Y. Gan, B. Mirzaei, Jose R. G. Silva, A. Khalatpour, Q. Hu, C. Groppi, J. Siles, F. V. D. Tak, Jiansong Gao
Generating multiple local oscillator beams is one challenge to develop large heterodyne receiver arrays (~100 pixels), which allow astronomical instrumentations mapping more area within limited space mission lifetime. Here, We combine a reflective Fourier grating with an unidirectional antenna coupled 3rd-order distributed feedback (DFB) quantum cascade laser (QCL) to generate 81 beams at 3.86 THz. We have measured the beam pattern of the diffracted 81 beams, which agrees well with a simulated result from COMSOL Multiphysics with respect to the angular distribution and power distribution among the 81 beams. The diffraction efficiency of the Fourier grating is derived to be 94±3%, which is very close to the simulated result of 97%. For an array of equal superconducting hot electron bolometer mixers, 64 out of 81 beams can pump the HEB mixers with similar power, resulting in receiver sensitivities within 10%. Such a combination of a Fourier grating and a QCL can create an LO with 100 beams or more, enabling a new generation of large heterodyne arrays for astronomical instrumentation. This paper is essentially a copy of our paper in Optics Express.
{"title":"Multi-beam local oscillator for a 100-pixel heterodyne array receiver at THz","authors":"Y. Gan, B. Mirzaei, Jose R. G. Silva, A. Khalatpour, Q. Hu, C. Groppi, J. Siles, F. V. D. Tak, Jiansong Gao","doi":"10.1117/12.2560939","DOIUrl":"https://doi.org/10.1117/12.2560939","url":null,"abstract":"Generating multiple local oscillator beams is one challenge to develop large heterodyne receiver arrays (~100 pixels), which allow astronomical instrumentations mapping more area within limited space mission lifetime. Here, We combine a reflective Fourier grating with an unidirectional antenna coupled 3rd-order distributed feedback (DFB) quantum cascade laser (QCL) to generate 81 beams at 3.86 THz. We have measured the beam pattern of the diffracted 81 beams, which agrees well with a simulated result from COMSOL Multiphysics with respect to the angular distribution and power distribution among the 81 beams. The diffraction efficiency of the Fourier grating is derived to be 94±3%, which is very close to the simulated result of 97%. For an array of equal superconducting hot electron bolometer mixers, 64 out of 81 beams can pump the HEB mixers with similar power, resulting in receiver sensitivities within 10%. Such a combination of a Fourier grating and a QCL can create an LO with 100 beams or more, enabling a new generation of large heterodyne arrays for astronomical instrumentation. This paper is essentially a copy of our paper in Optics Express.","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":"129310724","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}
Chao-Te Li, C. Tong, Ming-jye Wang, Tse-Jun Chen, Yen-Pin Chang, S. Yen, Jen-Chieh Cheng, Wei-Chun Lu, Yen-Ru Huang
Since the start of full science operations from 2004, the Submillimeter Array has been implementing plans to expand IF bandwidths and upgrade receivers and cryostats. Metal mesh low-pass filters were designed to block infrared (IR) radiation to reduce the thermal load on the cryostats. Filters were fabricated on a quartz wafer through photolithography and coated with anti-reflection (AR) material. The filters were tested from 200 to 400 GHz to verify their passband performances. The measurement results were found to be in good agreement with EM simulation results. They were tested in the far-infrared (FIR) frequency range to verify out-of-band rejection. The IR reflectivity was found to be approximately 70%, which corresponded to the percentage of the area blocked by metal.
{"title":"Metal mesh IR filter for wSMA","authors":"Chao-Te Li, C. Tong, Ming-jye Wang, Tse-Jun Chen, Yen-Pin Chang, S. Yen, Jen-Chieh Cheng, Wei-Chun Lu, Yen-Ru Huang","doi":"10.1117/12.2561174","DOIUrl":"https://doi.org/10.1117/12.2561174","url":null,"abstract":"Since the start of full science operations from 2004, the Submillimeter Array has been implementing plans to expand IF bandwidths and upgrade receivers and cryostats. Metal mesh low-pass filters were designed to block infrared (IR) radiation to reduce the thermal load on the cryostats. Filters were fabricated on a quartz wafer through photolithography and coated with anti-reflection (AR) material. The filters were tested from 200 to 400 GHz to verify their passband performances. The measurement results were found to be in good agreement with EM simulation results. They were tested in the far-infrared (FIR) frequency range to verify out-of-band rejection. The IR reflectivity was found to be approximately 70%, which corresponded to the percentage of the area blocked by metal.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"26 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":"123054468","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}
N. Okada, Takeru Matsumoto, Hiroshi Kondo, T. Takashima, S. Masui, Shota Ueda, A. Nishimura, T. Manabe, T. Onishi, H. Ogawa, Ryoko Amari, Toshihisa Tsutsumi, T. Aoki, S. Sawada-Satoh, K. Niinuma, K. Fujisawa, K. Kimura, T. Minamidani, C. Miyazawa, H. Kaneko, K. Torii, Shigeru Takahashi, Y. Miyamoto, K. Miyazawa, T. Oyama, S. Kameno, H. Imai
{"title":"Development of the multi-band simultaneous observation system of the Nobeyama 45-m Telescope in HINOTORI (Hybrid Installation project in NObeyama, Triple-band ORIented)","authors":"N. Okada, Takeru Matsumoto, Hiroshi Kondo, T. Takashima, S. Masui, Shota Ueda, A. Nishimura, T. Manabe, T. Onishi, H. Ogawa, Ryoko Amari, Toshihisa Tsutsumi, T. Aoki, S. Sawada-Satoh, K. Niinuma, K. Fujisawa, K. Kimura, T. Minamidani, C. Miyazawa, H. Kaneko, K. Torii, Shigeru Takahashi, Y. Miyamoto, K. Miyazawa, T. Oyama, S. Kameno, H. Imai","doi":"10.1117/12.2562137","DOIUrl":"https://doi.org/10.1117/12.2562137","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"34 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":"121924295","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}
Yukiko Sakurai, T. Matsumura, N. Katayama, K. Komatsu, R. Takaku, S. Sugiyama, Y. Nomura, T. Toda, Tommaso Ghigna, T. Iida, H. Sugai, H. Imada, M. Hazumi, H. Ishino, H. Ohsaki, Y. Terao, H. Enokida, Y. Ishida, Yosuke Iwata, Doa Jamil, K. Konishi, H. Sakurai, J. Yumoto, M. Kuwata-Gonokami, A. Kusaka, C. Hill
We present a breadboard model development status of the polarization modulator unit (PMU) for a low-frequency telescope (LFT) of the LiteBIRD space mission. LiteBIRD is a next-generation cosmic microwave background polarization satellite to measure the primordial B-mode with the science goal of σr < 0.001. The baseline design of LiteBIRD consists of reflective low-frequency and refractive medium-and-high-frequency telescopes. Each telescope employs the PMU based on a continuous rotating half-wave plate (HWP) at the aperture. The PMU is a critical instrument for the LiteBIRD to achieve the science goal because it significantly suppresses 1/f noise and mitigates systematic uncertainties. The LiteBIRD LFT PMU consists of a broadband achromatic HWP and a cryogenic rotation mechanism. In this presentation, we discuss requirements, design and systematic studies of the PMU, and we report the development status of the broadband HWP and the space-compatible cryogenic rotation mechanism.
{"title":"Breadboard model of polarization modulator unit based on a continuously rotating half-wave plate for the low-frequency telescope of the LiteBIRD space mission","authors":"Yukiko Sakurai, T. Matsumura, N. Katayama, K. Komatsu, R. Takaku, S. Sugiyama, Y. Nomura, T. Toda, Tommaso Ghigna, T. Iida, H. Sugai, H. Imada, M. Hazumi, H. Ishino, H. Ohsaki, Y. Terao, H. Enokida, Y. Ishida, Yosuke Iwata, Doa Jamil, K. Konishi, H. Sakurai, J. Yumoto, M. Kuwata-Gonokami, A. Kusaka, C. Hill","doi":"10.1117/12.2560289","DOIUrl":"https://doi.org/10.1117/12.2560289","url":null,"abstract":"We present a breadboard model development status of the polarization modulator unit (PMU) for a low-frequency telescope (LFT) of the LiteBIRD space mission. LiteBIRD is a next-generation cosmic microwave background polarization satellite to measure the primordial B-mode with the science goal of σr < 0.001. The baseline design of LiteBIRD consists of reflective low-frequency and refractive medium-and-high-frequency telescopes. Each telescope employs the PMU based on a continuous rotating half-wave plate (HWP) at the aperture. The PMU is a critical instrument for the LiteBIRD to achieve the science goal because it significantly suppresses 1/f noise and mitigates systematic uncertainties. The LiteBIRD LFT PMU consists of a broadband achromatic HWP and a cryogenic rotation mechanism. In this presentation, we discuss requirements, design and systematic studies of the PMU, and we report the development status of the broadband HWP and the space-compatible cryogenic rotation mechanism.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"36 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":"115682823","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. Gennet, D. Desforge, D. Dubreuil, J. Martignac, X. Navick, Albrecht Pöglitsh, V. Révéret, L. Rodriguez
{"title":"An optical test facility for the B-BOP bolometers of the SPICA mission","authors":"C. Gennet, D. Desforge, D. Dubreuil, J. Martignac, X. Navick, Albrecht Pöglitsh, V. Révéret, L. Rodriguez","doi":"10.1117/12.2561330","DOIUrl":"https://doi.org/10.1117/12.2561330","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"60 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":"121503535","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. S. Germaine, P. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Thakur, C. Bischoff, J. Bock, J. Bock, H. Boenish, E. Bullock, V. Buza, J. Cheshire, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, E. Denison, M. Dierickx, L. Duband, M. Eiben, S. Fatigoni, J. Filippini, S. Fliescher, N. Goeckner-wald, D. Goldfinger, J. Grayson, P. Grimes, G. Hall, M. Halpern, S. Harrison, S. Henderson, S. Hildebrandt, S. Hildebrandt, G. Hilton, J. Hubmayr, H. Hui, K. Irwin, K. Irwin, J. Kang, J. Kang, K. Karkare, E. Karpel, S. Kefeli, S. Kernasovskiy, J. Kovac, C. Kuo, K. Lau, E. Leitch, K. Megerian, L. Minutolo, L. Moncelsi, Y. Nakato, T. Namikawa, H. Nguyen, H. Nguyen, R. O’Brient, R. O’Brient, R. W. Ogburn, S. Palladino, N. Precup, T. Prouvé, C. Pryke, B. Racine, C. Reintsema, S. Richter, A. Schillaci, B. Schmitt, R. Schwartz, C. Sheehy, A. Soliman, B. Steinbach, R. Sudiwala, G. Teply, K. Thompson, J. Tolan, C. Tucker, A. Turner, C. Umilta, A. Vieregg, A. Wandui, A. Weber, D. Wiebe, J. Willmert, C. L. Wong, W. L. Wu, H
The Bicep/Keck Array experiment is a series of small-aperture refracting telescopes observing degree-scale Cosmic Microwave Background polarization from the South Pole in search of a primordial B-mode signature. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We use high-fidelity, in-situ measurements of the beam response to estimate the temperature-to-polarization (T → P) leakage in our latest data including observations from 2016 through 2018. This includes three years of Bicep3 observing at 95 GHz, and multifrequency data from Keck Array. Here we present band-averaged far-field beam maps, differential beam mismatch, and residual beam power (after filtering out the leading difference modes via deprojection) for these receivers. We show preliminary results of "beam map simulations," which use these beam maps to observe a simulated temperature (no Q/U) sky to estimate T → P leakage in our real data.
{"title":"Analysis of Temperature-to-Polarization Leakage in BICEP3 and Keck CMB Data from 2016 to 2018","authors":"T. S. Germaine, P. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Thakur, C. Bischoff, J. Bock, J. Bock, H. Boenish, E. Bullock, V. Buza, J. Cheshire, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, E. Denison, M. Dierickx, L. Duband, M. Eiben, S. Fatigoni, J. Filippini, S. Fliescher, N. Goeckner-wald, D. Goldfinger, J. Grayson, P. Grimes, G. Hall, M. Halpern, S. Harrison, S. Henderson, S. Hildebrandt, S. Hildebrandt, G. Hilton, J. Hubmayr, H. Hui, K. Irwin, K. Irwin, J. Kang, J. Kang, K. Karkare, E. Karpel, S. Kefeli, S. Kernasovskiy, J. Kovac, C. Kuo, K. Lau, E. Leitch, K. Megerian, L. Minutolo, L. Moncelsi, Y. Nakato, T. Namikawa, H. Nguyen, H. Nguyen, R. O’Brient, R. O’Brient, R. W. Ogburn, S. Palladino, N. Precup, T. Prouvé, C. Pryke, B. Racine, C. Reintsema, S. Richter, A. Schillaci, B. Schmitt, R. Schwartz, C. Sheehy, A. Soliman, B. Steinbach, R. Sudiwala, G. Teply, K. Thompson, J. Tolan, C. Tucker, A. Turner, C. Umilta, A. Vieregg, A. Wandui, A. Weber, D. Wiebe, J. Willmert, C. L. Wong, W. L. Wu, H","doi":"10.1117/12.2562729","DOIUrl":"https://doi.org/10.1117/12.2562729","url":null,"abstract":"The Bicep/Keck Array experiment is a series of small-aperture refracting telescopes observing degree-scale Cosmic Microwave Background polarization from the South Pole in search of a primordial B-mode signature. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We use high-fidelity, in-situ measurements of the beam response to estimate the temperature-to-polarization (T → P) leakage in our latest data including observations from 2016 through 2018. This includes three years of Bicep3 observing at 95 GHz, and multifrequency data from Keck Array. Here we present band-averaged far-field beam maps, differential beam mismatch, and residual beam power (after filtering out the leading difference modes via deprojection) for these receivers. We show preliminary results of \"beam map simulations,\" which use these beam maps to observe a simulated temperature (no Q/U) sky to estimate T → P leakage in our real data.","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":"131209000","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
H. Matsuo, H. Ezawa, H. Kiuchi, M. Honma, M. Ukibe, G. Fujii, Y. Murata, M. Hattori
{"title":"Technologies for space Terahertz intensity interferometry","authors":"H. Matsuo, H. Ezawa, H. Kiuchi, M. Honma, M. Ukibe, G. Fujii, Y. Murata, M. Hattori","doi":"10.1117/12.2562333","DOIUrl":"https://doi.org/10.1117/12.2562333","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"141 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":"132431028","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. Kurtz, T. Stander, D. Villiers, William Cerfonteyn, A. D. Witt, D. Ferrusca, D. Hiriart, D. Hughes, C. Jacobs, L. Loinard, Fanie van den Heever, M. Velázquez
The 50-meter Large Millimeter Telescope (LMT) operating on the Sierra Negra in Mexico is the largest single- dish millimeter-wave telescope in the world. Although designed to work in the 3 mm and 1 mm bands, there is significant potential for LMT observations at centimeter wavelengths. Here, we summarize the scientific case and operational arguments for a K-band receiver system on the LMT, describe several of the unique technical challenges that the proposed installation would entail, and mention some possible solutions to these challenges.
{"title":"The potential for a K-band receiver on the Large Millimeter Telescope","authors":"S. Kurtz, T. Stander, D. Villiers, William Cerfonteyn, A. D. Witt, D. Ferrusca, D. Hiriart, D. Hughes, C. Jacobs, L. Loinard, Fanie van den Heever, M. Velázquez","doi":"10.1117/12.2563132","DOIUrl":"https://doi.org/10.1117/12.2563132","url":null,"abstract":"The 50-meter Large Millimeter Telescope (LMT) operating on the Sierra Negra in Mexico is the largest single- dish millimeter-wave telescope in the world. Although designed to work in the 3 mm and 1 mm bands, there is significant potential for LMT observations at centimeter wavelengths. Here, we summarize the scientific case and operational arguments for a K-band receiver system on the LMT, describe several of the unique technical challenges that the proposed installation would entail, and mention some possible solutions to these challenges.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"19 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":"133642547","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}
Tetsuya Ito, Y. Fujii, M. Inata, T. Kamazaki, S. Sakamoto, S. Asayama
A new 790 – 940 GHz heterodyne receiver, ASTE Band 10, was installed in October 2019 on ASTE (Atacama Submillimeter Telescope Experiment), a 10 m submillimeter telescope near of the ALMA site in Chile. An ALMA Band 10 prototype receiver was upgraded with SIS mixers employing high-Jc junctions. The receiver noise temperature (TDSB) measured in the laboratory is between 175 K and 344 K. The achieved system noise temperature on ASTE toward the zenith was 2400 K (PWV <1.0 mm). Their Allan variances were less than 2.0 x 10-6 for timescales in the range of 0.05 sec < T <100 sec.
2019年10月，一个新的790 - 940 GHz外差接收器，ASTE波段10，安装在智利ALMA站点附近的10米亚毫米望远镜ASTE(阿塔卡马亚毫米望远镜实验)上。ALMA Band 10原型接收机升级为采用高jc结的SIS混频器。实验室测得的接收机噪声温度(TDSB)在175 ~ 344 K之间。在朝向天顶方向的ASTE上获得的系统噪声温度为2400 K (PWV <1.0 mm)。在0.05秒< T <100秒的时间尺度上，其Allan方差均小于2.0 × 10-6。
{"title":"Upgrade of an ALMA Band 10 prototype receiver for ASTE radio telescope","authors":"Tetsuya Ito, Y. Fujii, M. Inata, T. Kamazaki, S. Sakamoto, S. Asayama","doi":"10.1117/12.2561076","DOIUrl":"https://doi.org/10.1117/12.2561076","url":null,"abstract":"A new 790 – 940 GHz heterodyne receiver, ASTE Band 10, was installed in October 2019 on ASTE (Atacama Submillimeter Telescope Experiment), a 10 m submillimeter telescope near of the ALMA site in Chile. An ALMA Band 10 prototype receiver was upgraded with SIS mixers employing high-Jc junctions. The receiver noise temperature (TDSB) measured in the laboratory is between 175 K and 344 K. The achieved system noise temperature on ASTE toward the zenith was 2400 K (PWV <1.0 mm). Their Allan variances were less than 2.0 x 10-6 for timescales in the range of 0.05 sec < T <100 sec.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"18 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":"125307545","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
K. Harrington, C. Sierra, G. Chesmore, Shreya Sutariya, Aamir Ali, Steve K. Choi, N. Cothard, S. Dicker, N. Galitzki, S. Ho, A. Kofman, B. Koopman, J. Lashner, J. McMahon, M. Niemack, J. Orlowski-Scherer, J. Seibert, M. Silva-Feaver, E. Vavagiakis, Zhilei Xu, N. Zhu
The Simons Observatory (SO) will be a CMB survey experiment with three small-aperture telescopes and one large-aperture telescope (the LAT), which will observe from the Atacama Desert in Chile. In total, SO will field over 60,000 TES bolometers in six spectral bands centered between 27 and 280 GHz. The 6 m LAT, targeting the smaller angular scales of the CMB, utilizes a cryogenic receiver (LATR) designed to house up to 13 individual optics tubes. The scientific objectives of the SO project requires these optics tubes to achieve high-throughput optical performance while maintaining exquisite control of systematic effects. We describe the integration and testing program for the LATR optics tubes being carried out to verify the design and assembly of the tubes before deployment. The program includes a quick turn-around single tube test cryostat. We discuss the optical design specifications the tubes for deployment and the suite of optical test equipment prepared for these measurements.
{"title":"The integration and testing program for the Simons Observatory Large Aperture Telescope optics tubes","authors":"K. Harrington, C. Sierra, G. Chesmore, Shreya Sutariya, Aamir Ali, Steve K. Choi, N. Cothard, S. Dicker, N. Galitzki, S. Ho, A. Kofman, B. Koopman, J. Lashner, J. McMahon, M. Niemack, J. Orlowski-Scherer, J. Seibert, M. Silva-Feaver, E. Vavagiakis, Zhilei Xu, N. Zhu","doi":"10.1117/12.2562647","DOIUrl":"https://doi.org/10.1117/12.2562647","url":null,"abstract":"The Simons Observatory (SO) will be a CMB survey experiment with three small-aperture telescopes and one large-aperture telescope (the LAT), which will observe from the Atacama Desert in Chile. In total, SO will field over 60,000 TES bolometers in six spectral bands centered between 27 and 280 GHz. The 6 m LAT, targeting the smaller angular scales of the CMB, utilizes a cryogenic receiver (LATR) designed to house up to 13 individual optics tubes. The scientific objectives of the SO project requires these optics tubes to achieve high-throughput optical performance while maintaining exquisite control of systematic effects. We describe the integration and testing program for the LATR optics tubes being carried out to verify the design and assembly of the tubes before deployment. The program includes a quick turn-around single tube test cryostat. We discuss the optical design specifications the tubes for deployment and the suite of optical test equipment prepared for these measurements.","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":"116639591","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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