Astronomical Telescopes + Instrumentation最新文献_第9页

Blazed reflection gratings with electron-beam lithography and ion-beam etching 用电子束光刻和离子束蚀刻的燃烧反射光栅

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2637880

D. Miles, R. McEntaffer, F. Grisé

引用次数: 0

UV photocathodes for space detectors 空间探测器用紫外光电阴极

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2630747

J. Milnes, P. Hink, S. Harada, E. Urbain, Ashley Thomson, T. Conneely, J. Lapington

{"title":"UV photocathodes for space detectors","authors":"J. Milnes, P. Hink, S. Harada, E. Urbain, Ashley Thomson, T. Conneely, J. Lapington","doi":"10.1117/12.2630747","DOIUrl":"https://doi.org/10.1117/12.2630747","url":null,"abstract":"Vacuum photodetectors have a long history in ultraviolet (UV) sensing for both astronomy and remote sensing. One of the main advantages of this technology is the ability to use solar blind photocathodes to enable high sensitivity measurements of astronomical and atmospheric sources of Far UV (FUV) and Deep UV (DUV) emission in environments with high visible light (VIS) backgrounds. The use of microchannel plates (MCP) in vacuum photodetectors also allows single photon sensitivity for extremely weak signals. However, these detectors have typically suffered from lower Quantum Efficiency (QE) than their solid-state alternatives. Recent advances in photocathode technology have resulted in significant increases in QE for several UV sensitive photocathodes. We present test results of next generation high QE photocathodes appropriate for use in a wide range of FUV and DUV astronomy and remote sensing. A newly developed opaque Cesium Iodide (CsI) photocathode deposited on microchannel plates and sealed into vacuum photodetectors with a Magnesium Fluoride (MgF2) input window demonstrates QE of < 16% @ 130 nm. An optimized transmission mode solar blind (SB) alkali-telluride photocathode demonstrates 29% peak QE and 103 to 108 suppression of NUV and visible light, a significant improvement over previous alkali-telluride photocathodes. Finally, we present data from a new high QE S20 alkali-antimonide photocathode with < 40% QE at 254 nm, suitable for instruments requiring wideband DUV through VIS coverage. Improvements in collection efficiency of vacuum photodetector MCPs from 60% to 90% will also be presented, providing a further 50% boost to detective QE.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"67 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128921493","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

5.3 THz MgB2 hot electron bolometer mixer operated at 20 K 5.3在20k下工作的THz MgB2热电子测热计混频器

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2630161

J. Gao, Y. Gan, B. Mirzaei, J. Silva, S. Cherednichenko

{"title":"5.3 THz MgB2 hot electron bolometer mixer operated at 20 K","authors":"J. Gao, Y. Gan, B. Mirzaei, J. Silva, S. Cherednichenko","doi":"10.1117/12.2630161","DOIUrl":"https://doi.org/10.1117/12.2630161","url":null,"abstract":"Heterodyne receivers combining a NbN HEB mixer with a local oscillator (LO) are the work horse for high resolution ( ≥106 ) spectroscopic observations at supra-terahertz frequencies. We report an MgB2 HEB mixer working at 5.3 THz with 20 K operation temperature based on a previously published paper [Y. Gan et al, Appl. Phys. Lett., 119, 202601 (2021)]. The HEB consists of a 7 nm thick MgB2 submicron-bridge contacted with a spiral antenna. It has a Tc of 38.4 K. By using hot/cold blackbody loads and a Mylar beam splitter all in vacuum, and applying a 5.25 THz FIR gas laser as the LO, we measured a minimal DSB receiver noise temperature of 3960 K. The latter gives a DSB mixer noise temperature of 1470 K. This sensitivity is 28 times better than a room temperature Schottky mixer at 4.7 THz, but about 2.5 times less sensitive than an NbN HEB mixer. The latter must be operated around 4 K. The IF noise bandwidth is about 10 GHz, which is 2.5-3 times larger than an NbN HEB. With further optimization, such MgB2 HEBs are expected to reach a better sensitivity. That the low noise, wide IF bandwidth MgB2 HEB mixers can be operated in a compact, low dissipation 20 K Stirling cooler can significantly reduce the cost and complexity of heterodyne instruments and therefore facilitate new space missions.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"365 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"129047628","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 1

Design and testing of the structure of the eXTP optics eXTP光学元件结构的设计与测试

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2629781

Z. Song, J. Ma, J. Wang, A. Zhang, Y. Wang, Y. J. Yang, W. Jiang, Y. Chen, K. Yu, S. Yang, Y. Xu, H. He, F. Lu, S. Zhang, S. Basso, M. Civitani, G. Pareschi, G. Sironi, D. Spiga, V. Cotroneo, G. Tagliaferri, L. Sheng, Y. Q. Yan, P. Qiang, B. Zhao

{"title":"Design and testing of the structure of the eXTP optics","authors":"Z. Song, J. Ma, J. Wang, A. Zhang, Y. Wang, Y. J. Yang, W. Jiang, Y. Chen, K. Yu, S. Yang, Y. Xu, H. He, F. Lu, S. Zhang, S. Basso, M. Civitani, G. Pareschi, G. Sironi, D. Spiga, V. Cotroneo, G. Tagliaferri, L. Sheng, Y. Q. Yan, P. Qiang, B. Zhao","doi":"10.1117/12.2629781","DOIUrl":"https://doi.org/10.1117/12.2629781","url":null,"abstract":"The abbreviation “eXTP” represents the enhanced x-ray timing and polarimetry, which is a key science mission initiated by the Chinese scientists, designed to study the state of matter under extreme conditions of density, gravity and magnetism [1]. Various payloads would be on board of the satellite. The SFA, namely the spectroscopy focusing array, consisting of nine identical x-ray telescopes working in the energy range of 0.5-10 keV, will be the focus here [1]. SFA has a field-of-view of 12 arcmin for each and a collecting area of 900 cm2 and 550 cm2 for each at 2 keV and 6 keV respectively [1]. This paper starts with a brief introduction of the general optics, and then goes across some important design aspects. It covers contents from the structural and thermal designs to the CAE analyses as well as the current status. The large diameter and huge focal length of the optics will definitely bring big issues to the robustness of the carrying structure under the severe conditions given by the launcher. According to the current design, the mirror assembly will have 3 feet and 24 spokes. Vibration tests were already performed on a few prototypes by IHEP, and a preliminary evaluation on the feasibility of the design has been achieved. It clearly stated that the current design with only a single spider can probably survive the vibration tests assuming a compromised test condition somewhere. CAE models were adjusted thereafter to match the test results, which could be used for further assessments in a near future. Of course, there are always uncertainties associated with our arguments. More detailed prototypes with mechanically fully representative shells were still under design. Hopefully, highly reliable results could be retrieved soon.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"89 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115650578","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Gal/Xgal U/LDB Spectroscopic/Stratospheric THz Observatory: GUSTO Gal/Xgal U/LDB光谱/平流层太赫兹天文台:GUSTO

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2629051

C. Walker, C. Kulesa, A. Young, W. Verts, Jianxun Gao, Qing Hu, Jose R. G. Silva, B. Mirzaei, W. Laauwen, J. Hesler, C. Groppi, A. Emrich

{"title":"Gal/Xgal U/LDB Spectroscopic/Stratospheric THz Observatory: GUSTO","authors":"C. Walker, C. Kulesa, A. Young, W. Verts, Jianxun Gao, Qing Hu, Jose R. G. Silva, B. Mirzaei, W. Laauwen, J. Hesler, C. Groppi, A. Emrich","doi":"10.1117/12.2629051","DOIUrl":"https://doi.org/10.1117/12.2629051","url":null,"abstract":"Gal/Xgal U/LDB Spectroscopic/ Stratospheric THz Observatory (GUSTO) is a NASA Explorers Mission of Opportunity that will make large scale maps of the Milky Way and Large Magellanic Cloud in three important interstellar lines: [CII], [OI], and [NII] at 158, 63, and 205 µm, respectively. During its ~75 day stratospheric (~36 km) flight, GUSTO’s 0.9-meter balloon-borne telescope and THz heterodyne array receivers will provide the spectral and spatial resolution needed to untangle the complexities of the interstellar medium by probing all phases of its Life Cycle. The GUSTO payload consists of (1) a telescope; (2) three 8-pixel heterodyne array receivers; (3) autocorrelator spectrometers; (4) instrument control electronics; and (5) a cryostat. The GUSTO gondola is derived from successful APL designs. Much of the GUSTO instrument architecture and hardware is based on the experience gained in developing and flying the Stratospheric Terahertz Observatory (STO). GUSTO is currently undergoing integration and test and will launch from the NASA Long Duration Balloon (LDB) Facility near McMurdo, Antarctica in December 2023.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121102512","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 7

Optimization and experimental measurements of high impedance niobium-silicon (NbSi) transition edge sensors (TES) for high spectral and spatial resolution x-ray space-borne telescopes 用于高光谱和空间分辨率x射线星载望远镜的高阻抗铌硅(NbSi)过渡边缘传感器(TES)的优化和实验测量

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2630758

Benjamin Criton, J. Sauvageot, X. de la Broïse, S. Marnieros, C. Oriol, L. Bergé

{"title":"Optimization and experimental measurements of high impedance niobium-silicon (NbSi) transition edge sensors (TES) for high spectral and spatial resolution x-ray space-borne telescopes","authors":"Benjamin Criton, J. Sauvageot, X. de la Broïse, S. Marnieros, C. Oriol, L. Bergé","doi":"10.1117/12.2630758","DOIUrl":"https://doi.org/10.1117/12.2630758","url":null,"abstract":"Space-borne x-ray observations of supernova remnants, galactic clusters, x-ray binaries, and black holes are key elements in determining the structure of the universe. Astronomers require wide field of view with high spatial resolution but also very high spectral resolution to determine the physical conditions (temperatures, element abundances) with great accuracy. Today’s technologies (mostly TESs) obtain very high spectral resolutions to the detriment of power consumption, mostly due to their cold stage SQUID readout electronics. Their high power consumption limits the instrument’s field of view (FoV) by constraining the total number of pixels affordable at the 50 mK focal plane of a satellite cryostat. We use a new alloy technology: the high resistivity NbSi, enabling us to design TES sensors promising high spectral resolution and ultra low power consumption (below 10 pW). Their high impedance allows the use of a transistor readout at a hotter stage of the cryostat. This, in conjunction with the inherent ultra-low power dissipation of the sensors, raises drastically the number of pixels of the detector. In this article, we explore pixel optimization ways based on our electro-thermal model to reach spectral resolution of the order of 1.8 eV. We then use this model to manufacture a new batch of pixels on which we conduct experimental measurements. We measure the transient response, energy linearity and noise spectrum of our pixels with an Iron 55 source as well as an innovative on-chip pulse injection system. A low noise cryogenic amplifier as well as a cryogenic experimental setup have been designed to perform these measurements.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"162 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115757473","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A robust, efficient process to produce scalable, superconducting kilopixel far-IR detector arrays 一个强大的，有效的过程，以生产可扩展的，超导千像素远红外探测器阵列

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2629584

J. Staguhn, E. Sharp, S. Duff, G. Hilton, Ari D. Brown, F. Colazo, N. Costen, S. Moseley, Frederick H. Wang, Edward J. Wollack, Sang Yoon

{"title":"A robust, efficient process to produce scalable, superconducting kilopixel far-IR detector arrays","authors":"J. Staguhn, E. Sharp, S. Duff, G. Hilton, Ari D. Brown, F. Colazo, N. Costen, S. Moseley, Frederick H. Wang, Edward J. Wollack, Sang Yoon","doi":"10.1117/12.2629584","DOIUrl":"https://doi.org/10.1117/12.2629584","url":null,"abstract":"Robust, high sensitivity kilopixel format arrays with large focal plane filling factors and low cosmic ray cross sections that operate over the entire far-IR regime are required for future NASA missions, such as Origins and a future far-IR Probe. Our kilopixel Backshort Under Grid (BUG) detectors are designed to meet all those requirements: By bump-bonding two-dimensional detector arrays to readout multiplexers are gaplessly tileable in one spatial direction with the integration of the multiplexer scalable beyond wafer sizes. The detector arrays provide high filling factors (<90% at 1mm pixel pitch) and are designed for low Cosmic ray cross sections. The major missing technology is a detector array architecture that can be gaplessly tiled to deliver the desired pixel counts of npixel ~105, while being providing a robust process to produce these detector arrays. We introduce a new array architecture that is very flexible allowing for a variety of tileable solutions and describe its individual components and the tests of those. Our results demonstrate that this architecture allows for flexible designs with high yields and reliable superconducting bump-bond connections of detectors and the cold readout SQUID multiplexers directly under the detector array, or on a different board that can be connected with e.g. flex lines for compact tiling.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"99 3 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121055003","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

ATHENA optics technology development 雅典娜光学技术的发展

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2629894

M. Bavdaz, E. Wille, M. Ayre, I. Ferreira, B. Shortt, S. Fransen, M. Millinger, M. Collon, G. Vacanti, N. Barrière, B. Landgraf, M. Olde Riekerink, J. Haneveld, R. Start, C. van Baren, D. Della Monica Ferreira, S. Massahi, S. Svendsen, F. Christensen, M. Krumrey, E. Handick, V. Burwitz, G. Pareschi, B. Salmaso, A. Moretti, D. Spiga, G. Valsecchi, D. Vernani, Paul Lupton, William Mundon, G. Phillips, J. Schneider, T. Korhonen, A. Sánchez, D. Heinis, C. Colldelram, M. Tordi, S. de Lorenzi, R. Willingale

{"title":"ATHENA optics technology development","authors":"M. Bavdaz, E. Wille, M. Ayre, I. Ferreira, B. Shortt, S. Fransen, M. Millinger, M. Collon, G. Vacanti, N. Barrière, B. Landgraf, M. Olde Riekerink, J. Haneveld, R. Start, C. van Baren, D. Della Monica Ferreira, S. Massahi, S. Svendsen, F. Christensen, M. Krumrey, E. Handick, V. Burwitz, G. Pareschi, B. Salmaso, A. Moretti, D. Spiga, G. Valsecchi, D. Vernani, Paul Lupton, William Mundon, G. Phillips, J. Schneider, T. Korhonen, A. Sánchez, D. Heinis, C. Colldelram, M. Tordi, S. de Lorenzi, R. Willingale","doi":"10.1117/12.2629894","DOIUrl":"https://doi.org/10.1117/12.2629894","url":null,"abstract":"The next generation x-ray observatory ATHENA (advanced telescope for high energy astrophysics) requires an optics with unprecedented performance. It is the combination of low mass, large effective area and good angular resolution that is the challenge of the x-ray optics of such a mission. ATHENA is the second large class mission in the science programme of ESA, and is currently in a reformulation process, following a design-to-cost approach to meet the cost limit of an ESA L-class mission. The silicon pore optics (SPO) is the mission enabler being specifically developed for ATHENA, in a joint effort by industry, research institutions and ESA. All aspects of the optics are being addressed, from the mirror plates and their coatings, over the mirror modules and their assembly into the ATHENA telescope, to the facilities required to build and test the flight optics, demonstrating performance, robustness, and programmatic compliance. The SPO technology is currently being matured to the level required for the adoption of the ATHENA mission, i.e., the start of the mission implementation phase. The monocrystalline silicon material and pore structure of the SPO provide these optics with excellent thermal and mechanical properties. Benefiting from technology spin-in from the semiconductor industry, the equipment, processes, and materials used to produce the SPO are highly sophisticated and optimised.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134198097","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 10

Hardware development of Athena WFI frame processing module 雅典娜WFI帧处理模块的硬件开发

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2627846

J. Reiffers, Sebastian Albrecht, O. Hälker, Andreas Lederhuber, B. Mican, Francisco-Javier Veredas

{"title":"Hardware development of Athena WFI frame processing module","authors":"J. Reiffers, Sebastian Albrecht, O. Hälker, Andreas Lederhuber, B. Mican, Francisco-Javier Veredas","doi":"10.1117/12.2627846","DOIUrl":"https://doi.org/10.1117/12.2627846","url":null,"abstract":"The wide field imager (WFI) is one of the two focal plane instruments on-board the Athena x-ray astronomy mission, the second large-class mission of the European Space Agency. Athena is planned to be launched in 2034 and will be stationed in Lagrange point L1, from where it will perform observations in the x-ray spectrum, from 0.2 keV to 15 keV. The frame processing module (FPM) is part of the detector electronics (DE) of the Athena WFI, which has the main task of reading out the WFI detector array, digitizing it, performing real-time frame processing, and event extraction, using offset correction and threshold maps. The high number of 512×512 pixels on each large detector (LD), the fast readout cycle (5 ms) and the complex sequence of digital signals required to read out the WFI detectors present some stringent design requirements on the electronics used in the FPM as well as on the programmable logic implemented in the selected field programmable gate array (FPGA). This paper describes the hardware design of the FPM and the preliminary engineering model that has already been manufactured. Given the criticality of the FPM, this early development model already includes most of the flight-like electronics based on state-of-the-art radiation hard ADCs, FPGAs and SSRAM memories. Specific design challenges are addressed related to the electronic implementation of the FPM, which already fulfils most of the design rules according the ECSS standards.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"513 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133600177","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 2

Time distribution on the Athena WFI 雅典娜WFI的时间分布

Astronomical Telescopes + Instrumentation Pub Date : 2022-08-31 DOI: 10.1117/12.2627938

Francisco-Javier Veredas, S. Albrecht, D. Coutinho, Andreas Lederhuber, J. Reiffers

{"title":"Time distribution on the Athena WFI","authors":"Francisco-Javier Veredas, S. Albrecht, D. Coutinho, Andreas Lederhuber, J. Reiffers","doi":"10.1117/12.2627938","DOIUrl":"https://doi.org/10.1117/12.2627938","url":null,"abstract":"The wide field imager (WFI) is one of two instruments of the x-ray advanced telescope for high-energy astrophysics (Athena) mission selected by ESA. The WFI instrument uses a camera with a DEPFET sensor, Detector electronics (DE) to control the camera, and additional electronics units to communicate with the spacecraft on-board-computer (OBC). The spacecraft event time (SCET) is generated on the OBC and synchronized with ground. The SCET timing synchronization between the OBC and the sensor photon detection presents particular challenges. The science user requirement of the absolute knowledge error of the WFI time stamp relative to the OBC clock is 5 µs with a confidence level of 99.73%. In this paper, we present the WFI timing distribution implementation. The three main contributors of the timing distribution are: (1) time delays and jitter between OBC and DE, (2) internal delays of the DE, and (3) delay between a photon capture and the time stamping in the DE. The first contributor is the most critical and two solving methods are identified. The first method uses only the timecode of the SpaceWire (SpW) communication network, and the second method uses a combination of pulse-per-second (PPS) signal and SpW network. SpW network standard was published in 2003 and few missions such as ESA solar orbiter use it exclusively for time distribution. In our analysis, we found that using the second method with a PPS signal, delays contribution is in order of nanoseconds.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"11 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132997406","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 1