Astronomical Telescopes + Instrumentation最新文献

{"title":"Follow-up x-ray telescope (FXT) mirror module for the Einstein probe mission","authors":"D. Vernani, G. Bianucci, G. Grisoni, F. Marioni, G. Valsecchi, A. Keereman, Yong Chen, Min Cong, Yanji Yang, Juan Wang, V. Burwitz, J. Eder, P. Friedrich, G. Hartner, A. Langmeier, Thomas Mueller, S. Rukdee, T. Schmidt","doi":"10.1117/12.2630147","DOIUrl":"https://doi.org/10.1117/12.2630147","url":null,"abstract":"The Einstein Probe (EP) is a mission of the Chinese Academy of Sciences (CAS) dedicated to time-domain high-energy astrophysics. Its primary goals are to discover high-energy transients and monitor variable objects. The ESA Science Programme Committee (SPC) approved on 19 June 2018 the participation of ESA to the CAS EP mission as a mission of opportunity. Among other elements, CAS has requested ESA participation for the provision of the mirror modules of the follow-up x-ray telescope (FXT). FXT is a pair of Wolter-I telescopes operating in the 0.5-10 keV energy range, inheriting the design from eROSITA [2][3]. It provides field of view of about 1 deg diameter. The source localization error will be of 5-15 arcsec depending on the source strength [1]. The FXT is responsible for the quick follow-up observations of the triggered sources and will also observe other interested targets during the all-sky survey at the rest time. Three FXT mirror modules were produced: structural and thermal model (STM), qualification model (QM) and flight model (FM). Media Lario could leverage on the manufacturing and integration infrastructure still available at its premises from the eROSITA programme [3][4], including the complete set of 54 mandrels needed for the mirror repliforming, property of MPE. Media Lario produced and integrated the FXT mirror modules, each comprising 54 nested repliformed mirror shells; Max-Planck Institute (MPE) conducted the x-ray optical tests at the PANTER facility, for the acceptance of all the different models. This efficient collaboration enabled the on-time and in-quality delivery of the FXT mirror modules.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":" 28","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120943350","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":"Status of resolve instrument onboard X-Ray Imaging and Spectroscopy Mission (XRISM)","authors":"Y. Ishisaki, R. Kelley, H. Awaki, J. Balleza, K. Barnstable, T. Bialas, R. Boissay-Malaquin, G. Brown, E. Canavan, R. Cumbee, T. Carnahan, M. Chiao, Brian J. Comber, E. Costantini, J. D. den Herder, J. Dercksen, C. D. de Vries, M. Dipirro, M. Eckart, Y. Ezoe, C. Ferrigno, R. Fujimoto, N. Gorter, S. Graham, M. Grim, Leslie S. Hartz, R. Hayakawa, T. Hayashi, N. Hell, A. Hoshino, Y. Ichinohe, M. Ishida, K. Ishikawa, B. James, Steven J. Kenyon, C. Kilbourne, M. Kimball, S. Kitamoto, M. Leutenegger, Y. Maeda, D. McCammon, J. Miko, M. Mizumoto, T. Okajima, A. Okamoto, S. Paltani, F. Porter, Kosuke Sato, Toshiki Sato, M. Sawada, K. Shinozaki, R. Shipman, P. Shirron, G. Sneiderman, Y. Soong, R. Szymkiewicz, A. Szymkowiak, Y. Takei, K. Tamura, M. Tsujimoto, Y. Uchida, S. Wasserzug, M. Witthoeft, Rob Wolfs, S. Yamada, S. Yasuda","doi":"10.1117/12.2630654","DOIUrl":"https://doi.org/10.1117/12.2630654","url":null,"abstract":"The resolve instrument onboard the X-Ray Imaging and Spectroscopy Mission (XRISM) consists of an array of 6 × 6 silicon-thermistor microcalorimeters cooled down to 50 mK and a high-throughput x-ray mirror assembly (XMA) with a focal length of 5.6 m. XRISM is a recovery mission of ASTRO-H/Hitomi, and the Resolve instrument is a rebuild of the ASTRO-H soft x-ray spectrometer (SXS) and the Soft X-ray Telescope (SXT) that achieved energy resolution of ∼5 eV FWHM on orbit, with several important changes based on lessons learned from ASTRO-H. The flight models of the Dewar and the electronics boxes were fabricated and the instrument test and calibration were conducted in 2021. By tuning the cryocooler frequencies, energy resolution better than 4.9 eV FWHM at 6 keV was demonstrated for all 36 pixels and high resolution grade events, as well as energy-scale accuracy better than 2 eV up to 30 keV. The immunity of the detectors to microvibration, electrical conduction, and radiation was evaluated. The instrument was delivered to the spacecraft system in 2022-04 and is under the spacecraft system testing as of writing. The XMA was tested and calibrated separately. Its angular resolution is 1.27′ and the effective area of the mirror itself is 570 cm2 at 1 keV and 424 cm2 at 6 keV. We report the design and the major changes from the ASTRO-H SXS, the integration, and the results of the instrument test.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"145 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":"127308854","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":"Mission pointing optimisation of twin satellite system for all-sky burst monitoring","authors":"Xingbo Han, Fei Li, Liang Chang, Keke Zhang, Jinpei Yu, Hao Geng","doi":"10.1117/12.2629160","DOIUrl":"https://doi.org/10.1117/12.2629160","url":null,"abstract":"Currently, with the continuous enrichment of astronomical observation means (Ligo/Virgo for GW, Parkes, Arecibo and Green Bank Telescope for FRB, IceCube for neutrino observatory, etc…), multi-messenger observation has become one of the hot spots in current astronomical research. X /γ ray observation is one of the important means of multi-messenger observation. Considering the scarcity and preciseness of multi-messenger sources, a special all-sky x/γ-ray monitor is needed to monitor high-energy electromagnetic counterparts in real time. Considering the launch cost, it is an economical and efficient solution that launch low-orbit twin satellites to realize all day monitoring. Due to the constraints of x/γ-ray payload, high-energy payloads generally need to work in low attitude and low inclination orbit (to reduce the interference caused by high-energy particles, and in order to achieve all-day monitoring, the satellite attitude needs to ensure that payload pointing outside earth in real time. The satellite pointing should take into account both the payload pointing constrains and energy acquisition, as well as the operation of thermal control and STR. Different from the sun-synchronous orbit satellite, the satellite attitude needs to be specially designed. This paper presents a satellite pointing law suitable for all-sky monitor low orbit satellite. And the advantages of this pointing law are compared from the perspectives of constrains satisfaction, energy acquisition and economy. Then on this basis, implementation method, error analysis and on-orbit performance are given.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"156 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":"122615092","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":"Fabrication of lightweight silicon x-ray mirrors","authors":"R. Riveros, Kim D. Allgood, M. Biskach, Tabatha A. DeVita, M. Hlinka, J. Kearney, Ai Numata, Will Zhang","doi":"10.1117/12.2629017","DOIUrl":"https://doi.org/10.1117/12.2629017","url":null,"abstract":"Numerous scientific questions at the forefront of our modern physical understanding require enhanced x-ray astronomical observations beyond the capabilities of existing x-ray telescopes. These observations demand spaceborne x-ray telescopes of unprecedented imaging power. X-ray focusing optics which are simultaneously light weight and of sufficient quality are presently impossible to realize, given real-world constraints and current manufacturing technology. Our group at the National Aeronautics and Space Administration (NASA) Goddard Space Flight Center (GSFC) investigates the development of a x-ray mirror manufacturing process capable of meeting the stringent quality, production time, and cost requirements of the next-generation of x-ray telescopes. This process employs monocrystalline silicon: a lightweight, stiff, thermally conductive, and readily available material which is free of internal stress. These properties combined make silicon a nearly ideal material for thin mirror substrates. Presently, our process is capable of fabricating sub-arcsecond half-power-diameter (HPD) resolution mirror pairs (primary and secondary) at a sub-millimeter mirror thicknesses and of virtually any x-ray optical design (e.g. Wolter-I, Wolter-Schwarzschild, etc.). Further, the substrates include three-dimensional structures on their backsides to aid their alignment and bonding. The mirror substrate surface quality is generally superior to that of the mirrors on the Chandra X-ray Observatory. This paper describes the various manufacturing steps involved in the production of x-ray mirror substrates and a present status report.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"30 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":"115911457","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":"Evidence that evaporated Al/AlF3 bilayer thin films stored in a 327 K oven for over 2500 hours have not degraded","authors":"Kenan Fronk, D. Allred","doi":"10.1117/12.2630711","DOIUrl":"https://doi.org/10.1117/12.2630711","url":null,"abstract":"Four evaporated, thin-film Al samples protected by a thin (29±2 nm) aluminum fluoride (AlF3) overcoat stored in dry (dew point 276K ), 327 K air over a period of 2500 hours exhibited no significant changes in the thickness of the protective AlF3 layer nor growth in aluminum oxide as observed by variable-angled, spectroscopic ellipsometry. Two of the samples had AlF3 evaporated at T>200°C, two without substrate heating. No difference in aging was noted amongst the samples. Since many months may elapse between fabrication and launch of the completed observatory, this result contributes to understanding the boundaries in temperature and humidity separating negligible changes in fluoride-containing optical components from unacceptable degradation. While negligible changes in thicknesses were observed, there were changes in the ellipsometric data, psi and delta, with time. In this study, we also present our use of an effective medium approximation model in understanding changes in the fluoride layer with aging. The observed changes in SE parameters are here interpreted as changes in void fraction, though the presence of some water was not ruled out. Apparent void fraction fell by a factor of two by the end of the 2500 hours. The decreasing void fraction suggests that the films might be becoming more compact with time. Other surface sensitive techniques such as AFM are needed to narrow down possible explanations for observed changes.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"61 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":"116081822","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":"ASTENA: an innovative mission concept for broadband high-energy astrophysics","authors":"E. Virgilli, F. Frontera, L. Ferro, M. Moita, L. Cavazzini, P. Rosati, C. Guidorzi, M. Orlandini, C. Labanti, E. Caroli, N. Auricchio, J. Stephen, S. del Sordo, L. Amati","doi":"10.1117/12.2630080","DOIUrl":"https://doi.org/10.1117/12.2630080","url":null,"abstract":"Hard-x/soft gamma-rays are probes of the most powerful phenomena in the universe. Unlike soft x-ray astrophysics, this band has benefited less from the technological advancement due to the difficulty to absorb this radiation and to the lack of focusing instrumentation. For these reasons the quest for innovative soft gamma-ray instrumentation is pressing and their effective recognition and realization are urgent. In this context, and in the framework of the AHEAD project, funded by the European Commission, the ASTENA experiment was proposed as an innovative mission concept to face some of the most debated questions in hard x-/gamma-ray astronomy. This effort will be done through the use of instruments based on groundbreaking technologies, capable of providing unprecedented broad energy passband in a wide field of view, high sensitivity observations and, at the same time, sub-arcminute localization of gamma-ray sources and polarimetric measurement. In this paper we describe the instruments on board ASTENA, the technologies involved, the performances achievable with their exploitation and their level of readiness.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"10 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":"126691966","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":"A possibility to extend the IXPE energy band","authors":"F. La Monaca, F. Xie, P. Soffitta, E. Costa, A. Di Marco, S. Fabiani, F. Muleri, J. Rankin, L. Baldini, E. Del Monte, A. Manfreda, S. O’Dell, B. Ramsey, C. Sgro’, A. Tennant, M. Weisskopf","doi":"10.1117/12.2628931","DOIUrl":"https://doi.org/10.1117/12.2628931","url":null,"abstract":"This conference presentation was prepared for the Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray conference at SPIE Astronomical Telescopes + Instrumentation, 2022.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"137 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":"126867569","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":"Development of a prototype detector for the Gamma-RAy Polarimeter Experiment (GRAPE)","authors":"Karla Oñate Melecio, C. Bancroft, C. Ertley, F. Kislat, J. Legere, S. Longworth, M. McConnell, J. Ryan, Jimmy Zaid","doi":"10.1117/12.2629044","DOIUrl":"https://doi.org/10.1117/12.2629044","url":null,"abstract":"The gamma-ray polarimeter experiment (GRAPE) is a NASA-funded high-altitude scientific balloon experiment. For over a decade, GRAPE has been developing wide field of view (FoV) scintillator-based Compton polarimeters designed to measure gamma-ray polarization from GRBs over the energy range of 50-500 keV. A variant of a GRAPE design was tested in flight in 2011 and 2014. A new design is scheduled to fly in Fort Sumner, New Mexico in August of 2023. The new design of GRAPE incorporates an assemblage of 245 optically isolated high-Z and low-Z scintillators each read out by individual silicon photomultipliers (SiPMs) and arranged in a 3-dimensional 7x7x5 cuboid layout which provides moderate imaging capabilities. The cube design of GRAPE is expected to improve performance with respect to previous GRAPE missions by eliminating optical cross-talk and using the instrument’s imaging capability to reduce instrument background. To standardize the development process for the flight instrument, select optimal technology to optimize the design features, and build a framework for the analysis and simulation of the 245 detector instrument, a small-scale prototype instrument of the cube design was developed and studied in the lab using simulations and lab measurements of unpolarized sources. The results of these studies are presented here along with an overview of the 7x7x5 flight instrument and mission.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"246 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":"122076485","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":"BISOU: a balloon project for spectral observations of the early universe","authors":"B. Maffei, N. Aghanim, J. Aumont, E. Battistelli, J. Chluba, X. Coulon, P. de Bernardis, M. Douspis, J. Grain, J. C. Hill, A. Kogut, Joseph Kuruvilla, G. Lagache, Juan Macis-Perez, S. Masi, T. Matsumura, L. Mele, A. Monfardini, C. O'sullivan, L. Pagano, G. Pisano, N. Ponthieu, M. Remazeilles, A. Ritacco, A. Rotti, G. Savini, V. Sauvage, A. Shitvov, S. Stever, A. Tartari, L. Thiele, N. Trappe, Jean-François Aubrun, A. Laurens, D. Pheav, F. Vacher","doi":"10.1117/12.2630136","DOIUrl":"https://doi.org/10.1117/12.2630136","url":null,"abstract":"The BISOU (Balloon Interferometer for Spectral Observations of the Universe) project studies the viability and prospects of a balloon-borne spectrometer, pathfinder of a future space mission dedicated to the measurements of the CMB spectral distortions, while consolidating the instrumental concept and improving the readiness of some of its key sub-systems. A balloon concept based on a Fourier Transform Spectrometer, covering a spectral range from about 90 GHz to 2 THz, adapted from previous mission proposals such as PIXIE and FOSSIL, is being studied and modelled. Taking into account the requirements and conditions of balloon flights (i.e. residual atmosphere, observation strategy for instance), we present here the instrument concept together with the results of the CNES phase 0 study, evaluating the sensitivity to some of its potential observables. For instance, we forecast a detection of the CMB Compton y-distortion monopole with a signal-to-noise ratio of at least 5.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"48 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":"128206322","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":"Alignment and integration of the SPO mirror modules onto the ATHENA Telescope","authors":"G. Valsecchi, G. Bianucci, F. Marioni, D. Vernani, F. Zocchi, T. Korhonen, G. Pareschi, I. Ferreira, M. Bavdaz","doi":"10.1117/12.2629304","DOIUrl":"https://doi.org/10.1117/12.2629304","url":null,"abstract":"Several hundreds of Silicon Pore Optics (SPO) mirror modules will be integrated and co-aligned onto the ATHENA (Advanced Telescope for High-ENergy Astrophysics) Mirror Assembly Module (MAM). The integration process has been developed by Media Lario and exploits a full-size optical bench to capture the focal plane image of each mirror module when illuminated by an UV plane wavefront at 218 nm. Each mirror module, handled by a manipulator, focuses the collimated beam onto a CCD camera placed at the 12 m focal position of the ATHENA telescope. The image is processed in real time to calculate the centroid position and overlap it to the centroid of the already integrated Mirror modules. Media Lario with ESA support has designed the Assembly Integration and Test (AIT) facility, able to host the complete ATHENA telescope. The AIT facility is in construction and the 2.6 m Zerodur® parabolic mirror has been accepted for coating and ready to be delivered to Calar Alto Observatory (CAHA, Sierra de Los Filabres, Spain) for the reflective coating application. The building housing the AIT facility is under construction at the Media Lario premises near Milan, Italy, and extends 6.5 m below ground and 17 m above ground. The building also is dimensioned to accommodate the vertical X-ray (Vert-X) test facility. The co-location of these two facilities is strategic for the project and will permit regular checks of the mirror module alignment while the MAM is populated. The MAM will be moved on a rail system connecting the two facilities.","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":"129563076","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}