L. Burderi, T. di Salvo, A. Riggio, A. Gambino, A. Sanna, F. Fiore, Fabrizio Amarilli, L. Amati, F. Ambrosino, G. Amelino-Camelia, A. Anitra, M. Barbera, M. Bechini, P. Bellutti, Roberto Bertaccin, G. Bertuccio, R. Campana, Jiewei Cao, S. Capozziello, F. Ceraudo, Tianxiang Chen, M. Cinelli, M. Citossi, A. Clerici, A. Colagrossi, E. Costa, S. Curzel, M. De Laurentis, Giovanni Della Casa, M. Della Valle, E. Demenev, M. Del Santo, G. Dilillo, P. Efremov, Y. Evangelista, M. Feroci, Chiara Ferruglio, Fabrizio Ferrandi, M. Fiorini, M. Fiorito, F. Frontera, F. Fuschino, Dejan Gacnik, G. Galgóczi, N. Gao, M. Gandola, G. Ghirlanda, Andreja Gamboc, M. Grassi, C. Guidorzi, A. Guzmán, R. Iaria, M. Karlica, U. Kostic, C. Labanti, G. La Rosa, U. Lo Cicero, Borja Lopez Fernandez, P. Lunghi, P. Malcovati, A. Maselli, A. Manca, F. Mele, Dorottya Milánkovich, Angel Monge, G. Morgante, L. Nava, B. Negri, P. Nogara, M. Ohno, D. Ottolina, A. Pasquale, A. Pál, M. Perri, M. Piccinin, R. Piazzolla, S. Pirrotta, S. Pliego-Caballe
Within Quantum Gravity theories, different models for space-time quantisation predict an energy dependent speed for photons. Although the predicted discrepancies are minuscule, GRB, occurring at cosmological distances, could be used to detect this signature of space-time granularity with a new concept of modular observatory of huge overall collecting area consisting in a fleet of small satellites in low orbits, with sub-microsecond time resolution and wide energy band (keV-MeV). The enormous number of collected photons will allow to effectively search these energy dependent delays. Moreover, GrailQuest will allow to perform temporal triangulation of high signal-to-noise impulsive events with arc-second positional accuracies: an extraordinary sensitive X-ray/Gamma all-sky monitor crucial for hunting the elusive electromagnetic counterparts of GW. A pathfinder of GrailQuest is already under development through the HERMES project: a fleet of six 3U cube-sats to be launched by 2021/22.
{"title":"GrailQuest and HERMES: hunting for gravitational wave electromagnetic counterparts and probing space-time quantum foam","authors":"L. Burderi, T. di Salvo, A. Riggio, A. Gambino, A. Sanna, F. Fiore, Fabrizio Amarilli, L. Amati, F. Ambrosino, G. Amelino-Camelia, A. Anitra, M. Barbera, M. Bechini, P. Bellutti, Roberto Bertaccin, G. Bertuccio, R. Campana, Jiewei Cao, S. Capozziello, F. Ceraudo, Tianxiang Chen, M. Cinelli, M. Citossi, A. Clerici, A. Colagrossi, E. Costa, S. Curzel, M. De Laurentis, Giovanni Della Casa, M. Della Valle, E. Demenev, M. Del Santo, G. Dilillo, P. Efremov, Y. Evangelista, M. Feroci, Chiara Ferruglio, Fabrizio Ferrandi, M. Fiorini, M. Fiorito, F. Frontera, F. Fuschino, Dejan Gacnik, G. Galgóczi, N. Gao, M. Gandola, G. Ghirlanda, Andreja Gamboc, M. Grassi, C. Guidorzi, A. Guzmán, R. Iaria, M. Karlica, U. Kostic, C. Labanti, G. La Rosa, U. Lo Cicero, Borja Lopez Fernandez, P. Lunghi, P. Malcovati, A. Maselli, A. Manca, F. Mele, Dorottya Milánkovich, Angel Monge, G. Morgante, L. Nava, B. Negri, P. Nogara, M. Ohno, D. Ottolina, A. Pasquale, A. Pál, M. Perri, M. Piccinin, R. Piazzolla, S. Pirrotta, S. Pliego-Caballe","doi":"10.1117/12.2561779","DOIUrl":"https://doi.org/10.1117/12.2561779","url":null,"abstract":"Within Quantum Gravity theories, different models for space-time quantisation predict an energy dependent speed for photons. Although the predicted discrepancies are minuscule, GRB, occurring at cosmological distances, could be used to detect this signature of space-time granularity with a new concept of modular observatory of huge overall collecting area consisting in a fleet of small satellites in low orbits, with sub-microsecond time resolution and wide energy band (keV-MeV). The enormous number of collected photons will allow to effectively search these energy dependent delays. Moreover, GrailQuest will allow to perform temporal triangulation of high signal-to-noise impulsive events with arc-second positional accuracies: an extraordinary sensitive X-ray/Gamma all-sky monitor crucial for hunting the elusive electromagnetic counterparts of GW. A pathfinder of GrailQuest is already under development through the HERMES project: a fleet of six 3U cube-sats to be launched by 2021/22.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"6 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2021-01-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126665714","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}
SmallSats extend the frontiers of astrophysics, and present an opportunity with which to develop the next generation of scientists and engineers. Achieving high-impact research with SmallSats is increasingly feasible due to advances in technologies such as precision pointing, compact sensitive detectors and the miniaturization of propulsion systems. Science cases for SmallSat observatories (including CubeSats) being developed now include the discovery and characterization of exoplanets, stars, black holes and radio transients. SmallSats also represent a fantastic “on-ramp” to bring more people into mission development by providing opportunities for students and new PIs to get hands-on, end-to-end leadership, research and engineering experience. This combination of people development with new technology provides diverse opportunities to advance astrophysics knowledge.
{"title":"Frontiers of astrophysics with SmallSats","authors":"E. Shkolnik","doi":"10.1117/12.2590132","DOIUrl":"https://doi.org/10.1117/12.2590132","url":null,"abstract":"SmallSats extend the frontiers of astrophysics, and present an opportunity with which to develop the next generation of scientists and engineers. Achieving high-impact research with SmallSats is increasingly feasible due to advances in technologies such as precision pointing, compact sensitive detectors and the miniaturization of propulsion systems. Science cases for SmallSat observatories (including CubeSats) being developed now include the discovery and characterization of exoplanets, stars, black holes and radio transients. SmallSats also represent a fantastic “on-ramp” to bring more people into mission development by providing opportunities for students and new PIs to get hands-on, end-to-end leadership, research and engineering experience. This combination of people development with new technology provides diverse opportunities to advance astrophysics knowledge.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"10 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"129456308","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}
L. Damé, M. Meftah, N. Rouanet, P. Gilbert, P. Etcheto, J. Berthon
SUAVE (Solar Ultraviolet Advanced Variability Experiment) is a far UV imaging solar telescope (Lyman Alpha, 121.6 nm, Herzberg continuum, 200-242 nm, etc.) of novel design (off-axis telescope with "mushroom type" SiC mirrors) for ultimate thermal stability and long lasting performances over years instead of, often, a few weeks or months in this wavelength range. SUAVE has no entrance window for long and uncompromising observations in the UV (no coatings of mirrors, flux limited to less than 2 solar constants on filters to avoid their degradation), associated with an ultimate thermal control (no central obscuration resulting in limited thermal gradients and easier heat evacuation, focus control, stabilization). Design and anticipated performances will be detailed as well as results of representative thermal/optical tests performed on the SiC primary mirror and support regulated plate (SiC also). SUAVE is the main instrument of the Solar/Climate SoSWEET-SOUP constellation mission.
{"title":"SUAVE, a disruptive far UV telescope designed for long lasting performances in space","authors":"L. Damé, M. Meftah, N. Rouanet, P. Gilbert, P. Etcheto, J. Berthon","doi":"10.1117/12.2563375","DOIUrl":"https://doi.org/10.1117/12.2563375","url":null,"abstract":"SUAVE (Solar Ultraviolet Advanced Variability Experiment) is a far UV imaging solar telescope (Lyman Alpha, 121.6 nm, Herzberg continuum, 200-242 nm, etc.) of novel design (off-axis telescope with \"mushroom type\" SiC mirrors) for ultimate thermal stability and long lasting performances over years instead of, often, a few weeks or months in this wavelength range. SUAVE has no entrance window for long and uncompromising observations in the UV (no coatings of mirrors, flux limited to less than 2 solar constants on filters to avoid their degradation), associated with an ultimate thermal control (no central obscuration resulting in limited thermal gradients and easier heat evacuation, focus control, stabilization). Design and anticipated performances will be detailed as well as results of representative thermal/optical tests performed on the SiC primary mirror and support regulated plate (SiC also). SUAVE is the main instrument of the Solar/Climate SoSWEET-SOUP constellation mission.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"26 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121234805","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}
F. Porter, M. Eckart, M. Leutenegger, Tomomi Watanabe, C. Kilbourne, R. Kelley, Michael C. Witthoeft, R. Cumbee, M. Sawada, N. Hell, G. Brown, Y. Ishisaki, S. Yamada
The Resolve detector system is calibrated on the ground in three stages: at the focal plane assembly, at the calorimeter spectrometer insert, and at the full instrument level. We have just completed the first two stages and have measured the detailed core line shape and spectral redistribution functions, by pixel, and as a function of energy. In addition, we have measured the energy scale function that translates instrument units into spectral units, by pixel, and as a function of detector heat sink temperature. We discuss the results of the Resolve calibration program to date as well as implications for the calibration of future high resolution x-ray spectrometers.
{"title":"Initial ground calibration of the Resolve detector system on XRISM","authors":"F. Porter, M. Eckart, M. Leutenegger, Tomomi Watanabe, C. Kilbourne, R. Kelley, Michael C. Witthoeft, R. Cumbee, M. Sawada, N. Hell, G. Brown, Y. Ishisaki, S. Yamada","doi":"10.1117/12.2561477","DOIUrl":"https://doi.org/10.1117/12.2561477","url":null,"abstract":"The Resolve detector system is calibrated on the ground in three stages: at the focal plane assembly, at the calorimeter spectrometer insert, and at the full instrument level. We have just completed the first two stages and have measured the detailed core line shape and spectral redistribution functions, by pixel, and as a function of energy. In addition, we have measured the energy scale function that translates instrument units into spectral units, by pixel, and as a function of detector heat sink temperature. We discuss the results of the Resolve calibration program to date as well as implications for the calibration of future high resolution x-ray spectrometers.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"19 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"117206171","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}
T. Sakao, S. Matsuyama, J. Yamada, Takato Inoue, Kentaro Hata, Hiroyuki Yamaguchi, T. Hagiwara, Nami Nakamura, K. Yamauchi, Y. Kohmura, Y. Suematsu, N. Narukage
We present ongoing efforts on the development of precision Wolter mirrors for the Soft X-ray Imaging Spectrometer (SXIS) aboard PhoENiX mission proposed to JAXA for studying mechanism(s) of particle acceleration and its relationship with magnetic reconnection in solar flares. The Wolter mirrors for PhoENiX/SXIS are made by direct polishing of glass-ceramic substrates. So far, we succeeded in fabricating a small size of high precision Wolter surfaces (e.g., PSF core size of ~0.2 arcsec HPD at 8 keV) as well as good indication of extending the mirror area along the cylindrical direction. Recent status of the mirror development will be reported.
{"title":"Development of precision Wolter mirrors towards PhoENiX mission for the Sun","authors":"T. Sakao, S. Matsuyama, J. Yamada, Takato Inoue, Kentaro Hata, Hiroyuki Yamaguchi, T. Hagiwara, Nami Nakamura, K. Yamauchi, Y. Kohmura, Y. Suematsu, N. Narukage","doi":"10.1117/12.2562077","DOIUrl":"https://doi.org/10.1117/12.2562077","url":null,"abstract":"We present ongoing efforts on the development of precision Wolter mirrors for the Soft X-ray Imaging Spectrometer (SXIS) aboard PhoENiX mission proposed to JAXA for studying mechanism(s) of particle acceleration and its relationship with magnetic reconnection in solar flares. The Wolter mirrors for PhoENiX/SXIS are made by direct polishing of glass-ceramic substrates. So far, we succeeded in fabricating a small size of high precision Wolter surfaces (e.g., PSF core size of ~0.2 arcsec HPD at 8 keV) as well as good indication of extending the mirror area along the cylindrical direction. Recent status of the mirror development will be reported.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"29 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133999535","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":"Improving the performance and stability of ultraviolet optical coatings using atomic layer deposition","authors":"J. Hennessy, S. Nikzad, A. Jewell","doi":"10.1117/12.2563250","DOIUrl":"https://doi.org/10.1117/12.2563250","url":null,"abstract":"","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"79 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114809998","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}
H. Geoffray, S. Bandler, W. Doriese, M. Kirivanta, D. PRELE, L. Ravera, A. Argan, M. Barbera, J. Kuur, B. Leeuwen, H. Weers, R. Hoogeveen, J. Herder, S. Smith, J. Adams, J. Chervenak, M. Durkin, C. Reintsema, J. Ullom, Y. Parot, D. Barret, C. Macculi, L. Piro, F. Brachet, A. Ledot, B. Jackson
CNES (French Space Agency) is in charge of the development of the X-IFU instrument for Athena. The main sensor array detection chain sub-system of the X-IFU instrument is one of the major sub-subsystem of the instrument, as the main contributor to the performance. This sub-system involves major partners of the X-IFU instrument, e.g GFSC, SRON, VTT, APC, and IRAP. The purpose of this paper is to present the baseline of the definition of the X-IFU detection chain in the frame at end of phase A/beginning of phase B. The readout is based on Time Domain Multiplexing (TDM). There are strong design issues which couple the different sub-components of the detection chain (the main sensor array, the cold electronics stages, and the warm electronics). The detection chain environment (thermal, mechanical and EMI/EMC environment) also requires a transverse analysis. This paper focuses on those aspects while providing design description of the sub-components of the detection chain.
{"title":"Conceptual design of the detection chain for the X-IFU on Athena","authors":"H. Geoffray, S. Bandler, W. Doriese, M. Kirivanta, D. PRELE, L. Ravera, A. Argan, M. Barbera, J. Kuur, B. Leeuwen, H. Weers, R. Hoogeveen, J. Herder, S. Smith, J. Adams, J. Chervenak, M. Durkin, C. Reintsema, J. Ullom, Y. Parot, D. Barret, C. Macculi, L. Piro, F. Brachet, A. Ledot, B. Jackson","doi":"10.1117/12.2563628","DOIUrl":"https://doi.org/10.1117/12.2563628","url":null,"abstract":"CNES (French Space Agency) is in charge of the development of the X-IFU instrument for Athena. The main sensor array detection chain sub-system of the X-IFU instrument is one of the major sub-subsystem of the instrument, as the main contributor to the performance. This sub-system involves major partners of the X-IFU instrument, e.g GFSC, SRON, VTT, APC, and IRAP. The purpose of this paper is to present the baseline of the definition of the X-IFU detection chain in the frame at end of phase A/beginning of phase B. The readout is based on Time Domain Multiplexing (TDM). There are strong design issues which couple the different sub-components of the detection chain (the main sensor array, the cold electronics stages, and the warm electronics). The detection chain environment (thermal, mechanical and EMI/EMC environment) also requires a transverse analysis. This paper focuses on those aspects while providing design description of the sub-components of the detection chain.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"118 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115453852","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}
H. Akamatsu, D. Vaccaro, L. Gottardi, J. Kuur, C. Vries, S. Bandler, M. Bruijn, J. Chervenak, M. D’Andrea, Jiansong Gao, J. Herder, R. Hoogeveen, M. Kiviranta, A. Linden, B. Jackson, A. Miniussi, K. Nagayoshi, K. Ravensberg, M. Ridder, K. Sakai, S. Smith, E. Taralli, S. Visser, N. Wakeham, M. D. Wit
{"title":"Frequency domain multiplexing technology of transition-edge sensors for x-ray astronomy","authors":"H. Akamatsu, D. Vaccaro, L. Gottardi, J. Kuur, C. Vries, S. Bandler, M. Bruijn, J. Chervenak, M. D’Andrea, Jiansong Gao, J. Herder, R. Hoogeveen, M. Kiviranta, A. Linden, B. Jackson, A. Miniussi, K. Nagayoshi, K. Ravensberg, M. Ridder, K. Sakai, S. Smith, E. Taralli, S. Visser, N. Wakeham, M. D. Wit","doi":"10.1117/12.2561271","DOIUrl":"https://doi.org/10.1117/12.2561271","url":null,"abstract":"","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"36 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114379193","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}
P. Peille, D. Barret, V. Albouys, J. Herder, L. Piro, M. Cappi, J. Huovelin, R. Kelley, J. Mas-Hesse, K. Mitsuda, S. Paltani, G. Rauw, A. Różańska, J. Svoboda, J. Wilms
The X-ray Integral Field Unit (X-IFU) will be the cryogenic X-ray spectro-imager of the ESA Athena space observatory. It will implement a matrix of 3168 superconducting Transition Edge Sensors at 90 mK to provide a very high spectral resolution of 2.5 eV up to the energy of 7 keV, across a 5’ large field of view. The X-IFU successfully passed its Preliminary Requirements Review in mid-2019. After providing an overview of the driving science cases, the key requirements, I will present a status on the instrument development.
{"title":"The X-ray Integral Field Unit instrument: science, design, performances and status (Conference Presentation)","authors":"P. Peille, D. Barret, V. Albouys, J. Herder, L. Piro, M. Cappi, J. Huovelin, R. Kelley, J. Mas-Hesse, K. Mitsuda, S. Paltani, G. Rauw, A. Różańska, J. Svoboda, J. Wilms","doi":"10.1117/12.2562617","DOIUrl":"https://doi.org/10.1117/12.2562617","url":null,"abstract":"The X-ray Integral Field Unit (X-IFU) will be the cryogenic X-ray spectro-imager of the ESA Athena space observatory. It will implement a matrix of 3168 superconducting Transition Edge Sensors at 90 mK to provide a very high spectral resolution of 2.5 eV up to the energy of 7 keV, across a 5’ large field of view. The X-IFU successfully passed its Preliminary Requirements Review in mid-2019. After providing an overview of the driving science cases, the key requirements, I will present a status on the instrument development.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"48 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114975970","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. Schattenburg, R. Heilmann, H. Marshall, Brandon D. Chalifoux, E. Kara
We present a novel nested-shell Wolter x-ray telescope design that can achieve diffraction-limited performance over the entire telescope aperture. The new design features a compact single-spacecraft mirror assembly, similar in form to that proposed for Lynx, and a separate detector spacecraft. A wide range of design parameter space was considered. We present a specific example which features 10 micro-arcsec resolution, a wide band (0.1-10 keV) with > 2 m2 effective area out to 10 keV, a large flat field (>1010 pixels), achieving diffraction-limited performance (Strehl ratio > 0.8). We will also briefly discuss a potential science case for this telescope.
{"title":"A diffraction-limited Wolter nested-shell telescope concept with pico-radian resolution","authors":"M. Schattenburg, R. Heilmann, H. Marshall, Brandon D. Chalifoux, E. Kara","doi":"10.1117/12.2562496","DOIUrl":"https://doi.org/10.1117/12.2562496","url":null,"abstract":"We present a novel nested-shell Wolter x-ray telescope design that can achieve diffraction-limited performance over the entire telescope aperture. The new design features a compact single-spacecraft mirror assembly, similar in form to that proposed for Lynx, and a separate detector spacecraft. A wide range of design parameter space was considered. We present a specific example which features 10 micro-arcsec resolution, a wide band (0.1-10 keV) with > 2 m2 effective area out to 10 keV, a large flat field (>1010 pixels), achieving diffraction-limited performance (Strehl ratio > 0.8). We will also briefly discuss a potential science case for this telescope.","PeriodicalId":170593,"journal":{"name":"Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray","volume":"18 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125811443","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}
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