang, Juan Zhang, Li Zhang, Shuang-Nan Zhang, Xiao-Yun Zhao, Xing-Guang Liu","doi":"10.1007/s10686-025-09983-x","DOIUrl":"10.1007/s10686-025-09983-x","url":null,"abstract":"<div><p>The Space-based multi-band astronomical Variable Objects Monitor (SVOM) is a collaborative satellite developed by China and France, specifically designed for observing and studying Gamma-Ray Bursts (GRBs) as well as other variable sources. Among its four on-board payloads, the Gamma-Ray Monitor (GRM) is responsible for detecting high-energy photons ranging from 15 keV to 5 MeV, equipped with real-time triggering and localization capabilities. In this paper, we primarily focus on investigating the triggering performance of GRM. Firstly, the energy response matrix of each detector is obtained by using the Geant4 simulation toolkit. Based on the results of background simulations and given samples of GRB, the instrument’s sensitivity and the detection efficiency to GRBs from different directions are estimated. The results demonstrate that GRM exhibits superior sensitivity to GRBs with harder energy spectrum, enabling more than <span>(80%)</span> of the GRBs to be triggered within its field of view. By considering satellite orbit and attitude, we conduct a 3-year simulation of GRB observations which reveals that approximately 106 GRBs can be detected annually in the energy range of 50-300 keV by GRM. Moreover, it is observed that optimal triggering energy range correlates with the hardness index values of the GRBs. Finally, we discuss the on-orbit triggering algorithm that has been implemented by GRM along with developing a ground-based multi-timescale search algorithm for identifying potential GRB events. Our work contributes to understanding the on-orbit triggering performance characteristics demonstrated by GRM, while also providing a benchmark for refining ground-based strategies focused on detecting new instances of GRBs, thus amplifying the scientific output obtained from utilizing GRM’s capabilities.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143361647","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":"A multi-fidelity transfer learning strategy for surface deformation measurement of large reflector antennas","authors":"Zihan Zhang, Qian Ye, Na Wang, Guoxiang Meng","doi":"10.1007/s10686-025-09980-0","DOIUrl":"10.1007/s10686-025-09980-0","url":null,"abstract":"<div><p>As the observation frequency of large-aperture antennas increases, the requirements for measuring main reflector deformation have become more stringent. Recently, the rapid development of deep learning has led to its application in antenna deformation prediction. However, achieving high accuracy requires a large number of high-fidelity deformation samples, which is often challenging to obtain. To address these problems, this paper establishes a high-accuracy antenna surface deformation measurement model based on a multi-fidelity transfer learning neural network (MF-TLNN). Firstly, a low-fidelity surrogate model is constructed using a large number of simulation deformation samples to ensure its robustness. Secondly, the MF-TLNN structure is designed and trained using a small number of high-fidelity samples obtained from actual measurements of the main reflector deformation via out-of-focus (OOF) holography method. Thirdly, a Zernike correction module is utilized to provide additional constraints and ensure the stability of the results. Experimental results show that the proposed method can closely approximate radio holography measurements in terms of accuracy and is almost real-time in terms of speed.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143361942","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}
M. Anzorena, E. de la Fuente, K. Fujita, R. Garcia, K. Goto, Y. Hayashi, K. Hibino, N. Hotta, G. Imaizumi, A. Jimenez-Meza, Y. Katayose, C. Kato, S. Kato, T. Kawashima, K. Kawata, T. Koi, H. Kojima, T. Makishima, Y. Masuda, S. Matsuhashi, M. Matsumoto, R. Mayta, P. Miranda, A. Mizuno, K. Munakata, Y. Nakamura, M. Nishizawa, Y. Noguchi, S. Ogio, M. Ohnishi, S. Okukawa, A. Oshima, M. Raljevic, H. Rivera, T. Saito, T. Sako, T. K. Sako, T. Shibasaki, S. Shibata, A. Shiomi, M. Subieta, F. Sugimoto, N. Tajima, W. Takano, M. Takita, Y. Tameda, K. Tanaka, R. Ticona, I. Toledano-Juarez, H. Tsuchiya, Y. Tsunesada, S. Udo, R. Usui, G. Yamagishi, K. Yamazaki, Y. Yokoe
{"title":"(gamma )/hadron discrimination by analysis of the muon lateral distribution and the ALPAQUITA array","authors":"M. Anzorena, E. de la Fuente, K. Fujita, R. Garcia, K. Goto, Y. Hayashi, K. Hibino, N. Hotta, G. Imaizumi, A. Jimenez-Meza, Y. Katayose, C. Kato, S. Kato, T. Kawashima, K. Kawata, T. Koi, H. Kojima, T. Makishima, Y. Masuda, S. Matsuhashi, M. Matsumoto, R. Mayta, P. Miranda, A. Mizuno, K. Munakata, Y. Nakamura, M. Nishizawa, Y. Noguchi, S. Ogio, M. Ohnishi, S. Okukawa, A. Oshima, M. Raljevic, H. Rivera, T. Saito, T. Sako, T. K. Sako, T. Shibasaki, S. Shibata, A. Shiomi, M. Subieta, F. Sugimoto, N. Tajima, W. Takano, M. Takita, Y. Tameda, K. Tanaka, R. Ticona, I. Toledano-Juarez, H. Tsuchiya, Y. Tsunesada, S. Udo, R. Usui, G. Yamagishi, K. Yamazaki, Y. Yokoe","doi":"10.1007/s10686-025-09981-z","DOIUrl":"10.1007/s10686-025-09981-z","url":null,"abstract":"<div><p>A new method using the muon lateral distribution and an underground muon detector to achieve high discrimination power against hadrons is presented. The method is designed to be applied in the Andes Large-area PArticle detector for Cosmic-ray physics and Astronomy (ALPACA) experiment in Bolivia. This new observatory in the Southern hemisphere has the goal of detecting >100 TeV <span>(gamma )</span> rays in search for the origins of Galactic cosmic rays. The method uses the weighted sum of the lateral distribution of the muons detected by underground detectors to separate between air showers initiated by cosmic rays and <span>(gamma )</span> rays. We evaluate the performance of the method through Monte Carlo simulations with CORSIKA and Geant4 and apply the analysis to the prototype of ALPACA, ALPAQUITA. With the application of this method in ALPAQUITA, we achieve an improvement of about 18 % in the energy range from 60 to 100 TeV over the estimated sensitivity using only the total number of muons.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-09981-z.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143107878","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}
A. Mkrtchyan, A. Pozanenko, P. Minaev, A. Strizhak, A. Ivashkin, A. Baranov, S. Musin
{"title":"Calibration of segmented BGO scintillation detectors for space-based gamma-ray polarimeter","authors":"A. Mkrtchyan, A. Pozanenko, P. Minaev, A. Strizhak, A. Ivashkin, A. Baranov, S. Musin","doi":"10.1007/s10686-025-09977-9","DOIUrl":"10.1007/s10686-025-09977-9","url":null,"abstract":"<div><p>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 <span>(^{22}text {Na})</span>. Also, for comparison, a simulation of the registration of linear polarization was carried out using the Geant4 software package. The experimental results agree withing <span>(2sigma )</span> of simulations.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143108133","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}
Fatin Abrar Shams, Abdullah Al Mahmud Nafiz, Md. Salman Mohosheu, Maheen Mashrur Hoque, Samiur Rashid Abir, Rashed Hasan Ratul, Md. Mushfiqur Rahman Mushfique, Aftab Ibn Nazim, Rubaiat Rehman Khan, Md Mahmudunnobe, Mohsinul Kabir
{"title":"Asteroid family classification with machine learning: Investigative analysis of a novel two-step approach for categorizing known small asteroid families⋆","authors":"Fatin Abrar Shams, Abdullah Al Mahmud Nafiz, Md. Salman Mohosheu, Maheen Mashrur Hoque, Samiur Rashid Abir, Rashed Hasan Ratul, Md. Mushfiqur Rahman Mushfique, Aftab Ibn Nazim, Rubaiat Rehman Khan, Md Mahmudunnobe, Mohsinul Kabir","doi":"10.1007/s10686-025-09982-y","DOIUrl":"10.1007/s10686-025-09982-y","url":null,"abstract":"<div><p>The term “asteroid family” refers to a collection of asteroids that share similar proper orbital elements such as semi-major axis, eccentricities, and orbital inclinations. Detecting small asteroid families has proved to be a challenge for a long time because of their extremely low sample size. In general, standalone machine learning classifiers tend to exhibit a bias towards classes with larger sample sizes, resulting in the inadequate classification of asteroid families with limited data. In this paper, a two-step supervised model was proposed for the effective classification of the asteroid families, especially for the tiny, small, and lower groups of medium asteroid families. The proposed model uses two-step classification in an attempt to resolve the challenges that come with the imbalanced dataset where at first a binary classification of small and large families was done with an XGB (Extreme Gradient boosting) classifier and then in the second stage Random Forest classifier was used alongside previously identified binary features to classify asteroid families. The proposed model performed better with higher F1 scores for tiny and small asteroid families compared to other algorithms tested in this work. It also achieved a perfect F1 score for 90 families, among 112 families which were tested. As for the lower group of medium sized asteroid families, it performed slightly worse compared to the previously used machine learning algorithms. Along with this, four dataset imbalance handling techniques have been employed in this work and compared to the proposed algorithm.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-01-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143110091","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":"TARA: Concept study for an ESA Voyage Titan exploration mission","authors":"Brahma Gopalchetty, Andrew J. Coates","doi":"10.1007/s10686-025-09979-7","DOIUrl":"10.1007/s10686-025-09979-7","url":null,"abstract":"<div><p>As a study relevant to the ESA’s “Voyage 2050” programme, we present an ambitious L-class mission concept aimed at exploring one of the most intriguing bodies in the Solar System – Titan, Saturn’s largest moon. Titan is a planet-like moon rich in organic compounds and features complex interactions between its interior, surface, and atmosphere, similar to those seen on Earth. Additionally, Titan is one of the few places in the Solar System with the highest potential for eventual habitability. Despite the groundbreaking discoveries made by the Cassini-Huygens mission, Titan still holds many mysteries that demand further exploration using more advanced technologies and diverse exploration vehicles. Our proposed mission, named TARA (Titan Atmospheric Research Ascendant), aims to conduct both orbital and in situ investigations of Titan, surpassing the scientific and technological achievements of Cassini-Huygens. TARA would provide comprehensive and close-up exploration of Titan over extended periods, utilizing capabilities that were previously unattainable. The mission architecture consists of two primary components: an orbiter equipped with an extensive suite of instruments that would orbit Titan, ideally in a low-eccentricity circular polar orbit, and an ornithopter equipped with a set of in situ exploration elements, both aimed to study Titan’s atmospheric dynamics and the evolution of pre-biotic environment. The ideal mission timeline would target an arrival at Titan just before its next northern Spring equinox in 2039, a period of heightened activity for observing Titan’s still poorly understood seasonal atmospheric and surface changes. TARA’s focus on Titan’s northern latitudes would complement NASA’s upcoming Dragonfly mission, which is scheduled to explore Titan’s equatorial regions in the mid-2030s. Together, these missions would provide comprehensive temporal, spatial, and scientific coverage of this fascinating moon.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-01-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143110046","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}
Sean N. Pike, Steven E. Boggs, Gabriel Brewster, Sophia E. Haight, Jarred M. Roberts, Albert Y. Shih, Joanna Szornel, John A. Tomsick, Andreas Zoglauer
{"title":"Characterizing hole trap production due to proton irradiation in germanium cross-strip detectors","authors":"Sean N. Pike, Steven E. Boggs, Gabriel Brewster, Sophia E. Haight, Jarred M. Roberts, Albert Y. Shih, Joanna Szornel, John A. Tomsick, Andreas Zoglauer","doi":"10.1007/s10686-025-09978-8","DOIUrl":"10.1007/s10686-025-09978-8","url":null,"abstract":"<div><p>We present an investigation into the effects of high-energy proton damage on charge trapping in germanium cross-strip detectors with the goal of accomplishing three important measurements. First, we calibrated and characterized the spectral resolution of a spare COSI-balloon detector in order to determine the effects of intrinsic trapping, finding that electron trapping due to impurities dominates over hole trapping in the undamaged detector. Second, we performed two rounds of proton irradiation of the detector in order to quantify, for the first time, the rate at which charge traps are produced by proton irradiation. We find that the product of the hole trap density and cross-sectional area, <span>([nsigma ]_textrm{h})</span>, follows a linear relationship with the proton fluence, <span>(F_textrm{p})</span>, with a slope of <span>((5.4pm 0.4)times 10^{-11},mathrm {cm/p^{+}})</span>. Third, by utilizing our measurements of physical trapping parameters, we performed calibrations which corrected for the effects of trapping and mitigated degradation to the spectral resolution of the detector.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC11757935/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143045335","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}
Lorenzo V. Mugnai, Andrea Bocchieri, Enzo Pascale, Andrea Lorenzani, Andreas Papageorgiou
{"title":"ExoSim 2: the new exoplanet observation simulator applied to the Ariel space mission","authors":"Lorenzo V. Mugnai, Andrea Bocchieri, Enzo Pascale, Andrea Lorenzani, Andreas Papageorgiou","doi":"10.1007/s10686-024-09976-2","DOIUrl":"10.1007/s10686-024-09976-2","url":null,"abstract":"<div><p>ExoSim 2 is the next generation of the Exoplanet Observation Simulator (ExoSim) tailored for spectro-photometric observations of transiting exoplanets from space, ground, and sub-orbital platforms. This software is a complete rewrite implemented in Python 3, embracing object-oriented design principles, which allow users to replace each component with their functions when required. ExoSim 2 is publicly available on GitHub, serving as a valuable resource for the scientific community. ExoSim 2 employs a modular architecture using Task classes, encapsulating simulation algorithms and functions. This flexible design facilitates the extensibility and adaptability of ExoSim 2 to diverse instrument configurations to address the evolving needs of the scientific community. Data management within ExoSim 2 is handled by the Signal class, which represents a structured data cube incorporating time, space, and spectral dimensions. The code execution in ExoSim 2 follows a three-step workflow: the creation of focal planes, the production of Sub-Exposure blocks, and the generation of non-destructive reads (NDRs). Each step can be executed independently, optimizing time and computational resources. ExoSim 2 has been extensively validated against other tools like ArielRad and has demonstrated consistency in estimating photon conversion efficiency, saturation time, and signal generation. The simulator has also been validated independently for instantaneous read-out and jitter simulation, and for astronomical signal representation. In conclusion, ExoSim 2 offers a robust and flexible tool for exoplanet observation simulation, capable of adapting to diverse instrument configurations and evolving scientific needs. Its design principles and validation results underscore its potential as a valuable resource in the field of exoplanet research.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09976-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143109101","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}
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