M. Bautz, R. Foster, C. Grant, B. LaMarr, A. Malonis, E. Miller, G. Prigozhin, B. Burke, M. Cooper, K. Donlon, R. Lambert, K. Warner, D. Young, T. Chattopadhyay, S. Herrmann, R. Morris, C. Leitz, S. Allen
Future high-resolution x-ray imaging missions at both strategic (Probe and Great Observatory) and smaller scales require mega-pixel focal planes with high frame rates and near-theoretical spectroscopic performance. We report test results from advanced charge-coupled devices (CCDs) developed at MIT Lincoln Laboratory for such missions. These devices incorporate two new technologies already demonstrated in small devices: a single-polysilicon gate structure enabling efficient, low-power charge transfer, and a low-noise pJFET output amplifier capable of < 3 electrons RMS noise at megahertz pixel rates. Here we report results from the first application of these technologies in a prototype large format (2k x 1k pixel, 5 x 2.5 cm2) frame transfer CCD with eight parallel outputs. In architecture, total area, and pixel count this device meets requirements for strategic missions. First measurements of noise, charge transfer efficiency and spectral resolution and achieved frame-rate are compared with requirements of candidate missions. Next steps toward maturation of this technology are briefly discussed.
未来在战略(探测器和大天文台)和更小尺度上的高分辨率x射线成像任务都需要具有高帧率和接近理论光谱性能的百万像素焦平面。我们报告了麻省理工学院林肯实验室为此类任务开发的先进电荷耦合器件(ccd)的测试结果。这些器件结合了两种已经在小型器件中展示的新技术:一种能够实现高效、低功率电荷转移的单多晶硅栅极结构，以及一种低噪声pJFET输出放大器，能够在兆赫像素率下产生< 3个电子RMS噪声。在这里，我们报告了这些技术在具有8个并行输出的大画幅(2k x 1k像素，5 x 2.5 cm2)帧传输CCD原型中的首次应用结果。该设备在结构、总面积、像素数等方面均满足战略任务的要求。首先，将噪声、电荷转移效率、光谱分辨率和实现的帧率与候选任务的要求进行了比较。本文简要讨论了该技术走向成熟的后续步骤。
{"title":"Performance of high frame-rate x-ray CCDs for future strategic missions","authors":"M. Bautz, R. Foster, C. Grant, B. LaMarr, A. Malonis, E. Miller, G. Prigozhin, B. Burke, M. Cooper, K. Donlon, R. Lambert, K. Warner, D. Young, T. Chattopadhyay, S. Herrmann, R. Morris, C. Leitz, S. Allen","doi":"10.1117/12.2630139","DOIUrl":"https://doi.org/10.1117/12.2630139","url":null,"abstract":"Future high-resolution x-ray imaging missions at both strategic (Probe and Great Observatory) and smaller scales require mega-pixel focal planes with high frame rates and near-theoretical spectroscopic performance. We report test results from advanced charge-coupled devices (CCDs) developed at MIT Lincoln Laboratory for such missions. These devices incorporate two new technologies already demonstrated in small devices: a single-polysilicon gate structure enabling efficient, low-power charge transfer, and a low-noise pJFET output amplifier capable of < 3 electrons RMS noise at megahertz pixel rates. Here we report results from the first application of these technologies in a prototype large format (2k x 1k pixel, 5 x 2.5 cm2) frame transfer CCD with eight parallel outputs. In architecture, total area, and pixel count this device meets requirements for strategic missions. First measurements of noise, charge transfer efficiency and spectral resolution and achieved frame-rate are compared with requirements of candidate missions. Next steps toward maturation of this technology are briefly discussed.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"2 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":"124266485","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}
S. Svendsen, S. Massahi, D. Ferreira, N. Gellert, Arne 'S Jegers, F. Christensen, A. Thete, B. Landgraf, M. Collon, E. Handick, D. Skroblin, L. Cibik, C. Gollwitzer, M. Krumrey, I. Ferreira, B. Shortt, M. Bavdaz
The future Athena observatory will feature optics with unprecedented collecting area enabled by silicon pore optics technology. In order to achieve the telescope effective area requirements at 1 keV and 7 keV, thin film coatings of iridium with a low-density overcoat are deposited onto the mirror substrates. Assembling the coated silicon pore optics plates into mirror modules for the Athena optics requires wet chemical processing and thermal annealing. While iridium appears to be compatible with the post-coating processes, previous studies have shown degradation of the low-density material. The overcoat layer is particularly critical for the low-energy telescope performance, so several candidate materials (boron carbide, silicon carbide and carbon) have been studied to identify a compatible thin film design. We present the characterisation of x-ray mirror performance using x-ray reflectometry, as well as the measurements of residual film stress with stylus profilometry. Furthermore, we evaluate the effects of post-coating treatment in order to recommend the most suitable overcoat material for the telescope.
{"title":"Characterisation of iridium and low-density bilayer coatings for the Athena optics","authors":"S. Svendsen, S. Massahi, D. Ferreira, N. Gellert, Arne 'S Jegers, F. Christensen, A. Thete, B. Landgraf, M. Collon, E. Handick, D. Skroblin, L. Cibik, C. Gollwitzer, M. Krumrey, I. Ferreira, B. Shortt, M. Bavdaz","doi":"10.1117/12.2629976","DOIUrl":"https://doi.org/10.1117/12.2629976","url":null,"abstract":"The future Athena observatory will feature optics with unprecedented collecting area enabled by silicon pore optics technology. In order to achieve the telescope effective area requirements at 1 keV and 7 keV, thin film coatings of iridium with a low-density overcoat are deposited onto the mirror substrates. Assembling the coated silicon pore optics plates into mirror modules for the Athena optics requires wet chemical processing and thermal annealing. While iridium appears to be compatible with the post-coating processes, previous studies have shown degradation of the low-density material. The overcoat layer is particularly critical for the low-energy telescope performance, so several candidate materials (boron carbide, silicon carbide and carbon) have been studied to identify a compatible thin film design. We present the characterisation of x-ray mirror performance using x-ray reflectometry, as well as the measurements of residual film stress with stylus profilometry. Furthermore, we evaluate the effects of post-coating treatment in order to recommend the most suitable overcoat material for the telescope.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"26 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":"124303573","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}
X. Xi, Biao Yang, Z. Gao, Liubiao Chen, Junjie Wang
The refrigeration system of the Hot Universe Baryon Surveyor (HUBS) mission intends to use the FAA paramagnetic salt adiabatic demagnetization refrigerator (ADR) to obtain temperatures below 100 mK. In order to obtain the 1 K pre-cooling temperature required by the FAA stage, one option is to use a GGG paramagnetic salt ADR, and the other option is to use a helium sorption cooler. A helium sorption cooler and the corresponding helium gas gap heat switch have been developed, and a cooling temperature of 800 mK has been obtained. This paper gives a detailed introduction to the prototype's structure, cooling performance, existing problems, and the next optimization measures.
{"title":"An 800 mK helium sorption cooler for the HUBS mission","authors":"X. Xi, Biao Yang, Z. Gao, Liubiao Chen, Junjie Wang","doi":"10.1117/12.2629770","DOIUrl":"https://doi.org/10.1117/12.2629770","url":null,"abstract":"The refrigeration system of the Hot Universe Baryon Surveyor (HUBS) mission intends to use the FAA paramagnetic salt adiabatic demagnetization refrigerator (ADR) to obtain temperatures below 100 mK. In order to obtain the 1 K pre-cooling temperature required by the FAA stage, one option is to use a GGG paramagnetic salt ADR, and the other option is to use a helium sorption cooler. A helium sorption cooler and the corresponding helium gas gap heat switch have been developed, and a cooling temperature of 800 mK has been obtained. This paper gives a detailed introduction to the prototype's structure, cooling performance, existing problems, and the next optimization measures.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"73 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":"121830574","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}
Chau-Ching Chiong, F. Nakamura, Atsushi Nishimura, R. Burns, Chen Chien, K. Dobashi, Y. Fujii, Chin-Ting Ho, Ted Huang, Yuh-Jing Hwang, Shou-Ting Jian, R. Kawabe, K. Kimura, Sheng-Yuan Liu, S. Lai, H. Ogawa, N. Okada, S. Kameno, T. Shimoikura, S. Takakuwa, K. Taniguchi, Wei-hao Wang, You-Ting Yeh, Y. Yamasaki, Y. Yonekura
The Ka-/Q-band in the microwave region of the electromagnetic spectrum is important for astrophysical and astrochemical research, particularly in the subfield of interstellar medium (ISM). The two bands cover not only the fundamental lines of the abundant dense gas tracer CS and its isotopologues but also a vast number of transitions of relatively large, long-chain, and/or complex organic species. Here, through a Taiwan-Japan collaboration, an extended Q-band (30-50GHz) receiver is built for Nobeyama 45-m telescope. The receiver front-end was installed at Nobeyama 45-m telescope in Nov. 2021 and obtained its first light in the same month. Commissioning and science verification (CSV) of the receiver was conducted in the first half of 2022. After commissioning, this receiver will be the only one in the world providing capability to cover 3 Zeeman transitions simultaneously at 7mm wavelength installed at large single dish telescope. It will be one of the most powerful facilities to explore the magnetic fields towards the pre-protostellar cores.
{"title":"Extended Q-band (eQ) receiver for Nobeyama 45-m Telescope","authors":"Chau-Ching Chiong, F. Nakamura, Atsushi Nishimura, R. Burns, Chen Chien, K. Dobashi, Y. Fujii, Chin-Ting Ho, Ted Huang, Yuh-Jing Hwang, Shou-Ting Jian, R. Kawabe, K. Kimura, Sheng-Yuan Liu, S. Lai, H. Ogawa, N. Okada, S. Kameno, T. Shimoikura, S. Takakuwa, K. Taniguchi, Wei-hao Wang, You-Ting Yeh, Y. Yamasaki, Y. Yonekura","doi":"10.1117/12.2629811","DOIUrl":"https://doi.org/10.1117/12.2629811","url":null,"abstract":"The Ka-/Q-band in the microwave region of the electromagnetic spectrum is important for astrophysical and astrochemical research, particularly in the subfield of interstellar medium (ISM). The two bands cover not only the fundamental lines of the abundant dense gas tracer CS and its isotopologues but also a vast number of transitions of relatively large, long-chain, and/or complex organic species. Here, through a Taiwan-Japan collaboration, an extended Q-band (30-50GHz) receiver is built for Nobeyama 45-m telescope. The receiver front-end was installed at Nobeyama 45-m telescope in Nov. 2021 and obtained its first light in the same month. Commissioning and science verification (CSV) of the receiver was conducted in the first half of 2022. After commissioning, this receiver will be the only one in the world providing capability to cover 3 Zeeman transitions simultaneously at 7mm wavelength installed at large single dish telescope. It will be one of the most powerful facilities to explore the magnetic fields towards the pre-protostellar cores.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"39 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":"123087705","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. Pelizzo, M. Padovani, A. Corso, G. Santi, M. Uslenghi, D. Faccini, M. Fiorini, S. Incorvaia, G. Toso, E. Fabbrica, M. Carminati, C. Fiorini, G. Favaro, M. Bazzan, G. Maggioni, G. Naletto, V. Andretta, A. Milillo
The planetary extreme ultraviolet spectrometer (PLUS) is a project funded by the Italian Space Agency focused on the development of an extreme (EUV) and far-ultraviolet (FUV) high-performance spectrograph, which adopts a dual channel optical scheme. Thanks to an optimized layout based on the use of variable line space (VLS) gratings in an off-Rowland configuration, high spectral and spatial resolution are achieved. The efficiency improvement is obtained by the optimization of the coatings on the optical components. Improved detection limit, shorter observations integration time and unprecedented performance in terms of dynamic range will be achieved by the use of high resolution/dynamic range solar blind photon counting detectors. The photon counting detectors will be based on a micro-channel plate (MCP) coupled with an application specific integrated circuit (ASIC) read out system.
{"title":"Spectroscopic observation of planetary and Moon exospheres in the ultraviolet","authors":"M. Pelizzo, M. Padovani, A. Corso, G. Santi, M. Uslenghi, D. Faccini, M. Fiorini, S. Incorvaia, G. Toso, E. Fabbrica, M. Carminati, C. Fiorini, G. Favaro, M. Bazzan, G. Maggioni, G. Naletto, V. Andretta, A. Milillo","doi":"10.1117/12.2633821","DOIUrl":"https://doi.org/10.1117/12.2633821","url":null,"abstract":"The planetary extreme ultraviolet spectrometer (PLUS) is a project funded by the Italian Space Agency focused on the development of an extreme (EUV) and far-ultraviolet (FUV) high-performance spectrograph, which adopts a dual channel optical scheme. Thanks to an optimized layout based on the use of variable line space (VLS) gratings in an off-Rowland configuration, high spectral and spatial resolution are achieved. The efficiency improvement is obtained by the optimization of the coatings on the optical components. Improved detection limit, shorter observations integration time and unprecedented performance in terms of dynamic range will be achieved by the use of high resolution/dynamic range solar blind photon counting detectors. The photon counting detectors will be based on a micro-channel plate (MCP) coupled with an application specific integrated circuit (ASIC) read out system.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"70 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":"115261434","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}
C. Feldman, R. Willingale, J. Pearson, G. Butcher, Philip Peterson, T. Crawford, P. Houghton, R. Speight, A. Lodge, C. Bicknell, J. Osborne, P. O'Brien, M. Bradshaw, V. Burwitz, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, Thomas Schmidt, D. Götz, K. Mercier, J. Le Duigou, F. Gonzalez, E. Schyns, Romain Roudot, R. Fairbend, J. Séguy
The space-based multi-band astronomical variable objects monitor (SVOM) is a Chinese–French mission due to be launched in 2023. It is composed of four space borne instruments: ECLAIRs, for detecting x-ray and gamma-ray transients; GRM, a gamma-ray spectrometer; VT, a visible telescope and the Microchannel X-ray Telescope (MXT). The MXT’s main goal is to precisely localize, and spectrally characterize x-ray afterglows of gamma-ray bursts. The MXT is a narrow-field-optimised lobster eye x-ray focusing telescope comprising an array of 25 square micro pore optics (MPOs), with a detector-limited field of view of ∼1 square degree, working in the energy band 0.2-10 keV. The SVOM flight model (FM) MXT optic (MOP) was designed, built and initially tested at the University of Leicester and a full calibration of the MOP was completed at the PANTER facility (MPE). It was then integrated in to the full proto flight model (PFM) MXT instrument before it returned to PANTER for the PFM MXT’s full calibration. We present the optic performance as part of the full FM MXT instrument calibration. The response of the telescope was studied at 11 energies from C-K (0.28 keV) to Ge-K (9.89 keV), including measurements of the effective area and the PSF size and shape. The focal length of the instrument was determined and details of the modelling and analysis used to predict the performance are presented. The measurements demonstrate that the actual effective area and PSF are in good agreement with the modelling.
{"title":"Calibration of the flight model lobster eye optic for SVOM","authors":"C. Feldman, R. Willingale, J. Pearson, G. Butcher, Philip Peterson, T. Crawford, P. Houghton, R. Speight, A. Lodge, C. Bicknell, J. Osborne, P. O'Brien, M. Bradshaw, V. Burwitz, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, Thomas Schmidt, D. Götz, K. Mercier, J. Le Duigou, F. Gonzalez, E. Schyns, Romain Roudot, R. Fairbend, J. Séguy","doi":"10.1117/12.2628635","DOIUrl":"https://doi.org/10.1117/12.2628635","url":null,"abstract":"The space-based multi-band astronomical variable objects monitor (SVOM) is a Chinese–French mission due to be launched in 2023. It is composed of four space borne instruments: ECLAIRs, for detecting x-ray and gamma-ray transients; GRM, a gamma-ray spectrometer; VT, a visible telescope and the Microchannel X-ray Telescope (MXT). The MXT’s main goal is to precisely localize, and spectrally characterize x-ray afterglows of gamma-ray bursts. The MXT is a narrow-field-optimised lobster eye x-ray focusing telescope comprising an array of 25 square micro pore optics (MPOs), with a detector-limited field of view of ∼1 square degree, working in the energy band 0.2-10 keV. The SVOM flight model (FM) MXT optic (MOP) was designed, built and initially tested at the University of Leicester and a full calibration of the MOP was completed at the PANTER facility (MPE). It was then integrated in to the full proto flight model (PFM) MXT instrument before it returned to PANTER for the PFM MXT’s full calibration. We present the optic performance as part of the full FM MXT instrument calibration. The response of the telescope was studied at 11 energies from C-K (0.28 keV) to Ge-K (9.89 keV), including measurements of the effective area and the PSF size and shape. The focal length of the instrument was determined and details of the modelling and analysis used to predict the performance are presented. The measurements demonstrate that the actual effective area and PSF are in good agreement with the modelling.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"1994 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":"128638253","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. I. Gómez de Castro, C. Miravet, G. Taubmann, L. Díez, J. Casalta, M. Sachkov, J. C. Vallejo, León Restrepo Quirós, Miguel Chaves, S. Kameda
OUL is a wide field imager designed as a small, additional payload to be attached to the Luna 26 mission. The instrument has a field of view of 20° × 20° and provides images with angular resolution 3 arcmin in several far ultraviolet bands, including Lyman-α, He II at 164nm and several continuum bands. The imager is designed to monitor the Earth’s exosphere and the ecliptic (+/-20°) primary at Lyman-α and in the 125-140 nm and 145-170 nm bands. In this contribution, the optical design of the instrument, its mechanical layout and the science program to be implemented will be described.
OUL是一种宽视场成像仪，设计为附加在月球26号任务上的小型附加有效载荷。该仪器的视场为20°× 20°，在多个远紫外波段(包括Lyman-α， He II在164nm和几个连续波段)提供角分辨率为3角分的图像。该成像仪设计用于监测地球的外大气层和黄道(+/-20°)主要在莱曼α和125-140 nm和145-170 nm波段。在这篇文章中，将描述仪器的光学设计，其机械布局和要实施的科学计划。
{"title":"OUL: an ultraviolet wide field imager for the Luna 26 mission","authors":"A. I. Gómez de Castro, C. Miravet, G. Taubmann, L. Díez, J. Casalta, M. Sachkov, J. C. Vallejo, León Restrepo Quirós, Miguel Chaves, S. Kameda","doi":"10.1117/12.2630627","DOIUrl":"https://doi.org/10.1117/12.2630627","url":null,"abstract":"OUL is a wide field imager designed as a small, additional payload to be attached to the Luna 26 mission. The instrument has a field of view of 20° × 20° and provides images with angular resolution 3 arcmin in several far ultraviolet bands, including Lyman-α, He II at 164nm and several continuum bands. The imager is designed to monitor the Earth’s exosphere and the ecliptic (+/-20°) primary at Lyman-α and in the 125-140 nm and 145-170 nm bands. In this contribution, the optical design of the instrument, its mechanical layout and the science program to be implemented will be described.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"54 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":"116230446","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. Treuttel, T. Thúróczy, A. Feret, G. Gay, L. Gatilova, T. Vacelet, C. Chaumont, E. Sernoux, P. Mondal, J. Puech
Planetary atmospheres are rich in molecular species with spectral rotational and vibrational signatures in the millimeter and submillimeter frequency range. In particular, the 520-680 GHz frequency ranges offers access to a various amount of minor and major constituents of the atmosphere, including water vapour (H2O), carbon monoxide (CO), hydrogen cyanide (HCN), carbon monosulfide (CS) and their isotopes to derive temperature and wind velocities [1] or surface emissivity [2]. Recently, we have developed and manufactured the 560 GHz subharmonic mixer, showing the excellent performances in the 525-625 GHz frequency region with mixer noise temperature of about 870 K, around 30hf/kB [3]. In this paper we present an update and extensive measurement showing that the mixer’s RF bandwidth can be extended up to 25% keeping the excellent performances. Assessment study of the radiometer modelling and Schottky junction parameter deviations will be presented. A best fit of the junction I/V allows to derive the main diode DC parameters retrofitted to analytical models such as [4]. We discuss efforts on implementation of large bandwidth receiver system, including solutions for local power across large bandwidth [5] or in complex systems using simultaneous molecular line observations [6].
{"title":"Demonstration of a 25% bandwidth 520-680 GHz Schottky receiver front-end for planetary science and remote sensing","authors":"J. Treuttel, T. Thúróczy, A. Feret, G. Gay, L. Gatilova, T. Vacelet, C. Chaumont, E. Sernoux, P. Mondal, J. Puech","doi":"10.1117/12.2630052","DOIUrl":"https://doi.org/10.1117/12.2630052","url":null,"abstract":"Planetary atmospheres are rich in molecular species with spectral rotational and vibrational signatures in the millimeter and submillimeter frequency range. In particular, the 520-680 GHz frequency ranges offers access to a various amount of minor and major constituents of the atmosphere, including water vapour (H2O), carbon monoxide (CO), hydrogen cyanide (HCN), carbon monosulfide (CS) and their isotopes to derive temperature and wind velocities [1] or surface emissivity [2]. Recently, we have developed and manufactured the 560 GHz subharmonic mixer, showing the excellent performances in the 525-625 GHz frequency region with mixer noise temperature of about 870 K, around 30hf/kB [3]. In this paper we present an update and extensive measurement showing that the mixer’s RF bandwidth can be extended up to 25% keeping the excellent performances. Assessment study of the radiometer modelling and Schottky junction parameter deviations will be presented. A best fit of the junction I/V allows to derive the main diode DC parameters retrofitted to analytical models such as [4]. We discuss efforts on implementation of large bandwidth receiver system, including solutions for local power across large bandwidth [5] or in complex systems using simultaneous molecular line observations [6].","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"59 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":"133740103","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. Mészáros, A. Pál, N. Werner, J. Řípa, M. Ohno, B. Csák, J. Kapuš, M. Frajt, J. Hudec, M. Rezenov, P. Hanák
Since transient events, such as gamma-ray bursts (GRBs), can be expected from any direction at any time, their detection and localization is difficult. For localizing transient events, we proposed the Cubesats applied for measuring and localising transients mission (CAMELOT), which will be a fleet of nanosatellites distributed evenly on low Earth orbits. As the first step, we designed a technical demonstration for the CAMELOT mission, named GRBAlpha. Even though this 1U satellite has a reduced size scintillator and different mechanical constraints, all the electronic subsystems and communication protocols are the same. GRBAlpha is operating in orbit since 2021 March 22 and it already detected numerous confirmed GRBs. For further details of the early results and ongoing operations see the related presentation at this conference. After this first success, we continue with the design of the 3U prototype of the CAMELOT satellite, which will host an eight times larger detector system integrated into two walls of the satellite. The main difference is the mechanical constraints of mounting the detector in its casing. While for GRBAlpha the reduced sized scintillator is located on the top (Z+) side of the satellite, for CAMELOT it is located on two of the sides. Since the CubeSat standard does not allow enough lateral extension on the sides, the casing has to be sunk into the satellite where it could interfere with the standard PC/104 stacking. Here, we present a solution on how to integrate the scintillator casing, the uniquely designed electronics and commercially available satellite subsystems.
{"title":"Towards the CAMELOT fleet of GRB detecting nano-satellites: the design concept of the 3U members based on the GRBAlpha and VZLUSAT-2 heritage","authors":"L. Mészáros, A. Pál, N. Werner, J. Řípa, M. Ohno, B. Csák, J. Kapuš, M. Frajt, J. Hudec, M. Rezenov, P. Hanák","doi":"10.1117/12.2630179","DOIUrl":"https://doi.org/10.1117/12.2630179","url":null,"abstract":"Since transient events, such as gamma-ray bursts (GRBs), can be expected from any direction at any time, their detection and localization is difficult. For localizing transient events, we proposed the Cubesats applied for measuring and localising transients mission (CAMELOT), which will be a fleet of nanosatellites distributed evenly on low Earth orbits. As the first step, we designed a technical demonstration for the CAMELOT mission, named GRBAlpha. Even though this 1U satellite has a reduced size scintillator and different mechanical constraints, all the electronic subsystems and communication protocols are the same. GRBAlpha is operating in orbit since 2021 March 22 and it already detected numerous confirmed GRBs. For further details of the early results and ongoing operations see the related presentation at this conference. After this first success, we continue with the design of the 3U prototype of the CAMELOT satellite, which will host an eight times larger detector system integrated into two walls of the satellite. The main difference is the mechanical constraints of mounting the detector in its casing. While for GRBAlpha the reduced sized scintillator is located on the top (Z+) side of the satellite, for CAMELOT it is located on two of the sides. Since the CubeSat standard does not allow enough lateral extension on the sides, the casing has to be sunk into the satellite where it could interfere with the standard PC/104 stacking. Here, we present a solution on how to integrate the scintillator casing, the uniquely designed electronics and commercially available satellite subsystems.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"23 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":"133480386","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. Thibert, L. Jacques, G. Terrasa, E. Lallemand, G. Rauw, C. Kintziger
The Athena mission in general and the x-ray integral field unit (X-IFU) instrument in particular are designed to address a wealth of scientific questions related to the science theme of the hot and energetic universe. X-IFU provides medium spatial resolution and high resolving power by means of a calorimetric detector. As the X-IFU detector needs to be operated at 50mK, the instrument is contained in a dewar. The aperture cylinder consists of a set of structural and thermal elements that carry and position at correct distances from the detector the first three dewar thermal filters, provide adequate thermal interfaces and protect the filters from contamination. In this paper, we present the Phase A-B1 contribution of Centre Spatial de Liège (CSL) to the X-IFU consortium. This summarizes to the elaboration of a baseline design for the aperture cylinder, and several demonstration models as a de-risking activity with the intent to increase the aperture cylinder maturity.
一般来说，雅典娜任务和x射线积分场单元(X-IFU)仪器的设计是为了解决与热和高能宇宙的科学主题相关的大量科学问题。X-IFU通过量热检测器提供中等空间分辨率和高分辨率。由于X-IFU探测器需要在50mK下工作，所以仪器被装在杜瓦瓶中。孔径圆柱体由一组结构和热元件组成，它们携带并放置在与探测器正确距离的前三个杜瓦热过滤器，提供足够的热界面并保护过滤器免受污染。在本文中，我们介绍了Centre Spatial de li (CSL)对X-IFU联盟的A-B1期贡献。这总结为孔径柱的基线设计的阐述，以及几个示范模型作为降低风险的活动，旨在提高孔径柱的成熟度。
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