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}
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}
D. Henke, F. Jiang, S. Salem Hesari, A. Seyfollahi, B. Veidt, L. Knee
{"title":"Octave bandwidth receiver technology for radio and millimetre-wave telescopes","authors":"D. Henke, F. Jiang, S. Salem Hesari, A. Seyfollahi, B. Veidt, L. Knee","doi":"10.1117/12.2630537","DOIUrl":"https://doi.org/10.1117/12.2630537","url":null,"abstract":"In radio astronomy instrumentation, the benefit of increased spectral grasp must be evaluated against a decrease in overall system performance (e.g., system noise, stability, and optical efficiency) and considerable effort has gone into quantifying the best overall choice to define receiver bands for a particular telescope; present examples include the Square Kilometre Array (SKA) and the Next Generation Very Large Array (ngVLA) where the higher bands do not exceed a bandwidth of 1.7:1. During the last two years, NRC Herzberg has been researching wide bandwidth waveguide and active components in order to extend the bandwidth to a full 2:1 octave bandwidth. We report on recent innovation in front-end receiver components, including an octave bandwidth feed horn, OMT, and LNA, to enable wideband science","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12 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":"115057206","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}
{"title":"Blazed reflection gratings with electron-beam lithography and ion-beam etching","authors":"D. Miles, R. McEntaffer, F. Grisé","doi":"10.1117/12.2637880","DOIUrl":"https://doi.org/10.1117/12.2637880","url":null,"abstract":"In modern X-ray-grating development for astronomical applications, electron-beam lithography has emerged as a primary fabrication approach to producing high-performance reflection gratings for both current and future missions. The work presented here leverages years of development in electron-beam lithography for X-ray gratings to produce a grating pattern that is then blazed with ion-beam etching. The directional ion-beam etching reshapes the groove facets to a consistent, triangular profile with a facet angle specified by the grating application. An initial prototype X-ray reflection grating fabricated with a combination of electron-beam lithography and ion-beam etching is presented here, along with diffraction efficiency performance measured across the soft-X-ray bandpass. This first prototype achieves ≈33% absolute diffraction efficiency from 0.2 to 1.2 keV, with an average peak-order efficiency of ≈17%. The fabrication approach, efficiency measurements, and path toward improved performance are presented.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12181 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":"129401913","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}
Nianhua Jiang, L. Knee, D. Garcia, P. Niranjanan, I. Wevers
{"title":"Wideband cryogenic LNA design for the ngVLA Band-1 receiver","authors":"Nianhua Jiang, L. Knee, D. Garcia, P. Niranjanan, I. Wevers","doi":"10.1117/12.2629137","DOIUrl":"https://doi.org/10.1117/12.2629137","url":null,"abstract":"The next-generation Very Large Array (ngVLA) front end incorporates six dual-polarization receivers covering the frequency range from 1.2 to 116 GHz. The ngVLA Band-1 receiver covers a frequency range of 1.2 to 3.5 GHz. This wideband requirement presents a challenge for the extremely low noise design for the required cryogenic low noise amplifier (LNA). GaAs HEMT technology is very reliable at a gate length of 150 nm and that gate feature size is suitable for low noise amplifiers up to the microwave frequency range. Below 3 GHz, the transistor gate has a very large capacitive impedance, exhibiting like an open circuit, which requires large values of inductors for 50 Ω impedance and low noise matching. The hybrid circuit configuration allows the design to select high-Q discrete inductors and capacitors with large values to minimize loss/noise from passive components. A two-stage single-ended GaAs HEMT LNA was designed based on the hybrid configuration. A prototype ngVLA Band-1 LNA was assembled and fully tested at a physical temperature 12 K. This newly designed GaAs HEMT LNA achieved 1.6 K average noise temperature and 34 dB average high gain between 1.2 and 3.5 GHz, the total power consumption is about 10 mW, which can meet the current requirements of the ngVLA Band-1 receiver.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12190 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":"129673444","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}
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}
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}
R. den Hartog, P. Uttley, H. Hoevers, J. D. den Herder, M. Wise
{"title":"An AOCS concept for the x-ray interferometer mission","authors":"R. den Hartog, P. Uttley, H. Hoevers, J. D. den Herder, M. Wise","doi":"10.1117/12.2631579","DOIUrl":"https://doi.org/10.1117/12.2631579","url":null,"abstract":"An x-ray interferometer (XRI) has recently been proposed as a theme for ESA's voyage 2050 planning cycle, with the prospect to observe the x-ray sky with unprecedented angular resolution. A scientifically very interesting mission is possible on the basis of a single spacecraft with a resolving power of 100 micro arcsec (~0.5 nrad), owing to the compact 'telephoto' design proposed in 2004 by Willingale. One of the key challenges for such a mission is to acquire and maintain pointing to an absolute accuracy below that resolution. This challenge was already identified by Gendreau et al. in 2003. In this paper we re-address this issue in the light of recent technological developments.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"255 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":"133223835","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}
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}
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}
求助内容：
应助结果提醒方式：
京公网安备 11010802042870号
