Versatile Optics for X-ray Imaging (VOXI) is a technology that enables a wide range of missions and opens up new opportunities for scientific research over multiple disciplines including fundamental physics, heliophysics, astrophysics, lunar and planetary science, and laboratory physics. VOXI is well-suited to SmallSats, which have become powerful platforms from which to conduct leading scientific investigations and cutting-edge technology developments at low cost with rapid turn-arounds. At the Center for Astrophysics | Harvard and Smithsonian, in collaboration with other institutions, we have developed VOXI, a Wolter-I Xray telescope with a focal length of < 1.5 m. In this paper we describe the potential of these optics, and the applications for VOXI optics considered to date.
{"title":"VOXI: Versatile Optics for X-ray Imaging","authors":"S. Romaine, J. Hong, M. Elvis","doi":"10.1117/12.2630660","DOIUrl":"https://doi.org/10.1117/12.2630660","url":null,"abstract":"Versatile Optics for X-ray Imaging (VOXI) is a technology that enables a wide range of missions and opens up new opportunities for scientific research over multiple disciplines including fundamental physics, heliophysics, astrophysics, lunar and planetary science, and laboratory physics. VOXI is well-suited to SmallSats, which have become powerful platforms from which to conduct leading scientific investigations and cutting-edge technology developments at low cost with rapid turn-arounds. At the Center for Astrophysics | Harvard and Smithsonian, in collaboration with other institutions, we have developed VOXI, a Wolter-I Xray telescope with a focal length of < 1.5 m. In this paper we describe the potential of these optics, and the applications for VOXI optics considered to date.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"25 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":"116747087","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, B. Jackson, S. Bandler, S. Smith, W. Doriese, M. Durkin, J. van der Kuur, B. van Leeuwen, M. Kirivanta, D. PRELE, L. Ravera, Y. Parot, H. V. van Weers, J. D. den Herder, Joseph Adams, J. Chervenak, C. Reintsema, J. Ullom, F. Brachet, A. Ledot, P. Peille, D. Barret
The x-ray integral field unit (X-IFU) instrument is the high-resolution x-ray spectrometer of the ESA Athena x-ray observatory. X-IFU will deliver spectra from 0.2 to 12 keV with a spectral resolution of 2.5 eV up to 7 keV from 5" pixels, with a hexagonal field of view of 5' equivalent diameter. The main sensor array and its associated detection chain is one of the major sub-systems of the X-IFU instrument, and is the main contributor to X-IFU’s performance. CNES (the French Space Agency) is leading the development of X-IFU; additional major partners are NASA-GFSC, SRON, VTT, APC, NIST, and IRAP. This paper updates the B-phase definition of the X-IFU detection chain. The readout is based on time-division multiplexing (TDM). The different sub-components of the detection chain (the main sensor array, the cold electronics stages, and the warm electronics) require global design optimization in order to achieve the best performance. The detection chain’s sensitivity to the EMI/EMC environment requires detailed analysis and implementation of dedicated design solutions. This paper focuses on these aspects while providing an update to the detection-chain design description.
{"title":"Design of the detection chain for Athena X-IFU","authors":"H. Geoffray, B. Jackson, S. Bandler, S. Smith, W. Doriese, M. Durkin, J. van der Kuur, B. van Leeuwen, M. Kirivanta, D. PRELE, L. Ravera, Y. Parot, H. V. van Weers, J. D. den Herder, Joseph Adams, J. Chervenak, C. Reintsema, J. Ullom, F. Brachet, A. Ledot, P. Peille, D. Barret","doi":"10.1117/12.2629960","DOIUrl":"https://doi.org/10.1117/12.2629960","url":null,"abstract":"The x-ray integral field unit (X-IFU) instrument is the high-resolution x-ray spectrometer of the ESA Athena x-ray observatory. X-IFU will deliver spectra from 0.2 to 12 keV with a spectral resolution of 2.5 eV up to 7 keV from 5\" pixels, with a hexagonal field of view of 5' equivalent diameter. The main sensor array and its associated detection chain is one of the major sub-systems of the X-IFU instrument, and is the main contributor to X-IFU’s performance. CNES (the French Space Agency) is leading the development of X-IFU; additional major partners are NASA-GFSC, SRON, VTT, APC, NIST, and IRAP. This paper updates the B-phase definition of the X-IFU detection chain. The readout is based on time-division multiplexing (TDM). The different sub-components of the detection chain (the main sensor array, the cold electronics stages, and the warm electronics) require global design optimization in order to achieve the best performance. The detection chain’s sensitivity to the EMI/EMC environment requires detailed analysis and implementation of dedicated design solutions. This paper focuses on these aspects while providing an update to the detection-chain design description.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"104 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":"134491986","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}
Y. Ueda, Tomoki Uchino, Daiki Ishi, Y. Ezoe, K. Ishikawa, M. Numazawa, Aoto Fukushima, Sae Sakuda, A. Inagaki, H. Morishita, Luna Sekiguchi, Takatoshi Murakawa, Yukine Tsuji, K. Mitsuda, K. Morishita, K. Nakajima
We are developing a novel Bragg reflection x-ray polarimeter using hot plastic deformation of silicon wafers. A Bragg reflection polarimeter has the advantage of simple principle and large modulation factor but suffers from the disadvantage of a narrow detectable energy band and difficulty to focus an incident beam. We overcome these disadvantages by bending a silicon wafer at high temperature. The bent Bragg reflection polarimeter have a wide energy band using different angles on the wafer and enable focusing. We have succeeded in measuring x-ray polarization with this method for the first time using a sample optic made from a 4-inch silicon (100) wafer.
{"title":"Development of Bragg reflection-type x-ray polarimeter based on a bent silicon crystal using hot plastic deformation","authors":"Y. Ueda, Tomoki Uchino, Daiki Ishi, Y. Ezoe, K. Ishikawa, M. Numazawa, Aoto Fukushima, Sae Sakuda, A. Inagaki, H. Morishita, Luna Sekiguchi, Takatoshi Murakawa, Yukine Tsuji, K. Mitsuda, K. Morishita, K. Nakajima","doi":"10.1117/12.2629635","DOIUrl":"https://doi.org/10.1117/12.2629635","url":null,"abstract":"We are developing a novel Bragg reflection x-ray polarimeter using hot plastic deformation of silicon wafers. A Bragg reflection polarimeter has the advantage of simple principle and large modulation factor but suffers from the disadvantage of a narrow detectable energy band and difficulty to focus an incident beam. We overcome these disadvantages by bending a silicon wafer at high temperature. The bent Bragg reflection polarimeter have a wide energy band using different angles on the wafer and enable focusing. We have succeeded in measuring x-ray polarization with this method for the first time using a sample optic made from a 4-inch silicon (100) wafer.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"4 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":"116774920","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}
Y. Evangelista, F. Fiore, R. Campana, F. Ceraudo, Giovanni Della Casa, E. Demenev, G. Dilillo, M. Fiorini, M. Grassi, A. Guzmán, P. Hedderman, E. Marchesini, G. Morgante, F. Mele, P. Nogara, A. Nuti, R. Piazzolla, Samuel Pliego Caballero, I. Rashevskaya, F. Russo, G. Sottile, C. Labanti, Giulia Baroni, P. Bellutti, G. Bertuccio, Jiewei Cao, Tianxiang Chen, I. Dedolli, M. Feroci, F. Fuschino, M. Gandola, N. Gao, F. Ficorella, P. Malcovati, A. Picciotto, A. Rachevski, A. Santangelo, C. Tenzer, A. Vacchi, Lingjun Wang, Yupeng Xu, G. Zampa, N. Zampa, N. Zorzi
HERMES (high energy rapid modular ensemble of satellites) is a space-borne mission based on a constellation of nano-satellites flying in a low-Earth orbit (LEO). The six 3U CubeSat buses host new miniaturized instruments hosting a hybrid silicon drift detector/GAGG:Ce scintillator photodetector system sensitive to x-rays and gamma-rays. HERMES will probe the temporal emission of bright high-energy transients such as gamma-ray bursts (GRBs), ensuring a fast transient localization (with arcmin-level accuracy) in a field of view of several steradians exploiting the triangulation technique. With a foreseen launch date in late 2023, HERMES transient monitoring represents a keystone capability to complement the next generation of gravitational wave experiments. Moreover, the HERMES constellation will operate in conjunction with the space industry responsive intelligent thermal (SpIRIT) 6U CubeSat, to be launched in early 2023. SpIRIT is an Australian-Italian mission for high-energy astrophysics that will carry in a sun-synchronous orbit (SSO) an actively cooled HERMES detector system payload. On behalf of the HERMES collaboration, in this paper we will illustrate the HERMES and SpIRIT payload design, integration and tests, highlighting the technical solutions adopted to allow a wide-energy-band and sensitive x-ray and gamma-ray detector to be accommodated in a 1U CubeSat volume.
{"title":"Design, integration, and test of the scientific payloads on-board the HERMES constellation and the SpIRIT mission","authors":"Y. Evangelista, F. Fiore, R. Campana, F. Ceraudo, Giovanni Della Casa, E. Demenev, G. Dilillo, M. Fiorini, M. Grassi, A. Guzmán, P. Hedderman, E. Marchesini, G. Morgante, F. Mele, P. Nogara, A. Nuti, R. Piazzolla, Samuel Pliego Caballero, I. Rashevskaya, F. Russo, G. Sottile, C. Labanti, Giulia Baroni, P. Bellutti, G. Bertuccio, Jiewei Cao, Tianxiang Chen, I. Dedolli, M. Feroci, F. Fuschino, M. Gandola, N. Gao, F. Ficorella, P. Malcovati, A. Picciotto, A. Rachevski, A. Santangelo, C. Tenzer, A. Vacchi, Lingjun Wang, Yupeng Xu, G. Zampa, N. Zampa, N. Zorzi","doi":"10.1117/12.2628978","DOIUrl":"https://doi.org/10.1117/12.2628978","url":null,"abstract":"HERMES (high energy rapid modular ensemble of satellites) is a space-borne mission based on a constellation of nano-satellites flying in a low-Earth orbit (LEO). The six 3U CubeSat buses host new miniaturized instruments hosting a hybrid silicon drift detector/GAGG:Ce scintillator photodetector system sensitive to x-rays and gamma-rays. HERMES will probe the temporal emission of bright high-energy transients such as gamma-ray bursts (GRBs), ensuring a fast transient localization (with arcmin-level accuracy) in a field of view of several steradians exploiting the triangulation technique. With a foreseen launch date in late 2023, HERMES transient monitoring represents a keystone capability to complement the next generation of gravitational wave experiments. Moreover, the HERMES constellation will operate in conjunction with the space industry responsive intelligent thermal (SpIRIT) 6U CubeSat, to be launched in early 2023. SpIRIT is an Australian-Italian mission for high-energy astrophysics that will carry in a sun-synchronous orbit (SSO) an actively cooled HERMES detector system payload. On behalf of the HERMES collaboration, in this paper we will illustrate the HERMES and SpIRIT payload design, integration and tests, highlighting the technical solutions adopted to allow a wide-energy-band and sensitive x-ray and gamma-ray detector to be accommodated in a 1U CubeSat volume.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"19 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":"122115198","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. Amati, C. Labanti, S. Mereghetti, F. Frontera, R. Campana, N. Auricchio, G. Baldazzi, P. Bellutti, G. Bertuccio, M. Branchesi, R. C. Butler, M. Caballero-Garcia, A. Camisasca, A. Castro-Tirado, L. Cavazzini, R. Ciolfi, A. De Rosa, F. Evangelisti, R. Farinelli, L. Ferro, F. Ficorella, M. Fiorini, F. Fuschino, J. Gasent-Blesa, G. Ghirlanda, M. Grassi, C. Guidorzi, P. Hedderman, I. Kuvvetli, G. La Rosa, P. Lorenzi, P. Malcovati, E. Marchesini, M. Marisaldi, M. Melchiorri, F. Mele, Malgorzata Mikhalska, M. Orlandini, P. Orleanski, S. Pedersen, R. Piazzolla, A. Rachevski, I. Rashevskaya, P. Rosati, V. Reglero, S. Ronchini, A. Santangelo, R. Salvaterra, P. Sarra, F. Sortino, G. Sottile, G. Stratta, S. Squerzanti, J. Stephen, C. Tenzer, L. Terenzi, A. Trois, A. Vacchi, E. Virgilli, A. Volpe, M. Winkler, G. Zampa, N. Zampa, A. Zdziarski
We describe the science case, design and expected performances of the X/Gamma-ray Imaging Spectrometer (XGIS), a GRB and transients monitor developed and studied for the THESEUS mission project, capable of covering an exceptionally wide energy band (2 keV – 10 MeV), with imaging capabilities and location accuracy <15 arcmin up to 150 keV over a Field of View of 2sr, a few hundreds eV energy resolution in the X-ray band (<30 keV) and few micro seconds time resolution over the whole energy band. Thanks to a design based on a modular approach, the XGIS can be easily re-scaled and adapted for fitting the available resources and specific scientific objectives of future high-energy astrophysics missions, and especially those aimed at fully exploiting GRBs and high-energy transients for multi-messenger astrophysics and fundamental physics.
{"title":"The X/Gamma-ray Imaging Spectrometer (XGIS) for THESEUS and other mission opportunities","authors":"L. Amati, C. Labanti, S. Mereghetti, F. Frontera, R. Campana, N. Auricchio, G. Baldazzi, P. Bellutti, G. Bertuccio, M. Branchesi, R. C. Butler, M. Caballero-Garcia, A. Camisasca, A. Castro-Tirado, L. Cavazzini, R. Ciolfi, A. De Rosa, F. Evangelisti, R. Farinelli, L. Ferro, F. Ficorella, M. Fiorini, F. Fuschino, J. Gasent-Blesa, G. Ghirlanda, M. Grassi, C. Guidorzi, P. Hedderman, I. Kuvvetli, G. La Rosa, P. Lorenzi, P. Malcovati, E. Marchesini, M. Marisaldi, M. Melchiorri, F. Mele, Malgorzata Mikhalska, M. Orlandini, P. Orleanski, S. Pedersen, R. Piazzolla, A. Rachevski, I. Rashevskaya, P. Rosati, V. Reglero, S. Ronchini, A. Santangelo, R. Salvaterra, P. Sarra, F. Sortino, G. Sottile, G. Stratta, S. Squerzanti, J. Stephen, C. Tenzer, L. Terenzi, A. Trois, A. Vacchi, E. Virgilli, A. Volpe, M. Winkler, G. Zampa, N. Zampa, A. Zdziarski","doi":"10.1117/12.2630178","DOIUrl":"https://doi.org/10.1117/12.2630178","url":null,"abstract":"We describe the science case, design and expected performances of the X/Gamma-ray Imaging Spectrometer (XGIS), a GRB and transients monitor developed and studied for the THESEUS mission project, capable of covering an exceptionally wide energy band (2 keV – 10 MeV), with imaging capabilities and location accuracy <15 arcmin up to 150 keV over a Field of View of 2sr, a few hundreds eV energy resolution in the X-ray band (<30 keV) and few micro seconds time resolution over the whole energy band. Thanks to a design based on a modular approach, the XGIS can be easily re-scaled and adapted for fitting the available resources and specific scientific objectives of future high-energy astrophysics missions, and especially those aimed at fully exploiting GRBs and high-energy transients for multi-messenger astrophysics and fundamental physics.","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":"126034693","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}
A. Di Marco, F. Muleri, S. Fabiani, F. La Monaca, J. Rankin, P. Soffitta, L. Baldini, E. Costa, E. Del Monte, R. Ferrazzoli, C. Lefevre, L. Maiolo, F. Maita, A. Manfreda, A. Morbidini, S. O’Dell, B. Ramsey, A. Ratheesh, C. Sgro’, A. Trois, A. Tennant, M. Weisskopf
The imaging x-ray polarimetry explorer (IXPE) was launched on December 9, 2021, from Cape Canaveral into a low-Earth equatorial orbit. The mission, led by NASA in collaboration with the Italian Space Agency (ASI), features three identical telescopes, each with an imaging x-ray photoelectric polarimeter at the focus of an x-ray mirror assembly. Each focal-plane detector includes a set of four calibration sources powered by a 55Fe nuclide to monitor the detector’s performance. Of these sources, one produces polarized x-rays at two energies and the remaining three generate unpolarized radiation. Here we present the status of this monitoring program, starting from installation of the flight nuclides before on-ground environmental testing of the observatory through recent on-orbit measurements during science operations.
{"title":"In-orbit monitoring of the imaging x-ray polarimeters on-board IXPE","authors":"A. Di Marco, F. Muleri, S. Fabiani, F. La Monaca, J. Rankin, P. Soffitta, L. Baldini, E. Costa, E. Del Monte, R. Ferrazzoli, C. Lefevre, L. Maiolo, F. Maita, A. Manfreda, A. Morbidini, S. O’Dell, B. Ramsey, A. Ratheesh, C. Sgro’, A. Trois, A. Tennant, M. Weisskopf","doi":"10.1117/12.2629413","DOIUrl":"https://doi.org/10.1117/12.2629413","url":null,"abstract":"The imaging x-ray polarimetry explorer (IXPE) was launched on December 9, 2021, from Cape Canaveral into a low-Earth equatorial orbit. The mission, led by NASA in collaboration with the Italian Space Agency (ASI), features three identical telescopes, each with an imaging x-ray photoelectric polarimeter at the focus of an x-ray mirror assembly. Each focal-plane detector includes a set of four calibration sources powered by a 55Fe nuclide to monitor the detector’s performance. Of these sources, one produces polarized x-rays at two energies and the remaining three generate unpolarized radiation. Here we present the status of this monitoring program, starting from installation of the flight nuclides before on-ground environmental testing of the observatory through recent on-orbit measurements during science operations.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"71 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":"124186190","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. Gatilova, J. Valentin, J. Treuttel, A. Feret, G. Gay, S. Caroopen, T. Vacelet, S. Mignoni, J. Krieg, Y. Jin, J. Roux
The Submillimetre-Wave Instrument (SWI) is a passive microwave spectrometer of JUpiter ICy moons Explorer (JUICE), a large-class mission of ESA's Cosmic Vision. It consists of two 600 GHz and 1200 GHz dual channel radiometers that involve compact, non-cryogenic Schottky diodes based solid-state devices for the mixer and last stage local oscillator frequency multipliers that are passively cooled to 150K. In this paper we will present the exhaustive qualification and endurance testing of the 300 GHz doubler element, standing at the interface between the warm (300K) and cold (150K) electronic front-end for both 600GHz and 1200 GHz channels. We present its associated extensive set of screening and lot acceptance testing as a part of the delivery of the final MMIC subcomponents integrated in the flight and flight spare models including the test structures used, the tests conditions as well as the failure criteria (PDA, allowable drifts).
{"title":"Exhaustive qualification and endurance testing of the 300 GHz frequency doubler of the sub-millimeter instrument of the Jupiter Icy Moon Explorer mission","authors":"L. Gatilova, J. Valentin, J. Treuttel, A. Feret, G. Gay, S. Caroopen, T. Vacelet, S. Mignoni, J. Krieg, Y. Jin, J. Roux","doi":"10.1117/12.2630402","DOIUrl":"https://doi.org/10.1117/12.2630402","url":null,"abstract":"The Submillimetre-Wave Instrument (SWI) is a passive microwave spectrometer of JUpiter ICy moons Explorer (JUICE), a large-class mission of ESA's Cosmic Vision. It consists of two 600 GHz and 1200 GHz dual channel radiometers that involve compact, non-cryogenic Schottky diodes based solid-state devices for the mixer and last stage local oscillator frequency multipliers that are passively cooled to 150K. In this paper we will present the exhaustive qualification and endurance testing of the 300 GHz doubler element, standing at the interface between the warm (300K) and cold (150K) electronic front-end for both 600GHz and 1200 GHz channels. We present its associated extensive set of screening and lot acceptance testing as a part of the delivery of the final MMIC subcomponents integrated in the flight and flight spare models including the test structures used, the tests conditions as well as the failure criteria (PDA, allowable drifts).","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"60 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":"129478869","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}
The Sun is a privileged place to study particle acceleration, a fundamental astrophysical problem throughout the universe. The extreme ultra-violet (EUV) contains a number of narrow emission lines formed in all layers of the solar atmosphere whose profiles allow the measurement of plasma properties like density and temperature, along with the presence of non-Maxwellian particle distributions to be diagnosed. The only way to observe is from space, since EUV radiation is absorbed by the Earth’s atmosphere. Integral field spectroscopy combined with polarimetry is key for the study of the Sun, but the current EUV technology is limiting: the transmission of optical fibers IFUs (integral field units) is low and in-flight effects affect polarisation measurements. The best solution seems to be image slicers. However, this technology has not yet been developed for the EUV spectral range. This communication explores a new highly efficient and compact integral field spectrograph layout based on the application of image slicers combining the surfaces of the IFU with those of the spectrograph, suitable for space applications.
{"title":"Exploring the application of image slicers for the EUV for the next generation of solar space missions","authors":"Ariadna Calcines-Rosario, S. Matthews, H. Reid","doi":"10.1117/12.2626860","DOIUrl":"https://doi.org/10.1117/12.2626860","url":null,"abstract":"The Sun is a privileged place to study particle acceleration, a fundamental astrophysical problem throughout the universe. The extreme ultra-violet (EUV) contains a number of narrow emission lines formed in all layers of the solar atmosphere whose profiles allow the measurement of plasma properties like density and temperature, along with the presence of non-Maxwellian particle distributions to be diagnosed. The only way to observe is from space, since EUV radiation is absorbed by the Earth’s atmosphere. Integral field spectroscopy combined with polarimetry is key for the study of the Sun, but the current EUV technology is limiting: the transmission of optical fibers IFUs (integral field units) is low and in-flight effects affect polarisation measurements. The best solution seems to be image slicers. However, this technology has not yet been developed for the EUV spectral range. This communication explores a new highly efficient and compact integral field spectrograph layout based on the application of image slicers combining the surfaces of the IFU with those of the spectrograph, suitable for space applications.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"341 ","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120969171","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}
K. Tamura, T. Hayashi, R. Boissay-Malaquin, T. Okajima, Toshiki Sato, L. Olsen, R. Koenecke, Wilson Lara, Leor Bleier, M. Eckart, M. Leutenegger, T. Yaqoob, M. Chiao
The X-Ray Imaging and Spectroscopy Mission (XRISM) is an x-ray astronomy satellite being developed in collaboration between NASA, JAXA, and ESA, and is scheduled for launch in Japanese fiscal year 2022. The x-ray mirror assembly (XMA) for XRISM has been developed at NASA’s Goddard Space Flight Center (GSFC). Two units were fabricated, one each for a micro-calorimeter array (Resolve) and a CCD array (Xtend). The ground calibration and performance verification measurements for XRISM XMA were taken at the 100-m x-ray beamline at NASA/GSFC. X-ray images at the focal plane were taken by scanning across the entire mirror aperture with a 15 mm×15 mm pencil beam. These measurements were performed at seven different energies including 1.5 keV (Al Kα), 4.5 keV (Ti Kα), 6.4 keV (Fe Kα), 8.0 keV (Cu Kα), 9.4 keV (Pt Lα), 11.1 keV (Pt Lβ), 17.5 keV (Mo Kα). A method for background subtraction was developed using a back-illuminated CCD camera with a 30 mm×30 mm (i.e. 17′×17′) array at the focal plane. Results from the measurements on the imaging performance show a small energy dependence in the angular resolution. We will also present the results of the stray light measurements.
{"title":"Ground calibration of the x-ray mirror assembly for the X-Ray Imaging and Spectroscopy Mission (XRISM) II: imaging performance and stray light","authors":"K. Tamura, T. Hayashi, R. Boissay-Malaquin, T. Okajima, Toshiki Sato, L. Olsen, R. Koenecke, Wilson Lara, Leor Bleier, M. Eckart, M. Leutenegger, T. Yaqoob, M. Chiao","doi":"10.1117/12.2629534","DOIUrl":"https://doi.org/10.1117/12.2629534","url":null,"abstract":"The X-Ray Imaging and Spectroscopy Mission (XRISM) is an x-ray astronomy satellite being developed in collaboration between NASA, JAXA, and ESA, and is scheduled for launch in Japanese fiscal year 2022. The x-ray mirror assembly (XMA) for XRISM has been developed at NASA’s Goddard Space Flight Center (GSFC). Two units were fabricated, one each for a micro-calorimeter array (Resolve) and a CCD array (Xtend). The ground calibration and performance verification measurements for XRISM XMA were taken at the 100-m x-ray beamline at NASA/GSFC. X-ray images at the focal plane were taken by scanning across the entire mirror aperture with a 15 mm×15 mm pencil beam. These measurements were performed at seven different energies including 1.5 keV (Al Kα), 4.5 keV (Ti Kα), 6.4 keV (Fe Kα), 8.0 keV (Cu Kα), 9.4 keV (Pt Lα), 11.1 keV (Pt Lβ), 17.5 keV (Mo Kα). A method for background subtraction was developed using a back-illuminated CCD camera with a 30 mm×30 mm (i.e. 17′×17′) array at the focal plane. Results from the measurements on the imaging performance show a small energy dependence in the angular resolution. We will also present the results of the stray light measurements.","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":"122883594","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. Bloser, W. Vestrand, M. Hehlen, K. Katko, L. Parker, D. Beckman, J. Sedillo, Justin M. McGlown, John Michel, Rory H. Scobie, Anthony E. Nelson, T. Roth, Daniel C. Poulson
The origin of the cosmic diffuse gamma-ray (CDG) background in the 0.3–10 MeV energy range is a mystery that has persisted for over 40 years. The Mini Astrophysical MeV Background Observatory (MAMBO) is a new CubeSat mission under development at Los Alamos National Laboratory with the goal of addressing this longstanding puzzle. The concept is motivated by the fact that, since the MeV CDG is relatively bright, only a small detector is required to make high-quality measurements of it. Indeed, the sensitivity of space-based gamma-ray instruments to the CDG is limited not by size, but by the locally generated instrumental background produced by interactions of energetic particles in spacecraft materials. Comparatively tiny CubeSat platforms provide a uniquely quiet environment relative to previous MeV gamma-ray science missions. The MAMBO mission will provide the best measurements ever made of the MeV CDG spectrum and angular distribution, utilizing two key innovations: 1) low instrumental background on a 12U CubeSat platform; and 2) an innovative shielded spectrometer design that simultaneously measures signal and background. Los Alamos is partnering with commercial vendors for the 12U CubeSat bus and ground station network, which we expect will become a new paradigm for low-cost, fast-turnaround space science missions. We describe the MAMBO instrument and mission concept in detail and present the expected scientific return.
{"title":"The Mini Astrophysical MeV Background Observatory (MAMBO) CubeSat mission for gamma-ray astronomy","authors":"P. Bloser, W. Vestrand, M. Hehlen, K. Katko, L. Parker, D. Beckman, J. Sedillo, Justin M. McGlown, John Michel, Rory H. Scobie, Anthony E. Nelson, T. Roth, Daniel C. Poulson","doi":"10.1117/12.2629069","DOIUrl":"https://doi.org/10.1117/12.2629069","url":null,"abstract":"The origin of the cosmic diffuse gamma-ray (CDG) background in the 0.3–10 MeV energy range is a mystery that has persisted for over 40 years. The Mini Astrophysical MeV Background Observatory (MAMBO) is a new CubeSat mission under development at Los Alamos National Laboratory with the goal of addressing this longstanding puzzle. The concept is motivated by the fact that, since the MeV CDG is relatively bright, only a small detector is required to make high-quality measurements of it. Indeed, the sensitivity of space-based gamma-ray instruments to the CDG is limited not by size, but by the locally generated instrumental background produced by interactions of energetic particles in spacecraft materials. Comparatively tiny CubeSat platforms provide a uniquely quiet environment relative to previous MeV gamma-ray science missions. The MAMBO mission will provide the best measurements ever made of the MeV CDG spectrum and angular distribution, utilizing two key innovations: 1) low instrumental background on a 12U CubeSat platform; and 2) an innovative shielded spectrometer design that simultaneously measures signal and background. Los Alamos is partnering with commercial vendors for the 12U CubeSat bus and ground station network, which we expect will become a new paradigm for low-cost, fast-turnaround space science missions. We describe the MAMBO instrument and mission concept in detail and present the expected scientific return.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"409 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":"115855119","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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