Experimental Astronomy最新文献_第2页

A new method for identifying contaminating sources and locating target sources through the cross-arm features of micro pore optics 一种利用微孔光学交叉臂特征识别污染源和定位目标源的新方法

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2026-03-24 DOI: 10.1007/s10686-026-10046-y

Yiming Huang, Lian Tao, Jin-Yuan Liao, Shuang-Nan Zhang, Stéphane Schanne, Bertrand Cordier, Shaolin Xiong, Juan Zhang, Zhengwei Li, Qian-Qing Yin, Xiangyang Wen, Sheng Yang, Min Gao, Donghua Zhao, Xiang Ma, Yue Huang, Liang Zhang, Liming Song

{"title":"A new method for identifying contaminating sources and locating target sources through the cross-arm features of micro pore optics","authors":"Yiming Huang, Lian Tao, Jin-Yuan Liao, Shuang-Nan Zhang, Stéphane Schanne, Bertrand Cordier, Shaolin Xiong, Juan Zhang, Zhengwei Li, Qian-Qing Yin, Xiangyang Wen, Sheng Yang, Min Gao, Donghua Zhao, Xiang Ma, Yue Huang, Liang Zhang, Liming Song","doi":"10.1007/s10686-026-10046-y","DOIUrl":"10.1007/s10686-026-10046-y","url":null,"abstract":"<div>\u0000 \u0000 <p>The Pathfinder of the Type-A satellites in the Chasing All Transients Constellation Hunters (CATCH) space mission is equipped with Micro-Pore Optics (MPOs) and four single-pixel Silicon Drift Detectors (SDDs). Due to the lack of position resolution in an individual SDD, we propose a new method based on the cross-arms in the point spread function (PSF) of MPOs to enhance the satellite’s capability in identifying contaminating sources and locating target sources. By placing one detector on each of the horizontal and vertical cross-arms on the focal plane, we can use the changes in the relative counts on the cross-arms detectors to deduce the location of the source. Simulated observations demonstrate that, for a target source with a flux of 1 Crab and an exposure time of 200 s, the cross-arms detectors can identify contaminating source with the same flux level at an off-axis angle larger than <span>({8'})</span>, and improve positioning accuracy to <span>({6'})</span>. Furthermore, we extend the simulation study to CATCH Type-A, which plans to use an SDD array. In situations where sources exhibit the same flux of 1 Crab and the exposure time is merely 1 s, a 16<span>(times)</span>16 SDD array is capable of identifying contaminating source with an off-axis angle greater than <span>({2.4'})</span> and can achieve a positioning precision of <span>({1.8'})</span>.</p>\u0000 </div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 2","pages":""},"PeriodicalIF":2.2,"publicationDate":"2026-03-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147560788","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

A 5kHz modulator for pyramid wavefront sensors 用于金字塔波前传感器的5kHz调制器

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2026-03-16 DOI: 10.1007/s10686-026-10044-0

Maximilian Häberle, Vianak Naranjo, Yared Reinarz, Markus Feldt, Silvia Scheithauer, Thomas Bertram, Arne Bramigk, Harry Marth

{"title":"A 5kHz modulator for pyramid wavefront sensors","authors":"Maximilian Häberle, Vianak Naranjo, Yared Reinarz, Markus Feldt, Silvia Scheithauer, Thomas Bertram, Arne Bramigk, Harry Marth","doi":"10.1007/s10686-026-10044-0","DOIUrl":"10.1007/s10686-026-10044-0","url":null,"abstract":"<div>\u0000 \u0000 <p>Despite the emergence of new types of wavefront sensors, the modulated pyramid wavefront sensor remains the workhorse for ELT instrumentation, and is among the options even for advanced high-contrast, high-Strehl instrumentation like PCS and SAXO+. To achieve the required degree of wavefront control, an operation at frequencies of 3kHz, ideally up to 5kHz, is necessary, requiring an optomechanical device capable of delivering accurate circular modulation patterns with these frequencies. Here, we present tests of a novel type of high-frequency modulator based on shearing piezo actuators. The modulator prototype moves a flat circular mirror (15mm diameter) with a tip-tilt range of plus/minus 50 arcsec. At a typical 10mm pupil diameter on the modulator mirror, and operating at 2.2 µm, this will create a modulation circle with a radius of slightly greater than 2<span>(lambda )</span>/D. While this is less than conventionally specified for most instruments, it should already be sufficient for any practical application except for very bad conditions or extended targets. We performed modulation tests at frequencies between 250 Hz to 5 kHz using a test setup including a modulated laser beam probed with a high-speed camera. The prototype showed stable behaviour during a one-hour-long operation at a maximum frequency of 5 kHz and with negligible heat generation. The maximum modulation amplitude was 60 arcsec. We observed very accurate reproduction of the input modulation pattern with typical ellipticities less than 1% and random deviations below 0.2% for frequencies below 4.5 kHz. These tests demonstrate the prototype’s capabilities and could be followed by on-sky tests or the integration of the modulator into XAO testbeds.</p>\u0000 </div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 2","pages":""},"PeriodicalIF":2.2,"publicationDate":"2026-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-026-10044-0.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147559440","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

Design and performance of the coded mask for the Lunar Electromagnetic Monitor in X-rays (LEM-X) 月球x射线电磁监测仪（LEM-X）编码掩模的设计与性能

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2026-03-16 DOI: 10.1007/s10686-026-10047-x

Yuri Evangelista, Alessio Nuti, Francesco Ceraudo, Edoardo Giancarli, Giuseppe Dilillo, Riccardo Campana, Giovanni Della Casa, Ettore Del Monte, Marco Feroci, Mauro Fiorini, Giovanni Lombardi, Massimo Rapisarda, Francesca Esposito, Immacolata Donnarumma, Alessandro Turchi, Ugo Cortesi, Fabio D’Amico, Marco Gai, Andrea Argan

{"title":"Design and performance of the coded mask for the Lunar Electromagnetic Monitor in X-rays (LEM-X)","authors":"Yuri Evangelista, Alessio Nuti, Francesco Ceraudo, Edoardo Giancarli, Giuseppe Dilillo, Riccardo Campana, Giovanni Della Casa, Ettore Del Monte, Marco Feroci, Mauro Fiorini, Giovanni Lombardi, Massimo Rapisarda, Francesca Esposito, Immacolata Donnarumma, Alessandro Turchi, Ugo Cortesi, Fabio D’Amico, Marco Gai, Andrea Argan","doi":"10.1007/s10686-026-10047-x","DOIUrl":"10.1007/s10686-026-10047-x","url":null,"abstract":"<div>\u0000 \u0000 <p>The Lunar Electromagnetic Monitor in X-rays (LEM-X) is a proposed wide-field X-ray observatory designed for deployment on the Moon’s surface. Its primary scientific goal is to enhance multi-messenger astrophysics by detecting, localizing, and monitoring high-energy transient phenomena and variable X-ray sources across the sky. Building on the heritage of the eXTP and LOFT mission proposals, LEM-X employs pairs of coded-aperture cameras equipped with large-area linear Silicon Drift Detectors (SDDs), offering excellent spectral resolution (<span>(le )</span>350 eV at 6 keV) over the 2–50 keV energy range. Each camera provides a field of view of <span>(sim )</span>1 steradian at 25% effective area and achieves a Point-Source Location Accuracy (PSLA) of <span>(sim )</span>1 arcminute, with an on-axis sensitivity better than 5 mCrab in 50 ks and <span>(sim )</span>700 mCrab in 1 s. In this paper we describe the experiment and focus on the detailed design and optimization of the LEM-X coded mask, analyzing its scientific performance, imaging capabilities, and thermo-mechanical properties. We describe the mask code generation, decoding algorithms, and the trade-offs involved in achieving the required angular resolution, sensitivity, and structural integrity. Imaging simulations and mechanical analyses confirm the effectiveness of the proposed design, demonstrating its suitability for high-precision, wide-field X-ray imaging devoted to multi-messenger astrophysics and transient events detection.</p>\u0000 </div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 2","pages":""},"PeriodicalIF":2.2,"publicationDate":"2026-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-026-10047-x.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147559749","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

First demonstration of super-resolution with a single-aperture radio telescope 首次用单口径射电望远镜展示超分辨率

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2026-03-11 DOI: 10.1007/s10686-025-10041-9

Luca Olmi, Carlo Migoni, Matteo Murgia, Renzo Nesti, Sergio Poppi

{"title":"First demonstration of super-resolution with a single-aperture radio telescope","authors":"Luca Olmi, Carlo Migoni, Matteo Murgia, Renzo Nesti, Sergio Poppi","doi":"10.1007/s10686-025-10041-9","DOIUrl":"10.1007/s10686-025-10041-9","url":null,"abstract":"<div>\u0000 \u0000 <p>In this paper we report the first successful demonstration of angular super-resolution (SR) obtained with a single-aperture radio telescope observing in the microwave K-band. Despite the potential scientific applications, in the past few decades little efforts have been devoted to the development of SR imaging techniques for Astronomy, while most of the technological improvement has concentrated on focal plane instrumentation. In recent years, some complex and ambitious techniques have been proposed to achieve SR with astronomical telescopes, but none of these techniques has gone beyond the stage of basic principles or could be used as a real SR imaging method. Variable-transmittance pupils, and specifically Toraldo Pupils (TPs), represent one viable approach to achieving SR in radio astronomy. In this work we show that by exploiting the active surface of the Sardinia Radio Telescope (SRT) to emulate a TP at the entrance pupil of the telescope it is indeed possible to achieve a main beam narrower than that expected by diffraction. The reduction in the width of the main beam is achieved at the expense of a lower antenna efficiency and higher sidelobes. We have also used the resulting SR beam to map an astronomical source and we show that we are able to recover some of the compact structure not visible using the nominal diffraction-limited telescope beam. Once the method will be adequately tested and optimized, it will provide the telescope users with a new observing option, promising to expand the scientific capabilities of the SRT.</p>\u0000 </div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 2","pages":""},"PeriodicalIF":2.2,"publicationDate":"2026-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-10041-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147388622","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

EMC design for 110 m radio telescope RFSoC systems: hierarchical radiation quantification, waveguide-optimized shielding, and thermo-mechanical co-design 110米射电望远镜RFSoC系统的电磁兼容设计：分层辐射量化、波导优化屏蔽和热-机械协同设计

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2026-01-13 DOI: 10.1007/s10686-025-10042-8

Yao Zeng, Rong Li, Ziyue Wang, Qi Liu, Wei Wang, Min Kong, Yunyu Chen, Yuhao Fei, Juyong Zhang

{"title":"EMC design for 110 m radio telescope RFSoC systems: hierarchical radiation quantification, waveguide-optimized shielding, and thermo-mechanical co-design","authors":"Yao Zeng, Rong Li, Ziyue Wang, Qi Liu, Wei Wang, Min Kong, Yunyu Chen, Yuhao Fei, Juyong Zhang","doi":"10.1007/s10686-025-10042-8","DOIUrl":"10.1007/s10686-025-10042-8","url":null,"abstract":"<div><p>This study presents a multi-physics co-design framework addressing electromagnetic-thermal coupling challenges in radio frequency system-on-chip (RFSoC) modules for the 110 m QiTai radio Telescope (QTT). A hierarchical electromagnetic assessment methodology combining near-field scanning (2.4 ~ 40 GHz) and signature separation algorithms enables precise identification of nine dominant radiation sources at the component level, while board-level power loading analysis establishes a 70dB shielding effectiveness (SE) requirement for stable operation. The proposed electromagnetic-topology-optimized detachable shielding enclosure integrates nonlinear strain-compensated conductive elastomers (<i>σ</i> = 1.8 × 10³ S/m, ε<sub>max</sub> = 150%) and waveguide-embedded multi-mode optical interfaces (λ = 850/1310nm), achieving > 70dB SE with maintained optical communication integrity (BER < 10⁻¹²). Concurrent DELPHI-derived thermal network optimization results in a unified shielding-cooling architecture, reducing the maximum junction temperature from 84.1 °C to 40.0 ± 0.5 °C under 35 W/cm² power density through enhanced heat flux paths. Anechoic chamber measurements validate the frequency-dependent SE degradation mechanism of optical-fiber-embedded waveguides, confirming compliance with IEC 61000-4-21 Class A standards. The framework systematically resolves shielding-communication trade-offs and thermal accumulation constraints in high-density RFSoCs, providing a scalable paradigm for next-generation radio telescope electronics operating in extreme observational environments.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 1","pages":""},"PeriodicalIF":2.2,"publicationDate":"2026-01-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145982714","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

White Rabbit in radio interferometry 无线电干涉测量中的白兔

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2026-01-03 DOI: 10.1007/s10686-025-10038-4

E. Paul Boven, Jeroen C. J. Koelemeij, Chantal van Tour, Rob Smets, Rodrigo González Escudero, Huib Jan van Langevelde

{"title":"White Rabbit in radio interferometry","authors":"E. Paul Boven, Jeroen C. J. Koelemeij, Chantal van Tour, Rob Smets, Rodrigo González Escudero, Huib Jan van Langevelde","doi":"10.1007/s10686-025-10038-4","DOIUrl":"10.1007/s10686-025-10038-4","url":null,"abstract":"<div><p>Radio interferometry relies on distributed telescopes having precise time and frequency sources that allow them to operate coherently over timescales up to several hours. As radio telescopes are being connected to fiber-based high-speed communication networks, it is of interest to make use of these for time and frequency distribution. The White Rabbit protocol enables the accurate and precise distribution of time and frequency signals over telecommunication optical fibers. We set out to evaluate the quantitative limits for interferometers over a range of observing frequencies when synchronized through White Rabbit. We develop a method to quantify the possible loss of sensitivity due to the phase noise contribution of a White Rabbit link. Our findings include a new expression for the coherence loss due to flicker phase noise. As this type of noise is common in frequency transfer links, its use extends beyond the case of White Rabbit. Furthermore, we designed a calibration procedure to measure the dispersion on already deployed fiber networks. We demonstrate adding a White Rabbit signal to an existing high-speed production network, together with data traffic on other wavelengths on the same fiber. Finally we built a VLBI setup with fiber links of 35 and 169 km, connecting two radio telescopes together. The agreement between our predicted and measured coherence loss indicates the usefulness of our approach, and that White Rabbit is suitable for clock distribution in radio interferometry instruments. We find that regular White Rabbit v3 switches support observing frequencies up to 3.5 GHz, and their low-jitter version up to 15 GHz.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 1","pages":""},"PeriodicalIF":2.2,"publicationDate":"2026-01-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-10038-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145886884","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

Frequency and spatial-channel cross transformer for lightweight astronomical image super-resolution 用于轻型天文图像超分辨率的频率和空间通道交叉变压器

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2025-12-26 DOI: 10.1007/s10686-025-10040-w

Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao, Zhengpeng Li, Kunyang Wu

{"title":"Frequency and spatial-channel cross transformer for lightweight astronomical image super-resolution","authors":"Jiawei Miao, Liangping Tu, Hao Liu, Jian Zhao, Zhengpeng Li, Kunyang Wu","doi":"10.1007/s10686-025-10040-w","DOIUrl":"10.1007/s10686-025-10040-w","url":null,"abstract":"<div><p>With the advancement of astronomy, the demand for high-resolution astronomical images has become increasingly urgent. However, the imaging of ground-based telescopes is often affected by factors such as hardware limitations, atmospheric turbulence, and noise, thereby limiting the execution of high-precision scientific tasks. Moreover, due to the scarcity of paired high- and low-resolution observations, directly training super-resolution models on real data remains a significant challenge. Therefore, we construct a synthetic dataset, GalaxySR-DS, by simulating the degradation process using DownSampleGAN (DSGAN). In addition, we propose a lightweight super-resolution (SR) model, Frequency and Spatial-Channel Cross Transformer (FSCFormer). It combines the Frequency Transformation Module (FTB) and the Spatial-Channel Cross Transformation Module (SCCTB), and has complementary advantages in modeling high-frequency details and maintaining the global structure, thereby improving the reconstruction quality. We select ten representative lightweight SR models as baselines for comparison. Experimental results show that the FSCFormer model achieves an average PSNR improvement of 0.02-0.85 dB while maintaining lower computational cost. This study offers an effective approach for the high-precision analysis of astronomical observation data. In particular, under constrained observational resources, it maximizes the scientific value of existing data and promotes a paradigm shift in observational astronomy research. The code will be available at https://github.com/jiaweimmiao/FSCFormer.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 1","pages":""},"PeriodicalIF":2.2,"publicationDate":"2025-12-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145831522","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

Cosmic ray detection on resolved galaxies with deep learning 利用深度学习对已分辨星系进行宇宙射线探测

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2025-12-23 DOI: 10.1007/s10686-025-10039-3

Shoulin Wei, Junxi Tao, Xiaoli Zhang, Wei Dai, Bo Liang

{"title":"Cosmic ray detection on resolved galaxies with deep learning","authors":"Shoulin Wei, Junxi Tao, Xiaoli Zhang, Wei Dai, Bo Liang","doi":"10.1007/s10686-025-10039-3","DOIUrl":"10.1007/s10686-025-10039-3","url":null,"abstract":"<div>\u0000 \u0000 <p>High-energy charged particles in cosmic ray (CR) generate anomalous signals or noise artifacts when colliding with astronomical detectors, introducing distortions in both imaging and spectral data. This phenomenon poses a significant challenge in differentiating celestial signatures from cosmic ray-induced artifacts, particularly during observation scenarios involving resolved galaxies. In this study, we propose a deep learning framework that integrates the multi-scale attention mechanism and dynamic adaptive loss function for CR detection. The multi-scale linear attention mechanism is adopted to achieve a synergistic perception of global context modelling and local texture features in resolved galaxies. The large kernel selection block is used to effectively extend the capture range of global dependence of CR structures. The efficient multi-scale attention block is introduced to further enhance the texture differentiation between CR and celestial fringes of resolved galaxies. Furthermore, a dynamic weighted loss function based on a Gaussian residual response is introduced, with the aim of adjusting the negative sample gradient weights through statistical analysis of background noise patterns adaptively. This approach significantly improves model performance in class-imbalanced CR detection tasks. Experimental results demonstrate that the proposed model achieves consistent performance improvements on enhancements in CR detection for resolved galaxies.</p>\u0000 </div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"61 1","pages":""},"PeriodicalIF":2.2,"publicationDate":"2025-12-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145802398","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

Design of a two-lens telephoto collimator for CMAG coronagraph CMAG日冕仪双镜头远摄准直器设计

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2025-11-25 DOI: 10.1007/s10686-025-10037-5

Javier Sánchez Barranquero, Francisco J. Bailén, David Orozco Suárez

{"title":"Design of a two-lens telephoto collimator for CMAG coronagraph","authors":"Javier Sánchez Barranquero, Francisco J. Bailén, David Orozco Suárez","doi":"10.1007/s10686-025-10037-5","DOIUrl":"10.1007/s10686-025-10037-5","url":null,"abstract":"<div><p>Solar coronagraphs often include narrowband filters located at an image of the telescope pupil. These filters are commonly illuminated with collimated light coming from an intermediate telecentric image of the corona. In this configuration, the intermediate image is located at the front focal plane of a collimator, while the telescope pupil is formed at its back focal plane. Collimators employed to illuminate the filter have long focal lengths and usually need to be designed as telephoto lenses for the purpose of minimizing the distance from the intermediate image to the pupil. This is particularly important for spaceborne instruments, whose dimensions are strictly constrained. However, conventional telephoto lenses cannot be employed in this case as they unavoidably increase the front-to-back focal length of the system. Reducing the number of optical elements in coronagraphs is also essential to minimize stray light and ghost images. In this work, we derive the equations for two-component telephoto lenses needed to minimize the front-to-back focal distance. We apply these equations to design a collimator for CMAG coronagraph. We study the image quality as a function of the telephoto ratio, we athermalize our design and we carry out a tolerance analysis. We demonstrate that the front-to-back focal length can be reduced by <span>(textbf{45},mathbf {%})</span> for a field of view as large as 1.28° while keeping the root mean square wavefront error below <span>(varvec{lambda /20})</span>.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"60 3","pages":""},"PeriodicalIF":2.2,"publicationDate":"2025-11-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-10037-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145612798","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

Super-resolution-enabled atmospheric tomography for astronomical multi-wavefront-sensor adaptive-optics systems 天文多波前传感器自适应光学系统的超分辨率大气层析成像

IF 2.2 3区物理与天体物理

Experimental Astronomy Pub Date : 2025-11-21 DOI: 10.1007/s10686-025-10021-z

Carlos M. Correia, Pierre Jouve, Jesse Cranney, Guido Agapito, Cédric Taïssir Heritier

{"title":"Super-resolution-enabled atmospheric tomography for astronomical multi-wavefront-sensor adaptive-optics systems","authors":"Carlos M. Correia, Pierre Jouve, Jesse Cranney, Guido Agapito, Cédric Taïssir Heritier","doi":"10.1007/s10686-025-10021-z","DOIUrl":"10.1007/s10686-025-10021-z","url":null,"abstract":"<div><p>Recent work by Oberti et al, (<i>Astron. Astrophys.</i>, <i>667</i>, 48, 2022) argued and made a compelling case that classical astronomical adaptive optics (AO) tomography performance can be further enhanced by carefully designing and optically configuring the system to leverage inherent super-resolution (SR) capabilities. Our goal here is to further materialise the concept by providing the means to compute SR-enabling tomographic reconstructors for AO and showcase its broad uptake on soon every 10 m-class VIS/NIR telescopes and Giant Segmented Mirror Telescopes of up to 40 m in diameter. To that end we indicate the necessary tomography generalisations where we: <i>(i)</i> clarify how <i>model-and-deploy</i> is a generic methodological umbrella for linear minimum-mean-squared-error (LMMSE) tomographic reconstructors arising naturally from the solution of the tomographic inverse problem, thus unifying various solutions presented as distinct in the literature within a single framework, <i>(ii)</i> recall how such solutions are found as limiting cases of a model-based optimal control problem, thus elucidating how <i>pseudo-open-loop control</i> is a feature of the latter that allows LMMSE reconstructors to be adapted to closed-loop systems, <i>(iii)</i> review the two forms of the LMMSE tomographic reconstructors, highlighting the necessary adaptations to accommodate super-resolution, <i>(iv)</i> review the implementation in either dense-format vector-matrix-multiplication or sparse iterative forms and <i>(v)</i> discuss the implications for runtime and off-line real-time implementations, anticipating widespread adoption. We illustrate our examples with physical-optics numerical simulations for 10 m and 40 m-scale systems showing the performance benefits of super-resolution in the order of several tens of nm rms and the computational burden associated.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"60 3","pages":""},"PeriodicalIF":2.2,"publicationDate":"2025-11-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-025-10021-z.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145561656","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