D. Henke, D. Johnstone, L. Knee, S. Chapman, C. Ross, M. Fich, T. Nikola, Steve K. Choi, M. Niemack, S. Parshley, G. Stacey, E. Vavagiakis
{"title":"Optical design study for the 860 GHz first-light camera module of CCAT-p (Erratum)","authors":"D. Henke, D. Johnstone, L. Knee, S. Chapman, C. Ross, M. Fich, T. Nikola, Steve K. Choi, M. Niemack, S. Parshley, G. Stacey, E. Vavagiakis","doi":"10.1117/12.2594257","DOIUrl":"https://doi.org/10.1117/12.2594257","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"728 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2021-02-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134238730","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":"Front Matter: Volume 11453","authors":"","doi":"10.1117/12.2591723","DOIUrl":"https://doi.org/10.1117/12.2591723","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"45 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2021-01-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120946719","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. Komatsu, H. Ishino, H. Kataza, K. Konishi, M. Kuwata-Gonokami, N. Katayama, S. Sugiyama, T. Matsumura, H. Sakurai, Y. Sakurai, R. Takaku, J. Yumoto
We have developed a prototype half-wave plate (HWP) based polarization modulator (PMU) for Cosmic Microwave Background polarization measurement experiments. We built a 1/10 scaled PMU that consists of a 50 mm diameter five-layer achromatic HWP with a moth-eye broadband anti-reflection sub-wavelength structure mounted on a superconducting magnetic bearing. The entire system has cooled below 20 K in a cryostat chamber that has two millimeter-wave transparent windows. A coherent source and the diode detector are placed outside of the cryostat and the millimeter-wave goes through the PMU in the cryostat. We have measured the modulated signal by the PMU, analyzed the spectral signatures, and extracted the modulation efficiency over the frequency coverage of 34-161 GHz. We identified the peaks in the optical data, which are synchronous to the rotational frequency. We also identified the peaks that are originated from the resonance frequency of the levitating system. We also recovered the modulation efficiency as a function of the incident electromagnetic frequency and the data agrees to the predicted curves within uncertainties of the input parameters, i.e. the indices of refraction, thickness, and angle alignment. Finally, we discuss the implication of the results when this is applied to the LiteBIRD low-frequency telescope.
{"title":"Demonstration of five-layer phase-flat achromatic half-wave plate with anti-reflective structures and superconducting magnetic bearing for CMB polarization experiments","authors":"K. Komatsu, H. Ishino, H. Kataza, K. Konishi, M. Kuwata-Gonokami, N. Katayama, S. Sugiyama, T. Matsumura, H. Sakurai, Y. Sakurai, R. Takaku, J. Yumoto","doi":"10.1117/12.2560486","DOIUrl":"https://doi.org/10.1117/12.2560486","url":null,"abstract":"We have developed a prototype half-wave plate (HWP) based polarization modulator (PMU) for Cosmic Microwave Background polarization measurement experiments. We built a 1/10 scaled PMU that consists of a 50 mm diameter five-layer achromatic HWP with a moth-eye broadband anti-reflection sub-wavelength structure mounted on a superconducting magnetic bearing. The entire system has cooled below 20 K in a cryostat chamber that has two millimeter-wave transparent windows. A coherent source and the diode detector are placed outside of the cryostat and the millimeter-wave goes through the PMU in the cryostat. We have measured the modulated signal by the PMU, analyzed the spectral signatures, and extracted the modulation efficiency over the frequency coverage of 34-161 GHz. We identified the peaks in the optical data, which are synchronous to the rotational frequency. We also identified the peaks that are originated from the resonance frequency of the levitating system. We also recovered the modulation efficiency as a function of the incident electromagnetic frequency and the data agrees to the predicted curves within uncertainties of the input parameters, i.e. the indices of refraction, thickness, and angle alignment. Finally, we discuss the implication of the results when this is applied to the LiteBIRD low-frequency telescope.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"68 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131044473","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. Komatsu, H. Ishino, N. Katayama, T. Matsumura, Y. Sakurai, R. Takaku
Pancharatnam base achromatic half-wave plate (AHWP) achieves high polarization efficiency over broadband. It generally comes with a feature of which the optic axis of AHWP has dependence of the electromagnetic frequency of the incident radiation. When the AHWP is used to measure the incident polarized radiation with a finite detection bandwidth, this frequency dependence causes an uncertainty in the determination of the polarization angle due to the limited knowledge of a detection band shape and a source spectral shape. To mitigate this problem, we propose new designs of the AHWP that eliminate the frequency dependent optic axis over the bandwidth of which the polarization efficiency also achieves the same broadband width. We carried out the optimization by tuning the relative angles among the individual half-wave plates (HWP) of the five- and nine-layer AHWP. The optimized set of the relative angles achieves the frequency independent optic axis and covers the fractional bandwidth of 1.3 and 1.5 for five- and nine-layer AHWPs, respectively. We also study the susceptibility of the alignment accuracy, which can be chosen based on the requirement in each application.
{"title":"Design and demonstration of the frequency independent fast axis of the Pancharatnam base multi-layer half-wave plate for CMB polarization experiment","authors":"K. Komatsu, H. Ishino, N. Katayama, T. Matsumura, Y. Sakurai, R. Takaku","doi":"10.1117/12.2562092","DOIUrl":"https://doi.org/10.1117/12.2562092","url":null,"abstract":"Pancharatnam base achromatic half-wave plate (AHWP) achieves high polarization efficiency over broadband. It generally comes with a feature of which the optic axis of AHWP has dependence of the electromagnetic frequency of the incident radiation. When the AHWP is used to measure the incident polarized radiation with a finite detection bandwidth, this frequency dependence causes an uncertainty in the determination of the polarization angle due to the limited knowledge of a detection band shape and a source spectral shape. To mitigate this problem, we propose new designs of the AHWP that eliminate the frequency dependent optic axis over the bandwidth of which the polarization efficiency also achieves the same broadband width. We carried out the optimization by tuning the relative angles among the individual half-wave plates (HWP) of the five- and nine-layer AHWP. The optimized set of the relative angles achieves the frequency independent optic axis and covers the fractional bandwidth of 1.3 and 1.5 for five- and nine-layer AHWPs, respectively. We also study the susceptibility of the alignment accuracy, which can be chosen based on the requirement in each application.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"80 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126209260","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}
Y. Sekimoto, Y. Sekimoto, Y. Sekimoto, P. Ade, A. Adler, E. Allys, E. Allys, K. Arnold, D. Auguste, J. Aumont, R. Aurlien, J. Austermann, C. Baccigalupi, A. Banday, R. Banerji, R. B. Barreiro, S. Basak, J. Beall, D. Beck, S. Beckman, J. Bermejo, P. Bernardis, M. Bersanelli, J. Bonis, J. Borrill, J. Borrill, F. Boulanger, F. Boulanger, S. Bounissou, M. Brilenkov, Michael D Brown, M. Bucher, E. Calabrese, P. Campeti, A. Carones, F. Casas, A. Challinor, V. Chan, K. Cheung, Y. Chinone, J. Cliche, L. Colombo, F. Columbro, J. Cubas, A. Cukierman, A. Cukierman, D. Curtis, G. D’Alessandro, N. Dachlythra, M. Petris, C. Dickinson, P. Diego-Palazuelos, M. Dobbs, T. Dotani, L. Duband, S. Duff, J. Duval, K. Ebisawa, T. Elleflot, H. Eriksen, J. Errard, T. Essinger-Hileman, F. Finelli, R. Flauger, C. Franceschet, U. Fuskeland, M. Galloway, K. Ganga, Jiangsong Gao, R. Génova-Santos, M. Gerbino, M. Gervasi, Tommaso Ghigna, Tommaso Ghigna, E. Gjerløw, M. Gradziel, J. Grain, F. Grupp, A. Gruppuso, J. Gudmundsson, T. Haan, N
LiteBIRD has been selected as JAXA’s strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) B-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of -56 dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34–161 GHz), one of LiteBIRD’s onboard telescopes. It has a wide field-of-view (18° x 9°) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90◦ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at 5 K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented.
{"title":"Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD","authors":"Y. Sekimoto, Y. Sekimoto, Y. Sekimoto, P. Ade, A. Adler, E. Allys, E. Allys, K. Arnold, D. Auguste, J. Aumont, R. Aurlien, J. Austermann, C. Baccigalupi, A. Banday, R. Banerji, R. B. Barreiro, S. Basak, J. Beall, D. Beck, S. Beckman, J. Bermejo, P. Bernardis, M. Bersanelli, J. Bonis, J. Borrill, J. Borrill, F. Boulanger, F. Boulanger, S. Bounissou, M. Brilenkov, Michael D Brown, M. Bucher, E. Calabrese, P. Campeti, A. Carones, F. Casas, A. Challinor, V. Chan, K. Cheung, Y. Chinone, J. Cliche, L. Colombo, F. Columbro, J. Cubas, A. Cukierman, A. Cukierman, D. Curtis, G. D’Alessandro, N. Dachlythra, M. Petris, C. Dickinson, P. Diego-Palazuelos, M. Dobbs, T. Dotani, L. Duband, S. Duff, J. Duval, K. Ebisawa, T. Elleflot, H. Eriksen, J. Errard, T. Essinger-Hileman, F. Finelli, R. Flauger, C. Franceschet, U. Fuskeland, M. Galloway, K. Ganga, Jiangsong Gao, R. Génova-Santos, M. Gerbino, M. Gervasi, Tommaso Ghigna, Tommaso Ghigna, E. Gjerløw, M. Gradziel, J. Grain, F. Grupp, A. Gruppuso, J. Gudmundsson, T. Haan, N","doi":"10.1117/12.2561841","DOIUrl":"https://doi.org/10.1117/12.2561841","url":null,"abstract":"LiteBIRD has been selected as JAXA’s strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) B-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of -56 dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34–161 GHz), one of LiteBIRD’s onboard telescopes. It has a wide field-of-view (18° x 9°) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90◦ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at 5 K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"44 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132594567","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. Duell, E. Vavagiakis, J. Austermann, S. Chapman, Steve K. Choi, N. Cothard, B. Dober, P. Gallardo, Jiansong Gao, C. Groppi, T. Herter, G. Stacey, Z. Huber, J. Hubmayr, D. Johnstone, Yaqiong Li, P. Mauskopf, J. McMahon, M. Niemack, T. Nikola, K. Rossi, S. Simon, A. Sinclair, M. Vissers, J. Wheeler, B. Zou
The CCAT-prime project's first light array will be deployed in Mod-Cam, a single-module testbed and first light cryostat, on the Fred Young Submillimeter Telescope (FYST) in Chile's high Atacama desert in late 2022. FYST is a six-meter aperture telescope being built on Cerro Chajnantor at an elevation of 5600 meters to observe at millimeter and submillimeter wavelengths.1 Mod-Cam will pave the way for Prime-Cam, the primary first generation instrument, which will house up to seven instrument modules to simultaneously observe the sky and study a diverse set of science goals from monitoring protostars to probing distant galaxy clusters and characterizing the cosmic microwave background (CMB). At least one feedhorn-coupled array of microwave kinetic inductance detectors (MKIDs) centered on 280 GHz will be included in Mod-Cam at first light, with additional instrument modules to be deployed along with Prime-Cam in stages. The first 280 GHz detector array was fabricated by the Quantum Sensors Group at NIST in Boulder, CO and includes 3,456 polarization- sensitive MKIDs. Current mechanical designs allow for up to three hexagonal arrays to be placed in each single instrument module. We present details on this first light detector array, including mechanical designs and cold readout plans, as well as introducing Mod-Cam as both a testbed and predecessor to Prime-Cam.
{"title":"CCAT-prime: Designs and status of the first light 280 GHz MKID array and mod-cam receiver","authors":"C. Duell, E. Vavagiakis, J. Austermann, S. Chapman, Steve K. Choi, N. Cothard, B. Dober, P. Gallardo, Jiansong Gao, C. Groppi, T. Herter, G. Stacey, Z. Huber, J. Hubmayr, D. Johnstone, Yaqiong Li, P. Mauskopf, J. McMahon, M. Niemack, T. Nikola, K. Rossi, S. Simon, A. Sinclair, M. Vissers, J. Wheeler, B. Zou","doi":"10.1117/12.2562757","DOIUrl":"https://doi.org/10.1117/12.2562757","url":null,"abstract":"The CCAT-prime project's first light array will be deployed in Mod-Cam, a single-module testbed and first light cryostat, on the Fred Young Submillimeter Telescope (FYST) in Chile's high Atacama desert in late 2022. FYST is a six-meter aperture telescope being built on Cerro Chajnantor at an elevation of 5600 meters to observe at millimeter and submillimeter wavelengths.1 Mod-Cam will pave the way for Prime-Cam, the primary first generation instrument, which will house up to seven instrument modules to simultaneously observe the sky and study a diverse set of science goals from monitoring protostars to probing distant galaxy clusters and characterizing the cosmic microwave background (CMB). At least one feedhorn-coupled array of microwave kinetic inductance detectors (MKIDs) centered on 280 GHz will be included in Mod-Cam at first light, with additional instrument modules to be deployed along with Prime-Cam in stages. The first 280 GHz detector array was fabricated by the Quantum Sensors Group at NIST in Boulder, CO and includes 3,456 polarization- sensitive MKIDs. Current mechanical designs allow for up to three hexagonal arrays to be placed in each single instrument module. We present details on this first light detector array, including mechanical designs and cold readout plans, as well as introducing Mod-Cam as both a testbed and predecessor to Prime-Cam.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"11 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120918664","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. Lunde, P. Ade, M. Berthoud, R. Contente, N. DeNigris, S. Doyle, D. Ferrusca, J. Golec, Stephen Kuczarski, Dennis Lee, Zhiyuan Ma, P. Mauskopf, M. Mccrackan, J. McMahon, G. Novak, G. Pisano, S. Simon, K. Souccar, C. Tucker, M. Underhill, E. V. Camp, G. Wilson
TolTEC is an imaging polarimeter that will be mounted on the 50m diameter Large Millimeter Telescope (LMT) in Mexico. This camera simultaneously images the focal plane at three wavebands centered at 1.1, 1.4, and 2.0mm. TolTEC combines polarization-sensitive Kinetic Inductance Detectors (KIDs) with the LMT to produce 5-10 arcmin resolution maps of the sky in both total intensity and polarization. The light from the telescope is coupled to the TolTEC instrument using three room temperature mirrors. Before entering the cryostat, the light passes through a rapid-spinning achromatic half-wave plate, and once inside it passes through a 1 K Lyot stop that controls the telescope illumination. Inside the cryostat, a series of aluminum mirrors, silicon lenses, and dichroic filters split the light into three wavelength bands and direct each band to a different detector array. We will describe the design, and performance of the optics before installation at the telescope.
{"title":"The optical design and performance of TolTEC: a millimeter-wave imaging polarimeter","authors":"E. Lunde, P. Ade, M. Berthoud, R. Contente, N. DeNigris, S. Doyle, D. Ferrusca, J. Golec, Stephen Kuczarski, Dennis Lee, Zhiyuan Ma, P. Mauskopf, M. Mccrackan, J. McMahon, G. Novak, G. Pisano, S. Simon, K. Souccar, C. Tucker, M. Underhill, E. V. Camp, G. Wilson","doi":"10.1117/12.2562798","DOIUrl":"https://doi.org/10.1117/12.2562798","url":null,"abstract":"TolTEC is an imaging polarimeter that will be mounted on the 50m diameter Large Millimeter Telescope (LMT) in Mexico. This camera simultaneously images the focal plane at three wavebands centered at 1.1, 1.4, and 2.0mm. TolTEC combines polarization-sensitive Kinetic Inductance Detectors (KIDs) with the LMT to produce 5-10 arcmin resolution maps of the sky in both total intensity and polarization. The light from the telescope is coupled to the TolTEC instrument using three room temperature mirrors. Before entering the cryostat, the light passes through a rapid-spinning achromatic half-wave plate, and once inside it passes through a 1 K Lyot stop that controls the telescope illumination. Inside the cryostat, a series of aluminum mirrors, silicon lenses, and dichroic filters split the light into three wavelength bands and direct each band to a different detector array. We will describe the design, and performance of the optics before installation at the telescope.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"13 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124979179","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. O’Brient, C. Bradford, M. Kenyon, H. Nguyen, H. Hui, P. Echternach, G. Lange, Damian Audley, J. Kuur
We are developing ultra-low noise transition edge sensor (TES) bolometer arrays for the long-wavelength grating spectrometer modules of SAFARI, part of the cryogenically-cooled SPICA mission now in phase-A study in Europe. These devices target a per-pixel noise equivalent power (NEP) below 10^-19 WHz^-1/2 with a time-constant faster than 10ms. The SAFARI focal planes will be cooled to 50 mK, and we use a 100 mK thermistor formed from an annealed Titanium-Gold bilayer film. To minimize excess heat capacity, we have developed a new wet-release process which provides high yield in large (~250-pixel) sub-arrays. We will report on the fabrication, testing, and achieved performance of these detectors.We will also present the focal plane assembly designed to support the 5 (spatial) x 180 (spectral) format coupled to spectrometers thru multimodes horns. The focal plane is composed of four monolithic sub-arrays with integrated backshorts, all integrated onto a large silicon substrate.
{"title":"Ultra-low noise TES bolometer arrays for the US SAFARI contribution","authors":"R. O’Brient, C. Bradford, M. Kenyon, H. Nguyen, H. Hui, P. Echternach, G. Lange, Damian Audley, J. Kuur","doi":"10.1117/12.2563116","DOIUrl":"https://doi.org/10.1117/12.2563116","url":null,"abstract":"We are developing ultra-low noise transition edge sensor (TES) bolometer arrays for the long-wavelength grating spectrometer modules of SAFARI, part of the cryogenically-cooled SPICA mission now in phase-A study in Europe. These devices target a per-pixel noise equivalent power (NEP) below 10^-19 WHz^-1/2 with a time-constant faster than 10ms. The SAFARI focal planes will be cooled to 50 mK, and we use a 100 mK thermistor formed from an annealed Titanium-Gold bilayer film. To minimize excess heat capacity, we have developed a new wet-release process which provides high yield in large (~250-pixel) sub-arrays. We will report on the fabrication, testing, and achieved performance of these detectors.\u0000\u0000We will also present the focal plane assembly designed to support the 5 (spatial) x 180 (spectral) format coupled to spectrometers thru multimodes horns. The focal plane is composed of four monolithic sub-arrays with integrated backshorts, all integrated onto a large silicon substrate.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"21 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125408862","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. Toda, Yukiko Sakurai, H. Ishino, T. Matsumura, K. Komatsu, N. Katayama
A polarization modulator unit for a low-frequency telescope in LiteBIRD employs an achromatic half-wave plate (AHWP). It consists of five-layer a-cut sapphire plates, which are stacked based on a Pancharatnam recipe. In this way, the retardance of the AHWP is a half-wave over the bandwidth of 34 - 161 GHz. The diameter of a single sapphire plate is about 500mm and the thickness is about 5 mm. When a large diameter AHWP is used for a space mission, it is important for the AHWP to survive launch vibration. A preliminary study indicates that the five-layer-stacked HWP has a risk of breakage at the launch unless the 5 layers are glued together and mechanically treated as one disk. In this paper, we report our investigation using a sodium silicate solution which can bond between sapphire plates. This technique has been previously investigated as a candidate cryogenic glue for a mirror material, including sapphire, of the gravitational wave detector, LIGO and KAGRA. We experimentally studied the mechanical strength of the bonded interface for two different surface conditions, polished and unpolished. We demonstrated the tensile and shear strength of above 20MPa for samples with a polished surface, respectively. We also identified that samples glued on a polished surface show higher strength than unpolished ones by a factor of 2 for tensile and 18 for shear strength. We searched for any optical effects, e.g. extra gap or absorption by the bonding interface, by measuring the millimeter-wave transmission spectra in 90-140 GHz. We did not find any optical effect caused by the bonded interface within 2% error in transmittance that is originated from the measurement system.
{"title":"Mechanical strength and millimeter-wave transmission spectrum of stacked sapphire plates bonded by sodium silicate solution","authors":"T. Toda, Yukiko Sakurai, H. Ishino, T. Matsumura, K. Komatsu, N. Katayama","doi":"10.1117/12.2562366","DOIUrl":"https://doi.org/10.1117/12.2562366","url":null,"abstract":"A polarization modulator unit for a low-frequency telescope in LiteBIRD employs an achromatic half-wave plate (AHWP). It consists of five-layer a-cut sapphire plates, which are stacked based on a Pancharatnam recipe. In this way, the retardance of the AHWP is a half-wave over the bandwidth of 34 - 161 GHz. The diameter of a single sapphire plate is about 500mm and the thickness is about 5 mm. When a large diameter AHWP is used for a space mission, it is important for the AHWP to survive launch vibration. A preliminary study indicates that the five-layer-stacked HWP has a risk of breakage at the launch unless the 5 layers are glued together and mechanically treated as one disk. In this paper, we report our investigation using a sodium silicate solution which can bond between sapphire plates. This technique has been previously investigated as a candidate cryogenic glue for a mirror material, including sapphire, of the gravitational wave detector, LIGO and KAGRA. We experimentally studied the mechanical strength of the bonded interface for two different surface conditions, polished and unpolished. We demonstrated the tensile and shear strength of above 20MPa for samples with a polished surface, respectively. We also identified that samples glued on a polished surface show higher strength than unpolished ones by a factor of 2 for tensile and 18 for shear strength. We searched for any optical effects, e.g. extra gap or absorption by the bonding interface, by measuring the millimeter-wave transmission spectra in 90-140 GHz. We did not find any optical effect caused by the bonded interface within 2% error in transmittance that is originated from the measurement system.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"56 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127973137","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. Seibert, P. Ade, Aamir Ali, K. Arnold, N. Cothard, N. Galitzki, K. Harrington, S. Ho, B. Keating, L. Lowry, Megan B. Russell, M. Silva-Feaver, Praweeen Siritanasak, G. Teply, C. Tucker, E. Vavagiakis, Zhilei Xu, Zhilei Xu
The Simons Observatory (SO) is a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope, which will observe from the Atacama Desert in Chile. In total, SO will field over 60,000 transition edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities, as outlined in The Simons Observatory Collaboration et al. (2019). To verify consistency of fabrication and performance in line with our sensitivity requirements, we will perform in-lab optical tests on isolated SO detectors as well as full detector arrays. The tests include beam measurements, bandpass measurements, and polarization measurements, among others. Here, we will describe the development of a cryogenic testbed that enables optical characterization of SO's detectors. We include the infrared filtering strategy to allow suitable cryogenic performance, design and implementation of the test equipment used in characterization, and the preliminary results from our validation of the testbed's cryo-optical performance.
{"title":"Development of an optical detector testbed for the Simons Observatory","authors":"J. Seibert, P. Ade, Aamir Ali, K. Arnold, N. Cothard, N. Galitzki, K. Harrington, S. Ho, B. Keating, L. Lowry, Megan B. Russell, M. Silva-Feaver, Praweeen Siritanasak, G. Teply, C. Tucker, E. Vavagiakis, Zhilei Xu, Zhilei Xu","doi":"10.1117/12.2562045","DOIUrl":"https://doi.org/10.1117/12.2562045","url":null,"abstract":"The Simons Observatory (SO) is a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope, which will observe from the Atacama Desert in Chile. In total, SO will field over 60,000 transition edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities, as outlined in The Simons Observatory Collaboration et al. (2019). To verify consistency of fabrication and performance in line with our sensitivity requirements, we will perform in-lab optical tests on isolated SO detectors as well as full detector arrays. The tests include beam measurements, bandpass measurements, and polarization measurements, among others. Here, we will describe the development of a cryogenic testbed that enables optical characterization of SO's detectors. We include the infrared filtering strategy to allow suitable cryogenic performance, design and implementation of the test equipment used in characterization, and the preliminary results from our validation of the testbed's cryo-optical performance.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116650755","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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