Experimental Astronomy最新文献

{"title":"Receiver design for the REACH global 21-cm signal experiment","authors":"Ian L. V. Roque,&nbsp;Nima Razavi-Ghods,&nbsp;Steven H. Carey,&nbsp;John A. Ely,&nbsp;Will Handley,&nbsp;Alessio Magro,&nbsp;Riccardo Chiello,&nbsp;Tian Huang,&nbsp;P. Alexander,&nbsp;D. Anstey,&nbsp;G. Bernardi,&nbsp;H. T. J. Bevins,&nbsp;J. Cavillot,&nbsp;W. Croukamp,&nbsp;J. Cumner,&nbsp;E. de Lera Acedo,&nbsp;D. I. L. de Villiers,&nbsp;A. Fialkov,&nbsp;T. Gessey-Jones,&nbsp;Q. Gueuning,&nbsp;A. T. Josaitis,&nbsp;G. Kulkarni,&nbsp;S. A. K. Leeney,&nbsp;R. Maiolino,&nbsp;P. D. Meerburg,&nbsp;S. Mittal,&nbsp;M. Pagano,&nbsp;S. Pegwal,&nbsp;C. Pieterse,&nbsp;J. R. Pritchard,&nbsp;A. Saxena,&nbsp;K. H. Scheutwinkel,&nbsp;P. Scott,&nbsp;E. Shen,&nbsp;P. H. Sims,&nbsp;O. Smirnov,&nbsp;M. Spinelli,&nbsp;K. Zarb-Adami","doi":"10.1007/s10686-024-09975-3","DOIUrl":"10.1007/s10686-024-09975-3","url":null,"abstract":"<div><p>We detail the REACH radiometric system designed to enable measurements of the 21-cm neutral hydrogen line. Included is the radiometer architecture and end-to-end system simulations as well as a discussion of the challenges intrinsic to highly-calibratable system development. Following this, we share laboratory results based on the calculation of noise wave parameters utilising an over-constrained least squares approach. For five hours of integration on a custom-made source with comparable impedance to that of the antenna used in the field, we demonstrate a calibration RMSE of 80 mK. This paper therefore documents the state of the calibrator and data analysis in December 2022 in Cambridge before shipping to South Africa.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09975-3.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142994954","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":"Acoustic positioning for deep sea neutrino telescopes with a system of piezo sensors integrated into glass spheres","authors":"A. Albert,&nbsp;S. Alves,&nbsp;M. André,&nbsp;M. Ardid,&nbsp;S. Ardid,&nbsp;J.-J. Aubert,&nbsp;J. Aublin,&nbsp;B. Baret,&nbsp;S. Basa,&nbsp;Y. Becherini,&nbsp;B. Belhorma,&nbsp;M. Bendahman,&nbsp;F. Benfenati,&nbsp;V. Bertin,&nbsp;S. Biagi,&nbsp;J. Boumaaza,&nbsp;M. Bouta,&nbsp;M. C. Bouwhuis,&nbsp;H. Brânzaş,&nbsp;R. Bruijn,&nbsp;J. Brunner,&nbsp;J. Busto,&nbsp;B. Caiffi,&nbsp;D. Calvo,&nbsp;S. Campion,&nbsp;A. Capone,&nbsp;F. Carenini,&nbsp;J. Carr,&nbsp;V. Carretero,&nbsp;S. Celli,&nbsp;L. Cerisy,&nbsp;M. Chabab,&nbsp;R. Cherkaoui El Moursli,&nbsp;T. Chiarusi,&nbsp;M. Circella,&nbsp;J. A. B. Coelho,&nbsp;A. Coleiro,&nbsp;R. Coniglione,&nbsp;P. Coyle,&nbsp;A. Creusot,&nbsp;A. F. Díaz,&nbsp;B. De Martino,&nbsp;C. Distefano,&nbsp;I. Di Palma,&nbsp;C. Donzaud,&nbsp;D. Dornic,&nbsp;D. Drouhin,&nbsp;T. Eberl,&nbsp;A. Eddymaoui,&nbsp;T. van Eeden,&nbsp;D. van Eijk,&nbsp;S. El Hedri,&nbsp;N. El Khayati,&nbsp;A. Enzenhöfer,&nbsp;P. Fermani,&nbsp;G. Ferrara,&nbsp;F. Filippini,&nbsp;L. Fusco,&nbsp;S. Gagliardini,&nbsp;J. García,&nbsp;C. Gatius Oliver,&nbsp;P. Gay,&nbsp;N. Geißelbrecht,&nbsp;H. Glotin,&nbsp;R. Gozzini,&nbsp;R. Gracia Ruiz,&nbsp;K. Graf,&nbsp;C. Guidi,&nbsp;L. Haegel,&nbsp;H. van Haren,&nbsp;A. J. Heijboer,&nbsp;Y. Hello,&nbsp;L. Hennig,&nbsp;J. J. Hernández-Rey,&nbsp;J. Hößl,&nbsp;F. Huang,&nbsp;G. Illuminati,&nbsp;B. Jisse-Jung,&nbsp;M. de Jong,&nbsp;P. de Jong,&nbsp;M. Kadler,&nbsp;O. Kalekin,&nbsp;U. Katz,&nbsp;A. Kouchner,&nbsp;I. Kreykenbohm,&nbsp;V. Kulikovskiy,&nbsp;R. Lahmann,&nbsp;M. Lamoureux,&nbsp;A. Lazo,&nbsp;D. Lefèvre,&nbsp;E. Leonora,&nbsp;G. Levi,&nbsp;S. Le Stum,&nbsp;S. Loucatos,&nbsp;J. Manczak,&nbsp;M. Marcelin,&nbsp;A. Margiotta,&nbsp;A. Marinelli,&nbsp;J. A. Martínez-Mora,&nbsp;P. Migliozzi,&nbsp;A. Moussa,&nbsp;R. Muller,&nbsp;S. Navas,&nbsp;E. Nezri,&nbsp;B. Ó Fearraigh,&nbsp;E. Oukacha,&nbsp;A. Păun,&nbsp;G. E. Păvălaş,&nbsp;S. Peña-Martínez,&nbsp;M. Perrin-Terrin,&nbsp;P. Piattelli,&nbsp;C. Poirè,&nbsp;V. Popa,&nbsp;T. Pradier,&nbsp;N. Randazzo,&nbsp;D. Real,&nbsp;G. Riccobene,&nbsp;A. Romanov,&nbsp;A. Sánchez-Losa,&nbsp;A. Saina,&nbsp;F. Salesa Greus,&nbsp;D. F. E. Samtleben,&nbsp;M. Sanguineti,&nbsp;P. Sapienza,&nbsp;F. Schüssler,&nbsp;J. Seneca,&nbsp;M. Spurio,&nbsp;Th. Stolarczyk,&nbsp;M. Taiuti,&nbsp;Y. Tayalati,&nbsp;B. Vallage,&nbsp;G. Vannoye,&nbsp;V. Van Elewyck,&nbsp;S. Viola,&nbsp;D. Vivolo,&nbsp;J. Wilms,&nbsp;S. Zavatarelli,&nbsp;A. Zegarelli,&nbsp;J. D. Zornoza,&nbsp;J. Zúñiga","doi":"10.1007/s10686-024-09971-7","DOIUrl":"10.1007/s10686-024-09971-7","url":null,"abstract":"<div><p>Position calibration in the deep sea is typically done by means of acoustic multilateration using three or more acoustic emitters installed at known positions. Rather than using hydrophones as receivers that are exposed to the ambient pressure, the sound signals can be coupled to piezo ceramics glued to the inside of existing containers for electronics or measuring instruments of a deep sea infrastructure. The ANTARES neutrino telescope operated from 2006 until 2022 in the Mediterranean Sea at a depth exceeding <b>2000 m</b>. It comprised nearly 900 glass spheres with <b>432 mm</b> diameter and <b>15 mm</b> thickness, equipped with photomultiplier tubes to detect Cherenkov light from tracks of charged elementary particles. In an experimental setup within ANTARES, piezo sensors have been glued to the inside of such – otherwise empty – glass spheres. These sensors recorded signals from acoustic emitters with frequencies from <b>46545 to 60235 Hz</b>. Two waves propagating through the glass sphere are found as a result of the excitation by the waves in the water. These can be qualitatively associated with symmetric and asymmetric Lamb-like waves of zeroth order: a fast (early) one with <span>(varvec{v_e approx 5,{textbf {mm}}/mu text {s}})</span> and a slow (late) one with <span>(varvec{v_ell approx ,2,{textbf {mm}}/mu text {s}})</span>. Taking these findings into account improves the accuracy of the position calibration. The results can be transferred to the KM3NeT neutrino telescope, currently under construction at multiple sites in the Mediterranean Sea, for which the concept of piezo sensors glued to the inside of glass spheres has been adapted for monitoring the positions of the photomultiplier tubes.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2025-01-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09971-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142925539","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":"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":"https://doi.org/10.1007/s10686-025-09978-8","url":null,"abstract":"<p><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, <math> <msub><mrow><mo>[</mo> <mi>n</mi> <mi>σ</mi> <mo>]</mo></mrow> <mtext>h</mtext></msub> </math> , follows a linear relationship with the proton fluence, <math><msub><mi>F</mi> <mtext>p</mtext></msub> </math> , with a slope of <math> <mrow><mrow><mo>(</mo> <mn>5.4</mn> <mo>±</mo> <mn>0.4</mn> <mo>)</mo></mrow> <mo>×</mo> <msup><mn>10</mn> <mrow><mo>-</mo> <mn>11</mn></mrow> </msup> <mspace></mspace> <mrow><mi>cm</mi> <mo>/</mo> <msup><mi>p</mi> <mo>+</mo></msup> </mrow> </mrow> </math> . 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>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":"8"},"PeriodicalIF":2.7,"publicationDate":"2025-01-01","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}

{"title":"Ground testing and calibration of focal plane detector flight model on board the first pathfinder of CATCH","authors":"Panping Li,&nbsp;Kang Zhao,&nbsp;Xiangyang Wen,&nbsp;Zhengwei Li,&nbsp;Min Gao,&nbsp;Qian-Qing Yin,&nbsp;Lian Tao,&nbsp;Qingchang Zhao,&nbsp;Yusa Wang,&nbsp;Zijian Zhao,&nbsp;Shujie Zhao,&nbsp;Yiming Huang,&nbsp;Jingyu Xiao,&nbsp;Yifan Zhang,&nbsp;Bin Meng,&nbsp;Sheng Yang,&nbsp;Wen Chen,&nbsp;Heng Zhou,&nbsp;Yong Yang,&nbsp;Huilin He,&nbsp;Ruican Ma,&nbsp;Shuai Yang,&nbsp;Guoli Huang,&nbsp;YaJun Li,&nbsp;Jiewei Cao,&nbsp;Shu-Jin Hou,&nbsp;Xiaojing Liu,&nbsp;Jinzhou Wang,&nbsp;Liang Sun,&nbsp;Shuang-Nan Zhang,&nbsp;Shaolin Xiong,&nbsp;Xiang Ma,&nbsp;Yue Huang,&nbsp;Liming Song","doi":"10.1007/s10686-024-09966-4","DOIUrl":"10.1007/s10686-024-09966-4","url":null,"abstract":"<div><p><i>CATCH</i>-1, as the first satellite of Chasing All Transients Constellation Hunters (<i>CATCH</i>) space mission, was successfully launched into its expected orbit on June 22, 2024. The flight model underwent environmental tests before launch, including thermal cycling, thermal vacuum, and mechanical evaluations. The <i>CATCH</i>-1 detector system is equipped with a 4-pixel Silicon Drift Detector (SDD) array. To ensure the reliability and redundancy of the <i>CATCH</i>-1 detector system, two sets of data acquisition systems were independently designed and calibrated. Our focus is on presenting the ground calibration results of <i>CATCH</i>-1, which demonstrate a strong linear correlation between energy and channel. The main data acquisition system achieves an energy resolution of <span>(sim )</span> 120 eV@4 keV, while the backup data acquisition system has a slightly lower energy resolution of around 150 eV@4 keV, both meeting the design requirement of <span>(le )</span> 160 eV@4 keV. Additionally, the time resolution is <span>( sim 4,mu s)</span>, complying with the design requirement of <span>(le 10,mu s)</span>. The calibration database now includes the ground calibration results of <i>CATCH</i>-1, establishing a dependable basis for future data analysis. The development experience, calibration, and test results of this detector system will also provide a solid foundation for subsequent tasks such as <i>CATCH</i>-2.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-12-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142890485","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":"Study of Wind pattern at the incursion site of Pangong Tso near Merak Village","authors":"Belur Ravindra,&nbsp;Deepangkar Sarkar,&nbsp;Shantikumar Singh Ningombam,&nbsp;Stanzin Tundup,&nbsp;Namgyal Dorje,&nbsp;Angchuk Dorje,&nbsp;Prabhu Kesavan,&nbsp;Dipankar Banerjee","doi":"10.1007/s10686-024-09972-6","DOIUrl":"10.1007/s10686-024-09972-6","url":null,"abstract":"<div><p>This study analyzes twelve years of wind speed and direction data collected at the proposed National Large Solar Telescope (NLST) site near Pangong Tso, Merak village, Leh-Ladakh. A weather station from Campbell Scientific Instruments, installed in 2008, has been continuously monitoring meteorological parameters, including wind speed and direction. The data reveals a consistent pattern of predominantly northwest winds, particularly during morning hours, with speeds generally below 5 m/s. While seasonal variations influence wind speed and direction, the overall trend remains stable. To assess the site’s suitability for astronomical observations, we compared high-altitude wind speeds at various renowned astronomical sites using reanalysis data from 2008 to 2020. Strong correlations were observed between surface and high-altitude wind speeds at 10 m, 50 m, and 500 m. Statistical analysis of 200-mbar pressure level wind speeds identified La Palma as the most favorable site with a wind speed of 18.76 m/s. La Silla, on the other hand, exhibited the highest wind speed at 34.76 m/s. Merak’s estimated wind speed of 30.99 m/s, coupled with its favorable wind direction and low surface wind speeds, suggests its potential as a promising site for astronomical observations.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-12-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142875295","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":"Science filter characterization of the Solar Ultraviolet Imaging Telescope (SUIT) on board Aditya-L1.","authors":"Janmejoy Sarkar,&nbsp;Rushikesh Deogaonkar,&nbsp;Ravi Kesharwani,&nbsp;Sreejith Padinhatteeri,&nbsp;A. N. Ramaprakash,&nbsp;Durgesh Tripathi,&nbsp;Soumya Roy,&nbsp;Gazi A. Ahmed,&nbsp;Rwitika Chatterjee,&nbsp;Avyarthana Ghosh,&nbsp;Sankarasubramanian K.,&nbsp;Aafaque Khan,&nbsp;Nidhi Mehandiratta,&nbsp;Netra Pillai,&nbsp;Swapnil Singh","doi":"10.1007/s10686-024-09973-5","DOIUrl":"10.1007/s10686-024-09973-5","url":null,"abstract":"<div><p>The Solar Ultraviolet Imaging Telescope (<i>SUIT </i>) on board the Aditya-L1 mission is designed to observe the Sun across 200–400 nm wavelength. The telescope used 16 dichroic filters tuned at specific wavelengths in various combinations to achieve its science goals. For accurate measurements and interpretation, it is important to characterize these filters for spectral variations as a function of spatial location and tilt angle. Moreover, we also measured out-of-band and in-band transmission characteristics with respect to the inband transmissions. In this paper, we present the experimental setup, test methodology, and the analyzed results. Our findings reveal that the transmission properties of all filters meet the expected performance for spatial variation of transmission and the transmission band at a specific tilt angle. The out-of-band transmission for all filters is below 1% with respect to in-band, except for filters BB01 and NB01. These results confirm the capabilities of <i>SUIT </i>to effectively capture critical solar features in the anticipated layer of the solar atmosphere.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142844996","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":"Deep learning-based prediction approaches of binary star parameters","authors":"Islam Helmy,&nbsp;Mohamed Ismail,&nbsp;Doaa Eid","doi":"10.1007/s10686-024-09969-1","DOIUrl":"10.1007/s10686-024-09969-1","url":null,"abstract":"<div><p>The precise computation of binary star parameters is crucial for understanding their formation, evolution, and dynamics. However, large datasets of available astronomical measurements require substantial effort for computing using classic astronomical methods. Deep learning (DL) is a promising approach that can provide a proper solution for estimating the parameters and reducing the burden of the lengthy procedures of astronomical computations. This study proposes two DL-based models for estimating binary star parameters. The first is the well-known multi-layer perceptron (MLP) model, whereas the second is based on long short-term memory (LSTM). We rely on databases, such as large sky multi-object fiber spectroscopic telescope area (LAMOST), to train the proposed models. In addition, we verify the training ratio showing that the performance of both models at a low training ratio of <span>(30%)</span>, based on the mean square error (MSE), results in acceptable performance. Furthermore, the LSTM-based DL model outperforms the conventional MLP for different training ratios. Eventually, the two models have superiority compared to the benchmark methods.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09969-1.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142844997","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":"Preliminary design and development of the module back-end electronics for the large area detector onboard the eXTP mission","authors":"Hao Xiong,&nbsp;Jörg Bayer,&nbsp;Andrea Santangelo,&nbsp;Marco Feroci,&nbsp;Ettore Del Monte,&nbsp;Alejandro Guzman,&nbsp;Paul Hedderman,&nbsp;Gabriele Minervini,&nbsp;Samuel Pliego,&nbsp;Andreas Putz,&nbsp;Chris Tenzer,&nbsp;Alessio Trois,&nbsp;Xianqi Wang","doi":"10.1007/s10686-024-09974-4","DOIUrl":"10.1007/s10686-024-09974-4","url":null,"abstract":"<div><p>The Large Area Detector (LAD) is one of the science payloads of the enhanced X-ray Timing and Polarimetry (eXTP) mission. The LAD is a spectral-timing instrument with a broad energy response, covering a range from 2 to 30 keV, a good timing resolution of better than 10 µs, and an expected energy resolution of 260 eV at 6 keV. The LAD consists of 640 large-area multi-anode Silicon Drift Detectors (SDDs). Given the large number of detectors, the LAD uses a modular design. Each module comprises sixteen detectors, and each detector is equipped with dedicated Front-End Electronics (FEE), interfacing with two separate Module Back-End Electronics (MBEEs). Each MBEE is designed to process the data from 1,792 anode channels in 8 FEEs (224 anode channels per FEE), performing the energy reconstruction and time tagging for X-ray events. The MBEE uses the European Field Programmable Gate Array (FPGA) from NanoXplore™, based on a pipeline concept, which reduces dead time, making the LAD suitable for higher flux X-ray detection, and it can handle a sustained flux of &gt;500 mCrab and a continuous flux of &gt;15 Crab for up to 300 minutes (Feroci et al. 2018). Additionally, the MBEE serves as the central hub for configuring the module’s electronics, including the FEEs, the Power Supply Unit (PSU), and the MBEE itself, and it is also responsible for collecting housekeeping data to monitor the system’s status. The prototype MBEE was designed, manufactured, and programmed with FPGA firmware using VHDL. The basic functional test was conducted in this paper, and the results indicated that the MBEE could be operated in different modes to perform the functions mentioned above. Analysis and testing show that it can transmit event packets-containing timing tag, event type, position ID, and energy information-at a baud rate of 2 Mbps with an event loss fraction of 1.5%.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"59 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09974-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142826423","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":"Galaxy formation and symbiotic evolution with the inter-galactic medium in the age of ELT-ANDES","authors":"Valentina D’Odorico,&nbsp;James S. Bolton,&nbsp;Lise Christensen,&nbsp;Annalisa De Cia,&nbsp;Erik Zackrisson,&nbsp;Aron Kordt,&nbsp;Luca Izzo,&nbsp;Jiangtao Li,&nbsp;Roberto Maiolino,&nbsp;Alessandro Marconi,&nbsp;Philipp Richter,&nbsp;Andrea Saccardi,&nbsp;Stefania Salvadori,&nbsp;Irene Vanni,&nbsp;Chiara Feruglio,&nbsp;Michele Fumagalli,&nbsp;Johan P. U. Fynbo,&nbsp;Pasquier Noterdaeme,&nbsp;Polychronis Papaderos,&nbsp;Céline Péroux,&nbsp;Aprajita Verma,&nbsp;Paolo Di Marcantonio,&nbsp;Livia Origlia,&nbsp;Alessio Zanutta","doi":"10.1007/s10686-024-09967-3","DOIUrl":"10.1007/s10686-024-09967-3","url":null,"abstract":"<div><p>High-resolution absorption spectroscopy toward bright background sources has had a paramount role in understanding early galaxy formation, the evolution of the intergalactic medium and the reionisation of the Universe. However, these studies are now approaching the boundaries of what can be achieved at ground-based 8-10m class telescopes. The identification of primeval systems at the highest redshifts, within the reionisation epoch and even into the dark ages, and of the products of the first generation of stars and the chemical enrichment of the early Universe, requires observing very faint targets with a signal-to-noise ratio high enough to detect very weak spectral signatures. In this paper, we describe the giant leap forward that will be enabled by ANDES, the high-resolution spectrograph for the ELT, in these key science fields, together with a brief, non-exhaustive overview of other extragalactic research topics that will be pursued by this instrument, and its synergistic use with other facilities that will become available in the early 2030s.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"58 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142798437","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":"High strehl and high contrast for the ELT instrument METIS","authors":"Markus Feldt,&nbsp;Thomas Bertram,&nbsp;Carlos Correia,&nbsp;Olivier Absil,&nbsp;M. Concepción Cárdenas Vázquez,&nbsp;Hugo Coppejans,&nbsp;Martin Kulas,&nbsp;Andreas Obereder,&nbsp;Gilles Orban de Xivry,&nbsp;Silvia Scheithauer,&nbsp;Horst Steuer","doi":"10.1007/s10686-024-09968-2","DOIUrl":"10.1007/s10686-024-09968-2","url":null,"abstract":"<div><p>The Mid-infrared ELT Imager and Spectrograph (METIS) is a first-generation instrument for the Extremely Large Telescope (ELT), Europe’s next-generation 39 m ground-based telescope for optical and infrared wavelengths, which is currently under construction at the European Southern Observatory (ESO) site at Cerro Armazones in Chile. METIS will offer diffraction-limited imaging, low- and medium-resolution slit spectroscopy, and coronagraphy for high-contrast imaging between 3 and 13 microns, as well as high-resolution integral field spectroscopy between 3 and 5 microns. The main METIS science goals are the detection and characterisation of exoplanets, the investigation of proto-planetary disks, and the formation of planets. The Single-Conjugate Adaptive Optics (SCAO) system corrects atmospheric distortions and is thus essential for diffraction-limited observations with METIS. SCAO will be used for all observing modes, with high-contrast imaging imposing the most demanding requirements on its performance. The Final Design Review (FDR) of METIS took place in the fall of 2022; the development of the instrument, including its SCAO system, has since entered the Manufacturing, Assembly, Integration and Testing (MAIT) phase. Numerous challenging aspects of an ELT Adaptive Optics (AO) system are addressed in the mature designs for the SCAO control system and the SCAO hardware module: the complex interaction with the telescope entities that participate in the AO control, wavefront reconstruction with a fragmented and moving pupil, secondary control tasks to deal with differential image motion, non-common path aberrations and mis-registration. A <i>K</i>-band pyramid wavefront sensor and a GPU-based Real-Time Computer (RTC), tailored to the needs of METIS at the ELT, are core components. This current paper serves as a natural sequel to our previous work presented in Hippler et al. (2018). It reflects all the updates that were implemented between the Preliminary Design Review (PDR) and FDR, and includes updated performance estimations in terms of several key performance indicators, including achieved contrast curves. We outline all important design decisions that were taken, and present the major challenges we faced and the main analyses carried out to arrive at these decisions and eventually the final design. We also elaborate on our testing and verification strategy, and, last not least, comprehensively present the full design, hardware and software in this paper to provide a single source of reference which will remain valid at least until commissioning.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"58 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-11-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09968-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142736970","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}