I. Mizuno, P. Friberg, R. Berthold, H. Parsons, Chih-Chiang Han, Alexis Acohido, G. Bell, D. Berry, D. Bintley, Ming-Tang Chen, Alan L. Clark, J. Cookson, Vernon Demattos, J. Dempsey, Jason Fleck, Kuo-chieh Fu, Miriam Fuchs, S. Graves, P. Ho, Sung-Po Hsu, Yau-De Huang, Xue-Jian Jiang, D. Kubo, JohnKuroda, Shaoliang Li, S. Mairs, Callie Matulonis, Mailani Neal, Neal Oliveira, M. Purves, M. Rawlings, Ya-Che Shih, K. Silva, E. Sison, Patrice Smith, R. Srinivasan, William Stahm, A. Tetarenko, P. Torne, C. Walther, Chao-Ching Wang, T. Wei
Namakanui is an instrument containing three inserts in an ALMA type Dewar. The three inserts are Alaihi, Uu and Aweoweo operating around 86, 230 and 345GHz. The receiver is being commissioned on the JCMT. It will be used for both Single dish and VLBI observations. We will present commissioning results and the system.
{"title":"Commissioning of Nāmakanui on the JCMT","authors":"I. Mizuno, P. Friberg, R. Berthold, H. Parsons, Chih-Chiang Han, Alexis Acohido, G. Bell, D. Berry, D. Bintley, Ming-Tang Chen, Alan L. Clark, J. Cookson, Vernon Demattos, J. Dempsey, Jason Fleck, Kuo-chieh Fu, Miriam Fuchs, S. Graves, P. Ho, Sung-Po Hsu, Yau-De Huang, Xue-Jian Jiang, D. Kubo, JohnKuroda, Shaoliang Li, S. Mairs, Callie Matulonis, Mailani Neal, Neal Oliveira, M. Purves, M. Rawlings, Ya-Che Shih, K. Silva, E. Sison, Patrice Smith, R. Srinivasan, William Stahm, A. Tetarenko, P. Torne, C. Walther, Chao-Ching Wang, T. Wei","doi":"10.1117/12.2561742","DOIUrl":"https://doi.org/10.1117/12.2561742","url":null,"abstract":"Namakanui is an instrument containing three inserts in an ALMA type Dewar. The three inserts are Alaihi, Uu and Aweoweo operating around 86, 230 and 345GHz. The receiver is being commissioned on the JCMT. It will be used for both Single dish and VLBI observations. We will present commissioning results and the system.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"41 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":"128512713","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. Ito, L. Lowry, T. Elleflot, K. Crowley, L. Howe, Praweeen Siritanasak, T. Adkins, K. Arnold, C. Baccigalupi, D. Barron, B. Bixler, Y. Chinone, J. Groh, M. Hazumi, C. Hill, O. Jeong, B. Keating, A. Kusaka, A. Lee, Kayla Mitchell, M. Navaroli, A. Pham, C. Raum, C. Reichardt, T. Sasse, J. Seibert, A. Suzuki, S. Takakura, G. Teply, C. Tsai, B. Westbrook
{"title":"Detector and readout characterization for POLARBEAR-2b","authors":"J. Ito, L. Lowry, T. Elleflot, K. Crowley, L. Howe, Praweeen Siritanasak, T. Adkins, K. Arnold, C. Baccigalupi, D. Barron, B. Bixler, Y. Chinone, J. Groh, M. Hazumi, C. Hill, O. Jeong, B. Keating, A. Kusaka, A. Lee, Kayla Mitchell, M. Navaroli, A. Pham, C. Raum, C. Reichardt, T. Sasse, J. Seibert, A. Suzuki, S. Takakura, G. Teply, C. Tsai, B. Westbrook","doi":"10.1117/12.2562766","DOIUrl":"https://doi.org/10.1117/12.2562766","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"10 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":"124032070","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. C. Shaw, P. Ade, S. Akers, M. Amiri, J. Austermann, J. Beall, D. Becker, S. Benton, A. Bergman, J. Bock, J. Bond, S. Bryan, H. Chiang, C. Contaldi, R. Domagalski, O. Dor'e, S. Duff, A. Duivenvoorden, H. Eriksen, M. Farhang, J. Filippini, L. Fissel, A. Fraisse, K. Freese, M. Galloway, A. Gambrel, N. Gandilo, K. Ganga, A. Grigorian, R. Gualtieri, J. Gudmundsson, M. Halpern, J. Hartley, M. Hasselfield, G. Hilton, W. Holmes, V. Hristov, Z. Huang, J. Hubmayr, K. Irwin, W. Jones, A. Kahn, C. Kuo, Z. Kermish, A. Lennox, J. S. Leung, S. Li, P. Mason, K. Megerian, L. Mocanu, L. Moncelsi, T. Morford, J. Nagy, R. Nie, C. Netterfield, M. Nolta, B. Osherson, I. Padilla, A. Rahlin, S. Redmond, C. Reintsema, L. J. Romualdez, J. Ruhl, M. Runyan, J. Shariff, C. Shiu, J. Soler, X. Song, H. Thommesen, A. Trangsrud, C. Tucker, R. Tucker, A. Turner, J. Ullom, J. V. D. List, J. Lanen, M. Vissers, A. Weber, S. Wen, I. Wehus, D. Wiebe, E. Physics, U. I. Urbana-Champaign, S. O. Physics, Astronomy, Cardiff University, P. Depart
In this work we describe upgrades to the Spider balloon-borne telescope in preparation for its second flight, currently planned for December 2021. The Spider instrument is optimized to search for a primordial B-mode polarization signature in the cosmic microwave background at degree angular scales. During its first flight in 2015, Spider mapped ~10% of the sky at 95 and 150 GHz. The payload for the second Antarctic flight will incorporate three new 280 GHz receivers alongside three refurbished 95- and 150 GHz receivers from Spider's first flight. In this work we discuss the design and characterization of these new receivers, which employ over 1500 feedhorn-coupled transition-edge sensors. We describe pre-flight laboratory measurements of detector properties, and the optical performance of completed receivers. These receivers will map a wide area of the sky at 280 GHz, providing new information on polarized Galactic dust emission that will help to separate it from the cosmological signal.
{"title":"Design and pre-flight performance of SPIDER 280 GHz receivers","authors":"E. C. Shaw, P. Ade, S. Akers, M. Amiri, J. Austermann, J. Beall, D. Becker, S. Benton, A. Bergman, J. Bock, J. Bond, S. Bryan, H. Chiang, C. Contaldi, R. Domagalski, O. Dor'e, S. Duff, A. Duivenvoorden, H. Eriksen, M. Farhang, J. Filippini, L. Fissel, A. Fraisse, K. Freese, M. Galloway, A. Gambrel, N. Gandilo, K. Ganga, A. Grigorian, R. Gualtieri, J. Gudmundsson, M. Halpern, J. Hartley, M. Hasselfield, G. Hilton, W. Holmes, V. Hristov, Z. Huang, J. Hubmayr, K. Irwin, W. Jones, A. Kahn, C. Kuo, Z. Kermish, A. Lennox, J. S. Leung, S. Li, P. Mason, K. Megerian, L. Mocanu, L. Moncelsi, T. Morford, J. Nagy, R. Nie, C. Netterfield, M. Nolta, B. Osherson, I. Padilla, A. Rahlin, S. Redmond, C. Reintsema, L. J. Romualdez, J. Ruhl, M. Runyan, J. Shariff, C. Shiu, J. Soler, X. Song, H. Thommesen, A. Trangsrud, C. Tucker, R. Tucker, A. Turner, J. Ullom, J. V. D. List, J. Lanen, M. Vissers, A. Weber, S. Wen, I. Wehus, D. Wiebe, E. Physics, U. I. Urbana-Champaign, S. O. Physics, Astronomy, Cardiff University, P. Depart","doi":"10.1117/12.2562941","DOIUrl":"https://doi.org/10.1117/12.2562941","url":null,"abstract":"In this work we describe upgrades to the Spider balloon-borne telescope in preparation for its second flight, currently planned for December 2021. The Spider instrument is optimized to search for a primordial B-mode polarization signature in the cosmic microwave background at degree angular scales. During its first flight in 2015, Spider mapped ~10% of the sky at 95 and 150 GHz. The payload for the second Antarctic flight will incorporate three new 280 GHz receivers alongside three refurbished 95- and 150 GHz receivers from Spider's first flight. In this work we discuss the design and characterization of these new receivers, which employ over 1500 feedhorn-coupled transition-edge sensors. We describe pre-flight laboratory measurements of detector properties, and the optical performance of completed receivers. These receivers will map a wide area of the sky at 280 GHz, providing new information on polarized Galactic dust emission that will help to separate it from the cosmological signal.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"44 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":"127619003","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. Sayers, P. Day, D. Cunnane, B. Eom, H. Leduc, R. O’Brient, M. Runyan, S. Bryan, S. Gordon, P. Mauskopf, B. Johnson, H. McCarrick, T. Bhandarkar
{"title":"A four kilopixel 150 GHz KID imager paired with a 1.5 m crossed Dragone telescope","authors":"J. Sayers, P. Day, D. Cunnane, B. Eom, H. Leduc, R. O’Brient, M. Runyan, S. Bryan, S. Gordon, P. Mauskopf, B. Johnson, H. McCarrick, T. Bhandarkar","doi":"10.1117/12.2561647","DOIUrl":"https://doi.org/10.1117/12.2561647","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"10 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":"131384470","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. Salatino, J. Austermann, K. Thompson, P. Ade, Xiran Bai, J. Beall, D. Becker, Yi-Fu Cai, Z. Chang, Din Chen, Pisin Chen, J. Connors, J. Delabrouille, B. Dober, S. Duff, G. Gao, Shamik Ghosh, Richard C. Givhan, G. Hilton, B. Hu, J. Hubmayr, E. Karpel, C. Kuo, Hong Li, Mingzhe Li, Siyu Li, Xufang Li, Yongping Li, M. Link, Hao Liu, Liyong Liu, Yang Liu, F. Lu, Xue-Feng Lu, Tammy Lukas, J. Mates, Justin Mathewson, P. Mauskopf, J. Meinke, Jordi A. Montana-Lopez, Jenna Moore, Jingyan Shi, A. Sinclair, Ryan Stephenson, Wei Sun, Y. Tseng, C. Tucker, J. Ullom, L. Vale, J. Lanen, M. Vissers, S. Walker, Bo Wang, Guofeng Wang, Jiaxin Wang, E. Weeks, Di Wu, Yi-han Wu, J. Xia, Hexuan Xu, Ji Yao, Yong-qiang Yao, K. Yoon, B. Yue, Hua-jin Zhai, Aimei Zhang, Laiyu Zhang, Le Zhang, Pengjie Zhang, Tong Zhang, Xinmin Zhang, Yifei Zhang, Yongjie Zhang, Gong-Bo Zhao, Wen Zhao
AliCPT-1 is the first CMB degree scale polarimeter to be deployed to the Tibetan plateau at 5,250m asl. AliCPT-1 is a 95/150GHz 72cm aperture, two lens refracting telescope cooled down to 4K. Alumina lenses image the CMB on a 636mm wide focal plane. The modularized focal plane consists of dichroic polarization-sensitive Transition-Edge Sensors (TESes). Each module includes 1,704 optically active TESes fabricated on a 6in Silicon wafer. Each TES array is read out with a microwave multiplexing with a multiplexing factor up to 2,000. Such large factor has allowed to consider 10's of thousands of detectors in a practical way, enabling to design a receiver that can operate up to 19 TES arrays for a total of 32,300 TESes. AliCPT-1 leverages the technological advancements of AdvACT and BICEP-3. The cryostat receiver is currently under integration and testing. Here we present the AliCPT-1 receiver, underlying how the optimized design meets the experimental requirements.
{"title":"The design of the Ali CMB Polarization Telescope receiver","authors":"M. Salatino, J. Austermann, K. Thompson, P. Ade, Xiran Bai, J. Beall, D. Becker, Yi-Fu Cai, Z. Chang, Din Chen, Pisin Chen, J. Connors, J. Delabrouille, B. Dober, S. Duff, G. Gao, Shamik Ghosh, Richard C. Givhan, G. Hilton, B. Hu, J. Hubmayr, E. Karpel, C. Kuo, Hong Li, Mingzhe Li, Siyu Li, Xufang Li, Yongping Li, M. Link, Hao Liu, Liyong Liu, Yang Liu, F. Lu, Xue-Feng Lu, Tammy Lukas, J. Mates, Justin Mathewson, P. Mauskopf, J. Meinke, Jordi A. Montana-Lopez, Jenna Moore, Jingyan Shi, A. Sinclair, Ryan Stephenson, Wei Sun, Y. Tseng, C. Tucker, J. Ullom, L. Vale, J. Lanen, M. Vissers, S. Walker, Bo Wang, Guofeng Wang, Jiaxin Wang, E. Weeks, Di Wu, Yi-han Wu, J. Xia, Hexuan Xu, Ji Yao, Yong-qiang Yao, K. Yoon, B. Yue, Hua-jin Zhai, Aimei Zhang, Laiyu Zhang, Le Zhang, Pengjie Zhang, Tong Zhang, Xinmin Zhang, Yifei Zhang, Yongjie Zhang, Gong-Bo Zhao, Wen Zhao","doi":"10.1117/12.2560709","DOIUrl":"https://doi.org/10.1117/12.2560709","url":null,"abstract":"AliCPT-1 is the first CMB degree scale polarimeter to be deployed to the Tibetan plateau at 5,250m asl. AliCPT-1 is a 95/150GHz 72cm aperture, two lens refracting telescope cooled down to 4K. Alumina lenses image the CMB on a 636mm wide focal plane. The modularized focal plane consists of dichroic polarization-sensitive Transition-Edge Sensors (TESes). Each module includes 1,704 optically active TESes fabricated on a 6in Silicon wafer. Each TES array is read out with a microwave multiplexing with a multiplexing factor up to 2,000. Such large factor has allowed to consider 10's of thousands of detectors in a practical way, enabling to design a receiver that can operate up to 19 TES arrays for a total of 32,300 TESes. AliCPT-1 leverages the technological advancements of AdvACT and BICEP-3. The cryostat receiver is currently under integration and testing. Here we present the AliCPT-1 receiver, underlying how the optimized design meets the experimental requirements.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"339 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":"123399156","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}
Accurate optical modeling is important for the design and characterisation of current and next-generation experiments studying the Cosmic Microwave Background (CMB). Geometrical Optics (GO) cannot model diffractive effects. In this work, we discuss two methods that incorporate diffraction, Physical Optics (PO) and the Geometrical Theory of Diffraction (GTD). We simulate the optical response of a ground-based two-lens refractor design shielded by a ground screen with time-reversed simulations. In particular, we use GTD to determine the interplay between the design of the refractor's forebaffle and the sidelobes caused by interaction with the ground screen.
{"title":"Modeling sidelobe response for ground-based mm-wavelength telescopes with the geometrical theory of diffraction","authors":"A. Adler, J. Gudmundsson","doi":"10.1117/12.2576309","DOIUrl":"https://doi.org/10.1117/12.2576309","url":null,"abstract":"Accurate optical modeling is important for the design and characterisation of current and next-generation experiments studying the Cosmic Microwave Background (CMB). Geometrical Optics (GO) cannot model diffractive effects. In this work, we discuss two methods that incorporate diffraction, Physical Optics (PO) and the Geometrical Theory of Diffraction (GTD). We simulate the optical response of a ground-based two-lens refractor design shielded by a ground screen with time-reversed simulations. In particular, we use GTD to determine the interplay between the design of the refractor's forebaffle and the sidelobes caused by interaction with the ground screen.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"5 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":"128083709","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. P. Laguna, K. Karatsu, J. Bueno, S. Dabironezare, D. Thoen, V. Murugesan, A. Endo, J. Baselmans
{"title":"Filter-bank for broadband sub-mm wave superconducting on-chip spectrometers","authors":"A. P. Laguna, K. Karatsu, J. Bueno, S. Dabironezare, D. Thoen, V. Murugesan, A. Endo, J. Baselmans","doi":"10.1117/12.2560483","DOIUrl":"https://doi.org/10.1117/12.2560483","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"119 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":"131949022","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Phase-locked oscillator operated in a fiber-coupled repeater station","authors":"H. Kiuchi, B. Shillue","doi":"10.1117/12.2561170","DOIUrl":"https://doi.org/10.1117/12.2561170","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"11 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":"121197241","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. Yates, J. Bueno, A. Endo, A. Baryshev, L. Ferrari, V. Murugesan, D. Thoen, J. Baselmans
Far infra-red, mm and sub-mm astronomy requires very large arrays of detectors for future wide field cameras and spectrometers. We present an array of lens-antenna coupled Microwave Kinetic Inductance Detectors (MKID) for a wide field camera at 350 GHz. We discuss the optimization to maximize the usable detector yield and matching the array to the readout to enable array performance close to the background limit. We overview the optical characterization techniques required to have confidence in the instrument performance prior to on telescope integration, finally giving measured optical performance for an optimized array.
{"title":"On the design and performance of very large MKID arrays","authors":"S. Yates, J. Bueno, A. Endo, A. Baryshev, L. Ferrari, V. Murugesan, D. Thoen, J. Baselmans","doi":"10.1117/12.2562367","DOIUrl":"https://doi.org/10.1117/12.2562367","url":null,"abstract":"Far infra-red, mm and sub-mm astronomy requires very large arrays of detectors for future wide field cameras and spectrometers. We present an array of lens-antenna coupled Microwave Kinetic Inductance Detectors (MKID) for a wide field camera at 350 GHz. \u0000We discuss the optimization to maximize the usable detector yield and matching the array to the readout to enable array performance close to the background limit. We overview the optical characterization techniques required to have confidence in the instrument performance prior to on telescope integration, finally giving measured optical performance for an optimized array.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"43 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":"128483530","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. Brien, P. Ade, P. Barry, P. Barry, E. Castillo-Dom'inguez, D. Ferrusca, V. G'omez-Rivera, P. Hargrave, J. Rebollar, A. Hornsby, D. Hughes, J. M. J'auregui-Garc'ia, P. Mauskopf, D. Murias, A. Papageorgiou, E. Pascale, A. P'erez, S. Rowe, M. Smith, M. Tapia, C. Tucker, M. Vel'azquez, S. Ventura, S. Doyle
The Mexico-UK Submillimetre Camera for AsTronomy (MUSCAT) is a 1.1 mm receiver consisting of 1,500 lumped-element kinetic inductance detectors (LEKIDs) for the Large Millimeter Telescope (LMT; Volcan Sierra Negra in Puebla, Mexico). MUSCAT utilises the maximum field of view of the LMT's upgraded 50-metre primary mirror and is the first Mexico-UK collaboration to deploy a millimetre/sub-mm receiver on the Large Millimeter Telescope. Using a simplistic simulator, we estimate a predicted mapping speed for MUSCAT by combining the measured performance of MUSCAT with the observed sky conditions at the LMT. We compare this to a previously calculated bolometric-model mapping speed and find that our mapping speed is in good agreement when this is scaled by a previously reported empirical factor. Through this simulation we show that signal contamination due to sky fluctuations can be effectively removed through the use of principle component analysis. We also give an overview
{"title":"Pre-deployment verification and predicted mapping speed of MUSCAT","authors":"T. Brien, P. Ade, P. Barry, P. Barry, E. Castillo-Dom'inguez, D. Ferrusca, V. G'omez-Rivera, P. Hargrave, J. Rebollar, A. Hornsby, D. Hughes, J. M. J'auregui-Garc'ia, P. Mauskopf, D. Murias, A. Papageorgiou, E. Pascale, A. P'erez, S. Rowe, M. Smith, M. Tapia, C. Tucker, M. Vel'azquez, S. Ventura, S. Doyle","doi":"10.1117/12.2561305","DOIUrl":"https://doi.org/10.1117/12.2561305","url":null,"abstract":"The Mexico-UK Submillimetre Camera for AsTronomy (MUSCAT) is a 1.1 mm receiver consisting of 1,500 lumped-element kinetic inductance detectors (LEKIDs) for the Large Millimeter Telescope (LMT; Volcan Sierra Negra in Puebla, Mexico). MUSCAT utilises the maximum field of view of the LMT's upgraded 50-metre primary mirror and is the first Mexico-UK collaboration to deploy a millimetre/sub-mm receiver on the Large Millimeter Telescope. Using a simplistic simulator, we estimate a predicted mapping speed for MUSCAT by combining the measured performance of MUSCAT with the observed sky conditions at the LMT. We compare this to a previously calculated bolometric-model mapping speed and find that our mapping speed is in good agreement when this is scaled by a previously reported empirical factor. Through this simulation we show that signal contamination due to sky fluctuations can be effectively removed through the use of principle component analysis. We also give an overview","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"13 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126635822","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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