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1. The Simons Observatory: science goals andforecasts

Author

Peter Ade, James Aguirre, Zeeshan Ahmed, Simone Aiola, Aamir Ali, David Alonso, Marcelo A. Alvarez, Kam Arnold, Peter Ashton, Jason Austermann, Humna Awan, Carlo Baccigalupi, Taylor Baildon, Darcy Barron, Nick Battaglia, Richard Battye, Eric Baxter, Andrew Bazarko, James A. Beall, Rachel Bean, Dominic Beck, Shawn Beckman, Benjamin Beringue, Federico Bianchini, Steven Boada, David Boettger, J. Richard Bond, Julian Borrill, Michael L. Brown, Sarah Marie Bruno, Sean Bryan, Erminia Calabrese, Victoria Calafut, Paolo Calisse, Julien Carron, Anthony Challinor, Grace Chesmore, Yuji Chinone, Jens Chluba, Hsiao-Mei Sherry Cho, Steve Choi, Gabriele Coppi, Nicholas F. Cothard, Kevin Coughlin, Devin Crichton, Kevin D. Crowley, Kevin T. Crowley, Ari Cukierman, John M. D'Ewart, Rolando Dünner, Tijmen de Haan, Mark Devlin, Simon Dicker, Joy Didier, Matt Dobbs, Bradley Dober, Cody J. Duell, Shannon Duff, Adri Duivenvoorden, Jo Dunkley, John Dusatko, Josquin Errard, Giulio Fabbian, Stephen Feeney, Simone Ferraro, Pedro Fluxà, Katherine Freese, Josef C. Frisch, Andrei Frolov, George Fuller, Brittany Fuzia, Nicholas Galitzki, Patricio A. Gallardo, Jose Tomas Galvez Ghersi, Jiansong Gao, Eric Gawiser, Martina Gerbino, Vera Gluscevic, Neil Goeckner-Wald, Joseph Golec, Sam Gordon, Megan Gralla, Daniel Green, Arpi Grigorian, John Groh, Chris Groppi, Yilun Guan, Jon E. Gudmundsson, Dongwon Han, Peter Hargrave, Masaya Hasegawa, Matthew Hasselfield, Makoto Hattori, Victor Haynes, Masashi Hazumi, Yizhou He, Erin Healy, Shawn W. Henderson, Carlos Hervias-Caimapo, Charles A. Hill, J. Colin Hill, Gene Hilton, Matt Hilton, Adam D. Hincks, Gary Hinshaw, Renée Hložek, Shirley Ho, Shuay-Pwu Patty Ho, Logan Howe, Zhiqi Huang, Johannes Hubmayr, Kevin Huffenberger, John P. Hughes, Anna Ijjas, Margaret Ikape, Kent Irwin, Andrew H. Jaffe, Bhuvnesh Jain, Oliver Jeong, Daisuke Kaneko, Ethan D. Karpel, Nobuhiko Katayama, Brian Keating, Sarah S. Kernasovskiy, Reijo Keskitalo, Theodore Kisner, Kenji Kiuchi, Jeff Klein, Kenda Knowles, Brian Koopman, Arthur Kosowsky, Nicoletta Krachmalnicoff, Stephen E. Kuenstner, Chao-Lin Kuo, Akito Kusaka, Jacob Lashner, Adrian Lee, Eunseong Lee, David Leon, Jason S.-Y. Leung, Antony Lewis, Yaqiong Li, Zack Li, Michele Limon, Eric Linder, Carlos Lopez-Caraballo, Thibaut Louis, Lindsay Lowry, Marius Lungu, Mathew Madhavacheril, Daisy Mak, Felipe Maldonado, Hamdi Mani, Ben Mates, Frederick Matsuda, Loïc Maurin, Phil Mauskopf, Andrew May, Nialh McCallum, Chris McKenney, Jeff McMahon, P. Daniel Meerburg, Joel Meyers, Amber Miller, Mark Mirmelstein, Kavilan Moodley, Moritz Munchmeyer, Charles Munson, Sigurd Naess, Federico Nati, Martin Navaroli, Laura Newburgh, Ho Nam Nguyen, Michael Niemack, Haruki Nishino, John Orlowski-Scherer, Lyman Page, Bruce Partridge, Julien Peloton, Francesca Perrotta, Lucio Piccirillo, Giampaolo Pisano, Davide Poletti, Roberto Puddu, Giuseppe Puglisi, Chris Raum, Christian L. Reichardt, Mathieu Remazeilles, Yoel Rephaeli, Dominik Riechers, Felipe Rojas, Anirban Roy, Sharon Sadeh, Yuki Sakurai, Maria Salatino, Mayuri Sathyanarayana Rao, Emmanuel Schaan, Marcel Schmittfull, Neelima Sehgal, Joseph Seibert, Uros Seljak, Blake Sherwin, Meir Shimon, Carlos Sierra, Jonathan Sievers, Precious Sikhosana, Maximiliano Silva-Feaver, Sara M. Simon, Adrian Sinclair, Praween Siritanasak, Kendrick Smith, Stephen R. Smith, David Spergel, Suzanne T. Staggs, George Stein, Jason R. Stevens, Radek Stompor, Aritoki Suzuki, Osamu Tajima, Satoru Takakura, Grant Teply, Daniel B. Thomas, Ben Thorne, Robert Thornton, Hy Trac, Calvin Tsai, Carole Tucker, Joel Ullom, Sunny Vagnozzi, Alexander van Engelen, Jeff Van Lanen, Daniel D. Van Winkle, Eve M. Vavagiakis, Clara Vergès, Michael Vissers, Kasey Wagoner, Samantha Walker, Jon Ward, Ben Westbrook, Nathan Whitehorn, Jason Williams, Joel Williams, Edward J. Wollack, Zhilei Xu, Byeonghee Yu, Cyndia Yu, Fernando Zago, Hezi Zhang, and Ningfeng Zhu

Subjects
Astrophysics, Astronomy
Abstract

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 μK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r)=0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 μK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.

Published
2019
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3. Instrumental Performance and Scientific Requirements of Polarization Modulation Unit for LiteBIRD low frequency telescope

Author

Yuki Sakurai, Tomotake Matsumura, Nobuhiko Katayama, Kunimoto Komatsu, Ryota Takaku, Shinya Sugiyama, Yurika Hoshino, Takashi Hasebe, Tommaso Ghigna, Thuong D. Hoang, Teruhito Iida, Yusuke Takase, Hirokazu Ishino, Masashi Hazumi, Hiroyuki Ohsaki, Yutaka Terao, Takemi Onoue, Satsuki Okumura, Kuniaki Konishi, Junji Yumoto, Haruyuki Sakurai, Makoto K. Gonokami, and Akito Kusaka

Published
2022

4. Effect of Stray Impedance in Frequency-Division Multiplexed Readout of TES Sensors in POLARBEAR-2b

Author

Darcy Barron, Masashi Hazumi, L. N. Lowry, M. A. Dobbs, Joseph Seibert, Kam Arnold, Maximiliano Silva-Feaver, Oliver Jeong, Adrian T. Lee, Charles A. Hill, Jennifer Ito, John Groh, Kevin T. Crowley, Tucker Elleflot, S. Takakura, L. Howe, Masaya Hasegawa, Praween Siritanasak, Benjamin Westbrook, A. Suzuki, D. Kaneko, Christopher Raum, Brian Keating, Akito Kusaka, S. Takatori, C. Tsai, and Nobuhiko Katayama

Subjects
Physics, Frequency division multiplexed, business.industry, Cosmic microwave background, Bolometer, Condensed Matter Physics, Polarization (waves), 01 natural sciences, Multiplexing, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, law.invention, Frequency-division multiplexing, Optics, law, 0103 physical sciences, General Materials Science, Transition edge sensor, 010306 general physics, business, Electrical impedance
Abstract

POLARBEAR-2b (PB-2b) is the second of three cryogenic receivers of the Simons Array cosmic microwave background polarization experiment. PB-2b contains over 7500 transition-edge sensor (TES) bolometers cooled to 250 mK and read out using digital frequency-division multiplexing (DfMux). Stray impedance in the DfMux circuit obscures TES characterization and affects TES dynamic behavior. In order to accurately characterize TESs, it is necessary to account for stray impedance in the bias circuit. We define a stray impedance model, and we describe the technique used to measure model parameters in situ and to remove their effects on TES characterization. We use the same model to predict TES dynamic behavior and show good agreement between data and the model.

Published
2020

5. Design of a Testbed for the Study of System Interference in Space CMB Polarimetry

Author

Tomotake Matsumura, Yuki Sakurai, T. Ghigna, Masashi Hazumi, Benjamin Westbrook, Nobuhiko Katayama, Aritoki Suzuki, S. Stever, and Adrian T. Lee

Subjects
Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Cosmic microwave background, Polarimetry, FOS: Physical sciences, 01 natural sciences, 010305 fluids & plasmas, law.invention, Telescope, EMI, law, 0103 physical sciences, General Materials Science, Aerospace engineering, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, business.industry, Testbed, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract

LiteBIRD is a proposed JAXA satellite mission to measure the CMB B-mode polarization with unprecedented sensitivity ($\sigma_r\sim 0.001$). To achieve this goal, $4676$ state-of-the-art TES bolometers will observe the whole sky for 3 years from L2. These detectors, as well as the SQUID readout, are extremely susceptible to EMI and other instrumental disturbances e.g. static magnetic field and vibration. As a result, careful analysis of the interference between the detector system and the rest of the telescope instruments is essential. This study is particularly important during the early phase of the project, in order to address potential problems before the final assembly of the whole instrument. We report our plan for the preparation of a cryogenic testbed to study the interaction between the detectors and other subsystems, especially a polarization modulator unit consisting of a magnetically-rotating half wave plate. We also present the requirements, current status and preliminary results., Comment: 7 pages, 4 figures, 2 tables, submitted to the Journal of Low Temperature Physics: LTD18 Special Edition

Published
2020

6. Evaluation of the effect of gravity on the rotational loss of superconducting magnetic bearings for space applications

Author

Satsuki Okumura, Takemi Onoue, Doa Ahmad, Yutaka Terao, Hiroyuki Ohsaki, Yuki Sakurai, Tomotake Matsumura, and Nobuhiko Katayama

Subjects
History, Computer Science Applications, Education
Abstract

We study the relationship between the levitation gap change and losses in a superconducting magnetic bearing (SMB) system. We develop a polarization modulator bearing for a cosmic microwave background (CMB) polarization experiment. The heat generated by the polarization modulator needs to be kept very low. Therefore, it is essential to model the effect of the levitation gap change of a rotor due to gravity on the rotational loss. We have constructed a prototype small experimental platform of an axial-flux SMB with an array of high-temperature superconductors, YBCO, and a permanent magnet ring. In this system, the weight of the rotor can be set. We measured the effect of the change in the levitation gap of the rotor due to gravity on the loss. When the levitation force was 5.5 N and 16.0 N, the losses generated in the rotor were 9.1 × 10−3 W and 1.6 × 10−2 W, respectively. It was confirmed that the loss increases with the increase in the levitation force of the SMB.

Published
2022

7. Simons Observatory Small Aperture Telescope overview

Author

Heather McCarrick, Osamu Tajima, Yuji Chinone, Jon E. Gudmundsson, Nicholas Galitzki, Federico Nati, Gabriele Coppi, Andrew Bazako, Joseph Seibert, Kevin D. Crowley, Jason E. Austermann, Masaya Hasegawa, Grant Teply, Jacob Spisak, Tran Tsan, Bradley R. Johnson, Edward J. Wollack, Giulio Fabbian, Brian Keating, Simon Dicker, Mario Zannoni, Mayuri Sathyanarayana Rao, Yume Nishinomiya, Frederick Matsuda, Kam Arnold, Shunsuke Adachi, Ningfeng Zhu, Charles A. Hill, James A. Beall, Tomoki Terasaki, D. Kaneko, Akito Kusaka, Kevin T. Crowley, Bradley Dober, Samantha Walker, Lyman A. Page, Adrian T. Lee, Kenji Kiuchi, Kathleen Harrington, Shuay-Pwu Patty Ho, Nobuhiko Katayama, Makoto Hattori, Peter Ashton, Johannes Hubmayr, Joseph E. Golec, Kana Sakaguri, Masaaki Murata, Shannon M. Duff, Kyohei Yamada, Zhilei Xu, Yuki Sakurai, Jack Lashner, Christian L. Reichardt, Aamir Ali, Marshall, HK, Spyromilio, J, Usuda, T, Kiuchi, K, Adachi, S, Ali, A, Arnold, K, Ashton, P, Austermann, J, Bazako, A, Beall, J, Chinone, Y, Coppi, G, Crowley, K, Dicker, S, Dober, B, Duff, S, Fabbian, G, Galitzki, N, Golec, J, Gudmundsson, J, Harrington, K, Hasegawa, M, Hattori, M, Hill, C, Ho, S, Hubmayr, J, Johnson, B, Kaneko, D, Katayama, N, Keating, B, Kusaka, A, Lashner, J, Lee, A, Matsuda, F, Mccarrick, H, Murata, M, Nati, F, Nishinomiya, Y, Page, L, Rao, M, Reichardt, C, Sakaguri, K, Sakurai, Y, Sibert, J, Spisak, J, Tajima, O, Teply, G, Terasaki, T, Tsan, T, Walker, S, Wollack, E, Xu, Z, Yamada, K, Zannoni, M, and Zhu, N

Subjects
Aperture, Cosmic microwave background, FOS: Physical sciences, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, law.invention, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, law, Observatory, Cosmic Microwave Background, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, business.industry, Gravitational wave, Stray light, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Radio, Primordial gravitational wave, B-mode, Ground-Based Telescope, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Simons Observatory (SO) is a cosmic microwave background (CMB) experiment from the Atacama Desert in Chile comprising three small-aperture telescopes (SATs) and one large-aperture telescope (LAT). 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. In this work, we focus on the SATs which are optimized to search for primordial gravitational waves that are detected as parity-odd polarization patterns called a B-modes on degree scales in the CMB. Each SAT employs a single optics tube with TES arrays operating at 100 mK. The high throughput optics system has a 42 cm aperture and a 35-degree field of view coupled to a 36 cm diameter focal plane. The optics consist of three metamaterial anti-re ection coated silicon lenses. Cryogenic ring baffles with engineered blackbody absorbers are installed in the optics tube to minimize the stray light. The entire optics tube is cooled to 1 K. A cryogenic continuously rotating half-wave plate near the sky side of the aperture stop helps to minimize the effect of atmospheric uctuations. The telescope warm baffling consists of a forebaffle, an elevation stage mounted co-moving shield, and a fixed ground shield that together control the far side-lobes and mitigates ground-synchronous systematics. We present the status of the SAT development., Comment: 8 pages, 6 figures

Published
2021
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8. Design of a frequency-independent optic axis Pancharatnam-based achromatic half-wave plate

Author

K. Komatsu, Yuki Sakurai, Hirokazu Ishino, Nobuhiko Katayama, and Tomotake Matsumura

Subjects
Physics, Brewster's angle, business.industry, Mechanical Engineering, Bandwidth (signal processing), Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Polarization (waves), Waveplate, Electronic, Optical and Magnetic Materials, law.invention, Optical axis, symbols.namesake, Optics, Space and Planetary Science, Control and Systems Engineering, Achromatic lens, law, symbols, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation, Refractive index, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Pancharatnam-based achromatic half-wave plates (AHWP) achieve high polarization efficiency over a broad waveband. These AWHPs generally contain a property whereby the optic axis is dependent on the electromagnetic frequency of the incident radiation. When the AHWP is used to measure 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 the shape of the source spectrum and detection band. To mitigate this problem, we propose new designs of the AHWP which eliminate the frequency dependence of the optic axis over the bandwidth whilst maintaining high modulation efficiency. We carried out this optimization by tuning the relative angles among the individual half-wave plates of the five and nine layer AHWPs. The optimized set of relative angles achieves a frequency-independent optic axis over the fractional bandwidth, a bandwidth over which polarization efficiency is greater than 0.9, of 1.3 and 1.5 for the five and nine layer AHWPs, respectively. We also study the susceptibility of the alignment accuracy on the polarization efficiency and the frequency dependence of the optic axis, which provides a design guidance for each application., Comment: 14 pages, 6 figures, Journal Astronomical Telescopes, Instruments, and Systems, accepted

Published
2021
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9. Mechanical strength and millimeter-wave transmittance spectrum of stacked sapphire plates bonded by sodium silicate solution

Author

Takayuki Toda, Yuki Sakurai, Hirokazu Ishino, Tomotake Matsumura, Kunimoto Komatsu, and Nobuhiko Katayama

Subjects
Physics - Instrumentation and Detectors, Space and Planetary Science, Control and Systems Engineering, Mechanical Engineering, FOS: Physical sciences, Astronomy and Astrophysics, Instrumentation and Detectors (physics.ins-det), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Electronic, Optical and Magnetic Materials
Abstract

The polarization modulator unit for the low-frequency telescope in LiteBIRD employs an achromatic half-wave plate (AHWP). It consists of five layers of a-cut sapphire plate, which are stacked based on a Pancharatnam recipe. In this way, the retardance of the AHWP is a half-wave over a bandwidth of 34-161 GHz. The diameter of a single sapphire plate is about 500 mm and the thickness is 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 five layers are glued together and mechanically treated as one disk. We report our investigation using a sodium silicate solution that can bond the sapphire plates. This technique has been previously investigated as a candidate of cryogenic bonding for a mirror material, including sapphire, of the gravitational wave experiments: LIGO, VIRGO, and KAGRA. We experimentally studied the mechanical strength of the bonded interface for two different surface conditions: polished and unpolished. We demonstrated that the tensile and shear strength > 20 MPa for samples with a polished surface. This satisfied the requirement of 5.5 MPa derived from the mechanical simulation assuming a launch load of 30G. We identified that samples glued on a polished surface exhibit higher strength than unpolished ones by a factor of 2 for tensile and 18 for shear strength. We measured the millimeter-wave transmittance between 90 and 140 GHz using sapphire plates with a diameter of 50 mm before and after bonding. We did not find any optical effects caused by the bonded interface within 2% error in transmittance, which originates from the measurement system., 24 pages,10 figures

Published
2021
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10. Demonstration of five-layer phase-flat achromatic half-wave plate with anti-reflective structures and superconducting magnetic bearing for CMB polarization experiments

Author

Hirokazu Kataza, Haruyuki Sakurai, K. Komatsu, Junji Yumoto, Makoto Kuwata-Gonokami, Hirokazu Ishino, Nobuhiko Katayama, Kuniaki Konishi, Tomotake Matsumura, Yuki Sakurai, Ryota Takaku, and Shinya Sugiyama

Subjects
Cryostat, Physics, 3D optical data storage, Physics::Instrumentation and Detectors, business.industry, Cosmic microwave background, Polarization (waves), Waveplate, law.invention, Telescope, Optics, Achromatic lens, law, Extremely high frequency, business
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.

Published
2020

11. Demonstration of anti-reflective structures over a large area for CMB polarization experiments

Author

Y. Hoshino, Tomotake Matsumura, Kazuhisa Mitsuda, Haruyuki Sakurai, Hirokazu Ishino, Nobuhiko Katayama, Kuniaki Konishi, Karl Young, Junji Yumoto, Shaul Hanany, Qi Wen, Hiroaki Imada, Yuki Sakurai, Noriko Y. Yamasaki, Makoto Gonokami, Ryota Takaku, and K. Komatsu

Subjects
Materials science, Fabrication, Laser ablation, Silicon, business.industry, High-refractive-index polymer, chemistry.chemical_element, Polarization (waves), Optics, Thermal conductivity, chemistry, Sapphire, Millimeter, business
Abstract

Sapphire, alumina, and silicon present the following characteristics that make them suitable as optical elements for millimeter and sub-millimeter applications: low-loss, high thermal conductivity at cryogenic temperatures, and high refractive index ~3. However, the high index also leads to high reflection. We developed a technique to machine sub-wavelength structures (SWS) as a broadband anti-reflection coating on these materials through laser ablation. We describe here the status of our development: transmission measurements of fabricated samples in a diameter of 34.5 mm agree with predictions, and we are now focusing on increasing the fabrication area with high processing rate. This is motivated by the need of ~500 mm diameter optical elements for the next-generation cosmic microwave background polarization experiments. We show our large area machining method on the alumina and sapphire over an area of < 5200 mm2 with the processing rate of < 4:0 mm3=min:, and the transmission measurements are consistent with the predictions.

Published
2020

12. Design and demonstration of the frequency independent fast axis of the Pancharatnam base multi-layer half-wave plate for CMB polarization experiment

Author

Yuki Sakurai, Hirokazu Ishino, Nobuhiko Katayama, Ryota Takaku, Tomotake Matsumura, and K. Komatsu

Subjects
Physics, Spectral shape analysis, Brewster's angle, business.industry, Bandwidth (signal processing), Polarization (waves), Waveplate, law.invention, Optical axis, symbols.namesake, Optics, Achromatic lens, law, Broadband, symbols, business
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.

Published
2020

13. Mechanical strength and millimeter-wave transmission spectrum of stacked sapphire plates bonded by sodium silicate solution

Author

Tomotake Matsumura, Yuki Sakurai, T. Toda, Hirokazu Ishino, Nobuhiko Katayama, and K. Komatsu

Subjects
chemistry.chemical_compound, Materials science, Gravitational-wave observatory, chemistry, Ultimate tensile strength, Extremely high frequency, Transmittance, Sapphire, Sodium silicate, KAGRA, Composite material, Polarization (waves)
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.

Published
2020

14. Evaluation of reconstructed angular error of a continuous rotating HWP for LiteBIRD

Author

Ryota Takaku, Yuki Sakurai, Yukikatsu Terada, Satoru Katsuda, Tomotake Matsumura, Y. Hoshino, Makoto Tashiro, S. Takakura, Shinya Sugiyama, Nobuhiko Katayama, Kosuke Sato, and K. Komatsu

Subjects
Rotary encoder, Physics, Brewster's angle, business.industry, Cosmic microwave background, Breadboard, Position angle, Polarization (waves), law.invention, Telescope, symbols.namesake, Optics, law, symbols, business, Encoder
Abstract

We report the development of an optical encoder and its readout system for a cryogenically-cooled continuously rotating half-wave plate (HWP) polarization modulator unit (PMU) in the LiteBIRD low-frequency telescope. LiteBIRD is a cosmic microwave background polarization satellite mission to probe B-mode polarization, which originates from primordial gravitational waves, observing from the second Lagrange point (L2). LiteBIRD employs a continuously-rotating HWP to mitigate systematic effects. The knowledge of the position angle of the HWP is in a one-to-one relationship to the incident polarization angle. The required reconstruction accuracy is about 1 arcmin and the targeted rotational frequency stability is 1 mHz. A unique development constraint comes from a telemetry bandwidth limitation between the Earth and L2, and thus we implement a digital process to reduce the data volume assuming a future implementation of on-board processing of the encoder data before the downlink. The demonstrations were done experimentally using a breadboard model of the PMU: a readout system using FPGA (Spartan-6) and a rotational mechanism using a superconducting magnetic bearing and AC motor. We acquired the encoder data from the rotational mechanism operating under two conditions: liquid nitrogen at room pressure and below 10 K in a cryostat. We demonstrated the reconstruction of the position angle accuracy < 0.5 arcmin and the corresponding data volume of 0.12 GB/day, which is at least an order of magnitude smaller than the total data volume per day. We further discuss the sources of the position angle uncertainty and its implications to the observations.

Published
2020

15. Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission

Author

Ludovic Montier, Baptiste Mot, Paolo de Bernardis, Bruno Maffei, Giampaolo Pisano, Fabio Columbro, Jon E. Gudmundsson, Sophie Henrot-Versillé, Luca Lamagna, Joshua Montgomery, Thomas Prouvé, Megan Russell, Giorgio Savini, Samantha Stever, Keith L. Thompson, Masahiro Tsujimoto, Carole Tucker, Benjamin Westbrook, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, Ranajoy Banerji, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Masashi Hazumi, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Gianluca Morgante, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Gianluca Polenta, Davide Poletti, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), LiteBIRD, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, European Research Council, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Lystrup, Makenzie, Montier, L, Mot, B, de Bernardis, P, Maffei, B, Pisano, G, Columbro, F, Gudmundsson, J, Henrot-Versillé, S, Lamagna, L, Montgomery, J, Prouvé, T, Russell, M, Savini, G, Stever, S, Thompson, K, Tsujimoto, M, Tucker, C, Westbrook, B, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banerji, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Hazumi, M, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Morgante, G, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Polenta, G, Poletti, D, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, Zonca, A, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)

Subjects
cosmological model, experimental methods, detector: satellite, Cosmic microwave background, cosmic background radiation: polarization, detector: noise, magnetic field, 02 engineering and technology, LiteBIRD, cosmic microwave background, polarization measurements, space telescopes, 7. Clean energy, 01 natural sciences, law.invention, law, detector: calibration, media_common, Physics, conductivity: thermal, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, Polarization (waves), inflation: model, experimental equipment, B-mode, cosmic radiation, cryogenics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, cosmic background radiation: detector, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), lens, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, LiteBIRD, Polarization measurements, Space telescopes, Astrophysics::Cosmology and Extragalactic Astrophysics, bolometer: superconductivity, frequency: high, Radio spectrum, tensor scalar: ratio, 010309 optics, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: angular resolution, Astrophysics::Galaxy Astrophysics, Gravitational wave, synchrotron radiation, gravitational radiation: primordial, Astronomy, Physics::History of Physics, optics, detector: sensitivity, 13. Climate action, Sky, Satellite, temperature: stability, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy. European collaborators acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement Nos. 772253, 819478, and 849169). The European Space Agency (ESA) has led a Concurrent Design Facility study, focused on the MHFT and Sub-Kelvin coolers, and funded Technology Research Programmes for “Large radii Half-Wave Plate (HWP) development” (contract number: 4000123266/18/NL/AF) and for the ‘Development of Large Anti-Reflection Coated Lenses for Passive (Sub)Millimeter-Wave Science Instruments” (contract number: 4000128517/19/NL/AS).

Published
2020

16. LiteBIRD: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization

Author

Masashi Hazumi, Peter A. Ade, Alexandre Adler, Erwan Allys, Kam Arnold, Didier Auguste, Jonathan Aumont, Ragnhild Aurlien, Jason Austermann, Carlo Baccigalupi, Anthony J. Banday, R. Banjeri, Rita B. Barreiro, Soumen Basak, Jim Beall, Dominic Beck, Shawn Beckman, Juan Bermejo, Paolo de Bernardis, Marco Bersanelli, Julien Bonis, Julian Borrill, Francois Boulanger, Sophie Bounissou, Maksym Brilenkov, Michael Brown, Martin Bucher, Erminia Calabrese, Paolo Campeti, Alessandro Carones, Francisco J. Casas, Anthony Challinor, Victor Chan, Kolen Cheung, Yuji Chinone, Jean F. Cliche, Loris Colombo, Fabio Columbro, Javier Cubas, Ari Cukierman, David Curtis, Giuseppe D'Alessandro, Nadia Dachlythra, Marco De Petris, Clive Dickinson, Patricia Diego-Palazuelos, Matt Dobbs, Tadayasu Dotani, Lionel Duband, Shannon Duff, Jean M. Duval, Ken Ebisawa, Tucker Elleflot, Hans K. Eriksen, Josquin Errard, Thomas Essinger-Hileman, Fabio Finelli, Raphael Flauger, Cristian Franceschet, Unni Fuskeland, Mathew Galloway, Ken Ganga, Jian R. Gao, Ricardo Genova-Santos, Martina Gerbino, Massimo Gervasi, Tommaso Ghigna, Eirik Gjerløw, Marcin L. Gradziel, Julien Grain, Frank Grupp, Alessandro Gruppuso, Jon E. Gudmundsson, Tijmen de Haan, Nils W. Halverson, Peter Hargrave, Takashi Hasebe, Masaya Hasegawa, Makoto Hattori, Sophie Henrot-Versillé, Daniel Herman, Diego Herranz, Charles A. Hill, Gene Hilton, Yukimasa Hirota, Eric Hivon, Renee A. Hlozek, Yurika Hoshino, Elena de la Hoz, Johannes Hubmayr, Kiyotomo Ichiki, Teruhito Iida, Hiroaki Imada, Kosei Ishimura, Hirokazu Ishino, Greg Jaehnig, Tooru Kaga, Shingo Kashima, Nobuhiko Katayama, Akihiro Kato, Takeo Kawasaki, Reijo Keskitalo, Theodore Kisner, Yohei Kobayashi, Nozomu Kogiso, Alan Kogut, Kazunori Kohri, Eiichiro Komatsu, Kunimoto Komatsu, Kuniaki Konishi, Nicoletta Krachmalnicoff, Ingo Kreykenbohm, Chao-Lin L. Kuo, Akihiro Kushino, Luca Lamagna, Jeff V. Lanen, Massimiliano Lattanzi, Adrian T. Lee, Clément Leloup, François Levrier, Eric Linder, Thibaut Louis, Gemma Luzzi, Thierry Maciaszek, Bruno Maffei, Davide Maino, Muneyoshi Maki, Stefano Mandelli, Enrique Martinez-Gonzalez, Silvia Masi, Tomotake Matsumura, Aniello Mennella, Marina Migliaccio, Yuto Minami, Kazuhisa Mitsuda, Joshua Montgomery, Ludovic Montier, Gianluca Morgante, Baptiste Mot, Yasuhiro Murata, John A. Murphy, Makoto Nagai, Yuya Nagano, Taketo Nagasaki, Ryo Nagata, Shogo Nakamura, Toshiya Namikawa, Paolo Natoli, Simran Nerval, Toshiyuki Nishibori, Haruki Nishino, Fabio Noviello, Créidhe O'Sullivan, Hideo Ogawa, Hiroyuki Ogawa, Shugo Oguri, Hiroyuki Ohsaki, Izumi S. Ohta, Norio Okada, Nozomi Okada, Luca Pagano, Alessandro Paiella, Daniela Paoletti, Guillaume Patanchon, Julien Peloton, Francesco Piacentini, Giampaolo Pisano, Gianluca Polenta, Davide Poletti, Thomas Prouvé, Giuseppe Puglisi, Damien Rambaud, Christopher Raum, Sabrina Realini, Martin Reinecke, Mathieu Remazeilles, Alessia Ritacco, Gilles Roudil, Jose A. Rubino-Martin, Megan Russell, Haruyuki Sakurai, Yuki Sakurai, Maura Sandri, Manami Sasaki, Giorgio Savini, Douglas Scott, Joseph Seibert, Yutaro Sekimoto, Blake Sherwin, Keisuke Shinozaki, Maresuke Shiraishi, Peter Shirron, Giovanni Signorelli, Graeme Smecher, Samantha Stever, Radek Stompor, Hajime Sugai, Shinya Sugiyama, Aritoki Suzuki, Junichi Suzuki, Trygve L. Svalheim, Eric Switzer, Ryota Takaku, Hayato Takakura, Satoru Takakura, Yusuke Takase, Youichi Takeda, Andrea Tartari, Ellen Taylor, Yutaka Terao, Harald Thommesen, Keith L. Thompson, Ben Thorne, Takayuki Toda, Maurizio Tomasi, Mayu Tominaga, Neil Trappe, Matthieu Tristram, Masatoshi Tsuji, Masahiro Tsujimoto, Carole Tucker, Joe Ullom, Gerard Vermeulen, Patricio Vielva, Fabrizio Villa, Michael Vissers, Nicola Vittorio, Ingunn Wehus, Jochen Weller, Benjamin Westbrook, Joern Wilms, Berend Winter, Edward J. Wollack, Noriko Y. Yamasaki, Tetsuya Yoshida, Junji Yumoto, Mario Zannoni, Andrea Zonca, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LiteBIRD, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Hélium : du fondamental aux applications (NEEL - HELFA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Lystrup, Makenzie, Hazumi, M, Ade, P, Adler, A, Allys, E, Arnold, K, Auguste, D, Aumont, J, Aurlien, R, Austermann, J, Baccigalupi, C, Banday, A, Banjeri, R, Barreiro, R, Basak, S, Beall, J, Beck, D, Beckman, S, Bermejo, J, de Bernardis, P, Bersanelli, M, Bonis, J, Borrill, J, Boulanger, F, Bounissou, S, Brilenkov, M, Brown, M, Bucher, M, Calabrese, E, Campeti, P, Carones, A, Casas, F, Challinor, A, Chan, V, Cheung, K, Chinone, Y, Cliche, J, Colombo, L, Columbro, F, Cubas, J, Cukierman, A, Curtis, D, D'Alessandro, G, Dachlythra, N, De Petris, M, Dickinson, C, Diego-Palazuelos, P, Dobbs, M, Dotani, T, Duband, L, Duff, S, Duval, J, Ebisawa, K, Elleflot, T, Eriksen, H, Errard, J, Essinger-Hileman, T, Finelli, F, Flauger, R, Franceschet, C, Fuskeland, U, Galloway, M, Ganga, K, Gao, J, Genova-Santos, R, Gerbino, M, Gervasi, M, Ghigna, T, Gjerløw, E, Gradziel, M, Grain, J, Grupp, F, Gruppuso, A, Gudmundsson, J, de Haan, T, Halverson, N, Hargrave, P, Hasebe, T, Hasegawa, M, Hattori, M, Henrot-Versillé, S, Herman, D, Herranz, D, Hill, C, Hilton, G, Hirota, Y, Hivon, E, Hlozek, R, Hoshino, Y, de la Hoz, E, Hubmayr, J, Ichiki, K, Iida, T, Imada, H, Ishimura, K, Ishino, H, Jaehnig, G, Kaga, T, Kashima, S, Katayama, N, Kato, A, Kawasaki, T, Keskitalo, R, Kisner, T, Kobayashi, Y, Kogiso, N, Kogut, A, Kohri, K, Komatsu, E, Komatsu, K, Konishi, K, Krachmalnicoff, N, Kreykenbohm, I, Kuo, C, Kushino, A, Lamagna, L, Lanen, J, Lattanzi, M, Lee, A, Leloup, C, Levrier, F, Linder, E, Louis, T, Luzzi, G, Maciaszek, T, Maffei, B, Maino, D, Maki, M, Mandelli, S, Martinez-Gonzalez, E, Masi, S, Matsumura, T, Mennella, A, Migliaccio, M, Minami, Y, Mitsuda, K, Montgomery, J, Montier, L, Morgante, G, Mot, B, Murata, Y, Murphy, J, Nagai, M, Nagano, Y, Nagasaki, T, Nagata, R, Nakamura, S, Namikawa, T, Natoli, P, Nerval, S, Nishibori, T, Nishino, H, Noviello, F, O'Sullivan, C, Ogawa, H, Oguri, S, Ohsaki, H, Ohta, I, Okada, N, Pagano, L, Paiella, A, Paoletti, D, Patanchon, G, Peloton, J, Piacentini, F, Pisano, G, Polenta, G, Poletti, D, Prouvé, T, Puglisi, G, Rambaud, D, Raum, C, Realini, S, Reinecke, M, Remazeilles, M, Ritacco, A, Roudil, G, Rubino-Martin, J, Russell, M, Sakurai, H, Sakurai, Y, Sandri, M, Sasaki, M, Savini, G, Scott, D, Seibert, J, Sekimoto, Y, Sherwin, B, Shinozaki, K, Shiraishi, M, Shirron, P, Signorelli, G, Smecher, G, Stever, S, Stompor, R, Sugai, H, Sugiyama, S, Suzuki, A, Suzuki, J, Svalheim, T, Switzer, E, Takaku, R, Takakura, H, Takakura, S, Takase, Y, Takeda, Y, Tartari, A, Taylor, E, Terao, Y, Thommesen, H, Thompson, K, Thorne, B, Toda, T, Tomasi, M, Tominaga, M, Trappe, N, Tristram, M, Tsuji, M, Tsujimoto, M, Tucker, C, Ullom, J, Vermeulen, G, Vielva, P, Villa, F, Vissers, M, Vittorio, N, Wehus, I, Weller, J, Westbrook, B, Wilms, J, Winter, B, Wollack, E, Yamasaki, N, Yoshida, T, Yumoto, J, Zannoni, M, and Zonca, A

Subjects
cosmological model, experimental methods, detector: satellite, Physics beyond the Standard Model, Cosmic microwave background, LiteBIRD, cosmic inflation, cosmic microwave background, B-mode polarization, primordial gravi- tational waves, quantum gravity, space telescope, cosmic background radiation: polarization, detector: noise, 02 engineering and technology, 7. Clean energy, 01 natural sciences, expansion: multipole, Cosmology, General Relativity and Quantum Cosmology, B-mode: primordial, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), general relativity, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], B-mode polarization, media_common, Physics, new physics, quantum mechanics, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, BICEP, inflation: model, High Energy Physics - Phenomenology, error: statistical, experimental equipment, cryogenics, power spectrum: angular dependence, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], readout, Astrophysics::Earth and Planetary Astrophysics, dust, control system, 0210 nano-technology, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, cosmic inflation, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, primordial gravi- tational waves, Cosmic background radiation, space telescope, Lagrangian point, FOS: Physical sciences, LiteBIRD, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, polarization: sensitivity, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ionization, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic background radiation: power spectrum, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Inflation (cosmology), synchrotron radiation, primordial gravitational waves, gravitational radiation: primordial, Astronomy, calibration, Physics::History of Physics, recombination, detector: sensitivity, angular resolution, Sky, quantum gravity, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Satellite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], experimental results
Abstract

Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online.-- et al., LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA’s H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 µK-arcmin with a typical angular resolution of 0.5◦ at 100 GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes., This work is supported in Japan by ISAS/JAXA for Pre-Phase A2 studies, by the acceleration program of JAXA research and development directorate, by the World Premier International Research Center Initiative (WPI) of MEXT, by the JSPS Core-to-Core Program of A. Advanced Research Networks, and by JSPS KAKENHI Grant Numbers JP15H05891, JP17H01115, and JP17H01125. The Italian LiteBIRD phase A contribution is supported by the Italian Space Agency (ASI Grants No. 2020-9-HH.0 and 2016-24-H.1-2018), the National Institute for Nuclear Physics (INFN) and the National Institute for Astrophysics (INAF). The French LiteBIRD phase A contribution is supported by the Centre National d’Etudes Spatiale (CNES), by the Centre National de la Recherche Scientifique (CNRS), and by the Commissariat a l’Energie Atomique (CEA). The Canadian contribution is supported by the Canadian Space Agency. The US contribution is supported by NASA grant no. 80NSSC18K0132. Norwegian participation in LiteBIRD is supported by the Research Council of Norway (Grant No. 263011). The Spanish LiteBIRD phase A contribution is supported by the Spanish Agencia Estatal de Investigacion (AEI), project refs. PID2019-110610RB-C21 and AYA2017-84185-P. Funds that support the Swedish contributions come from the Swedish National Space Agency (SNSA/Rymdstyrelsen) and the Swedish Research Council (Reg. no. 2019-03959). The German participation in LiteBIRD is supported in part by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy (Grant No. EXC-2094 - 390783311). This research used resources of the Central Computing System owned and operated by the Computing Research Center at KEK, as well as resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy.

Published
2020

17. Breadboard model of polarization modulator unit based on a continuously rotating half-wave plate for the low-frequency telescope of the LiteBIRD space mission

Author

H. Enokida, Masashi Hazumi, Junji Yumoto, Doa Ahmad, T. Toda, K. Komatsu, Charles Hill, Hiroaki Imada, Yutaka Terao, Hiroyuki Ohsaki, Yosuke Iwata, Haruyuki Sakurai, Tomotake Matsumura, Hajime Sugai, Hirokazu Ishino, Nobuhiko Katayama, Kuniaki Konishi, Makoto Kuwata-Gonokami, Akito Kusaka, Yuki Sakurai, Yusuke Ishida, Shinya Sugiyama, T. Iida, Yoshiki Nomura, Ryota Takaku, and T. Ghigna

Subjects
Physics, business.industry, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Low frequency, Breadboard, Polarization (waves), Waveplate, law.invention, Telescope, Optics, Computer Science::Systems and Control, Achromatic lens, law, Broadband, business
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.

Published
2020

18. A minimal power-spectrum-based moment expansion for CMB B-mode searches

Author

T. Matsumura, S. Azzoni, David Alonso, Maximilian H. Abitbol, A. Gough, and Nobuhiko Katayama

Subjects
Physics, Spectral index, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Computer Science::Information Retrieval, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Upper and lower bounds, Small set, Standard deviation, 0103 physical sciences, Statistical physics, Decorrelation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The characterization and modeling of polarized foregrounds has become a critical issue in the quest for primordial B-modes. A typical method to proceed is to factorize and parametrize the spectral properties of foregrounds and their scale dependence (i.e. assuming that foreground spectra are well described everywhere by their sky average). Since in reality foreground properties vary across the Galaxy, this assumption leads to inaccuracies in the model that manifest themselves as biases in the final cosmological parameters (in this case the tensor-to-scalar ratio r). This is particularly relevant for surveys over large fractions of the sky, such as the Simons Observatory (SO), where the spectra should be modeled over a distribution of parameter values. Here we propose a method based on the existing “moment expansion” approach to address this issue in a power-spectrum-based analysis that is directly applicable in ground-based multi-frequency data. Additionally, the method uses only a small set of parameters with simple physical interpretation, minimizing the impact of foreground uncertainties on the final B-mode constraints. We validate the method using SO-like simulated observations, recovering an unbiased estimate of the tensor-to-scalar ratio r with standard deviation σ(r) ≃ 0.003, compatible with official forecasts. When applying the method to the public BICEP2/Keck data, we find an upper bound r < 0.06 (95% C.L.), compatible with the result found by BICEP2/Keck when parametrizing spectral index variations through a scale-independent frequency decorrelation parameter. We also discuss the formal similarities between the power spectrum-based moment expansion and methods used in the analysis of CMB lensing.

Published
2020

19. Broadband Anti-Reflection Moth-Eye Structures Realized in the Above 1 THz Region by Laser Processing

Author

Ryota Takaku, M. Matoba, Yuki Sakurai, Haruyuki Sakurai, Nobuhiko Katayama, Kuniaki Konishi, Tomotake Matsumura, Junji Yumoto, and Makoto Kuwata-Gonokami

Subjects
Fabrication, Materials science, Silicon, Terahertz radiation, business.industry, chemistry.chemical_element, Laser, law.invention, chemistry, law, Broadband, Femtosecond, Reflection (physics), Optoelectronics, business, Laser processing
Abstract

We fabricate terahertz (THz) moth-eye antireflection (AR) structures on the surface of high-resistivity silicon via low-power femtosecond laser processing. We observed broadband AR performance at near-unity above 0.8 THz, where the upper value was measurement limited. Such values are unprecedented for laser fabricated samples, and shows the high potential of laser processing-based approaches for THz optics fabrication.

Published
2020

20. Broadband, millimeter-wave anti-reflective structures on sapphire ablated with femto-second laser

Author

Ryota Takaku, Kazuhisa Mitsuda, Haruyuki Sakurai, Noriko Y. Yamasaki, Tomotake Matsumura, Makoto Kuwata-Gonokami, Junji Yumoto, K. Komatsu, Shaul Hanany, Karl Young, Hirokazu Ishino, Nobuhiko Katayama, Kuniaki Konishi, Qi Wen, Yuki Sakurai, and H. Imada

Subjects
Materials science, medicine.medical_treatment, FOS: Physical sciences, General Physics and Astronomy, 02 engineering and technology, engineering.material, 01 natural sciences, law.invention, Optics, Coating, law, 0103 physical sciences, Broadband, medicine, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010302 applied physics, Laser ablation, business.industry, 021001 nanoscience & nanotechnology, Ablation, Polarization (waves), Laser, Extremely high frequency, engineering, Sapphire, 0210 nano-technology, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We designed, fabricated, and measured anti-reflection coating (ARC) on sapphire that has 116% fractional bandwidth and transmission of at least 97% in the millimeter wave band. The ARC was based on patterning pyramid-like sub-wavelength structures (SWS) using ablation with a 15 W femto-second laser operating at 1030 nm. One side of each of two discs was fabricated with SWS that had a pitch of 0.54 mm and height of 2 mm. The average ablation volume removal rate was 1.6 mm$^{3}$/min. Measurements of the two-disc sandwich show transmission higher than 97% between 43 and 161 GHz. We characterize instrumental polarization (IP) arising from differential transmission due to asymmetric SWS. We find that with proper alignment of the two disc sandwich RMS IP across the band is predicted to be 0.07% at normal incidence, and less than 0.6% at incidence angles up to 20 degrees. These results indicate that laser ablation of SWS on sapphire and on other hard materials such as alumina is an effective way to fabricate broad-band ARC.

Published
2020

21. Fourier Power Function Shapelets (FPFS) shear estimator: performance on image simulations

Author

Surhud More, Masamune Oguri, Xiangchong Li, and Nobuhiko Katayama

Subjects
Physics, Point spread function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Iterative method, Multiplicative function, Mathematical analysis, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Estimator, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Amplitude, Fourier transform, Space and Planetary Science, Frequency domain, 0103 physical sciences, symbols, Power function, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We reinterpret the shear estimator developed by Zhang & Komatsu (2011) within the framework of Shapelets and propose the Fourier Power Function Shapelets (FPFS) shear estimator. Four shapelet modes are calculated from the power function of every galaxy's Fourier transform after deconvolving the Point Spread Function (PSF) in Fourier space. We propose a novel normalization scheme to construct dimensionless ellipticity and its corresponding shear responsivity using these shapelet modes. Shear is measured in a conventional way by averaging the ellipticities and responsivities over a large ensemble of galaxies. With the introduction and tuning of a weighting parameter, noise bias is reduced below one percent of the shear signal. We also provide an iterative method to reduce selection bias. The FPFS estimator is developed without any assumption on galaxy morphology, nor any approximation for PSF correction. Moreover, our method does not rely on heavy image manipulations nor complicated statistical procedures. We test the FPFS shear estimator using several HSC-like image simulations and the main results are listed as follows. (i) For simulations which only contain isolated galaxies, the amplitude of multiplicative bias is below 1 % . (ii) For more realistic simulations which also contain blended galaxies, the blended galaxies are deblended by the first generation HSC deblender before shear measurement. Multiplicative bias of (-5.71 +- 0.31) % is found. The blending bias is calibrated by image simulations. Finally, we test the consistency and stability of this calibration., 18 pages, 3 figures, accepted by MNRAS

Published
2018

22. Large diameter millimeter-wave low-pass filter made of alumina with laser ablated anti-reflection coating

Author

Qi Wen, Mark J. Devlin, Shaul Hanany, Haruyuki Sakurai, Junji Yumoto, Makoto Kuwata-Gonokami, Ryo-hei Yamada, Simon Dicker, T. Iida, Takashi Hasebe, Norikatsu Mio, Tomotake Matsumura, Nobuhiko Katayama, Kuniaki Konishi, Scott Cray, Yuki Sakurai, and Ryota Takaku

Subjects
Laser ablation, Materials science, Spatial filter, business.industry, Low-pass filter, FOS: Physical sciences, Optical power, Laser, Atomic and Molecular Physics, and Optics, law.invention, Optics, law, Filter (video), Extremely high frequency, Transmittance, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We fabricated a 302 mm diameter low-pass filter made of alumina that has an anti-reflection coating (ARC) made with laser-ablated sub-wavelength structures (SWS). The filter has been integrated into and is operating with the MUSTANG2 instrument, which is coupled to the Green Bank Telescope. The average transmittance of the filter in the MUSTANG2 operating band between 75 and 105 GHz is 98%. Reflective loss due to the ARC is 1%. The difference in transmission between the s- and p-polarization states is less than 1%. To within 1% accuracy we observe no variance in these results when transmission is measured in six independent filter spatial locations. The alumina filter replaced a prior MUSTANG2 Teflon filter. Data taken with the filter heat sunk to its nominal 40 K stage show performance consistent with expectations: a reduction of about 50% in filters-induced optical power load on the 300 mK stage, and in in-band optical loading on the detectors. It has taken less than 4 days to laser-ablate the SWS on both sides of the alumina disk. This is the first report of an alumina filter with SWS ARC deployed with an operating instrument, and the first demonstration of a large area fabrication of SWS with laser ablation., Comment: This version reflects the published version; 21 pages, 11 figures

Published
2021

24. FPFS Shear Estimator: Systematic Tests on the Hyper Suprime-Cam Survey First Year Data

Author

Wentao Luo, Masamune Oguri, Surhud More, Keigo Nakamura, Wenting Wang, Jiaxin Han, Hironao Miyatake, Xiangchong Li, and Nobuhiko Katayama

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Multiplicative function, Astrophysics::Instrumentation and Methods for Astrophysics, Estimator, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Residual, 01 natural sciences, Galaxy, symbols.namesake, Fourier transform, Space and Planetary Science, Observational cosmology, 0103 physical sciences, symbols, Power function, 010303 astronomy & astrophysics, Algorithm, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We apply the Fourier Power Function Shapelets (FPFS) shear estimator to the first year data of the Hyper Suprime-Cam survey to construct a shape catalog. The FPFS shear estimator has been demonstrated to have multiplicative bias less than $1\%$ in the absence of blending, regardless of complexities of galaxy shapes, smears of point spread functions (PSFs) and contamination from noise. The blending bias is calibrated with realistic image simulations, which include the impact of neighboring objects, using the COSMOS Hubble Space Telescope images. Here we carefully test the influence of PSF model residual on the FPFS shear estimation and the uncertainties in the shear calibration. Internal null tests are conducted to characterize potential systematics in the FPFS shape catalog and the results are compared with those measured using a catalog where the shapes were estimated using the re-Gaussianization algorithms. Furthermore, we compare various weak lensing measurements between the FPFS shape catalog and the re-Gaussianization shape catalog and conclude that the weak lensing measurements between these two shape catalogs are consistent with each other within the statistical uncertainty., 24 pages, 19 figures, accepted by ApJS

Published
2019

25. Femtosecond Laser Processing and Evaluation of Broadband THz Anti-Reflection Structures

Author

Tomotake Matsumura, Haruyuki Sakurai, Ryota Takaku, Yuki Sakurai, Natsuki Nemoto, Nobuhiko Katayama, Kuniaki Konishi, Makoto Kuwata-Gonokami, and Junji Yumoto

Subjects
Materials science, Fabrication, Silicon, Computer simulation, business.industry, Terahertz radiation, technology, industry, and agriculture, chemistry.chemical_element, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, 010309 optics, chemistry, 0103 physical sciences, Broadband, Femtosecond, Reflection (physics), Optoelectronics, 0210 nano-technology, business, Spectroscopy
Abstract

We fabricate terahertz anti-reflection structures on the surface of high-resistivity silicon via femtosecond laser processing. We measure its spectral properties by terahertz time-domain spectroscopy, and find a broadband increase in transmissivity over 0.3 - 2.5 THz. We investigate the observed spectral characteristics of this transmission by using numerical simulation. We successfully reproduce the observed result for all frequencies, including a previously undocumented high-frequency drop-off, when the model includes additional material losses. We believe these effects to be induced by the laser-ablation fabrication process.

Published
2019

26. Simultaneous determination of the cosmic birefringence and miscalibrated polarization angles from CMB experiments

Author

Nobuhiko Katayama, Eiichiro Komatsu, Tomotake Matsumura, Kiyotomo Ichiki, H. Ochi, and Yuto Minami

Subjects
Physics, Birefringence, COSMIC cancer database, 010308 nuclear & particles physics, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Computational physics, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We show that the cosmic birefringence and miscalibrated polarization angles can be determined simultaneously by cosmic microwave background (CMB) experiments using the cross-correlation between $E$- and $B$-mode polarization data. This is possible because the polarization angles of the CMB are rotated by both the cosmic birefringence and miscalibration effects, whereas those of the Galactic foreground emission are rotated only by the latter. Our method does not require prior knowledge of the $E$- and $B$-mode power spectra of the foreground emission, but uses only the knowledge of the CMB polarization spectra. Specifically, we relate the observed $EB$ correlation to the difference between the observed$E$- and $B$-mode spectra in the sky, and use different multipole dependences of the CMB (given by theory) and foreground spectra (given by data) to derive the likelihood for the miscalibration angle $\alpha$ and the birefringence angle $\beta$. We show that a future satellite mission similar to LiteBIRD can determine $\beta$ with a precision of 10 arcmin.

Published
2019

27. CMB-S4 Decadal Survey APC White Paper

Author

Shaul Hanany, Georges Obied, J. Colin Hill, Thomas Cecil, Keith L. Thompson, Adam Anderson, Michael L. Brown, Doug Johnstone, Lorenzo Moncelsi, Erminia Calabrese, Howard Hui, Haruki Nishino, Sara M. Simon, James Kerby, Theodore Kisner, K. T. Story, Moritz Münchmeyer, Aritoki Suzuki, Joseph J. Mohr, Adrian T. Lee, Bradley R. Johnson, Sanah Bhimani, W. C. Jones, A. E. Lowitz, Nathan Whitehorn, Valentine Novosad, Marcelo A. Alvarez, Anze Slosar, Kam Arnold, Kevork N. Abazajian, Mustafa A. Amin, Evan Grohs, Abigail G. Vieregg, Siavash Yasini, Mathew S. Madhavacheril, Julien Carron, Ritoban Basu Thakur, Jean-Baptiste Melin, Shawn W. Henderson, Asantha Cooray, Chris Stoughton, Peter Timbie, Matteo Bonato, Ki Won Yoon, Blakesley Burkhart, Salman Habib, T. Natoli, Jacques Delabrouille, Carlo Baccigalupi, Victor Guarino, Steven W. Allen, Kathy Bailey, Aurelien A. Fraisse, Osamu Tajima, Silvia Galli, Denis Barkats, Antony Lewis, Ari Cukierman, Johannes Hubmayr, Marilena LoVerde, Erik Shirokoff, G. P. Holder, James G. Bartlett, James Yeck, Dale Li, N. W. Halverson, Graeme E. Addison, Adam Mantz, Matthieu Tristram, Laura Newburgh, Sarah Shandera, Alessandro Schillaci, Lindsey Bleem, Raphael Flauger, Marcel Schmittfull, S. Pandey, Kent D. Irwin, N. Kurita, Gregory S. Tucker, Matthew Hasselfield, Reijo Keskitalo, Levon Pogosian, Rachel S. Somerville, C. D. Sheehy, Srini Rajagopalan, Jesse Treu, Giuseppe Puglisi, Eric J. Baxter, John M Kovac, Emmanuel Schaan, Marcel Demarteau, Akito Kusaka, Suzanne T. Staggs, Kirit Karkare, Josquin Errard, Thomas Essinger-Hileman, Anne Lähteenmäki, Mattia Negrello, Toshiya Namikawa, Zhilei Xu, Mark Halpern, Simone Ferraro, Edo Berger, François R. Bouchet, Zeeshan Ahmed, Frederick Matsuda, Joseph Eimer, Alexandra S. Rahlin, W. L. Kimmy Wu, Giulio Fabbian, Chao-Lin Kuo, Christian L. Reichardt, Marius Millea, Stephen Padin, A. T. Crites, Joel Meyers, William Edwards, R. Gualtieri, Jason W. Henning, Arthur Kosowsky, Edward J. Wollack, W. L. Holzapfel, Michael D. Niemack, John E. Carlstrom, Rachel Bean, Cora Dvorkin, Ely D. Kovetz, David Alonso, Nicholas Battaglia, Sean Bryan, Gianfranco De Zotti, Anthony Challinor, Graca Rocha, Federico Nati, Jeffrey P. Filippini, Katrin Heitmann, Eric V. Linder, Antony A. Stark, Martin Nordby, Grant Teply, Benjamin Saliwanchik, Peter Adshead, P. Daniel Meerburg, Victoria Calafut, Francis-Yan Cyr-Racine, M.E. Huffer, Chris Bebek, Lloyd Knox, Masashi Hazumi, Eleonora Di Valentino, Natalie A. Roe, Nicholas Galitzki, Masaya Hasegawa, Sarah Kernovsky, Victor Buza, Darcy Barron, C. Pryke, Tijmen de Haan, Tony Mroczkowski, Vera Gluscevic, Andrea Zonca, Daniel Green, Kimberly K. Boddy, Srinivasan Raghunathan, Jeff McMahon, J. E. Ruhl, Steve Kuhlmann, Blake D. Sherwin, Joaquin Vieira, Peter S. Barry, Daisuke Nagai, Karen Byrum, Neelima Sehgal, Murdock Gilchriese, Marco Raveri, M. Tomasi, Douglas Scott, James J. Bock, Martin White, Chang Feng, Ken Ganga, Martina Gerbino, Suvodip Mukherjee, Radek Stompor, Gensheng Wang, B. Racine, Mark Reichanadter, Paul O'Connor, Alexander van Engelen, Kevin M. Huffenberger, Maria Salatino, Kathleen Harrington, Nobuhiko Katayama, Bradford Benson, Daniel Grin, Colin A. Bischoff, Charles R. Lawrence, Mark Vogelsberger, Shannon M. Duff, Scott Watson, Sebastian Bocquet, C. Umiltà, Andrei V. Frolov, C. L. Chang, Johanna Nagy, J. Richard Bond, Philip Daniel Mauskopf, B. Flaugher, Robert R. Caldwell, Mark J. Devlin, Renée Hlozek, Anirban Roy, Elena Pierpaoli, Amy N. Bender, Bruce Partridge, E. Y. Young, Matt Dobbs, Julian Borrill, Adriaan J. Duivenvoorden, Yuji Chinone, Mathieu Remazeilles, T. M. Crawford, Jon E. Gudmundsson, Hsiao-Mei Sherry Cho, and Gunther Haller

Subjects
White paper, 010308 nuclear & particles physics, 0103 physical sciences, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Environmental science, Astrophysics::Cosmology and Extragalactic Astrophysics, Project plan, 010306 general physics, 01 natural sciences
Abstract

We provide an overview of the science case, instrument configuration and project plan for the next-generation ground-based cosmic microwave background experiment CMB-S4, for consideration by the 2020 Decadal Survey.

Published
2019

28. Deployment of Polarbear-2A

Author

Chang Feng, Radek Stompor, Takayuki Tomaru, Rolando Dünner, Josquin Errard, D. Tanabe, Praween Siritanasak, N. Stebor, Julien Carron, D. Leon, Davide Poletti, K. Cheung, C. Tsai, S. Takakura, Grant Teply, Yuto Minami, Yuki Inoue, Stephen M. Feeney, Yuji Chinone, Frederick Matsuda, D. Beck, Akito Kusaka, Y. Akiba, A. Suzuki, Nicoletta Krachmalnicoff, Adrian T. Lee, M. Aguilar Faúndez, J. Peloton, Colin Ross, Osamu Tajima, D. Boettger, B. Westbrook, A. T. P. Pham, M. Navaroli, N. W. Halverson, Y. Zhou, Federico Bianchini, A. Cukierman, Aashrita Mangu, Nobuhiko Katayama, T. Hamada, Tucker Elleflot, Y. Segawa, Masaya Hasegawa, G. Hall, Julian Borrill, Peter A. R. Ade, Eric V. Linder, Giulio Fabbian, H. Nishino, G. Jaehnig, Giuseppe Puglisi, Charles A. Hill, Shunsuke Adachi, S. Takatori, L. Howe, A. J. Gilbert, H. El-Bouhargani, Christian L. Reichardt, Kam Arnold, John Groh, Masashi Hazumi, Neil Goeckner-Wald, Nicholas Galitzki, S. Beckman, Brian Keating, M. A. Dobbs, Carlo Baccigalupi, Clara Vergès, Theodore Kisner, Reijo Keskitalo, Daisuke Kaneko, T. Fujino, S. Kikuchi, Darcy Barron, L. N. Lowry, Scott Chapman, Maximiliano Silva-Feaver, Oliver Jeong, Kevin T. Crowley, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS]Physics [physics], Settore FIS/05, Gravitational wave, Cosmic microwave background, Millimeter wave, First light, CMB, Condensed Matter Physics, 7. Clean energy, 01 natural sciences, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, Microwave emission, Settore FIS/05 - Astronomia e Astrofisica, TES bolometer, Planet, Software deployment, 0103 physical sciences, Extremely high frequency, B-mode polarization, General Materials Science, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Remote sensing
Abstract

International audience; Polarbear-2A is the first of three receivers in the Simons array, a cosmic microwave background experiment located on the Atacama Plateau in Chile. Polarbear-2A was deployed and achieved the first light in January 2019 by mapping the microwave emission from planet observations. Commissioning work is underway to prepare the receiver for science observations.

Published
2019

30. LiteBIRD: A Satellite for the Studies of B-Mode Polarization and Inflation from Cosmic Background Radiation Detection

Author

Josquin Errard, Kent D. Irwin, Ingunn Kathrine Wehus, Kazunori Kohri, Kam Arnold, Atsushi Okamoto, Osamu Tajima, T. Tomida, Hirokazu Ishino, L. Montier, T. Kawasaki, M. Willer, Ryo Yamamoto, Nobuhiko Katayama, B. Thorne, Eiichiro Komatsu, Takayuki Tomaru, Benjamin Westbrook, Toshiaki Iida, Tadayasu Dotani, Yuki Inoue, T. Funaki, Chiko Otani, Bruno Maffei, L. Hayes, Charles A. Hill, F. Vansyngel, T. Nagasaki, L. Duband, Tucker Elleflot, H. Imada, Johannes Hubmayr, A. Cukierman, M. Nakajima, T. Hasebe, Paul Turin, A. Dominjon, Eric V. Linder, S. Takatori, Toshifumi Shimizu, Yuto Minami, Shin Utsunomiya, Y. Sato, Yoshinori Uzawa, D. Tanabe, J. M. Duval, F. Boulanger, Takahiro Okamura, Jo Dunkley, Hiroyuki Sugita, Masato Naruse, Julian Borrill, Makoto Hattori, Theodore Kisner, Yuji Chinone, Tom Nitta, Dale Li, Mathieu Remazeilles, K. Ganga, Hideo Ogawa, Reijo Keskitalo, Masashi Hazumi, Giampaolo Pisano, E. Taylor, S. Takakura, H. Kanai, Jun-ichi Suzuki, N. Sato, Masahiro Tsujimoto, Yutaro Sekimoto, Shin-ichiro Sakai, Kimihiro Kimura, M. Nagai, N. W. Halverson, Anna Mangilli, Seongjae Cho, M. Tristram, S. A. Kernasovskiy, Jonathan Aumont, Blake D. Sherwin, Carole Tucker, Tomotake Matsumura, Kiyotomo Ichiki, Satoru Mima, T. de Haan, T. Hamada, N. Tomita, G. Patanchon, K. Komatsu, Shuji Matsuura, J. Grain, Paul L. Richards, Norio Okada, N. Hidehira, Kazuhisa Mitsuda, Soumen Basak, Yasuhiro Yamada, Aritoki Suzuki, H. K. Eriksen, Hajime Sugai, Shogo Nakamura, Peter A. R. Ade, Alex Lazarian, T. Fujino, Y. Akiba, Gabriel M. Rebeiz, H. Nishino, Nathan Whitehorn, Martin Bucher, R. Stompor, Shingo Kashima, A. Kibayashi, Y. Kida, Noah Kurinsky, D. W. Curtis, M. Inoue, Masaya Hasegawa, Adrian T. Lee, Shugo Oguri, Y. Segawa, David Alonso, A. Ducout, Carlo Baccigalupi, U. Fuskeland, S. Beckman, Uroš Seljak, R. Nagata, J. Fischer, Mitsuhiro Yoshida, K. L. Thompson, Darcy Barron, Gene C. Hilton, Noriko Y. Yamasaki, Erminia Calabrese, Neil Goeckner-Wald, R. Takaku, Suguru Takada, M. A. Dobbs, Oliver Jeong, Toshiya Namikawa, Yuki Sakurai, Chao-Lin Kuo, Kaori Hattori, Keisuke Shinozaki, D. Meilhan, M. Maki, Makoto Sawada, D. Kaneko, T. Yamashita, S. Uozumi, Takashi Noguchi, Akito Kusaka, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
detector: cryogenics, Cosmic microwave background, Cosmic background radiation, cosmic background radiation: polarization, Lagrangian point, B-mode polarization, Cosmic inflation, Primordial gravitational wave, Quantum gravity, Satellite, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 010305 fluids & plasmas, law.invention, Telescope, Settore FIS/05 - Astronomia e Astrofisica, bolometer, law, 0103 physical sciences, General Materials Science, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], detector: optical, 010306 general physics, Physics, Bolometer, gravitational radiation: primordial, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Polarization (waves), inflation: model, Atomic and Molecular Physics, and Optics, detector: sensitivity, modulation, Cardinal point, B-mode, angular resolution, moment: multipole, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Multipole expansion
Abstract

著者人数: 152名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 羽澄, 昌史; 堂谷, 忠靖; 長谷部, 孝; 今田, 大皓; 満田, 和久; 坂井, 真一郎; 関本, 裕太郎; Tomida, T.; 辻本, 匡弘; Yamamoto, R.; 山崎, 典子), Accepted: 2019-01-18, 資料番号: SA1180402000

Published
2019

31. The POLARBEAR Fourier Transform Spectrometer Calibrator and Spectroscopic Characterization of the POLARBEAR Instrument

Author

Hans P. Paar, Ben Westbrook, Joseph Seibert, Osamu Tajima, Aritoki Suzuki, Darcy Barron, L. N. Lowry, Haruki Nishino, Tucker Elleflot, Praween Siritanasak, Nobuhiko Katayama, Masaya Hasegawa, Mario Faundez, Brian Keating, Paul L. Richards, K. Cheung, Giulio Fabbian, Neil Goeckner-Wald, Giuseppe Puglisi, M. Navaroli, Kam Arnold, S. Takatori, C. Tsai, Adrian T. Lee, Yuji Chinone, Federico Bianchini, Frederick Matsuda, and D. Kaneko

Subjects
TA1501, Cosmic microwave background, FOS: Physical sciences, 01 natural sciences, 010305 fluids & plasmas, law.invention, Telescope, Optics, Engineering, QB0980, law, 0103 physical sciences, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Applied Physics, QB, 010302 applied physics, Physics, Settore FIS/05, business.industry, Parabolic reflector, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Steradian, Polarizer, Interferometry, Cardinal point, TA, Physical Sciences, Chemical Sciences, business, Astrophysics - Instrumentation and Methods for Astrophysics, astro-ph.IM
Abstract

We describe the Fourier Transform Spectrometer (FTS) used for in-field testing of the POLARBEAR receiver, an experiment located in the Atacama Desert of Chile which measures the cosmic microwave background (CMB) polarization. The POLARBEAR-FTS (PB-FTS) is a Martin-Puplett interferometer designed to couple to the Huan Tran Telescope (HTT) on which the POLARBEAR receiver is installed. The PB-FTS measured the spectral response of the POLARBEAR receiver with signal-to-noise ratio (SNR) $>20$ for $\sim$69% of the focal plane detectors due to three features: a high throughput of 15.1 steradian cm$^{2}$, optimized optical coupling to the POLARBEAR optics using a custom designed output parabolic mirror, and a continuously modulated output polarizer. The PB-FTS parabolic mirror is designed to mimic the shape of the 2.5 m-diameter HTT primary reflector which allows for optimum optical coupling to the POLARBEAR receiver, reducing aberrations and systematics. One polarizing grid is placed at the output of the PB-FTS, and modulated via continuous rotation. This modulation allows for decomposition of the signal into different harmonics that can be used to probe potentially pernicious sources of systematic error in a polarization-sensitive instrument. The high throughput and continuous output polarizer modulation features are unique compared to other FTS calibrators used in the CMB field. In-field characterization of the POLARBEAR receiver was accomplished using the PB-FTS in April 2014. We discuss the design, construction, and operation of the PB-FTS and present the spectral characterization of the POLARBEAR receiver. We introduce future applications for the PB-FTS in the next-generation CMB experiment, the Simons Array.

Published
2019
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32. The Simons Observatory: Astro2020 APC Whitepaper

Author

Abitbol, Maximilian H., Shunsuke, Adachi, Peter, Ade, James, Aguirre, Zeeshan, Ahmed, Simone, Aiola, Aamir, Ali, David, Alonso, Alvarez, Marcelo A., Kam, Arnold, Peter, Ashton, Zachary, Atkins, Jason, Austermann, Humna, Awan, Carlo, Baccigalupi, Taylor, Baildon, Anton Baleato Lizancos, Darcy, Barron, Nick, Battaglia, Richard, Battye, Eric, Baxter, Andrew, Bazarko, Beall, James A., Rachel, Bean, Dominic, Beck, Shawn, Beckman, Benjamin, Beringue, Tanay, Bhandarkar, Sanah, Bhimani, Federico, Bianchini, Steven, Boada, David, Boettger, Boris, Bolliet, Richard Bond, J., Julian, Borrill, Brown, Michael L., Sarah Marie Bruno, Sean, Bryan, Erminia, Calabrese, Victoria, Calafut, Paolo, Calisse, Julien, Carron, Carl, Fred. M., Juan, Cayuso, Anthony, Challinor, Grace, Chesmore, Yuji, Chinone, Jens, Chluba, Hsiao-Mei Sherry Cho, Steve, Choi, Susan, Clark, Philip, Clarke, Carlo, Contaldi, Gabriele, Coppi, Cothard, Nicholas F., Kevin, Coughlin, Will, Coulton, Devin, Crichton, Crowley, Kevin D., Crowley, Kevin T., Ari, Cukierman, D'Ewart, John M., Rolando, Dünner, Tijmen de Haan, Mark, Devlin, Simon, Dicker, Bradley, Dober, Duell, Cody J., Shannon, Duff, Adri, Duivenvoorden, Dunkley, Jo, Hamza El Bouhargani, Josquin, Errard, Giulio, Fabbian, Stephen, Feeney, James, Fergusson, Simone, Ferraro, Pedro, Fluxà, Katherine, Freese, Frisch, Josef C., Andrei, Frolov, George, Fuller, Nicholas, Galitzki, Gallardo, Patricio A., Jose Tomas Galvez Ghersi, Jiansong, Gao, Eric, Gawiser, Martina, Gerbino, Vera, Gluscevic, Neil, Goeckner-Wald, Joseph, Golec, Sam, Gordon, Megan, Gralla, Daniel, Green, Arpi, Grigorian, John, Groh, Chris, Groppi, Yilun, Guan, Gudmundsson, Jon E., Mark, Halpern, Dongwon, Han, Peter, Hargrave, Kathleen, Harrington, Masaya, Hasegawa, Matthew, Hasselfield, Makoto, Hattori, Victor, Haynes, Masashi, Hazumi, Erin, Healy, Henderson, Shawn W., Brandon, Hensley, Carlos, Hervias-Caimapo, Hill, Charles A., Colin Hill, J., Gene, Hilton, Matt, Hilton, Hincks, Adam D., Gary, Hinshaw, Renée, Hložek, Shirley, Ho, Shuay-Pwu Patty Ho, Hoang, Thuong D., Jonathan, Hoh, Hotinli, Selim C., Zhiqi, Huang, Johannes, Hubmayr, Kevin, Huffenberger, Hughes, John P., Anna, Ijjas, Margaret, Ikape, Kent, Irwin, Jaffe, Andrew H., Bhuvnesh, Jain, Oliver, Jeong, Matthew, Johnson, Daisuke, Kaneko, Karpel, Ethan D., Nobuhiko, Katayama, Brian, Keating, Reijo, Keskitalo, Theodore, Kisner, Kenji, Kiuchi, Jeff, Klein, Kenda, Knowles, Anna, Kofman, Brian, Koopman, Arthur, Kosowsky, Nicoletta, Krachmalnicoff, Akito, Kusaka, Phil, Laplante, Jacob, Lashner, Adrian, Lee, Eunseong, Lee, Antony, Lewis, Yaqiong, Li, Zack, Li, Michele, Limon, Eric, Linder, Jia, Liu, Carlos, Lopez-Caraballo, Thibaut, Louis, Marius, Lungu, Mathew, Madhavacheril, Daisy, Mak, Felipe, Maldonado, Hamdi, Mani, Ben, Mates, Frederick, Matsuda, Loïc, Maurin, Phil, Mauskopf, Andrew, May, Nialh, Mccallum, Heather, Mccarrick, Chris, Mckenney, Jeff, Mcmahon, Daniel Meerburg, P., James, Mertens, Joel, Meyers, Amber, Miller, Mark, Mirmelstein, Kavilan, Moodley, Jenna, Moore, Moritz, Munchmeyer, Charles, Munson, Masaaki, Murata, Sigurd, Naess, Toshiya, Namikawa, Federico, Nati, Martin, Navaroli, Laura, Newburgh, Ho Nam Nguyen, Andrina, Nicola, Mike, Niemack, Haruki, Nishino, Yume, Nishinomiya, John, Orlowski-Scherer, Luca, Pagano, Bruce, Partridge, Francesca, Perrotta, Phumlani, Phakathi, Lucio, Piccirillo, Elena, Pierpaoli, Giampaolo, Pisano, Davide, Poletti, Roberto, Puddu, Giuseppe, Puglisi, Chris, Raum, Reichardt, Christian L., Mathieu, Remazeilles, Yoel, Rephaeli, Dominik, Riechers, Felipe, Rojas, Aditya, Rotti, Anirban, Roy, Sharon, Sadeh, Yuki, Sakurai, Maria, Salatino, Mayuri Sathyanarayana Rao, Lauren, Saunders, Emmanuel, Schaan, Marcel, Schmittfull, Neelima, Sehgal, Joseph, Seibert, Uros, Seljak, Paul, Shellard, Blake, Sherwin, Meir, Shimon, Carlos, Sierra, Jonathan, Sievers, Cristobal, Sifon, Precious, Sikhosana, Maximiliano, Silva-Feaver, Simon, Sara M., Adrian, Sinclair, Kendrick, Smith, Wuhyun, Sohn, Rita, Sonka, David, Spergel, Jacob, Spisak, Staggs, Suzanne T., George, Stein, Stevens, Jason R., Radek, Stompor, Aritoki, Suzuki, Osamu, Tajima, Satoru, Takakura, Grant, Teply, Thomas, Daniel B., Ben, Thorne, Robert, Thornton, Trac, Hy, Jesse, Treu, Calvin, Tsai, Carole, Tucker, Joel, Ullom, Vagnozzi, Sunny, Alexander van Engelen, Jeff Van Lanen, Van Winkle, Daniel D., Vavagiakis, Eve M., Clara, Vergès, Michael, Vissers, Kasey, Wagoner, Samantha, Walker, Yuhan, Wang, Jon, Ward, Ben, Westbrook, Nathan, Whitehorn, Jason, Williams, Joel, Williams, Edward, Wollack, Zhilei, Xu, Siavash, Yasini, Edward, Young, Byeonghee, Yu, Cyndia, Yu, Fernando, Zago, Mario, Zannoni, Hezi, Zhang, Kaiwen, Zheng, Ningfeng, Zhu, and Andrea, Zonca

Published
2019

33. Modelling the Energy Losses of a Superconducting Magnetic Bearing due to the Change of the Levitation Height Under Gravity

Author

Yasunori Terao, D Ahmad, Tomotake Matsumura, Yuki Sakurai, Hiroyuki Ohsaki, Nobuhiko Katayama, Yusuke Ishida, H. Enokida, and Hajime Sugai

Subjects
Superconductivity, Physics, History, Rotor (electric), Stator, Mechanics, Dissipation, Polarization (waves), Computer Science Applications, Education, law.invention, Magnetic field, law, Condensed Matter::Superconductivity, Magnet, Levitation
Abstract

This paper describes the losses of the rotor of the prototype superconducting magnetic bearing (SMB) that is employed for a polarization modulator of a Cosmic Microwave Background polarization experiment. The stator is composed of 20 segmented YBCO bulks, and these multiple superconductors produce the inhomogeneous magnetic field particularly due to the gravitational displacement of the rotor magnet position from the initial field cooling. This inhomogeneity causes the power dissipation to the spinning rotor. We estimated the power dissipation originating from this inhomogeneous magnetic field by using a numerical approach. The superconductors were modelled as electrically conducting components in the numerical simulation to avoid the complexity in modelling superconductivity. The results show about 4 mW dissipated at the rotor.

Published
2021

34. Half-meter Scale Superconducting Magnetic Bearing for Cosmic Microwave Background Polarization Experiments

Author

Yuki Sakurai, Osamu Tajima, Kenji Kiuchi, Charles A. Hill, Peter Ashton, Akito Kusaka, and Nobuhiko Katayama

Subjects
Physics, History, Orthogonal polarization spectral imaging, Detector, Cosmic microwave background, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, Liquid nitrogen, Atmospheric noise, Polarization (waves), Computer Science Applications, Education, Computational physics, Superconducting magnetic bearing
Abstract

We report the development of a large-diameter superconducting magnetic bearing (SMB) used in a continuously rotating cryogenic half-wave plate (HWP) polarization modulator for cosmic microwave background (CMB) polarization experiments. A precise measurement of the CMB polarization will place tighter constrains on cosmic inflation, describing the rapid expansion of the early universe. The polarization modulator is a critical instrument for suppressing 1/f contamination, which is mainly caused by atmospheric noise, and for mitigating systematic uncertainties that arise when differencing orthogonal polarization detectors. To ensure a sufficient field of view and to reduce thermal emission, the polarization modulator must have a clear-aperture diameter of > 500 mm and must operate at cryogenic temperatures. We constructed a superconducting magnetic bearing (SMB) with an inner diameter of 550 mm, which is the largest used in any CMB polarization experiment to date. We tested the friction and stiffness of the bearing at liquid nitrogen temperatures. The measured total loss is 0.4 W and the spring constant is >105 N/m, which satisfies typical experimental requirements. Furthermore, we performed a performance test by changing the number of disk-shaped YBCO tiles, and then confirmed that the SMB performance was proportional to the YBCO volume.

Published
2020

35. The optical design and physical optics analysis of a cross-Dragonian telescope for LiteBIRD

Author

Junji Inatani, Hirokazu Ishino, Aritoki Suzuki, Masashi Hazumi, Nobuhiko Katayama, H. Imada, Yutaro Sekimoto, Kimihiro Kimura, Tomotake Matsumura, Shin Utsunomiya, Ryo Nagata, Shingo Kashima, T. Hasebe, Tadayasu Dotani, and Hajime Sugai

Subjects
Physics, Main lobe, Stray light, HFSS, business.industry, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, Physical optics, 01 natural sciences, law.invention, 010309 optics, Telescope, Optics, Side lobe, law, 0103 physical sciences, business, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The Lite satellite for the studies of B-mode polarization and Inflation from the cosmic microwave background (CMB) Radiation Detection (LiteBIRD) is a next generation CMB satellite dedicated to probing the inflationary universe. It has two telescopes, Low Frequency Telescope (LFT) and High Frequency Telescope (HFT) to cover wide observational bands from 34 GHz to 448 GHz. In this presentation, we report the optical design and characterization of the LFT. We have used the CODE-V to obtain the LFT optical design based on a cross- Dragonian telescope. It is an image-space telecentric system with an F number of 3.5 and 20 x 10 degrees2 field of view. The main, near and far side lobes at far-field have been calculated by using a combination of HFSS and GRASP 10. It is revealed that the LFT telescope has good main lobe properties to satisfy the requirements. On the other hand, the side lobes are affected by the stray light that stems from the triple reflection and the direct path from feed. In order to avoid the stray light, the way to block these paths is now under study.

Published
2018

36. Design and development of a polarization modulator unit based on a continuous rotating half-wave plate for LiteBIRD

Author

Akito Kusaka, Junji Yumoyo, Shin Utsunomiya, M. Maki, Hiroaki Imada, Toshiki Shimomura, T. Iida, T. Ghigna, Hajime Sugai, K. Komatsu, Hiroyuki Ohsaki, Masashi Hazumi, Yukikatsu Terada, Yuki Sakurai, Ryota Takaku, Shinya Sugiyama, Haruyuki Sakurai, Tomotake Matsumura, Yutaka Terao, Jun-ichi Suzuki, Shogo Nakamura, Ryo Yamamoto, Hirokazu Ishino, Nobuhiko Katayama, Makoto Tashiro, Kuniaki Konishi, Charles Hill, H. Kanai, and Hirokazu Kataza

Subjects
Physics, business.industry, Detector, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Rotation, Polarization (waves), 01 natural sciences, Waveplate, law.invention, 010309 optics, Telescope, Optics, Achromatic lens, law, 0103 physical sciences, Broadband, 010306 general physics, business
Abstract

We present our design and development of a polarization modulator unit (PMU) for LiteBIRD space mission. LiteBIRD is a next generation cosmic microwave background (CMB) polarization satellite to measure the primordial B-mode. The science goal of LiteBIRD is to measure the tensor-to-scalar ratio with the sensitivity of δr < 10-3. The baseline design of LiteBIRD is to employ the PMU based on a continuous rotating half-wave plate (HWP) at a telescope aperture with a diameter of 400 mm. It is an essential for LiteBIRD to achieve the science goal because it significantly reduces detector noise and systematic uncertainties. The LiteBIRD PMU consists of a multi-layered sapphire as a broadband achromatic HWP and a mechanism to continuously rotate it at 88 rpm. The whole system is maintained at below 10K to minimize the thermal emission from the HWP. In this paper, we discuss the current development status of the broadband achromatic HWP and the cryogenic rotation mechanism.

Published
2018

37. Prototype design and evaluation of the nine-layer achromatic half-wave plate for the LiteBIRD low frequency telescope

Author

Tomotake Matsumura, Masashi Hazumi, Ryota Takaku, Hiroaki Imada, Hirokazu Ishino, Nobuhiko Katayama, K. Komatsu, Hajime Sugai, Yuki Sakurai, Laboratoire de l'Accélérateur Linéaire (LAL), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
noise, satellite, measurement methods, Cosmic microwave background, cosmic background radiation: polarization, Low frequency, 01 natural sciences, Waveplate, law.invention, 010309 optics, Telescope, Optics, law, 0103 physical sciences, Broadband, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, activity report, Physics, business.industry, Bandwidth (signal processing), Polarization (waves), B-mode, efficiency, Achromatic lens, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business
Abstract

International audience; LiteBIRD is a satellite project to measure the polarization of the CMB with an unprecedented accuracy. LiteBIRD observes all sky for three years at the sun-earth second Lagrange point. The goal of LiteBIRD is to observe the B-mode polarization at large angular scales and to measure the tensor-to-scaler ratio r with an accuracy less than 0.001, exploring the energy scale of the inflation. In order to mitigate the system 1/f noise and systematics, we plan to use continuous rotating half-wave plates (HWPs) as a polarization modulator at each aperture of two telescopes. One of the telescopes, called a low frequency telescope (LFT), covers the frequency range from 34 to 270 GHz, requiring the HWP to have a high modulation efficiency in the wide bandwidth. We employ a Pancharatnam-type achromatic HWP (AHWP) to achieve the broadband coverage. The AHWP consists of nine layer stacked HWPs with the optic axes mutually rotated by the angles optimized for the LFT bandwidth. In this paper, we report our development status of the nine layer AHWP and measurement results on the modulation efficiency and the phase as a function of frequency.

Published
2018

38. Electrical characterization and tuning of the integrated POLARBEAR-2a focal plane and readout (Conference Presentation)

Author

J. Borrill, Paul L. Richards, Stephen M. Feeney, A. T. P. Pham, J. Peloton, Darcy Barron, Mario Aguilar, Josquin Errard, L. N. Lowry, D. Beck, A. Cukierman, Akito Kusaka, M. Le Jeune, Neil Goeckner-Wald, Max Silva Feaver, W. L. Holzapfel, Nicoletta Krachmalnicoff, Gabriele Coppi, H. Roberts, Peter Ashton, A. Tikhomirov, M. A. Dobbs, Osamu Tajima, D. Leon, Masashi Hazumi, P. A. R. Ade, Grant Teply, Nathan J. Miller, Colin Ross, Nicholas Galitzki, P. Siritanasak, Blake D. Sherwin, Tucker Elleflot, Y. Akiba, K. M. Rotermund, S. Beckman, A. J. Gilbert, Christian L. Reichardt, R. Dunner, Gary A. Fuller, Oliver Jeong, Eric V. Linder, A. Madurowicz, Giulio Fabbian, John Groh, Jessica Avva, Yuki Inoue, S. Takatori, G. Jaehnig, Carlo Baccigalupi, Giuseppe Puglisi, Charles A. Hill, S. Takakura, Andrew May, Scott Chapman, D. Plambeck, Kevin T. Crowley, D. Tanabe, Kam Arnold, Brian Keating, Aamir Ali, Benjamin Westbrook, M. Navroli, Adrian T. Lee, Jennifer Ito, Masaya Hasegawa, Aritoki Suzuki, Federico Bianchini, Theodore Kisner, Julien Carron, Tomotake Matsumura, Reijo Keskitalo, Daisuke Kaneko, Y. Segawa, T. Natoli, Frederick Matsuda, Yuji Chinone, N. W. Halverson, R. Stompor, T. de Haan, T. Hamada, A. Zahn, Amy N. Bender, D. Boettger, Takayuki Tomaru, R. Tat, A. Lowitz, Chang Feng, C. Tsai, Lucio Piccirillo, Leo Steinmetz, Nobuhiko Katayama, Daisy Mak, Davide Poletti, C. Verges, L. Howe, Haruki Nishino, A. Anderson, Yuto Minami, Gabriel M. Rebeiz, Nathan Whitehorn, Christopher Raum, Joshua Montgomery, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
temperature: transition, Cosmic microwave background, cosmic background radiation: polarization, frequency-division multiplexing, Astrophysics::Cosmology and Extragalactic Astrophysics, SQUID, 01 natural sciences, 010305 fluids & plasmas, law.invention, cosmic background radiation: B-mode, Optics, bolometer, gravitation: lens, law, 0103 physical sciences, millimeter-wave, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, 010306 general physics, Physics, Gravitational wave, business.industry, superconductivity, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Spectral density, cosmic microwave background polarization, stability, Polarization (waves), transition-edge sensor, Extremely high frequency, resonance: frequency, power spectrum: angular dependence, readout, dfmux, Transition edge sensor, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; POLARBEAR is a cosmic microwave background (CMB) polarization experiment located in the Atacama desert in Chile. The science goals of the POLARBEAR project are to do a deep search for CMB B-mode polarization created by inflationary gravitational waves, as well as characterize the CMB B-mode signal from gravitational lensing. POLARBEAR-1 started observations in 2012, and the POLARBEAR team has published a series of results from its first two seasons of observations, including the first measurement of a non-zero B-mode polarization angular power spectrum, measured at sub-degree scales where the dominant signal is gravitational lensing of the CMB. The Simons Array expands POLARBEAR to include an additional two telescopes with next-generation POLARBEAR-2 multi-chroic receivers, observing at 95, 150, 220, and 270 GHz.The POLARBEAR-2A focal plane has 7,588 transition-edge sensor bolometers, read out with frequency-division multiplexing, with 40 frequency channels within the readout bandwidth of 1.5 to 4.5 MHz. The frequency channels are defined by a low-loss lithographed aluminum spiral inductor and interdigitated capacitor in series with each bolometer, creating a resonant frequency for each channel's unique voltage bias and current readout. Characterization of the readout includes measuring resonant peak locations and heights and fitting to a circuit model both above and below the bolometer superconducting transition temperature. This information is used determine the optimal detector bias frequencies and characterize stray impedances which may affect bolometer operation and stability. The detector electrical characterization includes measurements of the transition properties by sweeping in temperature and in voltage bias, measurements of the bolometer saturation power, as well as measuring and removing any biases introduced by the readout circuit. We present results from the characterization, tuning, and operation of the fully integrated focal plane and readout for the first POLARBEAR-2 receiver, POLARBEAR-2A, during its pre-deployment integration run.

Published
2018

39. POLARBEAR-2: a new CMB polarization receiver system for the Simons array (Conference Presentation)

Author

Frederick Matsuda, Colin Ross, Josquin Errard, Dominic Beck, Theodore Kisner, Masashi Hazumi, Peter A. R. Ade, Reijo Keskitalo, Daisuke Kaneko, Nicholas Galitzki, Davide Poletti, N. W. Halverson, W. L. Holzapfel, Carlo Baccigalupi, Junichi Suzuki, Rolando Dünner, Gabriel M. Rebeiz, Blake D. Sherwin, H. Roberts, Scott Chapman, Haruki Nishino, Paul L. Richards, Clara Vergès, Amy N. Bender, Yuto Minami, Raymond Tat, Takahiro Okamura, Akito Kusaka, Suet Ying D. Mak, Nathan Whitehorn, Kevin T. Crowley, Stephen M. Feeney, Richard Plambeck, Giuseppe Puglisi, Chang Feng, Charles Hill, T. Hamada, Nicoletta Krachmalnicoff, D. Tanabe, Takayuki Tomaru, D. Leon, Julian Borrill, M. Navaroli, Federico Bianchini, S. Beckman, Andrew H. Jaffe, Neil Goeckner-Wald, D. Boettger, C. Tsai, A. T. P. Pham, Lucio Piccirillo, Tijmen de Haan, Maximiliano Silva-Feaver, Aamir Ali, Kaja Rotermund, Oliver Jeong, Yuji Chinone, Maude Jeune, Andrew Gilbert, Christopher Raum, A. Zahn, Radek Stompor, Osamu Tajima, Joshua Montgomery, Brian Keating, J. Peloton, George M. Fuller, Yuki Inoue, Darcy Barron, L. N. Lowry, Mario Aguilar, S. Takatori, Gabriele Coppi, Nathan J. Miller, Christian L. Reichardt, John Groh, Kam Arnold, Jennifer Ito, Greg Jaehnig, Tucker Elleflot, Eric V. Linder, Giulio Fabbian, L. Howe, Peter Ashton, Leo Steinmetz, Grant Teply, Y. Akiba, Ali Cukierman, Praween Siritanasak, Alex Madurowicz, Nobuhiko Katayama, Matt Dobbs, Andrew May, Ben Westbrook, Aritoki Suzuki, Adrian T. Lee, Julien Carron, Masaya Hasegawa, Y. Segawa, Tomotake Matsumura, S. Takakura, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
010504 meteorology & atmospheric sciences, Cosmic microwave background, optics: design, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Multiplexing, neutrino mass, law.invention, Telescope, Optics, bolometer, law, Polarization, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, activity report, detector: design, 0105 earth and related environmental sciences, Physics, business.industry, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Inflation, Cardinal point, TES bolometer, B-mode, cryogenics, electronics: readout, Neutrino, interference: quantum, business, performance
Abstract

International audience; POLARBEAR-2 is a new receiver system, which will be deployed on the Simons Array telescope platform, for the measurement of Cosmic Microwave Background (CMB) polarization. The science goals with POLARBEAR-2 are to characterize the B-mode signal both at degree and sub-degree angular-scales. The degree-scale polarization data can be used for quantitative studies on inflation, such as the reconstruction of the energy scale of inflation. The sub-degree polarization data is an excellent tracer of large-scale structure in the universe, and will lead to precise constraints on the sum of the neutrino masses. In order to achieve these goals, POLARBEAR-2 employs 7588 polarization-sensitive antenna-coupled transition-edge sensor (TES) bolometers on the focal plane cooled to 0.27K with a three-stage Helium sorption refrigerator, which is ~6 times larger array over the current receiver system. The large TES bolometer array is read-out by an upgraded digital frequency-domain multiplexing system capable of multiplexing 40 bolometers through a single superconducting quantum interference device (SQUID). The first POLARBEAR-2 receiver, POLARBEAR-2A is constructed and the end-to-end testing to evaluate the integrated performance of detector, readout, and optics system is being conducted in the laboratory with various types of test equipments. The POLARBEAR-2A is scheduled to be deployed in 2018 at the Atacama desert in Chile. To further increase measurement sensitivity, two more POLARBEAR-2 type receivers will be deployed soon after the deployment (Simons Array project). The Simons Array will cover four frequency bands at 95GHz, 150GHz, 220GH and 270GHz for better control of the foreground signal. The projected constraints on a tensor-to-scalar ratio (amplitude of inflationary B-mode signal) is σ(r=0.1) = $6.0 \times 10^{-3}$ after foreground removal ($4.0 \times 10^{-3}$ (stat.)), and the sensitivity to the sum of the neutrino masses when combined with DESI spectroscopic galaxy survey data is 40 meV at 1-sigma after foreground removal (19 meV(stat.)). We will present an overview of the design, assembly and status of the laboratory testing of the POLARBEAR-2A receiver system as well as the Simons Array project overview.

Published
2018

40. Design and Thermal Characteristics of a 400 mm Diameter Levitating Rotor in a Superconducting Magnetic Bearing Operating Below at 10 K for a CMB Polarization Experiment

Author

Ryo Yamamoto, Tomotake Matsumura, H. Kanai, Nobuhiko Katayama, Hirokazu Kataza, Yutaka Terao, Toshiki Shimomura, T. Iida, Yuki Sakurai, Hiroyuki Ohsaki, Hajime Sugai, H. Imada, and Shin Utsunomiya

Subjects
Superconductivity, Materials science, Stator, 02 engineering and technology, 021001 nanoscience & nanotechnology, Condensed Matter Physics, Polarization (waves), 01 natural sciences, Electronic, Optical and Magnetic Materials, law.invention, Computational physics, 010309 optics, Thermal conductivity, Neodymium magnet, law, Magnet, 0103 physical sciences, Thermal, Magnetic levitation, Levitation, bearings, thermal conductivity, Electrical and Electronic Engineering, 0210 nano-technology
Abstract

著者人数: 13名, Accepted: 2018-01-15, 資料番号: SA1180027000

Published
2018

41. Finding the chiral gravitational wave background of an axion- SU(2) inflationary model using CMB observations and laser interferometers

Author

Maresuke Shiraishi, Masashi Hazumi, Nobuhiko Katayama, B. Thorne, Eiichiro Komatsu, and Tomohiro Fujita

Subjects
Physics, 010308 nuclear & particles physics, Cosmic microwave background, Spectral density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), 01 natural sciences, Gravitational wave background, Gravitational lens, Non-Gaussianity, 0103 physical sciences, 010303 astronomy & astrophysics, Axion, Quantum fluctuation
Abstract

A detection of B-mode polarization of the cosmic microwave background (CMB) anisotropies would confirm the presence of a primordial gravitational wave background (GWB). In the inflation paradigm, this would be an unprecedented probe of the energy scale of inflation as it is directly proportional to the power spectrum of the GWB. However, similar tensor perturbations can be produced by the matter fields present during inflation, breaking the simple relationship between energy scale and the tensor-to-scalar ratio $r$. It is therefore important to find ways of distinguishing between the generation mechanisms of the GWB. Without doing a full model selection, we analyze the detectability of a new axion-$SU(2)$ gauge field model by calculating the signal-to-noise ratio of future CMB and interferometer observations sensitive to the chirality of the tensor spectrum. We forecast the detectability of the resulting CMB temperature and B-mode (TB) or E-mode and B-mode (EB) cross-correlation by the LiteBIRD satellite, considering the effects of residual foregrounds, gravitational lensing, and assess the ability of such an experiment to jointly detect primordial TB and EB spectra and self-calibrate its polarimeter. We find that LiteBIRD will be able to detect the chiral signal for ${r}_{*}g0.03$, with ${r}_{*}$ denoting the tensor-to-scalar ratio at the peak scale, and that the maximum signal-to-noise ratio for ${r}_{*}l0.07$ is $\ensuremath{\sim}2$. We go on to consider an advanced stage of a LISA-like mission, which is designed to be sensitive to the intensity and polarization of the GWB. We find that such experiments would complement CMB observations as they would be able to detect the chirality of the GWB with high significance on scales inaccessible to the CMB. We conclude that CMB two-point statistics are limited in their ability to distinguish this model from a conventional vacuum fluctuation model of GWB generation, due to the fundamental limits on their sensitivity to parity violation. In order to test the predictions of such a model as compared to vacuum fluctuations, it will be necessary to test deviations from the self-consistency relation or use higher order statistics to leverage the non-Gaussianity of the model. On the other hand, in the case of a spectrum peaked at very small scales inaccessible to the CMB, a highly significant detection could be made using space-based laser interferometers.

Published
2018

42. Developing a new template foreground cleaning method for the LiteBird experiment

Author

Kiyotomo Ichiki, Eiichiro Komatsu, Tetsu Yamashita, Nobuhiko Katayama, and H. Kanai

Subjects
Gravitational wave background, Physics, Sky, Frequency band, media_common.quotation_subject, Isotropy, Cosmic microwave background, Thermal, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), Galaxy, media_common, Computational physics
Abstract

Detecting gravitational wave background generated during inflation through B-mode polarization of the cosmic microwave background (CMB) is one of the main scientific goals of future CMB experiments. However, it has already become clear that the synchrotron and thermal dust emissions from our galaxy hinder the cosmological B-mode signal across the sky. Here, assuming only Gaussianity and statistical isotropy and homogeneity of the CMB map, we develop a new template cleaning method taking into account spatial variations of spectral indices of the foreground emissions, and apply it to various foreground models using Monte-Carlo simulation technique. We find that the method successfully remove the unwanted bias in determining the tensor-to-scalar ratio $r$ that was found in the simple template cleaning method presented in Katayama and Komatsu 2011. In this poster, we present how small $r$ we will be able to reach according to the frequency band and noise specification proposed for the LiteBird experiment.

Published
2017

43. The POLARBEAR-2 and Simons Array Focal Plane Fabrication Status

Author

Adrian T. Lee, Neil Goeckner-Wald, D. Beck, D. Leon, A. Cukierman, M. Navaroli, Brian Keating, Y. Segawa, Tucker Elleflot, Masaya Hasegawa, Maximiliano Silva-Feaver, Peter A. R. Ade, Y. Akiba, Matt Dobbs, Julian Borrill, Paul L. Richards, Stephen M. Feeney, Rolando Dünner, K. M. Rotermund, C. Tsai, Oliver Jeong, Osamu Tajima, A. T. P. Pham, Eric V. Linder, Gabriel M. Rebeiz, Josquin Errard, S. Takakura, D. Plambeck, Lucio Piccirillo, Nathan Whitehorn, Yuji Chinone, S. Beckman, Giulio Fabbian, L. Howe, M. Le Jeune, Federico Bianchini, Christopher Raum, Daisy Mak, Grant Teply, W. L. Holzapfel, Andrew May, Joshua Montgomery, Carlo Baccigalupi, H. Roberts, S. Takatori, Christian L. Reichardt, Reijo Keskitalo, A. J. Gilbert, Gary A. Fuller, R. Tat, Akito Kusaka, Nobuhiko Katayama, D. Boettger, A. Tikhomirov, John Groh, Benjamin Westbrook, Giuseppe Puglisi, Charles A. Hill, Scott Chapman, Nicoletta Krachmalnicoff, Colin Ross, Amy N. Bender, A. Madurowicz, Darcy Barron, J. Peloton, N. W. Halverson, L. N. Lowry, Aritoki Suzuki, Chang Feng, Andrew H. Jaffe, Takayuki Tomaru, Davide Poletti, A. Zahn, Radek Stompor, Mario Ferrada Aguilar, Theodore Kisner, T. de Haan, T. Hamada, Gabriele Coppi, Yuto Minami, Yuki Inoue, Nathan J. Miller, D. Tanabe, H. Nishino, G. Jaehnig, Masashi Hazumi, Nicholas Galitzki, Blake D. Sherwin, Kevin D. Crowley, Kam Arnold, Frederick Matsuda, D. Kaneko, Praween Siritanasak, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Westbrook, B, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bender, A, Bianchini, F, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Coppi, G, Crowley, K, Cukierman, A, de Haan, T, Dunner, R, Dobbs, M, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fuller, G, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Holzapfel, W, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Kusaka, A, Le Jeune, M, Lee, A, Leon, D, Linder, E, Lowry, L, Madurowicz, A, Mak, D, Matsuda, F, May, A, Miller, N, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Piccirillo, L, Plambeck, D, Poletti, D, Puglisi, G, Raum, C, Rebeiz, G, Reichardt, C, Richards, P, Roberts, H, Ross, C, Rotermund, K, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Tat, R, Teply, G, Tikhomirov, A, Tomaru, T, Tsai, C, Whitehorn, N, Zahn, A, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
Cosmic microwave background, cosmic background radiation: polarization, CMB, Dichroic glass, 01 natural sciences, law.invention, law, Atomic and Molecular Physics, Polarization, General Materials Science, silicon: nitrogen, Instrumentation, Mathematical Physics, 010302 applied physics, Physics, Settore FIS/05, superconductivity, Detector, Detectors, Polarization (waves), Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Cardinal point, Materials Science (all), silicon: oxygen, Astrophysics - Instrumentation and Methods for Astrophysics, Transition edge sensor, performance, Astrophysics - Cosmology and Nongalactic Astrophysics, Fabrication, Sinuous antenna, Inflation, General Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Classical Physics, FOS: Physical sciences, Telescope, Optics, Settore FIS/05 - Astronomia e Astrofisica, bolometer, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), detector: design, activity report, business.industry, Bolometer, and Optics, business
Abstract

著者人数: 93名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 羽澄, 昌史), Accepted: 2018-08-27, 資料番号: SA1180208000

Published
2017

44. The Hyper Suprime-Cam SSP Survey: Overview and Survey Design

Author

Hiroaki Aihara, Nobuo Arimoto, Robert Armstrong, Stéphane Arnouts, Neta A Bahcall, Steven Bickerton, James Bosch, Kevin Bundy, Peter L Capak, James H H Chan, Masashi Chiba, Jean Coupon, Eiichi Egami, Motohiro Enoki, Francois Finet, Hiroki Fujimori, Seiji Fujimoto, Hisanori Furusawa, Junko Furusawa, Tomotsugu Goto, Andy Goulding, Johnny P Greco, Jenny E Greene, James E Gunn, Takashi Hamana, Yuichi Harikane, Yasuhiro Hashimoto, Takashi Hattori, Masao Hayashi, Yusuke Hayashi, Krzysztof G Hełminiak, Ryo Higuchi, Chiaki Hikage, Paul T P Ho, Bau-Ching Hsieh, Kuiyun Huang, Song Huang, Hiroyuki Ikeda, Masatoshi Imanishi, Akio K Inoue, Kazushi Iwasawa, Ikuru Iwata, Anton T Jaelani, Hung-Yu Jian, Yukiko Kamata, Hiroshi Karoji, Nobunari Kashikawa, Nobuhiko Katayama, Satoshi Kawanomoto, Issha Kayo, Jin Koda, Michitaro Koike, Takashi Kojima, Yutaka Komiyama, Akira Konno, Shintaro Koshida, Yusei Koyama, Haruka Kusakabe, Alexie Leauthaud, Chien-Hsiu Lee, Lihwai Lin, Yen-Ting Lin, Robert H Lupton, Rachel Mandelbaum, Yoshiki Matsuoka, Elinor Medezinski, Sogo Mineo, Shoken Miyama, Hironao Miyatake, Satoshi Miyazaki, Rieko Momose, Anupreeta More, Surhud More, Yuki Moritani, Takashi J Moriya, Tomoki Morokuma, Shiro Mukae, Ryoma Murata, Hitoshi Murayama, Tohru Nagao, Fumiaki Nakata, Mana Niida, Hiroko Niikura, Atsushi J Nishizawa, Yoshiyuki Obuchi, Masamune Oguri, Yukie Oishi, Nobuhiro Okabe, Sakurako Okamoto, Yuki Okura, Yoshiaki Ono, Masato Onodera, Masafusa Onoue, Ken Osato, Masami Ouchi, Paul A Price, Tae-Soo Pyo, Masao Sako, Marcin Sawicki, Takatoshi Shibuya, Kazuhiro Shimasaku, Atsushi Shimono, Masato Shirasaki, John D Silverman, Melanie Simet, Joshua Speagle, David N Spergel, Michael A Strauss, Yuma Sugahara, Naoshi Sugiyama, Yasushi Suto, Sherry H Suyu, Nao Suzuki, Philip J Tait, Masahiro Takada, Tadafumi Takata, Naoyuki Tamura, Manobu M Tanaka, Masaomi Tanaka, Masayuki Tanaka, Yoko Tanaka, Tsuyoshi Terai, Yuichi Terashima, Yoshiki Toba, Nozomu Tominaga, Jun Toshikawa, Edwin L Turner, Tomohisa Uchida, Hisakazu Uchiyama, Keiichi Umetsu, Fumihiro Uraguchi, Yuji Urata, Tomonori Usuda, Yousuke Utsumi, Shiang-Yu Wang, Wei-Hao Wang, Kenneth C Wong, Kiyoto Yabe, Yoshihiko Yamada, Hitomi Yamanoi, Naoki Yasuda, Sherry Yeh, Atsunori Yonehara, Suraphong Yuma, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universitat de Barcelona, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille ( LAM ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Aix Marseille Université ( AMU ) -Centre National d'Etudes Spatiales ( CNES )

Subjects
media_common.quotation_subject, FOS: Physical sciences, 01 natural sciences, 0103 physical sciences, 14. Life underwater, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Summit, geography.geographical_feature_category, Cosmologia, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Survey research, Galaxies, Galàxies, Cosmology, Geography, Space and Planetary Science, Sky, Magnitude (astronomy), Subaru Telescope, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2m Subaru telescope on the summit of Maunakea in Hawaii. A team of scientists from Japan, Taiwan and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400 deg$^2$ in five broad bands ($grizy$), with a $5\,\sigma$ point-source depth of $r \approx 26$. The Deep layer covers a total of 26~deg$^2$ in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5 deg$^2$). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey., Comment: 14 pages, 7 figures, 5 tables. Corrected for a typo in the coordinates of HSC-Wide spring equatorial field in Table 5

Published
2017

45. First Data Release of the Hyper Suprime-Cam Subaru Strategic Program

Author

Naoshi Sugiyama, Surhud More, Chiaki Hikage, Nobuo Arimoto, Shiro Mukae, Paul T. P. Ho, Chien-Hsiu Lee, Hiroaki Aihara, Hisanori Furusawa, Tomoki Morokuma, Suraphong Yuma, Masato Onodera, Nobunari Kashikawa, Masao Hayashi, Nobuhiro Okabe, Fumihiro Uraguchi, Masamune Oguri, Song Huang, Tsuyoshi Terai, Yukie Oishi, James Bosch, Yukiko Kamata, Philip J. Tait, Yoshiyuki Obuchi, Yen-Ting Lin, Haruka Kusakabe, Yoshihiko Yamada, Yoko Tanaka, Anton T. Jaelani, Anupreeta More, Masahiro Takada, S. Koshida, Rachel Mandelbaum, Masami Ouchi, Atsushi J. Nishizawa, Nobuhiko Katayama, Tomonori Usuda, Akira Konno, Kazuhiro Shimasaku, Robert Armstrong, Yoshiaki Ono, Hiroyuki Ikeda, Joshua S. Speagle, Tomotsugu Goto, Ryoma Murata, Masayuki Tanaka, Yusuke Hayashi, Yuma Sugahara, J. Furusawa, Hitomi Yamanoi, Yoshiki Matsuoka, Rieko Momose, Kuiyun Huang, Sherry Yeh, Yuji Urata, Robert H. Lupton, Michitaro Koike, Shoken Miyama, Michael A. Strauss, James E. Gunn, Shiang-Yu Wang, Krzysztof G. Hełminiak, Yuki Okura, Hisakazu Uchiyama, Melanie Simet, Yoshiki Toba, Ikuru Iwata, Lihwai Lin, Ryo Higuchi, Jean Coupon, Nao Suzuki, Hung-Yu Jian, Takashi Kojima, Hiroshi Karoji, Paul A. Price, Takatoshi Shibuya, Andy D. Goulding, Tomohisa Uchida, Hiroko Niikura, Steven J. Bickerton, Manobu Tanaka, Mana Niida, Edwin L. Turner, Yasushi Suto, Hironao Miyatake, Sogo Mineo, Yuichi Harikane, Dustin Lang, Bau-Ching Hsieh, Hitoshi Murayama, Tohru Nagao, François Finet, Alexie Leauthaud, Masashi Chiba, Fumiaki Nakata, Yousuke Utsumi, M. Onoue, Satoshi Kawanomoto, Takashi Hattori, Masatoshi Imanishi, Tadafumi Takata, Seiji Fujimoto, Yutaka Komiyama, Keiichi Umetsu, Elinor Medezinski, David N. Spergel, Tae-Soo Pyo, Naoki Yasuda, Hiroki Fujimori, and Satoshi Miyazaki

Subjects
Image quality, media_common.quotation_subject, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Field (computer science), Computer graphics (images), 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, Pipeline (software), Astrophysics - Astrophysics of Galaxies, Object detection, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Sky, Data quality, Astrophysics of Galaxies (astro-ph.GA), Subaru Telescope, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) is a three-layered imaging survey aimed at addressing some of the most outstanding questions in astronomy today, including the nature of dark matter and dark energy. The survey has been awarded 300 nights of observing time at the Subaru Telescope and it started in March 2014. This paper presents the first public data release of HSC-SSP. This release includes data taken in the first 1.7 years of observations (61.5 nights) and each of the Wide, Deep, and UltraDeep layers covers about 108, 26, and 4 square degrees down to depths of i~26.4, ~26.5, and ~27.0 mag, respectively (5sigma for point sources). All the layers are observed in five broad bands (grizy), and the Deep and UltraDeep layers are observed in narrow bands as well. We achieve an impressive image quality of 0.6 arcsec in the i-band in the Wide layer. We show that we achieve 1-2 per cent PSF photometry (rms) both internally and externally (against Pan-STARRS1), and ~10 mas and 40 mas internal and external astrometric accuracy, respectively. Both the calibrated images and catalogs are made available to the community through dedicated user interfaces and database servers. In addition to the pipeline products, we also provide value-added products such as photometric redshifts and a collection of public spectroscopic redshifts. Detailed descriptions of all the data can be found online. The data release website is https://hsc-release.mtk.nao.ac.jp/., 34 pages, 20 figures, 7 tables, moderate revision, accepted for publication in PASJ

Published
2017

46. A wide field-of-view crossed Dragone optical system using the anamorphic aspherical surfaces

Author

Masashi Hazumi, Hajime Sugai, Nobuhiko Katayama, Yutaro Sekimoto, H. Imada, Tomotake Matsumura, and Shingo Kashima

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Field of view, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, 010309 optics, Radio telescope, Telescope, Optics, law, 0103 physical sciences, Electrical and Electronic Engineering, Engineering (miscellaneous), Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Strehl ratio, 021001 nanoscience & nanotechnology, Polarization (waves), Physical optics, Atomic and Molecular Physics, and Optics, Cardinal point, 0210 nano-technology, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A side-fed crossed Dragone telescope provides a wide field-of-view. This type of a telescope is commonly employed in the measurement of cosmic microwave background (CMB) polarization, which requires an image-space telecentric telescope with a large focal plane over broadband coverage. We report the design of the wide field-of-view crossed Dragone optical system using the anamorphic aspherical surfaces with correction terms up to the 10th order. We achieved the Strehl ratio larger than 0.95 over 32 by 18 square degrees at 150 GHz. This design is an image-space telecentric and fully diffraction-limited system below 400 GHz. We discuss the optical performance in the uniformity of the axially symmetric point spread function and telecentricity over the field-of-view. We also address the analysis to evaluate the polarization properties, including the instrumental polarization, extinction rate, and polarization angle rotation. This work is a part of programs to design a compact multi-color wide field-of-view telescope for LiteBIRD, which is a next generation CMB polarization satellite., Comment: 7 pages, 10 figures, submitted to Applied Optics

Published
2017
Full Text
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47. Making maps of cosmic microwave background polarization for B-mode studies: the POLARBEAR example

Author

Eric V. Linder, Josquin Errard, Davide Poletti, Tucker Elleflot, Osamu Tajima, Giulio Fabbian, Theodore Kisner, Julian Borrill, Maude Le Jeune, Grantland Hall, Aritoki Suzuki, Akito Kusaka, L. Howe, Praween Siritanasak, Yuji Chinone, Ari Cukierman, Brian Keating, D. Leon, M. Navaroli, Kam Arnold, Reijo Keskitalo, Giuseppe Puglisi, Bryan Steinbach, Stephen M. Feeney, Frederick Matsuda, Colin Ross, J. Peloton, Nathan Whitehorn, Charles Hill, Andrew H. Jaffe, Masashi Hazumi, Christian L. Reichardt, John Groh, Neil Goeckner-Wald, Yuki Inoue, Scott Chapman, Darcy Barron, L. N. Lowry, Nathan Stebor, Masaya Hasegawa, Oliver Jeong, S. Beckman, Hans P. Paar, Carlo Baccigalupi, Nobuhiko Katayama, Grant Teply, Radek Stompor, A. Ducout, Adrian T. Lee, Science and Technology Facilities Council, Science and Technology Facilities Council (STFC), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Poletti, D, Fabbian, G, Le Jeune, M, Peloton, J, Arnold, K, Baccigalupi, C, Barron, D, Beckman, S, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, Ducout, A, Elleflot, T, Errard, J, Feeney, S, Goeckner-Wald, N, Groh, J, Hall, G, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaffe, A, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kisner, T, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Matsuda, F, Navaroli, M, Paar, H, Puglisi, G, Reichardt, C, Ross, C, Siritanasak, P, Stebor, N, Steinbach, B, Stompor, R, Suzuki, A, Tajima, O, Teply, G, and Whitehorn, N

Subjects
Computer science, POWER SPECTRUM, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, cosmic background radiation: polarization, cosmic background radiation, STATISTICAL-ANALYSIS, 01 natural sciences, Spectral line, estimator, 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], media_common, Settore FIS/05, Estimator, Polarization (waves), observations [cosmology], 3. Good health, PLANCK, B-mode, DATA SETS, Cosmology: Observation, Physical Sciences, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, cosmology: observations, performance, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Infrasound, FOS: Physical sciences, Astronomy & Astrophysics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, DESTRIPING TECHNIQUE, structure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], FIELD, numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), Science & Technology, 010308 nuclear & particles physics, MAKING ALGORITHM, Astronomy and Astrophysics, 0201 Astronomical And Space Sciences, frequency: low, Space and Planetary Science, Sky, correlation, atmosphere, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract

Analysis of cosmic microwave background (CMB) datasets typically requires some filtering of the raw time-ordered data. Filtering is frequently used to minimize the impact of low frequency noise, atmospheric contributions and/or scan synchronous signals on the resulting maps. In this work we explicitly construct a general filtering operator, which can unambiguously remove any set of unwanted modes in the data, and then amend the map-making procedure in order to incorporate and correct for it. We show that such an approach is mathematically equivalent to the solution of a problem in which the sky signal and unwanted modes are estimated simultaneously and the latter are marginalized over. We investigate the conditions under which this amended map-making procedure can render an unbiased estimate of the sky signal in realistic circumstances. We then study the effects of time-domain filtering on the noise correlation structure in the map domain, as well as impact it may have on the performance of the popular pseudo-spectrum estimators. We conclude that although maps produced by the proposed estimators arguably provide the most faithful representation of the sky possible given the data, they may not straightforwardly lead to the best constraints on the power spectra of the underlying sky signal and special care may need to be taken to ensure this is the case. By contrast, simplified map-makers which do not explicitly correct for time-domain filtering, but leave it to subsequent steps in the data analysis, may perform equally well and be easier and faster to implement. We focus on polarization-sensitive measurements targeting the B-mode component of the CMB signal and apply the proposed methods to realistic simulations based on characteristics of an actual CMB polarization experiment, POLARBEAR., Comment: 26 pages

Published
2016

48. Demonstration of the broadband half-wave plate using the nine-layer sapphire for the cosmic microwave background polarization experiment

Author

Hirokazu Ishino, Tomotake Matsumura, Nobuhiko Katayama, Hiroaki Imada, Yuki Sakurai, and K. Komatsu

Subjects
Materials science, business.industry, Mechanical Engineering, Cosmic microwave background, Phase (waves), Astronomy and Astrophysics, Polarization (waves), 01 natural sciences, Waveplate, Electronic, Optical and Magnetic Materials, law.invention, 010309 optics, Optics, Space and Planetary Science, Control and Systems Engineering, Achromatic lens, law, 0103 physical sciences, Broadband, Extremely high frequency, Sapphire, business, 010303 astronomy & astrophysics, Instrumentation
Abstract

We report the development of the achromatic half-wave plate (AHWP) at millimeter wave for cosmic microwave background polarization experiments. We fabricate an AHWP consisting of nine a-cut sapphire plates based on the Pancharatnam recipe to cover a wide frequency range. The modulation efficiency and the phase are measured in a frequency range of 33 to 260 GHz with incident angles up to 10 degrees. We find the measurements at room temperature are in good agreement with the predictions. This is the broadest demonstration of the AHWP at the millimeter wave.

Published
2019

49. Development of a contact-less cryogenic rotation mechanism employed for a polarization modulator unit in cosmic microwave background polarization experiments

Author

H. Enokida, T. Iida, Yuki Sakurai, Hiroyuki Ohsaki, Yukimasa Hirota, Tomotake Matsumura, K. Komatsu, Hajime Sugai, Yutaka Terao, and Nobuhiko Katayama

Subjects
Physics, History, Optics, business.industry, Cosmic microwave background, business, Polarization (waves), Computer Science Applications, Education
Abstract

We present the design and the performance of a contact-less cryogenic rotation mechanism used in cosmic microwave background (CMB) experiments. A precise measurement of the CMB polarization is possible to verify the cosmic inflation theory that describes the very beginning (10−38 seconds) of the early universe. The polarization modulator, that rotates a half wave plate continuously at the aperture of the telescope, is one of the key instruments in the experiments. In order to reduce noise and systematic uncertainties, the polarization modulator is required a stable rotation with minimal heat dissipation in a cryogenic environment less than 20 K. Thus, we adopted the rotation mechanism that combines completely contact-less bearing and motor, a superconducting magnetic bearing, and a hollow bore synchronous motor. The heat dissipation and the load torque due to the friction can be minimized by avoiding physical contacts. We constructed the prototype of the rotation mechanism and carried out mechanical and thermal performance tests. A continuous rotation test in cryogenic temperature is performed, and it is confirmed that the rotation stability is less than 1% with the rotation frequency between 0.5 Hz and 3.0 Hz. We also conducted a thermal performance test, and obtained the heat dissipation at the rotor of 9.0 mW. We discussed the reduction of heat dissipation using a developed magnetic circuit with improved magnetic field uniformity.

Published
2019

50. Evaluation of loss characteristics of superconducting magnetic bearings for LiteBIRD satellite by three-dimensional finite element method analysis

Author

Hajime Sugai, Hiroyuki Ohsaki, Yasunori Terao, Nobuhiko Katayama, Tomotake Matsumura, H. Enokida, Y. Hirota, and Yuki Sakurai

Subjects
Superconductivity, History, Materials science, business.industry, Magnetic bearing, Finite element method analysis, Satellite, Aerospace engineering, business, Computer Science Applications, Education
Abstract

The polarization modulator of LiteBIRD satellite is required to be used by continuously rotating the half-wave retarder under a low temperature environment of about 10 K. Then, it becomes an important issue to reduce heat generation due to rotation loss. Therefore, a rotation mechanism in a cryogenic environment by a superconducting magnetic bearing (SMB) using the pinning effect of the bulk superconductor has been studied. In SMB, because of the pinning effect of superconductor, it is possible to rotate the half-wave retarder with stably floating, and it is possible to avoid frictional heat due to contact. The half-wave retarder is incorporated inside the rotating part of the superconducting magnetic bearing composed of the permanent magnet ring and the iron yoke. At this time, since the permanent magnet ring divides the parallel magnetized permanent magnets into pieces, a gap is formed at the joint of the permanent magnets. For this reason, the magnetic field distribution generated by the permanent magnet ring is not uniform. Although SMB can reduce friction as compared to mechanical bearings, the magnetic properties of the bulk superconductor change due to the magnetic field fluctuation caused by such ununiformity of the magnetic field, resulting in energy loss. In this study, heat generation in bulk superconductor in SMB is evaluated by three-dimensional finite element method. First, using JMAG Designer 17.0, the magnetic field distribution created by the rotor side is obtained by static magnetic field analysis. Next, using the COMSOL Multiphysics 5.3a, by applying the magnetic field distribution created by the rotor side obtained above and rotate the magnetic field, the loss generated in the bulk superconductor is investigated. The resulting loss value satisfied the required value.

Published
2019

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