{"title":"Design of all-in-one 2SB mixer for ALMA Band 10","authors":"Y. Fujii, T. Kojima, M. Kroug, Y. Uzawa","doi":"10.1117/12.2562032","DOIUrl":"https://doi.org/10.1117/12.2562032","url":null,"abstract":"","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":"114458268","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. Gascard, G. Pisano, S. Doyle, A. Shitvov, J. Austermann, J. Beall, J. Hubmayr, Benjamin Raymond, N. Halverson, G. Jaehnig, C. Mckenney, A. Suzuki
The next generations of ground-based cosmic microwave background experiments will require polarisation sensitive, multichroic pixels of large focal planes comprising several thousand detectors operating at the photon noise limit. One approach to achieve this goal is to couple light from the telescope to a polarisation sensitive antenna structure connected to a superconducting diplexer network where the desired frequency bands are filtered before being fed to individual ultra-sensitive detectors such as Transition Edge Sensors. Traditionally, arrays constituted of horn antennas, planar phased antennas or anti-reflection coated micro-lenses have been placed in front of planar antenna structures to achieve the gain required to couple efficiently to the telescope optics. In this paper are presented the design concept and a preliminary analysis of the measured performances of a phase-engineered metamaterial flat-lenslet. The flat lens design is inherently matched to free space, avoiding the necessity of an anti-reflection coating layer. It can be fabricated lithographically, making scaling to large format arrays relatively simple. Furthermore, this technology is compatible with the fabrication process required for the production of large-format lumped element kinetic inductance detector arrays which have already demonstrated the required sensitivity along with multiplexing ratios of order 1000 detectors/channel.
{"title":"Design and experimental investigation of a planar metamaterial silicon based lenslet","authors":"T. Gascard, G. Pisano, S. Doyle, A. Shitvov, J. Austermann, J. Beall, J. Hubmayr, Benjamin Raymond, N. Halverson, G. Jaehnig, C. Mckenney, A. Suzuki","doi":"10.1117/12.2562692","DOIUrl":"https://doi.org/10.1117/12.2562692","url":null,"abstract":"The next generations of ground-based cosmic microwave background experiments will require polarisation sensitive, multichroic pixels of large focal planes comprising several thousand detectors operating at the photon noise limit. One approach to achieve this goal is to couple light from the telescope to a polarisation sensitive antenna structure connected to a superconducting diplexer network where the desired frequency bands are filtered before being fed to individual ultra-sensitive detectors such as Transition Edge Sensors. Traditionally, arrays constituted of horn antennas, planar phased antennas or anti-reflection coated micro-lenses have been placed in front of planar antenna structures to achieve the gain required to couple efficiently to the telescope optics. In this paper are presented the design concept and a preliminary analysis of the measured performances of a phase-engineered metamaterial flat-lenslet. The flat lens design is inherently matched to free space, avoiding the necessity of an anti-reflection coating layer. It can be fabricated lithographically, making scaling to large format arrays relatively simple. Furthermore, this technology is compatible with the fabrication process required for the production of large-format lumped element kinetic inductance detector arrays which have already demonstrated the required sensitivity along with multiplexing ratios of order 1000 detectors/channel.","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":"114506777","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}
Naeun Shin, Yong-Sun Park, H. Kang, Jinguk Seo, S. Trippe, Dongkok Kim, D. Byun, K. Asada, Wen-Ping Lo, B. Sohn
Seoul National University Radio Astronomy Observatory (SRAO), a 6-meter single-dish telescope recently applied new 100GHz and 230GHz dual-band receiver. The SRAO had been inactive for several years, but resumed operation by adapting the Combined Array for Research in Millimeter-wave Astronomy (CARMA) receiver. We succeeded in the single-dish observations in 2019 March. We upgraded the SRAO to the mm-VLBI station and participated in the test observation of East Asia VLBI Network (EAVN) with several telescopes worldwide. The simultaneous single dish and VLBI observation is possible. We are going to design the new receiver and import a wideband 230GHz mixer and have a VLBI observation with Korean VLBI Network (KVN). Also, we are planning to test the phase reference technique between 100Ghz and 230GHz.
{"title":"The new era of Seoul National University Radio Astronomy Observatory (SRAO)","authors":"Naeun Shin, Yong-Sun Park, H. Kang, Jinguk Seo, S. Trippe, Dongkok Kim, D. Byun, K. Asada, Wen-Ping Lo, B. Sohn","doi":"10.1117/12.2560902","DOIUrl":"https://doi.org/10.1117/12.2560902","url":null,"abstract":"Seoul National University Radio Astronomy Observatory (SRAO), a 6-meter single-dish telescope recently applied new 100GHz and 230GHz dual-band receiver. The SRAO had been inactive for several years, but resumed operation by adapting the Combined Array for Research in Millimeter-wave Astronomy (CARMA) receiver. We succeeded in the single-dish observations in 2019 March. We upgraded the SRAO to the mm-VLBI station and participated in the test observation of East Asia VLBI Network (EAVN) with several telescopes worldwide. The simultaneous single dish and VLBI observation is possible. We are going to design the new receiver and import a wideband 230GHz mixer and have a VLBI observation with Korean VLBI Network (KVN). Also, we are planning to test the phase reference technique between 100Ghz and 230GHz.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"20 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":"129979408","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. Crites, J. Bock, M. Bradford, V. Butler, Tzu-Ching Chang, Yun-Ting Cheng, N. Emerson, C. Frez, J. Hunacek, R. Keenan, Chao-Te Li, P. Madonia, D. Marrone, L. Moncelsi, T. Prouvé, Guochao Sun, I. Trumper, A. Turner, A. Weber, T. Wei, M. Zemcov, Tess Case-Cortes
{"title":"A status update on TIME: a mm-wavelength spectrometer designed to probe the Epoch of Reionization","authors":"A. Crites, J. Bock, M. Bradford, V. Butler, Tzu-Ching Chang, Yun-Ting Cheng, N. Emerson, C. Frez, J. Hunacek, R. Keenan, Chao-Te Li, P. Madonia, D. Marrone, L. Moncelsi, T. Prouvé, Guochao Sun, I. Trumper, A. Turner, A. Weber, T. Wei, M. Zemcov, Tess Case-Cortes","doi":"10.1117/12.2561865","DOIUrl":"https://doi.org/10.1117/12.2561865","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"68 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":"121452487","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. Nishino, D. Barron, A. Bender, Y. Chinone, K. Crowley, T. Elleflot, J. Groh, M. Hasegawa, M. Hazumi, C. Hill, H. Hirose, L. Howe, D. Kaneko, S. Kikuchi, T. Kisner, A. Kusaka, J. Montgomery, A. Rahlin, Praweeen Siritanasak, G. Smecher, S. Takakura, S. Takatori, D. Tanabe, B. Westbrook, N. Whitehorn, A. Zahn, Yuyang Zhou
The Simons Array upgrades the POLARBEAR experiment, which measures the cosmic microwave background from the Atacama Desert in Chile, with three newly developed receivers. Each receiver has 7,588 transition-edge sensor bolometers with a raw data rate of approximately 20 MB/s. This significantly increased data rate required us to develop a new data-acquisition (DAQ) and data-management system. As the network bandwidth from our observatory to our data-storage sites outside Chile is not high enough to send all the raw data, we compress the raw data on-site. The expected yearly compressed data rate is approximately 60 TB from each receiver. We have also developed a new housekeeping DAQ system. The new housekeeping DAQ system is a distributed system to handle the various newly added monitoring systems and to better understand our instruments and environments. Those data can also be fetched by another module for real-time monitoring of our instrument from all over the world with latencies on the order of minutes. We deployed the first receiver in late 2018 and started the commissioning of the DAQ system. The DAQ system has been working without significant problems and already accumulates a considerable amount of the new receiver data from the commissioning observations. In this presentation, we summarize and report the status of the new systems.
{"title":"Data acquisition and management system for the CMB polarization experiment: Simons Array","authors":"H. Nishino, D. Barron, A. Bender, Y. Chinone, K. Crowley, T. Elleflot, J. Groh, M. Hasegawa, M. Hazumi, C. Hill, H. Hirose, L. Howe, D. Kaneko, S. Kikuchi, T. Kisner, A. Kusaka, J. Montgomery, A. Rahlin, Praweeen Siritanasak, G. Smecher, S. Takakura, S. Takatori, D. Tanabe, B. Westbrook, N. Whitehorn, A. Zahn, Yuyang Zhou","doi":"10.1117/12.2560616","DOIUrl":"https://doi.org/10.1117/12.2560616","url":null,"abstract":"The Simons Array upgrades the POLARBEAR experiment, which measures the cosmic microwave background from the Atacama Desert in Chile, with three newly developed receivers. Each receiver has 7,588 transition-edge sensor bolometers with a raw data rate of approximately 20 MB/s. This significantly increased data rate required us to develop a new data-acquisition (DAQ) and data-management system. As the network bandwidth from our observatory to our data-storage sites outside Chile is not high enough to send all the raw data, we compress the raw data on-site. The expected yearly compressed data rate is approximately 60 TB from each receiver. We have also developed a new housekeeping DAQ system. The new housekeeping DAQ system is a distributed system to handle the various newly added monitoring systems and to better understand our instruments and environments. Those data can also be fetched by another module for real-time monitoring of our instrument from all over the world with latencies on the order of minutes. We deployed the first receiver in late 2018 and started the commissioning of the DAQ system. The DAQ system has been working without significant problems and already accumulates a considerable amount of the new receiver data from the commissioning observations. In this presentation, we summarize and report the status of the new systems.","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":"130352731","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. Nitta, M. Nagai, Y. Murayama, R. Hikawa, Ryuji Suzuki, Y. Sekimoto, H. Takakura, T. Hasebe, K. Noda, Satoshi Saeki, H. Matsuo, N. Kuno, N. Nakai
We are developing a 100-GHz band 109-pixel MKID camera for the Nobeyama 45-m telescope. The camera optics contains plano-convex silicon (Si) lenses with 300- and 154-mm diameters located at the 4-K and 1-K stages, and a vacuum window of 320-mm diameter. Antireflective subwavelength structures (SWSs) for the Si lenses and the vacuum window were designed to reduce surface reflection. Cyclo olefin polymer (COP) was chosen as the base material for vacuum window as the dielectric loss is comparable with high-density polyethylene and it is easy to fabricate. Antireflective SWSs optimized for 100-GHz band were simulated using ANSYS HFSS. A one-layer rectangular pillar was designed for a Si lens of 300-mm diameter and a 320-mm diameter COP window to examine the fabrication process in large areas. For 154-mm diameter Si lens, a 1.2-mm depth tapered structure was used to obtain broadband characteristics. These designed structures were fabricated on both sides using a three-axis numerically-controlled machine. An end mill and a metal-bonded dicing blade were used for cutting the COP and Si, respectively. W-band vector network analyzer was used for S-parameter measurements of the SWS formed flat surface at an ambient temperature. Average surface reflectance of Si lenses and transmittance of the COP window in the 90–110 GHz range were found at approximately 1% and 98%, respectively.
{"title":"Anti-reflection structures for large-aperture cryogenic lenses and vacuum window in 100-GHz band","authors":"T. Nitta, M. Nagai, Y. Murayama, R. Hikawa, Ryuji Suzuki, Y. Sekimoto, H. Takakura, T. Hasebe, K. Noda, Satoshi Saeki, H. Matsuo, N. Kuno, N. Nakai","doi":"10.1117/12.2560900","DOIUrl":"https://doi.org/10.1117/12.2560900","url":null,"abstract":"We are developing a 100-GHz band 109-pixel MKID camera for the Nobeyama 45-m telescope. The camera optics contains plano-convex silicon (Si) lenses with 300- and 154-mm diameters located at the 4-K and 1-K stages, and a vacuum window of 320-mm diameter. Antireflective subwavelength structures (SWSs) for the Si lenses and the vacuum window were designed to reduce surface reflection. Cyclo olefin polymer (COP) was chosen as the base material for vacuum window as the dielectric loss is comparable with high-density polyethylene and it is easy to fabricate. Antireflective SWSs optimized for 100-GHz band were simulated using ANSYS HFSS. A one-layer rectangular pillar was designed for a Si lens of 300-mm diameter and a 320-mm diameter COP window to examine the fabrication process in large areas. For 154-mm diameter Si lens, a 1.2-mm depth tapered structure was used to obtain broadband characteristics. These designed structures were fabricated on both sides using a three-axis numerically-controlled machine. An end mill and a metal-bonded dicing blade were used for cutting the COP and Si, respectively. W-band vector network analyzer was used for S-parameter measurements of the SWS formed flat surface at an ambient temperature. Average surface reflectance of Si lenses and transmittance of the COP window in the 90–110 GHz range were found at approximately 1% and 98%, respectively.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"22 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":"130937969","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. Orlando, Christopher N. Thomas, D. Goldie, P. Hargrave, R. Sudiwala, Prateek Kumar Dongre, S. Withington
{"title":"A millimeter-wave on-chip superconducting filter bank spectrometer for atmospheric science","authors":"A. Orlando, Christopher N. Thomas, D. Goldie, P. Hargrave, R. Sudiwala, Prateek Kumar Dongre, S. Withington","doi":"10.1117/12.2564383","DOIUrl":"https://doi.org/10.1117/12.2564383","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"47 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":"114395429","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. Gonzalez, K. Kaneko, R. Sakai, T. Kojima, Y. Uzawa
In recent years, NAOJ has contributed designs and production of waveguide and optics components for ALMA bands 1 (35-50 GHz) and 2 (67-116 GHz) receivers. This includes several novel ideas in the design of corrugated horns and OMTs and the application of 3D printing for the fabrication of key components of radio receivers. These frequency bands coincide approximately with bands 5 and 6 of ngVLA, the most promising project in the 2020s to exploit synergies with ALMA with the goal of increasing the scientific output of both facilities. This paper reports on the recent ALMA development results and discusses their future application to ngVLA.
{"title":"Development of receiver optics for ALMA bands 1 and 2, and possible synergies with ngVLA","authors":"A. Gonzalez, K. Kaneko, R. Sakai, T. Kojima, Y. Uzawa","doi":"10.1117/12.2561595","DOIUrl":"https://doi.org/10.1117/12.2561595","url":null,"abstract":"In recent years, NAOJ has contributed designs and production of waveguide and optics components for ALMA bands 1 (35-50 GHz) and 2 (67-116 GHz) receivers. This includes several novel ideas in the design of corrugated horns and OMTs and the application of 3D printing for the fabrication of key components of radio receivers. These frequency bands coincide approximately with bands 5 and 6 of ngVLA, the most promising project in the 2020s to exploit synergies with ALMA with the goal of increasing the scientific output of both facilities. This paper reports on the recent ALMA development results and discusses their future application to ngVLA.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"87 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":"127458135","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. Mckenney, J. Austermann, J. Beall, N. Halverson, J. Hubmayr, G. Jaehnig, G. Pisano, Sarah A. Stevenson, A. Suzuki, Jonathan A. Thompson
Large imaging arrays of detectors at millimeter and submillimeter wavelengths have applications that include measurements of the faint polarization signal in the Cosmic Microwave Background (CMB), and submillimeter astrophysics. We are developing planar lenslet arrays for millimeter-wavelength imaging using metamaterials microlithically fabricated using silicon wafers. This metamaterial technology has many potential advantages compared to conventional hemispherical lenslet arrays, including high precision and homogeneity, planar integrated anti-reflection layers, and a coefficient of thermal expansion matched to the silicon detector wafer. Here we describe the design process for a gradient-index (GRIN) metamaterial lenslet using metal-mesh patterned on silicon and a combination of metal-mesh and etched-hole metamaterial anti-reflection layers. We optimize the design using a bulk-material model to rapidly simulate and iterate on the lenslet design. We fabricated prototype GRIN metamaterial lenslet array and mounted it on a Polarbear/Simons Array 90/150~GHz band transition edge sensor (TES) bolometer detector array with sinuous planar antennas. Beam measurements of a prototype lenslet array agree reasonably well with the model simulations. We plan to further optimize the design and combine it with a broadband anti-reflection coating to achieve operation over 70--350~GHz bandwidth.
{"title":"Planar silicon metamaterial lenslet arrays for millimeter-wavelength imaging","authors":"C. Mckenney, J. Austermann, J. Beall, N. Halverson, J. Hubmayr, G. Jaehnig, G. Pisano, Sarah A. Stevenson, A. Suzuki, Jonathan A. Thompson","doi":"10.1117/12.2565532","DOIUrl":"https://doi.org/10.1117/12.2565532","url":null,"abstract":"Large imaging arrays of detectors at millimeter and submillimeter wavelengths have applications that include measurements of the faint polarization signal in the Cosmic Microwave Background (CMB), and submillimeter astrophysics. We are developing planar lenslet arrays for millimeter-wavelength imaging using metamaterials microlithically fabricated using silicon wafers. This metamaterial technology has many potential advantages compared to conventional hemispherical lenslet arrays, including high precision and homogeneity, planar integrated anti-reflection layers, and a coefficient of thermal expansion matched to the silicon detector wafer. Here we describe the design process for a gradient-index (GRIN) metamaterial lenslet using metal-mesh patterned on silicon and a combination of metal-mesh and etched-hole metamaterial anti-reflection layers. We optimize the design using a bulk-material model to rapidly simulate and iterate on the lenslet design. We fabricated prototype GRIN metamaterial lenslet array and mounted it on a Polarbear/Simons Array 90/150~GHz band transition edge sensor (TES) bolometer detector array with sinuous planar antennas. Beam measurements of a prototype lenslet array agree reasonably well with the model simulations. We plan to further optimize the design and combine it with a broadband anti-reflection coating to achieve operation over 70--350~GHz bandwidth.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"25 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":"127459272","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. Kohno, R. Kawabe, Y. Tamura, A. Endo, J. Baselmans, K. Karatsu, A. Inoue, K. Moriwaki, N. H. Hayatsu, N. Yoshida, Y. Yoshimura, B. Hatsukade, H. Umehata, T. Oshima, T. Takekoshi, A. Taniguchi, P. Klaassen, T. Mroczkowski, C. Cicone, F. Bertoldi, H. Dannerbauer, T. Tosaki
We present a conceptual study of a large format imaging spectrograph for next-generation large (50-m class) single-dish telescopes, i.e., the Large Submillimeter Telescope (LST) and Atacama Large Aperture Submillimeter Telescope (AtLAST). Recent discoveries of high-redshift star-forming galaxies at z=8-9 and candidate quiescent galaxies at z~6 indicate the onset of earliest star formation just a few 100 million years after the Big Bang (i.e., z = 12 - 15), and LST/AtLAST will provide a unique pathway to uncover spectroscopically-identified ``first forming galaxies’’ in the pre-reionization era, once it will be equipped with a large format imaging spectrograph. We describe the preliminary of 3-band, medium resolution (R=2000) imaging spectrograph with ~1.5 M detectors in total based on the KATANA concept (Karatsu et al.~2019), which exploits technologies of the integrated superconducting spectrometer (ISS) and a large-format imaging array like A-MKID.
我们提出了下一代大型(50米级)单碟望远镜，即大亚毫米望远镜(LST)和阿塔卡马大口径亚毫米望远镜(AtLAST)的大画幅成像光谱仪的概念研究。最近发现的z=8-9的高红移恒星形成星系和z~6的候选静止星系表明，最早的恒星形成开始于大爆炸后的几亿年(即z= 12 - 15)， LST/AtLAST将提供一个独特的途径，揭示光谱识别的“第一次形成星系”在预再电离时代，一旦它将配备一个大格式成像光谱仪。基于KATANA概念(Karatsu et al.~2019)，利用集成超导光谱仪(ISS)和a - mkid等大画幅成像阵列技术，初步设计了3波段、中分辨率(R=2000)、总检测器约1.5 M的成像光谱仪。
{"title":"Large format imaging spectrograph for the Large Submillimeter Telescope (LST)","authors":"K. Kohno, R. Kawabe, Y. Tamura, A. Endo, J. Baselmans, K. Karatsu, A. Inoue, K. Moriwaki, N. H. Hayatsu, N. Yoshida, Y. Yoshimura, B. Hatsukade, H. Umehata, T. Oshima, T. Takekoshi, A. Taniguchi, P. Klaassen, T. Mroczkowski, C. Cicone, F. Bertoldi, H. Dannerbauer, T. Tosaki","doi":"10.1117/12.2561238","DOIUrl":"https://doi.org/10.1117/12.2561238","url":null,"abstract":"We present a conceptual study of a large format imaging spectrograph for next-generation large (50-m class) single-dish telescopes, i.e., the Large Submillimeter Telescope (LST) and Atacama Large Aperture Submillimeter Telescope (AtLAST). Recent discoveries of high-redshift star-forming galaxies at z=8-9 and candidate quiescent galaxies at z~6 indicate the onset of earliest star formation just a few 100 million years after the Big Bang (i.e., z = 12 - 15), and LST/AtLAST will provide a unique pathway to uncover spectroscopically-identified ``first forming galaxies’’ in the pre-reionization era, once it will be equipped with a large format imaging spectrograph. We describe the preliminary of 3-band, medium resolution (R=2000) imaging spectrograph with ~1.5 M detectors in total based on the KATANA concept (Karatsu et al.~2019), which exploits technologies of the integrated superconducting spectrometer (ISS) and a large-format imaging array like A-MKID.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"61 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131000593","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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