M. Tapia, P. Ade, P. Barry, T. Brien, 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, C. Tucker, M. Vel'azquez, S. Ventura, S. Doyle
The Mexico-UK Submillimetre Camera for Astronomy (MUSCAT) is the second-generation large-format continuum camera operating in the 1.1 mm band to be installed on the 50-m diameter Large Millimeter Telescope (LMT) in Mexico. The focal plane of the instrument is made up of 1458 horn coupled lumped-element kinetic inductance detectors (LEKID) divided equally into six channels deposited on three silicon wafers. Here we present the preliminary results of the complete characterisation in the laboratory of the MUSCAT focal plane. Through the instrument's readout system, we perform frequency sweeps of the array to identify the resonance frequencies, and continuous timestream acquisitions to measure and characterise the intrinsic noise and 1/f knee of the detectors. Subsequently, with a re-imaging lens and a blackbody point source, the beams of every detector are mapped, obtaining a mean FWHM size of ~3.27 mm, close to the expected 3.1 mm. Then, by varying the intensity of a beam filling blackbody source, we measure the responsivity and noise power spectral density (PSD) for each detector under an optical load of 300 K, obtaining the noise equivalent power (NEP), with which we verify that the majority of the detectors are photon noise limited. Finally, using a Fourier Transform Spectrometer (FTS), we measure the spectral response of the instrument, which indicate a bandwidth of 1.0-1.2 mm centred on 1.1 mm, as expected.
{"title":"MUSCAT focal plane verification","authors":"M. Tapia, P. Ade, P. Barry, T. Brien, 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, C. Tucker, M. Vel'azquez, S. Ventura, S. Doyle","doi":"10.1117/12.2576219","DOIUrl":"https://doi.org/10.1117/12.2576219","url":null,"abstract":"The Mexico-UK Submillimetre Camera for Astronomy (MUSCAT) is the second-generation large-format continuum camera operating in the 1.1 mm band to be installed on the 50-m diameter Large Millimeter Telescope (LMT) in Mexico. The focal plane of the instrument is made up of 1458 horn coupled lumped-element kinetic inductance detectors (LEKID) divided equally into six channels deposited on three silicon wafers. Here we present the preliminary results of the complete characterisation in the laboratory of the MUSCAT focal plane. Through the instrument's readout system, we perform frequency sweeps of the array to identify the resonance frequencies, and continuous timestream acquisitions to measure and characterise the intrinsic noise and 1/f knee of the detectors. Subsequently, with a re-imaging lens and a blackbody point source, the beams of every detector are mapped, obtaining a mean FWHM size of ~3.27 mm, close to the expected 3.1 mm. Then, by varying the intensity of a beam filling blackbody source, we measure the responsivity and noise power spectral density (PSD) for each detector under an optical load of 300 K, obtaining the noise equivalent power (NEP), with which we verify that the majority of the detectors are photon noise limited. Finally, using a Fourier Transform Spectrometer (FTS), we measure the spectral response of the instrument, which indicate a bandwidth of 1.0-1.2 mm centred on 1.1 mm, as expected.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"96 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122754079","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. Lapinov, S. Lapinova, L. Petrov, D. P. C. A. I. O. S. A. Sciences, N. Novgorod, Russia., M. University, Lobachevsky State University, Higher School of Economics, Nasa Gsfc, Greenbelt, Md., Usa, Instituto Nacional de Astrof'isica, 'optica y Electr'onica, Puebla, M'exico.
Thanks to the first mm studies on the territory of the former USSR in the early 1960s and succeeding sub-mm measurements in the 1970s – early 1980s at wavelengths up to 0.34 mm, a completely unique astroclimate was revealed in the Eastern Pamirs, only slightly inferior to the available conditions on the Chajnantor plateau in Chile and Mauna Kea. Due to its high plateau altitude (4300 – 4500 m) surrounded from all sides by big (~7000 m) air-drying icy mountains and remoteness from oceans this area has the lowest relative humidity in the former USSR and extremely high atmospheric stability. In particular, direct measurements of precipitated water vapor in the winter months showed typical pwv=0.8 – 0.9 mm with sometimes of 0.27 mm. To validate previous studies and to compare them with results for other similar regions we performed opacity calculations at mm – sub-mm wavelengths for different sites in the Eastern Pamirs, Tibet, Indian Himalayas, APEX, ALMA, JCM, LMT and many others. To do this we integrate radiative transfer equations using the output of NASA Global Modeling and Assimilation Office model GEOS-FPIT for more than 12 years. We confirm previous conclusions about exceptionally good astroclimate in the Eastern Pamirs. Due to its geographical location, small infrastructure and the absence of any interference in radio and optical bands, this makes the Eastern Pamirs the best place in the Eastern Hemisphere for both optical and sub-mm astronomy.
{"title":"On the benefits of the Eastern Pamirs for sub-mm astronomy","authors":"A. Lapinov, S. Lapinova, L. Petrov, D. P. C. A. I. O. S. A. Sciences, N. Novgorod, Russia., M. University, Lobachevsky State University, Higher School of Economics, Nasa Gsfc, Greenbelt, Md., Usa, Instituto Nacional de Astrof'isica, 'optica y Electr'onica, Puebla, M'exico.","doi":"10.1117/12.2560250","DOIUrl":"https://doi.org/10.1117/12.2560250","url":null,"abstract":"Thanks to the first mm studies on the territory of the former USSR in the early 1960s and succeeding sub-mm measurements in the 1970s – early 1980s at wavelengths up to 0.34 mm, a completely unique astroclimate was revealed in the Eastern Pamirs, only slightly inferior to the available conditions on the Chajnantor plateau in Chile and Mauna Kea. Due to its high plateau altitude (4300 – 4500 m) surrounded from all sides by big (~7000 m) air-drying icy mountains and remoteness from oceans this area has the lowest relative humidity in the former USSR and extremely high atmospheric stability. In particular, direct measurements of precipitated water vapor in the winter months showed typical pwv=0.8 – 0.9 mm with sometimes of 0.27 mm. To validate previous studies and to compare them with results for other similar regions we performed opacity calculations at mm – sub-mm wavelengths for different sites in the Eastern Pamirs, Tibet, Indian Himalayas, APEX, ALMA, JCM, LMT and many others. To do this we integrate radiative transfer equations using the output of NASA Global Modeling and Assimilation Office model GEOS-FPIT for more than 12 years. We confirm previous conclusions about exceptionally good astroclimate in the Eastern Pamirs. Due to its geographical location, small infrastructure and the absence of any interference in radio and optical bands, this makes the Eastern Pamirs the best place in the Eastern Hemisphere for both optical and sub-mm astronomy.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"51 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132480526","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
L. Moncelsi, P. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Thakur, C. Bischoff, J. Bock, J. Bock, V. Buza, V. Buza, J. Cheshire, J. Connors, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, E. Denison, M. Dierickx, L. Duband, M. Eiben, S. Fatigoni, J. Filippini, N. Goeckner-wald, D. Goldfinger, J. Grayson, P. Grimes, G. Hall, G. Hall, M. Halpern, S. Harrison, S. Henderson, S. Hildebrandt, S. Hildebrandt, G. Hilton, J. Hubmayr, H. Hui, K. Irwin, J. Kang, J. Kang, K. Karkare, K. Karkare, S. Kefeli, J. Kovac, C. Kuo, K. Lau, E. Leitch, K. Megerian, L. Minutolo, Y. Nakato, Y. Nakato, T. Namikawa, T. Namikawa, H. Nguyen, R. O’Brient, R. O’Brient, S. Palladino, N. Precup, T. Prouvé, C. Pryke, B. Racine, C. Reintsema, A. Schillaci, B. Schmitt, A. Soliman, T. S. Germaine, T. S. Germaine, B. Steinbach, R. Sudiwala, K. Thompson, C. Tucker, A. Turner, C. Umilta, C. Umilta, A. Vieregg, A. Wandui, A. Weber, D. Wiebe, J. Willmert, W. L. K. Wu, E. Yang, K. Yoon, E. Young, C. Yu, L. Zeng, C. Zhang, S. Zhang
A detection of curl-type ($B$-mode) polarization of the primary CMB would be direct evidence for the inflationary paradigm of the origin of the Universe. The BICEP/Keck Array (BK) program targets the degree angular scales, where the power from primordial $B$-mode polarization is expected to peak, with ever-increasing sensitivity and has published the most stringent constraints on inflation to date. BICEP Array (BA) is the Stage-3 instrument of the BK program and will comprise four BICEP3-class receivers observing at 30/40, 95, 150 and 220/270 GHz with a combined 32,000+ detectors; such wide frequency coverage is necessary for control of the Galactic foregrounds, which also produce degree-scale $B$-mode signal. The 30/40 GHz receiver is designed to constrain the synchrotron foreground and has begun observing at the South Pole in early 2020. By the end of a 3-year observing campaign, the full BICEP Array instrument is projected to reach $sigma_r$ between 0.002 and 0.004, depending on foreground complexity and degree of removal of $B$-modes due to gravitational lensing (delensing). This paper presents an overview of the design, measured on-sky performance and calibration of the first BA receiver. We also give a preview of the added complexity in the time-domain multiplexed readout of the 7,776-detector 150 GHz receiver.
{"title":"Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole","authors":"L. Moncelsi, P. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Thakur, C. Bischoff, J. Bock, J. Bock, V. Buza, V. Buza, J. Cheshire, J. Connors, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, E. Denison, M. Dierickx, L. Duband, M. Eiben, S. Fatigoni, J. Filippini, N. Goeckner-wald, D. Goldfinger, J. Grayson, P. Grimes, G. Hall, G. Hall, M. Halpern, S. Harrison, S. Henderson, S. Hildebrandt, S. Hildebrandt, G. Hilton, J. Hubmayr, H. Hui, K. Irwin, J. Kang, J. Kang, K. Karkare, K. Karkare, S. Kefeli, J. Kovac, C. Kuo, K. Lau, E. Leitch, K. Megerian, L. Minutolo, Y. Nakato, Y. Nakato, T. Namikawa, T. Namikawa, H. Nguyen, R. O’Brient, R. O’Brient, S. Palladino, N. Precup, T. Prouvé, C. Pryke, B. Racine, C. Reintsema, A. Schillaci, B. Schmitt, A. Soliman, T. S. Germaine, T. S. Germaine, B. Steinbach, R. Sudiwala, K. Thompson, C. Tucker, A. Turner, C. Umilta, C. Umilta, A. Vieregg, A. Wandui, A. Weber, D. Wiebe, J. Willmert, W. L. K. Wu, E. Yang, K. Yoon, E. Young, C. Yu, L. Zeng, C. Zhang, S. Zhang","doi":"10.1117/12.2561995","DOIUrl":"https://doi.org/10.1117/12.2561995","url":null,"abstract":"A detection of curl-type ($B$-mode) polarization of the primary CMB would be direct evidence for the inflationary paradigm of the origin of the Universe. The BICEP/Keck Array (BK) program targets the degree angular scales, where the power from primordial $B$-mode polarization is expected to peak, with ever-increasing sensitivity and has published the most stringent constraints on inflation to date. BICEP Array (BA) is the Stage-3 instrument of the BK program and will comprise four BICEP3-class receivers observing at 30/40, 95, 150 and 220/270 GHz with a combined 32,000+ detectors; such wide frequency coverage is necessary for control of the Galactic foregrounds, which also produce degree-scale $B$-mode signal. The 30/40 GHz receiver is designed to constrain the synchrotron foreground and has begun observing at the South Pole in early 2020. By the end of a 3-year observing campaign, the full BICEP Array instrument is projected to reach $sigma_r$ between 0.002 and 0.004, depending on foreground complexity and degree of removal of $B$-modes due to gravitational lensing (delensing). This paper presents an overview of the design, measured on-sky performance and calibration of the first BA receiver. We also give a preview of the added complexity in the time-domain multiplexed readout of the 7,776-detector 150 GHz receiver.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"129808392","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}
I. Lowe, P. Ade, P. Ashton, J. Austermann, G. Coppi, Erin G. Cox, M. Devlin, B. Dober, V. Fanfani, L. Fissel, N. Galitzki, Jiansong Gao, S. Gordon, C. Groppi, G. Hilton, J. Hubmayr, J. Klein, Dale Li, N. Lourie, H. Mani, P. Mauskopf, C. Mckenney, F. Nati, G. Novak, G. Pisano, J. Romualdez, J. Soler, A. Sinclair, C. Tucker, J. Ullom, M. Vissers, C. Wheeler, P. Williams
The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID pixels, respectively. The pixels are formed from two orthogonally oriented, crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to sub 300mK temperatures and stabilized via a closed cycle $^3$He sorption fridge in combination with a $^4$He vacuum pot. The detectors are read out through a combination of the second-generation Reconfigurable Open Architecture Computing Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The firmware and software designed to readout and characterize these detectors was built from scratch by the BLAST team around these detectors, and has been adapted for use by other MKID instruments such as TolTEC and OLIMPO. We present an overview of these systems as well as in-depth methodology of the ground-based characterization and the measured in-flight performance.
{"title":"Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver","authors":"I. Lowe, P. Ade, P. Ashton, J. Austermann, G. Coppi, Erin G. Cox, M. Devlin, B. Dober, V. Fanfani, L. Fissel, N. Galitzki, Jiansong Gao, S. Gordon, C. Groppi, G. Hilton, J. Hubmayr, J. Klein, Dale Li, N. Lourie, H. Mani, P. Mauskopf, C. Mckenney, F. Nati, G. Novak, G. Pisano, J. Romualdez, J. Soler, A. Sinclair, C. Tucker, J. Ullom, M. Vissers, C. Wheeler, P. Williams","doi":"10.1117/12.2560854","DOIUrl":"https://doi.org/10.1117/12.2560854","url":null,"abstract":"The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID pixels, respectively. The pixels are formed from two orthogonally oriented, crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to sub 300mK temperatures and stabilized via a closed cycle $^3$He sorption fridge in combination with a $^4$He vacuum pot. The detectors are read out through a combination of the second-generation Reconfigurable Open Architecture Computing Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The firmware and software designed to readout and characterize these detectors was built from scratch by the BLAST team around these detectors, and has been adapted for use by other MKID instruments such as TolTEC and OLIMPO. We present an overview of these systems as well as in-depth methodology of the ground-based characterization and the measured in-flight performance.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"75 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127266990","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. Nishimura, A. Ohama, K. Kimura, D. Tsutsumi, Yudai Matsue, R. Yamada, Mariko Sakamoto, K. Matsunaga, Yutaka Hasegawa, Taisei Minami, Takeru Matsumoto, Kazuki Shiotani, S. Okuda, Kakeru Fujishiro, K. Sakasai, Masahiro Suzuki, Shun Saeki, Kouki Satani, K. Urushihara, C. Kato, T. Kondo, K. Okawa, D. Kurita, T. Inaba, S. Maruyama, Masako Koga, K. Noda, M. Kohno, Hiroaki Iwamura, Yuki Hyoto, Y. Hori, Kaoru Nishikawa, Takeru Nishioka, Thoqin Pang, H. Sano, R. Enokiya, S. Yoshiike, S. Fujita, Katsuhiro Hayashi, K. Torii, T. Hayakawa, A. Taniguchi, K. Tsuge, Y. Yamane, Y. Hattori, T. Ohno, Shota Ueda, S. Masui, Y. Yamasaki, Hiroshi Kondo, Kazuji Suzuki, Kazuhiro Kobayashi, Y. Fujii, Y. Fujii, T. Minamidani, T. Okuda, H. Yamamoto, K. Tachihara, T. Onishi, A. Mizuno, H. Ogawa, Y. Fukui
We report the current status of the NASCO (NAnten2 Super CO survey as legacy) project which aims to provide all-sky CO data cube of southern hemisphere using the NANTEN2 4-m submillimeter telescope installed at the Atacama Desert through developing a new multi-beam receiver and a new telescope control system. The receiver consists of 5 beams. The four beams, located at the four corners of a square with the beam separation of 720$''$, are installed with a 100 GHz band SIS receiver having 2-polarization sideband-separation filter. The other beam, located at the optical axis, is installed with a 200 GHz band SIS receiver having 2-polarization sideband-separation filter. The cooled component is modularized for each beam, and cooled mirrors are used. The IF bandwidths are 8 and 4 GHz for 100 and 200 GHz bands, respectively. Using XFFTS spectrometers with a bandwidth of 2 GHz, the lines of $^{12}$CO, $^{13}$CO, and C$^{18}$O of $J$=1$-$0 or $J$=2$-$1 can be observed simultaneously for each beam. The control system is reconstructed on the ROS architecture, which is an open source framework for robot control, to enable a flexible observation mode and to handle a large amount of data. The framework is commonly used and maintained in a robotic field, and thereby reliability, flexibility, expandability, and efficiency in development are improved as compared with the system previously used. The receiver and control system are installed on the NANTEN2 telescope in December 2019, and its commissioning and science verification are on-going. We are planning to start science operation in early 2021.
本文报道了安装在阿塔卡马沙漠的NAnten2 4-m亚毫米望远镜通过研制新型多波束接收机和新型望远镜控制系统，提供南半球全天CO数据立方体的NASCO (NAnten2 Super CO survey as legacy)项目的现状。接收机由5束组成。四个波束位于一个方框的四角，波束间距为720$ " $，安装一个带有2极化边带分离滤波器的100ghz频段SIS接收机。另一束位于光轴上，安装了一个200 GHz带SIS接收器，具有2极化边带分离滤波器。每个光束的冷却组件都是模块化的，并使用冷却镜。100 GHz和200 GHz频段的中频带宽分别为8 GHz和4 GHz。利用带宽为2ghz的XFFTS光谱仪，可以同时观测到$J$=1$-$0或$J$=2$-$1的$^{12}$CO、$^{13}$CO和$J$ ^{18}$O谱线。控制系统采用开源机器人控制框架ROS架构进行重构，实现了灵活的观察模式和大数据处理能力。该框架是机器人领域常用和维护的，因此与以前使用的系统相比，开发的可靠性、灵活性、可扩展性和效率都得到了提高。接收机和控制系统已于2019年12月安装在南天2号望远镜上，目前正在进行调试和科学验证。我们计划在2021年初开始科学操作。
{"title":"Development of the new multi-beam receiver and telescope control system for NASCO","authors":"A. Nishimura, A. Ohama, K. Kimura, D. Tsutsumi, Yudai Matsue, R. Yamada, Mariko Sakamoto, K. Matsunaga, Yutaka Hasegawa, Taisei Minami, Takeru Matsumoto, Kazuki Shiotani, S. Okuda, Kakeru Fujishiro, K. Sakasai, Masahiro Suzuki, Shun Saeki, Kouki Satani, K. Urushihara, C. Kato, T. Kondo, K. Okawa, D. Kurita, T. Inaba, S. Maruyama, Masako Koga, K. Noda, M. Kohno, Hiroaki Iwamura, Yuki Hyoto, Y. Hori, Kaoru Nishikawa, Takeru Nishioka, Thoqin Pang, H. Sano, R. Enokiya, S. Yoshiike, S. Fujita, Katsuhiro Hayashi, K. Torii, T. Hayakawa, A. Taniguchi, K. Tsuge, Y. Yamane, Y. Hattori, T. Ohno, Shota Ueda, S. Masui, Y. Yamasaki, Hiroshi Kondo, Kazuji Suzuki, Kazuhiro Kobayashi, Y. Fujii, Y. Fujii, T. Minamidani, T. Okuda, H. Yamamoto, K. Tachihara, T. Onishi, A. Mizuno, H. Ogawa, Y. Fukui","doi":"10.1117/12.2562053","DOIUrl":"https://doi.org/10.1117/12.2562053","url":null,"abstract":"We report the current status of the NASCO (NAnten2 Super CO survey as legacy) project which aims to provide all-sky CO data cube of southern hemisphere using the NANTEN2 4-m submillimeter telescope installed at the Atacama Desert through developing a new multi-beam receiver and a new telescope control system. The receiver consists of 5 beams. The four beams, located at the four corners of a square with the beam separation of 720$''$, are installed with a 100 GHz band SIS receiver having 2-polarization sideband-separation filter. The other beam, located at the optical axis, is installed with a 200 GHz band SIS receiver having 2-polarization sideband-separation filter. The cooled component is modularized for each beam, and cooled mirrors are used. The IF bandwidths are 8 and 4 GHz for 100 and 200 GHz bands, respectively. Using XFFTS spectrometers with a bandwidth of 2 GHz, the lines of $^{12}$CO, $^{13}$CO, and C$^{18}$O of $J$=1$-$0 or $J$=2$-$1 can be observed simultaneously for each beam. The control system is reconstructed on the ROS architecture, which is an open source framework for robot control, to enable a flexible observation mode and to handle a large amount of data. The framework is commonly used and maintained in a robotic field, and thereby reliability, flexibility, expandability, and efficiency in development are improved as compared with the system previously used. The receiver and control system are installed on the NANTEN2 telescope in December 2019, and its commissioning and science verification are on-going. We are planning to start science operation in early 2021.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"148 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-11-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116440921","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}
R. Duan, Musicos Team, Xinxin Zhang, C. Niu, Di Li
A substantial amount of important scientific information is contained within astronomical data at the submillimeter and far-infrared (FIR) wavelengths, including information regarding dusty galaxies, galaxy clusters, and star-forming regions; however, these wavelengths are among the least-explored fields in astronomy because of the technological difficulties involved in such research. Over the past 20 years, considerable efforts have been devoted to developing submillimeter- and millimeter-wavelength astronomical instruments and telescopes. The number of detectors is an important property of such instruments and is the subject of the current study. Future telescopes will require as many as hundreds of thousands of detectors to meet the necessary requirements in terms of the field of view, scan speed, and resolution. A large pixel count is one benefit of the development of multiplexable detectors that use kinetic inductance detector (KID) technology. This paper presents the development of all aspects of the readout electronics for a KID-based instrument, which enabled one of the largest detector counts achieved to date in submillimeter-/millimeter-wavelength imaging arrays: a total of 2304 detectors. The work presented in this paper had been implemented in the MUltiwavelength Submillimeter Inductance Camera (MUSIC), a instrument for the Caltech Submillimeter Observatory (CSO) between 2013 and 2015.
{"title":"Readout for kinetic-inductance-detector-based submillimeter radio astronomy","authors":"R. Duan, Musicos Team, Xinxin Zhang, C. Niu, Di Li","doi":"10.1117/12.2576399","DOIUrl":"https://doi.org/10.1117/12.2576399","url":null,"abstract":"A substantial amount of important scientific information is contained within astronomical data at the submillimeter and far-infrared (FIR) wavelengths, including information regarding dusty galaxies, galaxy clusters, and star-forming regions; however, these wavelengths are among the least-explored fields in astronomy because of the technological difficulties involved in such research. Over the past 20 years, considerable efforts have been devoted to developing submillimeter- and millimeter-wavelength astronomical instruments and telescopes. \u0000The number of detectors is an important property of such instruments and is the subject of the current study. Future telescopes will require as many as hundreds of thousands of detectors to meet the necessary requirements in terms of the field of view, scan speed, and resolution. A large pixel count is one benefit of the development of multiplexable detectors that use kinetic inductance detector (KID) technology. \u0000This paper presents the development of all aspects of the readout electronics for a KID-based instrument, which enabled one of the largest detector counts achieved to date in submillimeter-/millimeter-wavelength imaging arrays: a total of 2304 detectors. The work presented in this paper had been implemented in the MUltiwavelength Submillimeter Inductance Camera (MUSIC), a instrument for the Caltech Submillimeter Observatory (CSO) between 2013 and 2015.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"61 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-08-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131776828","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":"Calibration of QUBIC: The Q and U bolometric interferometer for cosmology (Erratum)","authors":"J. Zmuidzinas, Jianxun Gao","doi":"10.1117/12.2592760","DOIUrl":"https://doi.org/10.1117/12.2592760","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"57 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127284026","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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