M. Feroci, G. Ambrosi, F. Ambrosino, M. Antonelli, A. Argan, Viktor Babinec, M. Barbera, J. Bayer, P. Bellutti, B. Bertucci, G. Bertuccio, X. Bi, M. Boezio, W. Bonvicini, G. Borghi, E. Bozzo, D. Baudin, F. Bouyjou, D. Brienza, F. Cadoux, R. Campana, Jiewei Cao, E. Cavazzuti, F. Ceraudo, Tianxiang Chen, Wen Chen, D. Cirrincione, Nicolas De Angelis, A. De Rosa, E. Del Monte, S. Di Cosimo, G. Dilillo, R. Dohnal, I. Donnarumma, Y. Evangelista, Qingmei Fan, Y. Favre, E. Fiandrini, F. Ficorella, F. Fuschino, N. Gao, O. Gevin, M. Grassi, M. Guedel, Xingbo Han, H. He, P. Hedderman, J. D. den Herder, R. Hynek, Bin Hong, G. Jin, M. Kole, V. Karas, M. Komarek, C. Labanti, Loghui Li, Tianming Li, Hong-guang Liang, O. Limousin, Rui Liu, U. Lo Cicero, Jens Lohering, G. Lombardi, F. Lu, T. Luo, P. Malcovati, Hanqi Mao, A. Marinucci, F. Mele, V. Mendes, Martin Merkl, A. Meuris, M. Michalska, A. Morbidini, G. Morgante, F. Muleri, R. Munini, L. Mussolin, B. Negri, P. Novák, W. Nowosielski, A. Nuti, P. Orleanski, R. Ottensa
The Large Area Detector (LAD) is the high-throughput, spectral-timing instrument onboard the eXTP mission, a flagship mission of the Chinese Academy of Sciences and the China National Space Administration, with a large European participation coordinated by Italy and Spain. The eXTP mission is currently performing its phase B study, with a target launch at the end-2027. The eXTP scientific payload includes four instruments (SFA, PFA, LAD and WFM) offering unprecedented simultaneous wide-band X-ray timing and polarimetry sensitivity. The LAD instrument is based on the design originally proposed for the LOFT mission. It envisages a deployed 3.2 m2 effective area in the 2-30 keV energy range, achieved through the technology of the large-area Silicon Drift Detectors - offering a spectral resolution of up to 200 eV FWHM at 6 keV - and of capillary plate collimators - limiting the field of view to about 1 degree. In this paper we will provide an overview of the LAD instrument design, its current status of development and anticipated performance.
大面积探测器(LAD)是中国科学院和中国国家航天局的旗舰任务eXTP任务上的高通量光谱定时仪器，由意大利和西班牙协调的大型欧洲参与。eXTP任务目前正在进行B阶段研究，目标是在2027年底发射。eXTP科学有效载荷包括四个仪器(SFA, PFA, LAD和WFM)，提供前所未有的同时宽带x射线定时和偏振灵敏度。LAD仪器是基于最初为LOFT任务提出的设计。它设想在2-30 keV能量范围内部署3.2 m2的有效面积，通过大面积硅漂移探测器技术实现-在6 keV时提供高达200 eV FWHM的光谱分辨率-以及毛细管板准直器-将视场限制在约1度。在本文中，我们将概述LAD仪器的设计，其目前的发展状况和预期性能。
{"title":"The large area detector onboard the eXTP mission","authors":"M. Feroci, G. Ambrosi, F. Ambrosino, M. Antonelli, A. Argan, Viktor Babinec, M. Barbera, J. Bayer, P. Bellutti, B. Bertucci, G. Bertuccio, X. Bi, M. Boezio, W. Bonvicini, G. Borghi, E. Bozzo, D. Baudin, F. Bouyjou, D. Brienza, F. Cadoux, R. Campana, Jiewei Cao, E. Cavazzuti, F. Ceraudo, Tianxiang Chen, Wen Chen, D. Cirrincione, Nicolas De Angelis, A. De Rosa, E. Del Monte, S. Di Cosimo, G. Dilillo, R. Dohnal, I. Donnarumma, Y. Evangelista, Qingmei Fan, Y. Favre, E. Fiandrini, F. Ficorella, F. Fuschino, N. Gao, O. Gevin, M. Grassi, M. Guedel, Xingbo Han, H. He, P. Hedderman, J. D. den Herder, R. Hynek, Bin Hong, G. Jin, M. Kole, V. Karas, M. Komarek, C. Labanti, Loghui Li, Tianming Li, Hong-guang Liang, O. Limousin, Rui Liu, U. Lo Cicero, Jens Lohering, G. Lombardi, F. Lu, T. Luo, P. Malcovati, Hanqi Mao, A. Marinucci, F. Mele, V. Mendes, Martin Merkl, A. Meuris, M. Michalska, A. Morbidini, G. Morgante, F. Muleri, R. Munini, L. Mussolin, B. Negri, P. Novák, W. Nowosielski, A. Nuti, P. Orleanski, R. Ottensa","doi":"10.1117/12.2628814","DOIUrl":"https://doi.org/10.1117/12.2628814","url":null,"abstract":"The Large Area Detector (LAD) is the high-throughput, spectral-timing instrument onboard the eXTP mission, a flagship mission of the Chinese Academy of Sciences and the China National Space Administration, with a large European participation coordinated by Italy and Spain. The eXTP mission is currently performing its phase B study, with a target launch at the end-2027. The eXTP scientific payload includes four instruments (SFA, PFA, LAD and WFM) offering unprecedented simultaneous wide-band X-ray timing and polarimetry sensitivity. The LAD instrument is based on the design originally proposed for the LOFT mission. It envisages a deployed 3.2 m2 effective area in the 2-30 keV energy range, achieved through the technology of the large-area Silicon Drift Detectors - offering a spectral resolution of up to 200 eV FWHM at 6 keV - and of capillary plate collimators - limiting the field of view to about 1 degree. In this paper we will provide an overview of the LAD instrument design, its current status of development and anticipated performance.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"28 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":"114879406","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. Salem Hesari, D. Henke, V. Reshetov, B. Veidt, A. Seyfollahi, F. Jiang, L. Knee
The radio instrumentation team (RIT) at NRC’s (National Research Council Canada) Herzberg astronomy and astrophysics research center (HAA) is currently developing a dual-linear polarization, single-feed Q-band cryogenic radio astronomy receiver to develop and demonstrate important technologies needed for front-end development for the next generation very large array (ngVLA) project lead by the National Radio Astronomy Observatory (NRAO). The specific target is the ngVLA band-5 receiver, which covers the frequency range 30.5–50.5 GHz. It also serves as a technology demonstrator for component development for ngVLA bands-3, 4, and 6. The Q-band receiver system is designed to achieve a receiver noise temperature of less than 20 K over 70% of the bandwidth and better than 24 K over the complete operating bandwidth, and is compliant with the current ngVLA Band-5 receiver requirement. The receiver system consists of a cryostat with a cooled feed horn, a turnstile OMT (orthomode transducer) plus two noise couplers for calibration, two cryogenic mHEMT low noise amplifiers with noise temperature lower than 14 K, IR filters, and a vacuum window for low-loss transmission of electromagnetic fields into the cryostat.
{"title":"Design and analysis of the NRC Q-band receiver for ngVLA Band-5","authors":"S. Salem Hesari, D. Henke, V. Reshetov, B. Veidt, A. Seyfollahi, F. Jiang, L. Knee","doi":"10.1117/12.2627870","DOIUrl":"https://doi.org/10.1117/12.2627870","url":null,"abstract":"The radio instrumentation team (RIT) at NRC’s (National Research Council Canada) Herzberg astronomy and astrophysics research center (HAA) is currently developing a dual-linear polarization, single-feed Q-band cryogenic radio astronomy receiver to develop and demonstrate important technologies needed for front-end development for the next generation very large array (ngVLA) project lead by the National Radio Astronomy Observatory (NRAO). The specific target is the ngVLA band-5 receiver, which covers the frequency range 30.5–50.5 GHz. It also serves as a technology demonstrator for component development for ngVLA bands-3, 4, and 6. The Q-band receiver system is designed to achieve a receiver noise temperature of less than 20 K over 70% of the bandwidth and better than 24 K over the complete operating bandwidth, and is compliant with the current ngVLA Band-5 receiver requirement. The receiver system consists of a cryostat with a cooled feed horn, a turnstile OMT (orthomode transducer) plus two noise couplers for calibration, two cryogenic mHEMT low noise amplifiers with noise temperature lower than 14 K, IR filters, and a vacuum window for low-loss transmission of electromagnetic fields into the cryostat.","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":"114670139","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. Sachkov, A. I. Gómez de Castro, B. Shustov, S. Sichevsky, A. Shugarov
The World Space Observatory–Ultraviolet mission (Spektr-UF, WSO-UV) is an efficient multipurpose orbital observatory for high- and low-resolution spectroscopy, high sensitivity imaging and slitless spectroscopy in the ultraviolet wavelength range. It will open new opportunities in (exo)planetary science, extragalactic astronomy, stellar astrophysics and cosmology. The observatory is based on a complex of scientific instruments including the T-170M telescope (aperture 170 cm), spectrographs and imagers. The payload should be ready in 2025. We briefly describe the current status of the mission.
{"title":"World Space Observatory: ultraviolet mission: status 2022","authors":"M. Sachkov, A. I. Gómez de Castro, B. Shustov, S. Sichevsky, A. Shugarov","doi":"10.1117/12.2629580","DOIUrl":"https://doi.org/10.1117/12.2629580","url":null,"abstract":"The World Space Observatory–Ultraviolet mission (Spektr-UF, WSO-UV) is an efficient multipurpose orbital observatory for high- and low-resolution spectroscopy, high sensitivity imaging and slitless spectroscopy in the ultraviolet wavelength range. It will open new opportunities in (exo)planetary science, extragalactic astronomy, stellar astrophysics and cosmology. The observatory is based on a complex of scientific instruments including the T-170M telescope (aperture 170 cm), spectrographs and imagers. The payload should be ready in 2025. We briefly describe the current status of the mission.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"76 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":"123222702","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. Civitani, S. Basso, V. Cotroneo, M. Demmer, M. Ghigo, S. Incorvaia, L. Lessio, G. Pareschi, G. Parodi, E. Redaelli, S. Schuler, D. Spiga, G. Toso, G. Vecchi
An X-ray Observatory, with superb imaging capabilities and with large throughput, has been recognised as a strategic missions in the Astro2020 decadal survey. The traditional solution foreseen for the realisation of very large x-ray mirror modules (diameters above 1 m) is the partition of the optics in azimuthal and radial modules (like Silicon Pore Optics in Athena). Even if this approach solves the initial problem of the procurement and the handling of very large substrates, it moves the difficulties in the second phase, when thousands of segments have to be assembled without degrading their optical performances. On the contrary, a simpler large mirror module design could correspond to less than a few hundred thin monolithic shells. As an example, the complete opto-mechanical design, compliant with the Lynx mass budget and based on fused silica, foresees that the shell thickness ranges between 2 and 4 mm (for mirror shells between 0.4 and 3 m diameter). The conceptual design of such an mirror module could be refined for smaller scale mission, keeping both the advantage of the design simplicity and of the high-resolution capability, achievable through the direct polishing approach. A technology development roadmap for this approach is funded in Italy by ASI and led by INAF-OAB. In this paper, we present the advancements obtained in the development of the different phases of the process and in the realisation of two new single-reflection shells (SR shells), almost representative of the final optical configuration foreseen for the mirror assembly. The first shell will be used to prove the figuring process in a lab-mount, built upon elements of the previous supporting structure concept. The second shell will be hosted in an upgraded lab-mount structure, which guarantees better performances (frequencies, gravity and thermo-elastic response) and which is suitable to test the transfer of the shell to a spider-like configuration.
{"title":"Progress on the realisation of high-resolution thin monolithic shells","authors":"M. Civitani, S. Basso, V. Cotroneo, M. Demmer, M. Ghigo, S. Incorvaia, L. Lessio, G. Pareschi, G. Parodi, E. Redaelli, S. Schuler, D. Spiga, G. Toso, G. Vecchi","doi":"10.1117/12.2628982","DOIUrl":"https://doi.org/10.1117/12.2628982","url":null,"abstract":"An X-ray Observatory, with superb imaging capabilities and with large throughput, has been recognised as a strategic missions in the Astro2020 decadal survey. The traditional solution foreseen for the realisation of very large x-ray mirror modules (diameters above 1 m) is the partition of the optics in azimuthal and radial modules (like Silicon Pore Optics in Athena). Even if this approach solves the initial problem of the procurement and the handling of very large substrates, it moves the difficulties in the second phase, when thousands of segments have to be assembled without degrading their optical performances. On the contrary, a simpler large mirror module design could correspond to less than a few hundred thin monolithic shells. As an example, the complete opto-mechanical design, compliant with the Lynx mass budget and based on fused silica, foresees that the shell thickness ranges between 2 and 4 mm (for mirror shells between 0.4 and 3 m diameter). The conceptual design of such an mirror module could be refined for smaller scale mission, keeping both the advantage of the design simplicity and of the high-resolution capability, achievable through the direct polishing approach. A technology development roadmap for this approach is funded in Italy by ASI and led by INAF-OAB. In this paper, we present the advancements obtained in the development of the different phases of the process and in the realisation of two new single-reflection shells (SR shells), almost representative of the final optical configuration foreseen for the mirror assembly. The first shell will be used to prove the figuring process in a lab-mount, built upon elements of the previous supporting structure concept. The second shell will be hosted in an upgraded lab-mount structure, which guarantees better performances (frequencies, gravity and thermo-elastic response) and which is suitable to test the transfer of the shell to a spider-like configuration.","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":"128455141","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}
Peter M. Solly, M. Biskach, Kai-wing Chan, J. Mazzarella, R. Mcclelland, R. Riveros, T. Saha, Will Zhang
The construction of x-ray telescopes that exhibit both high resolution and a low mass to effective area ratio poses many unique challenges. As the development of lightweight silicon x-ray mirrors approaches sub-arc-second resolution, previously inconsequential effects and complications must be addressed. This paper will address the structural analysis methods and experimental data that has been collected in attempts to address and resolve these issues for silicon mirror modules. Various parameters are run through trade space using finite element (FE) models and ray trace algorithms in attempts to contribute to the understanding of challenging and extremely sensitive conditions. Results and experimental data are then used to guide the on-going development of optics modules meeting the requirements of ambitious future x-ray missions. In this paper we discuss how the stringent distortion requirements of a high-resolution telescope are combined with launch vibration strength requirements to design optimized mirror modules.
{"title":"Design, analysis, and testing of x-ray mirror modules","authors":"Peter M. Solly, M. Biskach, Kai-wing Chan, J. Mazzarella, R. Mcclelland, R. Riveros, T. Saha, Will Zhang","doi":"10.1117/12.2629536","DOIUrl":"https://doi.org/10.1117/12.2629536","url":null,"abstract":"The construction of x-ray telescopes that exhibit both high resolution and a low mass to effective area ratio poses many unique challenges. As the development of lightweight silicon x-ray mirrors approaches sub-arc-second resolution, previously inconsequential effects and complications must be addressed. This paper will address the structural analysis methods and experimental data that has been collected in attempts to address and resolve these issues for silicon mirror modules. Various parameters are run through trade space using finite element (FE) models and ray trace algorithms in attempts to contribute to the understanding of challenging and extremely sensitive conditions. Results and experimental data are then used to guide the on-going development of optics modules meeting the requirements of ambitious future x-ray missions. In this paper we discuss how the stringent distortion requirements of a high-resolution telescope are combined with launch vibration strength requirements to design optimized mirror modules.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"5 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":"125552628","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}
V. Burwitz, G. Vacanti, M. Collon, N. Barrière, M. Bavdaz, I. Ferreira, M. Ayre, Emily Tipper, J. Eder, E. Breunig, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, T. Schmidt
Silicon pore optic (SPO) mirror modules (MMs) are being developed and produced for ESA’s ATHENA mission. The optics have, and will be, tested at MPEs PANTER x-ray test facility. We present the results obtained from tests performed at the PANTER x-ray test facility for the SPO MM-0050 that was produced to verify the latest optical performance (half energy width (HEW), effective area) of SPOs, supporting the ESA reviews of their optical performance. The preparations are ongoing at PANTER, ESA, cosine and Media Lario to perform complex opto-thermo-mechanical tests of the two full scale 1/6th sectors of the final ATHENA mirror assembly structure produced by the potential ATHENA primes Airbus Defence and Space and Thales Alenia Space. For these tests a set of three SPO MMs have been produced following the flight configuration. The MMs will be incorporated into the full scale 1/6th sectors to measure the impact of thermal gradients on the thermoelastic deformation of the structure and therefore the HEW performance. A description of the tests is presented here. PANTER is also involved in the development, testing, and fabrication of the mirror adapter structure (MAS) to support the 2.6-m diameter ATHENA mirror assembly module demonstrators (MAMD) during the planned x-ray tests at XRCF. A description of the PANTER tests and results will be presented in this paper together with a short overview of the MAS MGSE for XRCF.
{"title":"X-ray testing ATHENA optics at PANTER","authors":"V. Burwitz, G. Vacanti, M. Collon, N. Barrière, M. Bavdaz, I. Ferreira, M. Ayre, Emily Tipper, J. Eder, E. Breunig, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, T. Schmidt","doi":"10.1117/12.2630414","DOIUrl":"https://doi.org/10.1117/12.2630414","url":null,"abstract":"Silicon pore optic (SPO) mirror modules (MMs) are being developed and produced for ESA’s ATHENA mission. The optics have, and will be, tested at MPEs PANTER x-ray test facility. We present the results obtained from tests performed at the PANTER x-ray test facility for the SPO MM-0050 that was produced to verify the latest optical performance (half energy width (HEW), effective area) of SPOs, supporting the ESA reviews of their optical performance. The preparations are ongoing at PANTER, ESA, cosine and Media Lario to perform complex opto-thermo-mechanical tests of the two full scale 1/6th sectors of the final ATHENA mirror assembly structure produced by the potential ATHENA primes Airbus Defence and Space and Thales Alenia Space. For these tests a set of three SPO MMs have been produced following the flight configuration. The MMs will be incorporated into the full scale 1/6th sectors to measure the impact of thermal gradients on the thermoelastic deformation of the structure and therefore the HEW performance. A description of the tests is presented here. PANTER is also involved in the development, testing, and fabrication of the mirror adapter structure (MAS) to support the 2.6-m diameter ATHENA mirror assembly module demonstrators (MAMD) during the planned x-ray tests at XRCF. A description of the PANTER tests and results will be presented in this paper together with a short overview of the MAS MGSE for XRCF.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"53 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":"123319081","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 Hot Universe Baryon Surveyor (HUBS) mission requires a refrigeration system with temperatures below 100 mK to meet the high-resolution detection requirements of its superconducting transition edge sensor. The refrigeration scheme is to use a 4 K mechanical cryocooler as the pre-cooling stage and then use adiabatic demagnetization refrigerators (ADR) to obtain mK temperatures. One option for the pre-cooling stage is to use a pulse tube cryocooler. At present, a thermalcoupled and gas-coupled composite prototype based on helium-4 as the working gas has been successfully developed, a no-load temperature of 3.1 K, and a maximum cooling capacity of 22.0 mW at 4.2 K has been obtained, which can barely meet the demand. The calculation results show that the use of helium-3 instead of helium-4 as the working gas of the gas-coupled second and third stage is expected to further increase the cooling capacity to 53.1mW/4.2K, but 53 standard liters of helium-3 needs to be charged at room temperature. In order to reduce the amount of helium-3, a thermal-coupled three-stage pulse tube cryocooler is further designed. When the first and second compressors and their cold fingers use helium-4, while the third compressor and its cold finger use helium-3 as the working gas, the calculation results show that a cooling capacity of 57.5 mW/4.2 K can be obtained, and the amount of helium-3 that needs to be charged at room temperature is 11 standard liters, which effectively reduces the cost.
{"title":"A 4 K pulse tube cryocooler for the HUBS mission","authors":"Liubiao Chen, Z. Gao, Biao Yang, Junjie Wang","doi":"10.1117/12.2629334","DOIUrl":"https://doi.org/10.1117/12.2629334","url":null,"abstract":"The Hot Universe Baryon Surveyor (HUBS) mission requires a refrigeration system with temperatures below 100 mK to meet the high-resolution detection requirements of its superconducting transition edge sensor. The refrigeration scheme is to use a 4 K mechanical cryocooler as the pre-cooling stage and then use adiabatic demagnetization refrigerators (ADR) to obtain mK temperatures. One option for the pre-cooling stage is to use a pulse tube cryocooler. At present, a thermalcoupled and gas-coupled composite prototype based on helium-4 as the working gas has been successfully developed, a no-load temperature of 3.1 K, and a maximum cooling capacity of 22.0 mW at 4.2 K has been obtained, which can barely meet the demand. The calculation results show that the use of helium-3 instead of helium-4 as the working gas of the gas-coupled second and third stage is expected to further increase the cooling capacity to 53.1mW/4.2K, but 53 standard liters of helium-3 needs to be charged at room temperature. In order to reduce the amount of helium-3, a thermal-coupled three-stage pulse tube cryocooler is further designed. When the first and second compressors and their cold fingers use helium-4, while the third compressor and its cold finger use helium-3 as the working gas, the calculation results show that a cooling capacity of 57.5 mW/4.2 K can be obtained, and the amount of helium-3 that needs to be charged at room temperature is 11 standard liters, which effectively reduces the cost.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"105 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":"122417880","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}
Randall K. Smith, M. Bautz, J. Bregman, L. Brenneman, N. Brickhouse, E. Bulbul, V. Burwitz, Joseph Bushman, C. Canizares, D. Chakrabarty, P. Cheimets, E. Costantini, C. DeRoo, A. Falcone, A. Foster, L. Gallo, C. Grant, H. M. Guenther, R. Heilmann, S. Heine, B. Hine, D. Huenemoerder, Steve Jara, J. Kaastra, E. Kara, I. Kreykenbohm, K. Madsen, H. Marshall, M. McDonald, R. McEntaffer, Jonathan M. Miller, E. Miller, R. Mushotzky, K. Nandra, M. Nowak, F. Paerels, R. Petre, K. Poppenhaeger, A. Ptak, P. Reid, K. Ronzano, A. Różańska, J. Samra, J. Sanders, M. Schattenburg, J. Schonfeld, N. Schulz, A. Smale, P. Temi, L. Valencic, S. Walker, J. Wilms, S. Wolk
Supermassive black holes (SMBH) interact with gas in the interstellar and intergalactic media (ISM/IGM) in a process termed “feedback” that is key to the formation and evolution of galaxies and clusters. Characterizing the origins and physical mechanisms governing this feedback requires tracing the propagation of outflowing mass, energy and momentum from the vicinity of the SMBH out to megaparsec scales. Our ability to understand the interplay between feedback and structure evolution across multiple scales, as well as a wide range of other important astrophysical phenomena, depends on diagnostics only available in soft x-ray spectra (10-50 Å). Arcus combines high-resolution, efficient, lightweight x-ray gratings with silicon pore optics to provide R~2500 with an average effective area of ~200 cm2, an order of magnitude larger than the Chandra gratings. Flight-proven CCDs and instrument electronics are strong heritage components, while spacecraft and mission operations also reuse highly successful designs.
{"title":"Arcus: exploring the formation and evolution of clusters, galaxies, and stars","authors":"Randall K. Smith, M. Bautz, J. Bregman, L. Brenneman, N. Brickhouse, E. Bulbul, V. Burwitz, Joseph Bushman, C. Canizares, D. Chakrabarty, P. Cheimets, E. Costantini, C. DeRoo, A. Falcone, A. Foster, L. Gallo, C. Grant, H. M. Guenther, R. Heilmann, S. Heine, B. Hine, D. Huenemoerder, Steve Jara, J. Kaastra, E. Kara, I. Kreykenbohm, K. Madsen, H. Marshall, M. McDonald, R. McEntaffer, Jonathan M. Miller, E. Miller, R. Mushotzky, K. Nandra, M. Nowak, F. Paerels, R. Petre, K. Poppenhaeger, A. Ptak, P. Reid, K. Ronzano, A. Różańska, J. Samra, J. Sanders, M. Schattenburg, J. Schonfeld, N. Schulz, A. Smale, P. Temi, L. Valencic, S. Walker, J. Wilms, S. Wolk","doi":"10.1117/12.2628628","DOIUrl":"https://doi.org/10.1117/12.2628628","url":null,"abstract":"Supermassive black holes (SMBH) interact with gas in the interstellar and intergalactic media (ISM/IGM) in a process termed “feedback” that is key to the formation and evolution of galaxies and clusters. Characterizing the origins and physical mechanisms governing this feedback requires tracing the propagation of outflowing mass, energy and momentum from the vicinity of the SMBH out to megaparsec scales. Our ability to understand the interplay between feedback and structure evolution across multiple scales, as well as a wide range of other important astrophysical phenomena, depends on diagnostics only available in soft x-ray spectra (10-50 Å). Arcus combines high-resolution, efficient, lightweight x-ray gratings with silicon pore optics to provide R~2500 with an average effective area of ~200 cm2, an order of magnitude larger than the Chandra gratings. Flight-proven CCDs and instrument electronics are strong heritage components, while spacecraft and mission operations also reuse highly successful designs.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"28 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":"133716607","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. Scowen, R. Ignace, K. Gayley, G. Vasudevan, R. Woodruff, C. Neiner, S. Richardson, A. Nordt, T. Hull, S. Nikzad, C. Shapiro
Polstar combines, for the first time, the complementary benefits of spectroscopy and polarimetry to probe the complex interface between massive stars and the interstellar medium. Furthermore, it leverages an innovative combination of effective area and time coverage, to reach the diversity of targets necessary to transform our understanding of the ecology of star and planet creation. Detailed knowledge of these bright, yet distant objects, is crucial for understanding the transformation of our galaxy, from the barren landscape of the early Big Bang, into the chemically enriched environment that produced the solar system we call home. Polstar will map stellar wind and magnetospheric structures by uniting time domain, polarimetry and spectroscopy capability in the near- and far-UV (NUV and FUV), which are densely populated with high-opacity resonance lines encoding a rich array of diagnostic information. UV spectropolarimetry is equally important for probing interstellar dust and protoplanetary disks. The instrument combines advances in high reflectivity UV coatings and delta-doped CCDs with high quantum efficiencies to provide dedicated FUV spectropolarimetry for the first time in 25 years. The FUV channel (Ch1), covers 122-200nm at resolution R>30k, while the NUV channel (Ch2) covers 122-320nm at R~140-4,000. The instrumental polarization stability is built to provide signal-to-noise ratios (SNR) for UV polarimetry precision of 1x10-3 per exposure per resolution element (resel). Precision can be further improved with spectral binning and/or stacking multiple exposures. Polstar spectral resolution in Ch1 is >30x better than WUPPE, with 10x better effective area, while reaching shorter wavelength than WUPPE to access strong lines of species like NIV and SiIV. The 3-year mission of Polstar is 100x longer than WUPPE with orders of magnitude gains in stellar and interstellar observations.
{"title":"The Polstar high resolution spectropolarimetry MIDEX mission","authors":"P. Scowen, R. Ignace, K. Gayley, G. Vasudevan, R. Woodruff, C. Neiner, S. Richardson, A. Nordt, T. Hull, S. Nikzad, C. Shapiro","doi":"10.1117/12.2630103","DOIUrl":"https://doi.org/10.1117/12.2630103","url":null,"abstract":"Polstar combines, for the first time, the complementary benefits of spectroscopy and polarimetry to probe the complex interface between massive stars and the interstellar medium. Furthermore, it leverages an innovative combination of effective area and time coverage, to reach the diversity of targets necessary to transform our understanding of the ecology of star and planet creation. Detailed knowledge of these bright, yet distant objects, is crucial for understanding the transformation of our galaxy, from the barren landscape of the early Big Bang, into the chemically enriched environment that produced the solar system we call home. Polstar will map stellar wind and magnetospheric structures by uniting time domain, polarimetry and spectroscopy capability in the near- and far-UV (NUV and FUV), which are densely populated with high-opacity resonance lines encoding a rich array of diagnostic information. UV spectropolarimetry is equally important for probing interstellar dust and protoplanetary disks. The instrument combines advances in high reflectivity UV coatings and delta-doped CCDs with high quantum efficiencies to provide dedicated FUV spectropolarimetry for the first time in 25 years. The FUV channel (Ch1), covers 122-200nm at resolution R>30k, while the NUV channel (Ch2) covers 122-320nm at R~140-4,000. The instrumental polarization stability is built to provide signal-to-noise ratios (SNR) for UV polarimetry precision of 1x10-3 per exposure per resolution element (resel). Precision can be further improved with spectral binning and/or stacking multiple exposures. Polstar spectral resolution in Ch1 is >30x better than WUPPE, with 10x better effective area, while reaching shorter wavelength than WUPPE to access strong lines of species like NIV and SiIV. The 3-year mission of Polstar is 100x longer than WUPPE with orders of magnitude gains in stellar and interstellar observations.","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":"122756330","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. Shitvov, G. Savini, P. Hargrave, P. Ade, C. Tucker, R. Sudiwala, Jin Zhang, J. Gudmundsson, B. Winter, G. Pisano, M. van der Vorst
This paper presents recent results of ongoing European Space Agency funded program of work aimed at developing large dielectric lenses suitable for future satellite missions, with a particular focus on requirements for CMB polarimetry. Two lens solutions are being investigated: (i) polymer lenses with broadband multi-layer antireflection coatings; (ii) silicon lenses with surface-structured anti-reflection coating represented by directly machined pyramidal features. For each solution, base materials with and without coatings have been optically characterized over a range of temperatures down to ~10 K. Full lens solutions are under manufacture and will be tested in a bespoke large cryo-optical facility.
{"title":"Broadband coated lens solutions for FIR-mm-wave instruments","authors":"A. Shitvov, G. Savini, P. Hargrave, P. Ade, C. Tucker, R. Sudiwala, Jin Zhang, J. Gudmundsson, B. Winter, G. Pisano, M. van der Vorst","doi":"10.1117/12.2629968","DOIUrl":"https://doi.org/10.1117/12.2629968","url":null,"abstract":"This paper presents recent results of ongoing European Space Agency funded program of work aimed at developing large dielectric lenses suitable for future satellite missions, with a particular focus on requirements for CMB polarimetry. Two lens solutions are being investigated: (i) polymer lenses with broadband multi-layer antireflection coatings; (ii) silicon lenses with surface-structured anti-reflection coating represented by directly machined pyramidal features. For each solution, base materials with and without coatings have been optically characterized over a range of temperatures down to ~10 K. Full lens solutions are under manufacture and will be tested in a bespoke large cryo-optical facility.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"27 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":"116210330","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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