Zhilei Xu, T. Bhandarkar, G. Coppi, A. Kofman, J. Orlowski-Scherer, N. Zhu, Aamir Ali, K. Arnold, J. Austermann, Steve K. Choi, J. Connors, N. Cothard, M. Devlin, S. Dicker, B. Dober, S. Duff, G. Fabbian, N. Galitzki, Saianeesh K. Haridas, K. Harrington, E. Healy, S. Ho, J. Hubmayr, J. Iuliano, J. Lashner, Yaqiong Li, M. Limon, B. Koopman, H. McCarrick, Jenna Moore, F. Nati, M. Niemack, C. Reichardt, K. P. Sarmiento, J. Seibert, M. Silva-Feaver, Rita F. Sonka, S. Staggs, R. Thornton, E. Vavagiakis, M. Vissers, S. Walker, Yuhan Wang, Edward J. Wollack, K. Zheng
The Simons Observatory (SO) will observe the cosmic microwave background (CMB) from Cerro Toco in the Atacama Desert of Chile. The observatory consists of three 0.5 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT), covering six frequency bands centering around 30, 40, 90, 150, 230, and 280 GHz. The SO observations will transform the understanding of our universe by characterizing the properties of the early universe, measuring the number of relativistic species and the mass of neutrinos, improving our understanding of galaxy evolution, and constraining the properties of cosmic reionization. As a critical instrument, the Large Aperture Telescope Receiver (LATR) is designed to cool $sim$ 60,000 transition-edge sensors (TES) to $<$ 100 mK on a 1.7 m diameter focal plane. The unprecedented scale of the LATR drives a complex design. In this paper, we will first provide an overview of the LATR design. Integration and validation of the LATR design are discussed in detail, including mechanical strength, optical alignment, and cryogenic performance of the five cryogenic stages (80 K, 40 K, 4 K, 1 K, and 100 mK). We will also discuss the microwave-multiplexing ($mu$Mux) readout system implemented in the LATR and demonstrate the operation of dark prototype TES bolometers. The $mu$Mux readout technology enables one coaxial loop to read out $mathcal{O}(10^3)$ TES detectors. Its implementation within the LATR serves as a critical validation for the complex RF chain design. The successful validation of the LATR performance is not only a critical milestone within the Simons Observatory, it also provides a valuable reference for other experiments, e.g. CCAT-prime and CMB-S4.
{"title":"The Simons Observatory: the Large Aperture Telescope Receiver (LATR) integration and validation results","authors":"Zhilei Xu, T. Bhandarkar, G. Coppi, A. Kofman, J. Orlowski-Scherer, N. Zhu, Aamir Ali, K. Arnold, J. Austermann, Steve K. Choi, J. Connors, N. Cothard, M. Devlin, S. Dicker, B. Dober, S. Duff, G. Fabbian, N. Galitzki, Saianeesh K. Haridas, K. Harrington, E. Healy, S. Ho, J. Hubmayr, J. Iuliano, J. Lashner, Yaqiong Li, M. Limon, B. Koopman, H. McCarrick, Jenna Moore, F. Nati, M. Niemack, C. Reichardt, K. P. Sarmiento, J. Seibert, M. Silva-Feaver, Rita F. Sonka, S. Staggs, R. Thornton, E. Vavagiakis, M. Vissers, S. Walker, Yuhan Wang, Edward J. Wollack, K. Zheng","doi":"10.1117/12.2576151","DOIUrl":"https://doi.org/10.1117/12.2576151","url":null,"abstract":"The Simons Observatory (SO) will observe the cosmic microwave background (CMB) from Cerro Toco in the Atacama Desert of Chile. The observatory consists of three 0.5 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT), covering six frequency bands centering around 30, 40, 90, 150, 230, and 280 GHz. The SO observations will transform the understanding of our universe by characterizing the properties of the early universe, measuring the number of relativistic species and the mass of neutrinos, improving our understanding of galaxy evolution, and constraining the properties of cosmic reionization. As a critical instrument, the Large Aperture Telescope Receiver (LATR) is designed to cool $sim$ 60,000 transition-edge sensors (TES) to $<$ 100 mK on a 1.7 m diameter focal plane. The unprecedented scale of the LATR drives a complex design. In this paper, we will first provide an overview of the LATR design. Integration and validation of the LATR design are discussed in detail, including mechanical strength, optical alignment, and cryogenic performance of the five cryogenic stages (80 K, 40 K, 4 K, 1 K, and 100 mK). We will also discuss the microwave-multiplexing ($mu$Mux) readout system implemented in the LATR and demonstrate the operation of dark prototype TES bolometers. The $mu$Mux readout technology enables one coaxial loop to read out $mathcal{O}(10^3)$ TES detectors. Its implementation within the LATR serves as a critical validation for the complex RF chain design. The successful validation of the LATR performance is not only a critical milestone within the Simons Observatory, it also provides a valuable reference for other experiments, e.g. CCAT-prime and CMB-S4.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"51 4 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121890364","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}
E. Healy, Aamir Ali, K. Arnold, J. Austermann, J. Beall, S. M. Bruno, Steve K. Choi, J. Connors, J. Connors, N. Cothard, B. Dober, B. Dober, S. Duff, N. Galitzki, G. Hilton, S. Ho, J. Hubmayr, B. Johnson, Yaqiong Li, M. Link, T. Lucas, H. McCarrick, M. Niemack, M. Silva-Feaver, Rita F. Sonka, S. Staggs, E. Vavagiakis, M. Vissers, Yuhan Wang, Edward J. Wollack, Zhilei Xu, Zhilei Xu, B. Westbrook, K. Zheng
The Simons Observatory is a suite of instruments sensitive to temperature and polarization of the cosmic microwave background. Five telescopes will host over 60,000 highly multiplexed transition edge sensor (TES) detectors. The universal focal plane modules (UFMs) package multichroic TES detectors with microwave multiplexing electronics compatible with all five receivers. The low-frequency arrays are lenslet-coupled sinuous antennas sensitive to 30 and 40 GHz. The mid-frequency and ultra-high-frequency UFMs are horn-coupled orthomode transducer arrays sensitive to 90/150 GHz and 225/280 GHz, respectively. Here we present the design, assembly details, and initial results of the first UFM.
{"title":"Assembly development for the Simons Observatory focal plane readout module","authors":"E. Healy, Aamir Ali, K. Arnold, J. Austermann, J. Beall, S. M. Bruno, Steve K. Choi, J. Connors, J. Connors, N. Cothard, B. Dober, B. Dober, S. Duff, N. Galitzki, G. Hilton, S. Ho, J. Hubmayr, B. Johnson, Yaqiong Li, M. Link, T. Lucas, H. McCarrick, M. Niemack, M. Silva-Feaver, Rita F. Sonka, S. Staggs, E. Vavagiakis, M. Vissers, Yuhan Wang, Edward J. Wollack, Zhilei Xu, Zhilei Xu, B. Westbrook, K. Zheng","doi":"10.1117/12.2561743","DOIUrl":"https://doi.org/10.1117/12.2561743","url":null,"abstract":"The Simons Observatory is a suite of instruments sensitive to temperature and polarization of the cosmic microwave background. Five telescopes will host over 60,000 highly multiplexed transition edge sensor (TES) detectors. The universal focal plane modules (UFMs) package multichroic TES detectors with microwave multiplexing electronics compatible with all five receivers. The low-frequency arrays are lenslet-coupled sinuous antennas sensitive to 30 and 40 GHz. The mid-frequency and ultra-high-frequency UFMs are horn-coupled orthomode transducer arrays sensitive to 90/150 GHz and 225/280 GHz, respectively. Here we present the design, assembly details, and initial results of the first UFM.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"91 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121899086","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. Cournoyer, Éric Carbonneau, P. Gilbert, L. Bibeau, Simon Houle, Hugo Bourque, I. Silversides, F. Grandmont, D. Naylor, B. Gom, Sudhakar Gunuganti, D. Loon, W. Jellema
The high spectral resolution mode of the SpicA FAR-infrared Instrument (SAFARI) is enabled by inserting a Fourier Transform Spectrometer (FTS), based on a Martin-Puplett interferometer, into the signal path of the instrument. The cryogenic mechanism (FTSM) enables linear scans of two back-to-back rooftop mirrors sharing a common apex. ABB Inc. is under contract with the Canadian Space Agency to develop and test at 4 K an FTSM Engineering Demonstration Unit (EDU) for TRL-5 demonstration. The main SAFARI FTSM performance drivers are the stringent mechatronic demands (position stability of roof-top mirrors <10 nm RMS, <34 mm linear stroke), severely constrained by a tight thermal budget (heat dissipation <1.5 mW) under a specific micro-vibrations environment (30 μg/√Hz external), all at cryogenic temperatures (4 K). In this paper, we describe a novel cryogenic FTSM design using a reactionless and longstroke flexure-based 4-bar linkage with stiffness compensation. This 1-DOF mechanism passively controls the guiding of the roof-top mirrors with flex pivots while the axial scanning is actuated and controlled with a custom moving magnet actuator (MMA). Static and dynamic balancing of the FTSM ensures that low vibration levels are transferred to/from the FTSM baseplate, and compensation of the mechanism stiffness reduces the force and drive current required from the MMA by a factor <10. Both features lead to MMA power consumption/dissipation <1.5 mW. Results from an engineering analysis of a dynamic model developed for the FTSM EDU are discussed to assess the compliance of this design to the challenging cryogenic SAFARI FTSM performance requirements.
{"title":"Design of a novel cryogenic stiffness-compensated reactionless scan mechanism for the Fourier transform spectrometer of SPICA SAFARI instrument","authors":"A. Cournoyer, Éric Carbonneau, P. Gilbert, L. Bibeau, Simon Houle, Hugo Bourque, I. Silversides, F. Grandmont, D. Naylor, B. Gom, Sudhakar Gunuganti, D. Loon, W. Jellema","doi":"10.1117/12.2560530","DOIUrl":"https://doi.org/10.1117/12.2560530","url":null,"abstract":"The high spectral resolution mode of the SpicA FAR-infrared Instrument (SAFARI) is enabled by inserting a Fourier Transform Spectrometer (FTS), based on a Martin-Puplett interferometer, into the signal path of the instrument. The cryogenic mechanism (FTSM) enables linear scans of two back-to-back rooftop mirrors sharing a common apex. ABB Inc. is under contract with the Canadian Space Agency to develop and test at 4 K an FTSM Engineering Demonstration Unit (EDU) for TRL-5 demonstration. The main SAFARI FTSM performance drivers are the stringent mechatronic demands (position stability of roof-top mirrors <10 nm RMS, <34 mm linear stroke), severely constrained by a tight thermal budget (heat dissipation <1.5 mW) under a specific micro-vibrations environment (30 μg/√Hz external), all at cryogenic temperatures (4 K). In this paper, we describe a novel cryogenic FTSM design using a reactionless and longstroke flexure-based 4-bar linkage with stiffness compensation. This 1-DOF mechanism passively controls the guiding of the roof-top mirrors with flex pivots while the axial scanning is actuated and controlled with a custom moving magnet actuator (MMA). Static and dynamic balancing of the FTSM ensures that low vibration levels are transferred to/from the FTSM baseplate, and compensation of the mechanism stiffness reduces the force and drive current required from the MMA by a factor <10. Both features lead to MMA power consumption/dissipation <1.5 mW. Results from an engineering analysis of a dynamic model developed for the FTSM EDU are discussed to assess the compliance of this design to the challenging cryogenic SAFARI FTSM performance requirements.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"12 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127234276","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. Tominaga, M. Tsujimoto, S. Stever, Tommaso Ghigna, H. Ishino, K. Ebisawa
Mayu Tominagaa,b, Masahiro Tsujimotoa, Samantha Lynn Steverc,e, Tommaso Ghignad,e, Hirokazu Ishinoc, Ken Ebisawaa for the LiteBIRD Joint Study Group aJapan Aerospace Exploration Agency (JAXA), Institute of Space and Astronautical Science (ISAS), Sagamihara, Kanagawa, 252-5210 Japan; bDepartment of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo, Japan; cDepartment of Physics, Okayama University, 2-1-1, Okayama, Okayama, 700-8530 Japan; dDepartment of Physics, University of Oxford, Oxford, OX1, 2JD, United Kingdom; eKavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), The University of Tokyo, Kashiwa, 277-8583, Japan;
{"title":"Simulation of the cosmic ray effects for the LiteBIRD satellite observing the CMB B-mode polarization","authors":"M. Tominaga, M. Tsujimoto, S. Stever, Tommaso Ghigna, H. Ishino, K. Ebisawa","doi":"10.1117/12.2576127","DOIUrl":"https://doi.org/10.1117/12.2576127","url":null,"abstract":"Mayu Tominagaa,b, Masahiro Tsujimotoa, Samantha Lynn Steverc,e, Tommaso Ghignad,e, Hirokazu Ishinoc, Ken Ebisawaa for the LiteBIRD Joint Study Group aJapan Aerospace Exploration Agency (JAXA), Institute of Space and Astronautical Science (ISAS), Sagamihara, Kanagawa, 252-5210 Japan; bDepartment of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo, Japan; cDepartment of Physics, Okayama University, 2-1-1, Okayama, Okayama, 700-8530 Japan; dDepartment of Physics, University of Oxford, Oxford, OX1, 2JD, United Kingdom; eKavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), The University of Tokyo, Kashiwa, 277-8583, Japan;","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"56 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116571624","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}
Kuan-Yu Liu, Ming-jye Wang, C. Tong, P. Friberg, G. Fuller, Tse-Jun Chen, Yen-Pin Chang, Wei-Chun Lu, D. Bintley, Ming-Tang Chen, Chih-Chiang Han, S. Yen, J. Dempsey, Shaoliang Li, C. Walther, Vernon Demattos, J. Cookson, G. Bell, Xue-Jian Jiang, H. Parson, I. Mizuno, Taishi Nammoto, Weiye Zhong
We have fabricated new superconductor-insulator-superconductor (SIS) mixers chips for the 16-element Heterodyne Array Receiver Program (HARP) instrument on the James Clerk Maxwell Telescope (JCMT). The original spare mixer chips were limited and not performed as well as the used ones in HARP. The ability to manufacture new mixer chips would therefore be important for the repair and upgrade of HARP. Our immediate goal is to replace the current nonfunctional mixers in HARP with new chips. We modified the designs of waveguide probe and the matching circuit of the SIS mixer chip. The newly designed chips were fabricated with a quality factor (Rsg/Rn) over 10. The double-sideband (DSB) receiver noise temperature (Trx) is lower than 80K at frequencies between 325 GHz and 375 GHz, which is comparable to the best of the original devices. Three of the sixteen mixers have been replaced and they work very well.
{"title":"SIS mixers study on Heterodyne Array Receiver Program (HARP) at JCMT","authors":"Kuan-Yu Liu, Ming-jye Wang, C. Tong, P. Friberg, G. Fuller, Tse-Jun Chen, Yen-Pin Chang, Wei-Chun Lu, D. Bintley, Ming-Tang Chen, Chih-Chiang Han, S. Yen, J. Dempsey, Shaoliang Li, C. Walther, Vernon Demattos, J. Cookson, G. Bell, Xue-Jian Jiang, H. Parson, I. Mizuno, Taishi Nammoto, Weiye Zhong","doi":"10.1117/12.2561192","DOIUrl":"https://doi.org/10.1117/12.2561192","url":null,"abstract":"We have fabricated new superconductor-insulator-superconductor (SIS) mixers chips for the 16-element Heterodyne Array Receiver Program (HARP) instrument on the James Clerk Maxwell Telescope (JCMT). The original spare mixer chips were limited and not performed as well as the used ones in HARP. The ability to manufacture new mixer chips would therefore be important for the repair and upgrade of HARP. Our immediate goal is to replace the current nonfunctional mixers in HARP with new chips. We modified the designs of waveguide probe and the matching circuit of the SIS mixer chip. The newly designed chips were fabricated with a quality factor (Rsg/Rn) over 10. The double-sideband (DSB) receiver noise temperature (Trx) is lower than 80K at frequencies between 325 GHz and 375 GHz, which is comparable to the best of the original devices. Three of the sixteen mixers have been replaced and they work very well.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"40 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122735037","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}
G. Stankowiak, M. Piat, E. Battistelli, G. D’Alessandro, P. Bernardis, M. Petris, Manuel Gonzalez, L. Grandsire, J. Hamilton, T. Hoang, S. Masi, S. Marnieros, A. Mennella, L. Mousset, C. O'sullivan, D. PRELE, A. Tartari, J. Thermeau, S. Torchinsky, F. Voisin, M. Zannoni, P. Ade, J. G. Alberro, A. Almela, G. Amico, L. H. Arnaldi, D. Auguste, J. Aumont, S. Azzoni, S. Banfi, B. Belier, A. Baù, D. Bennett, L. Bergé, J. Bernard, M. Bersanelli, M. Bigot-Sazy, J. Bonaparte, J. Bonis, E. Bunn, D. Burke, D. Buzi, F. Cavaliere, P. Chanial, C. Chapron, R. Charlassier, A. Cerutti, F. Columbro, A. Coppolecchia, G. Gasperis, M. Leo, S. Dheilly, C. Duca, L. Dumoulin, A. Etchegoyen, A. Fasciszewski, L. Ferreyro, D. Fracchia, C. Franceschet, M. M. G. Lerena, K. Ganga, B. Garcia, M. Redondo, M. Gaspard, D. Gayer, M. Gervasi, M. Giard, V. Gilles, Y. Giraud-Héraud, M. G. Berisso, M. Gradziel, M. Hampel, D. Harari, S. Henrot-Versillé, F. Incardona, E. Jules, J. Kaplan, C. Kristukat, L. Lamagna, S. Loucatos, T. Louis, B. Maffe
The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10-16W= p √Hz
{"title":"Detection chain and electronic readout of the QUBIC instrument","authors":"G. Stankowiak, M. Piat, E. Battistelli, G. D’Alessandro, P. Bernardis, M. Petris, Manuel Gonzalez, L. Grandsire, J. Hamilton, T. Hoang, S. Masi, S. Marnieros, A. Mennella, L. Mousset, C. O'sullivan, D. PRELE, A. Tartari, J. Thermeau, S. Torchinsky, F. Voisin, M. Zannoni, P. Ade, J. G. Alberro, A. Almela, G. Amico, L. H. Arnaldi, D. Auguste, J. Aumont, S. Azzoni, S. Banfi, B. Belier, A. Baù, D. Bennett, L. Bergé, J. Bernard, M. Bersanelli, M. Bigot-Sazy, J. Bonaparte, J. Bonis, E. Bunn, D. Burke, D. Buzi, F. Cavaliere, P. Chanial, C. Chapron, R. Charlassier, A. Cerutti, F. Columbro, A. Coppolecchia, G. Gasperis, M. Leo, S. Dheilly, C. Duca, L. Dumoulin, A. Etchegoyen, A. Fasciszewski, L. Ferreyro, D. Fracchia, C. Franceschet, M. M. G. Lerena, K. Ganga, B. Garcia, M. Redondo, M. Gaspard, D. Gayer, M. Gervasi, M. Giard, V. Gilles, Y. Giraud-Héraud, M. G. Berisso, M. Gradziel, M. Hampel, D. Harari, S. Henrot-Versillé, F. Incardona, E. Jules, J. Kaplan, C. Kristukat, L. Lamagna, S. Loucatos, T. Louis, B. Maffe","doi":"10.1117/12.2561567","DOIUrl":"https://doi.org/10.1117/12.2561567","url":null,"abstract":"The Q and U Bolometric Interferometer for Cosmology (QUBIC) Technical Demonstrator (TD) aiming to shows the feasibility of the combination of interferometry and bolometric detection. The electronic readout system is based on an array of 128 NbSi Transition Edge Sensors cooled at 350mK readout with 128 SQUIDs at 1K controlled and amplified by an Application Specific Integrated Circuit at 40K. This readout design allows a 128:1 Time Domain Multiplexing. We report the design and the performance of the detection chain in this paper. The technological demonstrator unwent a campaign of test in the lab. Evaluation of the QUBIC bolometers and readout electronics includes the measurement of I-V curves, time constant and the Noise Equivalent Power. Currently the mean Noise Equivalent Power is ~ 2 x 10-16W= p √Hz","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"51 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"117247404","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}
Luis A. Cuevas, G. Serandour, Rafael Rodríguez, Daniel Lühr, R. Reeves
The technology of 3D printing using a polymeric substrate and the fused deposition modeling (FDM) method, as a flexible method of creating a variety of parts, has the possibility of leading solutions in various fields of technology. The control of the surface quality achieved by its deposition on polished surfaces, such as glass, allows to bring the terminations of the exposed faces to values below 0.8 μm (N6). These qualities, obtained by printing on glass, in conjunction with the adaptation of the print head, allow for the manufacturing of flat concave or convex surfaces with excellent surface finish. Additionally, the electroless process described by Merino (2010) on NFC, which has been adapted for a PLA polymeric substrate, has permitted the deposition of a layer of copper (Cu) on the substrate, creating a surface conducting for an electromagnetic signal. Combining these two methods it is possible to manufacture a horn type antenna (horn) such as shown in figure 1, which complies with the necessary geometry to be used for the reception of electromagnetic signals. The antenna will be used in radio astronomy for the frequency band between 10 GHz and 30 GHz, and will be put to the test, comparing its performance against a series antenna.
{"title":"3D printed pyramidal horn antenna for K band frequency applications","authors":"Luis A. Cuevas, G. Serandour, Rafael Rodríguez, Daniel Lühr, R. Reeves","doi":"10.1117/12.2563079","DOIUrl":"https://doi.org/10.1117/12.2563079","url":null,"abstract":"The technology of 3D printing using a polymeric substrate and the fused deposition modeling (FDM) method, as a flexible method of creating a variety of parts, has the possibility of leading solutions in various fields of technology. The control of the surface quality achieved by its deposition on polished surfaces, such as glass, allows to bring the terminations of the exposed faces to values below 0.8 μm (N6). These qualities, obtained by printing on glass, in conjunction with the adaptation of the print head, allow for the manufacturing of flat concave or convex surfaces with excellent surface finish. Additionally, the electroless process described by Merino (2010) on NFC, which has been adapted for a PLA polymeric substrate, has permitted the deposition of a layer of copper (Cu) on the substrate, creating a surface conducting for an electromagnetic signal. Combining these two methods it is possible to manufacture a horn type antenna (horn) such as shown in figure 1, which complies with the necessary geometry to be used for the reception of electromagnetic signals. The antenna will be used in radio astronomy for the frequency band between 10 GHz and 30 GHz, and will be put to the test, comparing its performance against a series antenna.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128532504","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. Chapman, E. Vavagiakis, C. Duell, M. Niemack, G. Stacey, M. Fich, S. Parshley, Steve K. Choi, T. Nikola, T. Herter, C. Ross
The Cerro Chajnantor Atacama Telescope prime (CCAT-p) Observatory is a widefield, 6 meter aperture submillimeter telescope. Prime-Cam will be a powerful, first light camera for CCAT-p with imagers working at several wavelengths and a spectroscopic instrument aimed at intensity mapping during the epoch of reionization. We present the design of an instrument module in Prime-Cam, operating at 350 microns — the shortest wavelength on the instrument, and the most novel for astronomical surveys, taking full advantage of the atmospheric transparency at the high 5600 meter CCAT-p siting on Cerro Chajnantor. This instrument module will provide unprecedented broadband intensity and polarization measurement capabilities to address pressing astrophysical questions regarding galaxy formation, Big Bang cosmology, and star formation within our own Galaxy. We present the overall optical and mechanical design for the module, and laboratory characterization of the 860-GHz KID array.
{"title":"A 350 micron camera module for the Prime-Cam instrument on CCAT-prime","authors":"S. Chapman, E. Vavagiakis, C. Duell, M. Niemack, G. Stacey, M. Fich, S. Parshley, Steve K. Choi, T. Nikola, T. Herter, C. Ross","doi":"10.1117/12.2562869","DOIUrl":"https://doi.org/10.1117/12.2562869","url":null,"abstract":"The Cerro Chajnantor Atacama Telescope prime (CCAT-p) Observatory is a widefield, 6 meter aperture submillimeter telescope. Prime-Cam will be a powerful, first light camera for CCAT-p with imagers working at several wavelengths and a spectroscopic instrument aimed at intensity mapping during the epoch of reionization. \u0000We present the design of an instrument module in Prime-Cam, operating at 350 microns — the shortest wavelength on the instrument, and the most novel for astronomical surveys, taking full advantage of the atmospheric transparency at the high 5600 meter CCAT-p siting on Cerro Chajnantor. This instrument module will provide unprecedented broadband intensity and polarization measurement capabilities to address pressing astrophysical questions regarding galaxy formation, Big Bang cosmology, and star formation within our own Galaxy. We present the overall optical and mechanical design for the module, and laboratory characterization of the 860-GHz KID array.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"96 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128583828","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. Tong, S. Leiker, R. Wilson, R. Rao, B. Force, P. Grimes, N. Patel, R. Christensen
{"title":"A distributed Raspberry-Pi control system for wSMA frontend","authors":"C. Tong, S. Leiker, R. Wilson, R. Rao, B. Force, P. Grimes, N. Patel, R. Christensen","doi":"10.1117/12.2561887","DOIUrl":"https://doi.org/10.1117/12.2561887","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"16 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125631375","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. Kojima, K. Uemizu, H. Kiuchi, T. Tamura, K. Kaneko, R. Sakai, A. Miyachi, W. Shan, Y. Uzawa, Álvaro González, M. Kroug, T. Sakai
NAOJ have studied wideband receiver technologies at submillimeter wavelengths toward implementation as future upgrades into the Atacama Large Millimeter/submillimeter Array telescope. We have developed critical components and devices such as waveguide components and superconductor-insulator-superconductor (SIS) mixers targeting radio frequencies (RF) in the 275-500 GHz range and an intermediate frequency (IF) bandwidth of 3-22 GHz. Based on the developed components, quantum-limited low-noise performance has been demonstrated by using a double-sideband receiver frontend in combination with a high-speed digitizer. In addition, a preliminary demonstration of a wideband RF/IF sideband-separating SIS mixer was performed. This paper describes the status of our efforts to develop technology toward wideband receivers for ALMA.
{"title":"Wideband technology development to increase the RF and instantaneous bandwidth of ALMA receivers","authors":"T. Kojima, K. Uemizu, H. Kiuchi, T. Tamura, K. Kaneko, R. Sakai, A. Miyachi, W. Shan, Y. Uzawa, Álvaro González, M. Kroug, T. Sakai","doi":"10.1117/12.2561240","DOIUrl":"https://doi.org/10.1117/12.2561240","url":null,"abstract":"NAOJ have studied wideband receiver technologies at submillimeter wavelengths toward implementation as future upgrades into the Atacama Large Millimeter/submillimeter Array telescope. We have developed critical components and devices such as waveguide components and superconductor-insulator-superconductor (SIS) mixers targeting radio frequencies (RF) in the 275-500 GHz range and an intermediate frequency (IF) bandwidth of 3-22 GHz. Based on the developed components, quantum-limited low-noise performance has been demonstrated by using a double-sideband receiver frontend in combination with a high-speed digitizer. In addition, a preliminary demonstration of a wideband RF/IF sideband-separating SIS mixer was performed. This paper describes the status of our efforts to develop technology toward wideband receivers for ALMA.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"69 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131576150","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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