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1. The Simons Observatory: Design, Integration, and Testing of the Small Aperture Telescopes

Author

Nicholas Galitzki, Tran Tsan, Jake Spisak, Michael Randall, Max Silva-Feaver, Joseph Seibert, Jacob Lashner, Shunsuke Adachi, Sean M. Adkins, Thomas Alford, Kam Arnold, Peter C. Ashton, Jason E. Austermann, Carlo Baccigalupi, Andrew Bazarko, James A. Beall, Sanah Bhimani, Bryce Bixler, Gabriele Coppi, Lance Corbett, Kevin D. Crowley, Kevin T. Crowley, Samuel Day-Weiss, Mark J. Devlin, Simon Dicker, Brooke DiGia, Peter N. Dow, Cody J. Duell, Shannon M. Duff, Remington G. Gerras, John C. Groh, Jon E. Gudmundsson, Kathleen Harrington, Masaya Hasegawa, Erin Healy, Shawn W. Henderson, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keating, Ben Keller, Kenji Kiuchi, Anna M. Kofman, Brian J. Koopman, Akito Kusaka, Adrian T. Lee, Richard A. Lew, Lawrence T. Lin, Michael J. Link, Tammy J. Lucas, Marius Lungu, Aashrita Mangu, Jeffrey J McMahon, Amber D. Miller, Jenna E. Moore, Magdy Morshed, Hironobu Nakata, Federico Nati, Laura B. Newburgh, David V. Nguyen, Michael D. Niemack, Lyman A. Page, Kana Sakaguri, Yuki Sakurai, Mayuri Sathyanarayana Rao, Lauren J. Saunders, Jordan E. Shroyer, Junna Sugiyama, Osamu Tajima, Atsuto Takeuchi, Refilwe Tanah Bua, Grant Teply, Tomoki Terasaki, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Yuhan Wang, Zhilei Xu, Kyohei Yamada, and Kaiwen Zheng

Subjects
Cosmic microwave background radiation, Millimeter astronomy, Ground telescopes, Telescopes, Astrophysics, QB460-466
Abstract

The Simons Observatory (SO) is a cosmic microwave background survey experiment that includes small-aperture telescopes (SATs) observing from an altitude of 5200 m in the Atacama Desert in Chile. The SO SATs will cover six spectral bands between 27 and 280 GHz to search for primordial B-modes to a sensitivity of σ ( r ) = 0.002, with quantified systematic errors well below this value. Each SAT is a self-contained cryogenic telescope with a 35° field of view, 42 cm diameter optical aperture, 40 K half-wave plate, 1 K refractive optics, and 12,000 transition edge sensor detectors. We describe the nominal design of the SATs and present details about the integration and testing for one operating at 93 and 145 GHz.

Published
2024
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2. The Simons Observatory: Gain, Bandpass and Polarization-angle Calibration Requirements for B-mode Searches

Author

Maximilian H Abitbol, David Alonso, Sara M Simon, Jack Lashner, Kevin T Crowley, Aamir M Ali, Susanna Azzoni, Carlo Baccigalupi, Darcy Barron, Michael L Brown, Erminia Calabrese, Julien Carron, Yuji Chinone, Jens Chluba, Gabriele Coppi, Kevin D Crowley, Mark Devlin, Jo Dunkley, Josquin Errard, Valentina Fanfani, Nicholas Galitzki, Martina Gerbino, J Colin Hill, Bradley R Johnson, Baptiste Jost, Brian Keating, Nicoletta Krachmalnicoff, Akito Kusaka, Adrian T Lee, Thibaut Louis, Mathew S Madhavacheril, Heather McCarrick, Jeffrey McMahon, P Daniel Meerburg, Federico Nati, Haruki Nishino, Lyman A Page, Davide Poletti, Giuseppe Puglisi, Michael J Randall, Aditya Rotti, Jacob Spisak, Aritoki Suzuki, Grant P Teply, Clara Verges, Edward J Wollack, Zhilei Xu, and Mario Zannoni

Subjects
Astrophysics
Published
2021
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3. Development of the Characterization Methods Without Electrothermal Feedback for TES Bolometers for CMB Measurements

Author

Yume Nishinomiya, Akito Kusaka, Kenji Kiuchi, Tomoki Terasaki, Johannes Hubmayr, Adrian Lee, Heather McCarrick, Aritoki Suzuki, and Benjamin Westbrook

Subjects
FOS: Physical sciences, General Materials Science, Astrophysics - Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Atomic and Molecular Physics, and Optics
Abstract

Superconducting Transition-Edge Sensor (TES) bolometers are used for cosmic microwave background (CMB) observations. We used a testbed to evaluate the thermal performance of TES bolometers in regard to the saturation power Psat and intrinsic thermal time constant tau0. We developed an evaluation method that is complementary to methods with electrothermal feedback. In our method, the antenna termination resistor of the bolometer is directly biased with DC or AC electric power to simulate optical power, and the TES is biased with small power, which allows Psat and tau0 to be determined without contribution from the negative electrothermal feedback. We describe the method and results of the measurement using it. We evaluated Psat of five samples by applying DC power and confirmed the overall trend between Psat and the inverse leg length. We evaluated tau0 of the samples by applying DC plus AC power, and the measured value was reasonable in consideration of the expected values of other TES parameters. This evaluation method enables us to verify whether a TES has been fabricated with the designed values and to provide feedback for fabrication for future CMB observations., 7 pages, 6 figures, LTD19 Conference Proceedings

Published
2022

4. The Cross Correlation of the ABS and ACT Maps

Author

Zack Li, Sigurd Naess, Simone Aiola, David Alonso, John W Appel, J Richard Bond, Erminia Calabrese, Steve K Choi, Kevin T Crowley, Thomas Essinger-Hileman, Shannon M Duff, Joanna Dunkley, J W Fowler, Patricio Gallardo, Shuay-Pwu Patty Ho, Johannes Hubmayr, Akito Kusaka, Thibaut Louis, Mathew S Madhavacheril, Jeffrey McMahon, Federico Nati, Michael D Niemac, Lyman Page, Lucas Parker, Bruce Partridge, Maria Salatino, Jonathan L Sievers, Cristobal Sifon, Sara M Simon, Suzanne T Staggs, Emilie Storer, and Edward J Wollack

Subjects
Astrophysics
Abstract

One of the most important checks for systematic errors in CMB studies is the cross correlation of maps made by independent experiments. In this paper, we report on the cross correlation between maps from the Atacama B-mode Search (ABS) and Atacama Cosmology Telescope (ACT) experiments in both temperature and polarization. These completely different measurements have a clear correlation with each other and with the Planck satellite in both the EE and TE spectra at l < 400 over the roughly 1100 deg(exp 2) common to all three. The TB, EB, and BB cross spectra are consistent with noise. Exploiting such cross-correlations will be important for future experiments operating in Chile that aim to probe the 30 < l < 8,000 range.

Published
2020
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5. Small Aperture Telescopes for the Simons Observatory

Author

Aamir M. Ali, Shunsuke Adachi, Kam Arnold, Peter Ashton, Andrew Bazarko, Yuji Chinone, Gabriele Coppi, Lance Corbett, KevinD Crowley, Kevin T Crowley, Mark Devlin, Simon Dicker, Shannon Duff, Chris Ellis, Nicholas Galitzki, Neil Goeckner-Wald, Kathleen Harrington, Erin Healy, Charles A Hill, Shuay-Pwu Patty Ho, Johannes Hubmayr, Brian Keating, Kenji Kiuchi, Akito Kusaka, Adrian T Lee, Michael Ludlam, Aashrita Mangu, Frederick Matsuda, Heather McCarrick, Federico Nati, Michael D. Niemack, Haruki Nishino, John Orlowski-Scherer, MayuriSathyanarayana Rao, Christopher Raum, YukiSakurai, Maria Salatino, Trevor Sasse, Joseph Seibert, Carlos Sierra, Maximiliano Silva-Feaver, Jacob Spisak, Sara M Simon, Suzanne Staggs, Osamu Tajima, ·Grant Teply, Tran Tsan, Edward Wollack, Bejamin Westbrook, Zhilei Xu, Mario Zannoni, and Ningfeng Zhu

Subjects
Instrumentation And Photography
Abstract

The Simons Observatory (SO) is an upcoming cosmic microwave background(CMB) experiment located on Cerro Toco, Chile, that will map the microwave sky in temperature and polarization in six frequency bands spanning 27 to 285 GHz. SO will consist of one 6-meter Large Aperture Telescope (LAT) fielding∼30,000 detectors and an array of three 0.42-meter Small Aperture Telescopes (SATs) fielding an additional 30,000 detectors. This synergy will allow for the extremely sensitive characterization of the CMB over an-gular scales ranging from an arcmin to tens of degrees, enabling a wide range of scientific output. Here we focus on the SATs targeting degree angular scales with successive dichroic instruments observing at Mid-Frequency (MF: 93/145 GHz), Ultra-High-Frequency (UHF:225/285 GHz), and Low-Frequency (LF: 27/39 GHz). The three SATs will be able to map∼10% of the sky to a noise level of∼2 μK-arcmin when combining 93 and 145 GHz. The multiple frequency bands will allow the CMB to be separated from galactic foregrounds (primarily synchrotron and dust), with the primary science goal of characterizing the primordial tensor-to-scalar ratio, r, at a target level ofσ(r)≈0.003.

Published
2020
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7. 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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9. 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

10. Development of Large Array of Kinetic Inductance Detectors Using Commercial-Class External Foundries

Author

C. Otani, Shugo Oguri, Satoru Mima, Kenji Kiuchi, and Akito Kusaka

Subjects
Materials science, Fabrication, business.industry, Coplanar waveguide, Ranging, Condensed Matter Physics, Chip, 01 natural sciences, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, Frequency-division multiplexing, Resonator, 0103 physical sciences, Optoelectronics, General Materials Science, Wafer, Dilution refrigerator, 010306 general physics, business
Abstract

This study focuses on kinetic inductance detectors (KIDs) fabricated in external foundries using 6 and 8-inch processes. These processes allow us to fabricate large arrays of KIDs in a scalable manner. The support of such a wide variety of astronomical and particle-physics applications requires large numbers of superconducting detectors. For example, the sensitivity of the cosmic microwave background measurements has exponentially improved over the past few decades. The most significant advantage of KIDs is scalability to a large array due to the intrinsic frequency multiplexing scheme. The first step of fabricating a large array of KIDs is designing test chips to check the performance of the 6 and 8-inch micro-electro-mechanical system processes. The KIDs are made of a single pure aluminum film and consist of coplanar waveguide quarter wavelength resonators with a feedline. Each wafer is filled with 32 chips, where the chip size is 20 × 20 mm2, with 48 resonators on each chip. The chips are evaluated using a dilution refrigerator at temperatures ranging from 100 to 500 mK. The quality factor of the resonators, temperature dependency of the resonance frequency, and yields are comparable with those of the KIDs fabricated in a dedicated clean room for superconducting detectors.

Published
2020

11. 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

12. Simons Observatory Microwave SQUID Multiplexing Readout: Cryogenic RF Amplifier and Coaxial Chain Design

Author

Suzanne T. Staggs, Maria Salatino, Shuay-Pwu Patty Ho, Justin Mathewson, Trevor Sasse, Zhilei Xu, Jenna Moore, Philip Daniel Mauskopf, Aashrita Mangu, Nicholas Galitzki, Ningfeng Zhu, Shawn W. Henderson, Kam Arnold, Akito Kusaka, Bradley Dober, Maximiliano Silva-Feaver, Peter Ashton, Shannon M. Duff, Heather McCarrick, Eve M. Vavagiakis, Michael D. Niemack, Jonathan Hoh, Christopher Raum, Aamir Ali, Benjamin Westbrook, Joel N. Ullom, Grant Teply, Erin Healy, Jason R. Stevens, Adrian T. Lee, Cody J. Duell, Sara M. Simon, A. M. Kofman, Mayuri Sathyanarayana Rao, Joseph Seibert, and Robert Thornton

Subjects
Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Coaxial cable, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Multiplexing, 010305 fluids & plasmas, law.invention, law, biology.animal, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Squid, biology, business.industry, RF power amplifier, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Optoelectronics, Transition edge sensor, Coaxial, Astrophysics - Instrumentation and Methods for Astrophysics, business, Microwave
Abstract

The Simons Observatory (SO) is an upcoming polarization-sensitive Cosmic Microwave Background (CMB) experiment on the Cerro Toco Plateau (Chile) with large overlap with other optical and infrared surveys (e.g., DESI, LSST, HSC). To enable the readout of \bigO(10,000) detectors in each of the four telescopes of SO, we will employ the microwave SQUID multiplexing technology. With a targeted multiplexing factor of \bigO{(1,000)}, microwave SQUID multiplexing has never been deployed on the scale needed for SO. Here we present the design of the cryogenic coaxial cable and RF component chain that connects room temperature readout electronics to superconducting resonators that are coupled to Transition Edge Sensor bolometers operating at sub-Kelvin temperatures. We describe design considerations including cryogenic RF component selection, system linearity, noise, and thermal power dissipation., 10 pages, 2 figures

Published
2020

13. 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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14. A cryogenic continuously rotating half-wave plate mechanism for the POLARBEAR-2b cosmic microwave background receiver

Author

Tomotake Matsumura, Peter Ashton, Yuki Sakurai, S. Ganjam, Kam Arnold, Charles A. Hill, B. Bixler, Y. Zhou, Frederick Matsuda, Adrian T. Lee, Tylor Adkins, R. Tat, P. Barton, and Akito Kusaka

Subjects
Cryostat, Electric motor, Cosmic microwave background, FOS: Physical sciences, 7. Clean energy, 01 natural sciences, Waveplate, Radio spectrum, 010305 fluids & plasmas, Optics, Engineering, 0103 physical sciences, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Applied Physics, 010302 applied physics, Physics, Rotary encoder, business.industry, Detector, Polarization (waves), Physical Sciences, Chemical Sciences, business, Astrophysics - Instrumentation and Methods for Astrophysics, astro-ph.IM
Abstract

We present the design and laboratory evaluation of a cryogenic continuously rotating half-wave plate (CHWP) for the POLARBEAR-2b (PB-2b) cosmic microwave background (CMB) receiver, the second installment of the Simons Array. PB-2b will observe at 5,200 m elevation in the Atacama Desert of Chile in two frequency bands centered at 90 and 150 GHz. In order to suppress atmospheric 1/f noise and mitigate systematic effects that arise when differencing orthogonal detectors, PB-2b modulates linear sky polarization using a CHWP rotating at 2 Hz. The CHWP has a 440 mm clear aperture diameter and is cooled to $\approx$ 50 K in the PB-2b receiver cryostat. It consists of a low-friction superconducting magnetic bearing (SMB) and a low-torque synchronous electromagnetic motor, which together dissipate < 2 W. During cooldown, a grip-and-release mechanism centers the rotor to < 0.5 mm, and during continuous rotation, an incremental optical encoder measures the rotor angle with a noise level of 0.1 $\mathrm{��rad / \sqrt{Hz}}$. We discuss the experimental requirements for the PB-2b CHWP, the designs of its various subsystems, and the results of its evaluation in the laboratory. The presented CHWP has been deployed to Chile and is expected to see first light on PB-2b in 2020 or 2021., PREPRINT. Submitted to Review of Scientific Instruments, September 2020. v2 updates refs 41-42

Published
2020

15. Detector and readout characterization for POLARBEAR-2b

Author

Charles A. Hill, Masashi Hazumi, Kayla Mitchell, M. Navaroli, Kam Arnold, P. Siritanasak, Oliver Jeong, Jennifer Ito, Calvin Tsai, A. T. P. Pham, Trevor Sasse, Darcy Barron, Christopher Raum, L. N. Lowry, Tucker Elleflot, Carlo Baccigalupi, Aritoki Suzuki, Akito Kusaka, Joseph Seibert, B. Bixler, Brian Keating, Yuji Chinone, L. Howe, Kevin T. Crowley, Benjamin Westbrook, Christian L. Reichardt, John Groh, Adrian T. Lee, Tylor Adkins, S. Takakura, and Grant Teply

Subjects
Physics, Gravitational wave, business.industry, Detector, Cosmic microwave background, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Multiplexing, law.invention, Telescope, Resonator, Optics, law, Astrophysics::Earth and Planetary Astrophysics, Antenna (radio), business, Astrophysics::Galaxy Astrophysics
Abstract

The Simons Array is a set of three millimeter-wavelength telescopes in the Atacama Desert in northern Chile. It is designed to measure the polarization of the cosmic microwave background caused by density perturbations, gravitational lensing, and primordial gravitational waves. Polarbear-2b (PB-2b) is the receiver that will be mounted onto the Paul Simons Telescope, the second Simons Array telescope. Each pixel in the PB-2b focal plane has a broadband sinuous antenna coupled to transition-edge sensor (TES) bolometers. In all, there are more than 7,500 antenna-coupled TES bolometers which are biased and read out using a digital frequency-domain multiplexing framework. We implement a multiplexing factor of 40 with resonator frequencies ranging from 1.6 MHz to 4.6 MHz. These resonators are connected to superconducting quantum interference device arrays that provide a signal amplification stage. We present Polarbear-2b detector and readout characterization results from in-lab testing that enabled the deployment of PB-2b to Chile in March 2020.

Published
2020

16. Data acquisition and management system for the CMB polarization experiment: Simons Array

Author

Theodore Kisner, P. Siritanasak, Nathan Whitehorn, Kevin T. Crowley, Y. Zhou, Daisuke Kaneko, Tucker Elleflot, Akito Kusaka, Benjamin Westbrook, Alexandra S. Rahlin, S. Takakura, L. Howe, Haruaki Hirose, H. Nishino, John Groh, Joshua Montgomery, Masashi Hazumi, Masaya Hasegawa, Darcy Barron, S. Kikuchi, A. Zahn, Charles A. Hill, D. Tanabe, S. Takatori, Graeme Smecher, Amy N. Bender, and Yuji Chinone

Subjects
Data acquisition, business.industry, Observatory, Computer science, Data management, Cosmic microwave background, Real-time computing, Bandwidth (signal processing), Management system, business, Data rate, Raw data
Abstract

The Simons Array upgrades the POLARBEAR experiment, which measures the cosmic microwave background from the Atacama Desert in Chile, with three newly developed receivers. Each receiver has 7,588 transition-edge sensor bolometers with a raw data rate of approximately 20 MB/s. This significantly increased data rate required us to develop a new data-acquisition (DAQ) and data-management system. As the network bandwidth from our observatory to our data-storage sites outside Chile is not high enough to send all the raw data, we compress the raw data on-site. The expected yearly compressed data rate is approximately 60 TB from each receiver. We have also developed a new housekeeping DAQ system. The new housekeeping DAQ system is a distributed system to handle the various newly added monitoring systems and to better understand our instruments and environments. Those data can also be fetched by another module for real-time monitoring of our instrument from all over the world with latencies on the order of minutes. We deployed the first receiver in late 2018 and started the commissioning of the DAQ system. The DAQ system has been working without significant problems and already accumulates a considerable amount of the new receiver data from the commissioning observations. In this presentation, we summarize and report the status of the new systems.

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. The Simons Observatory: A large-diameter truss for a refracting telescope cooled to 1 K

Author

Kevin D. Crowley, Peter Dow, Jordan E. Shroyer, John C. Groh, Bradley Dober, Jacob Spisak, Nicholas Galitzki, Tanay Bhandarkar, Mark J. Devlin, Simon Dicker, Patricio A. Gallardo, Kathleen Harrington, Jeffrey Iuliano, Bradley R. Johnson, Delwin Johnson, Anna M. Kofman, Akito Kusaka, Adrian Lee, Michele Limon, Federico Nati, John Orlowski-Scherer, Lyman Page, Michael Randall, Grant Teply, Tran Tsan, Edward J. Wollack, Zhilei Xu, Ningfeng Zhu, Crowley, K, Dow, P, Shroyer, J, Groh, J, Dober, B, Spisak, J, Galitzki, N, Bhandarkar, T, Devlin, M, Dicker, S, Gallardo, P, Harrington, K, Iuliano, J, Johnson, B, Johnson, D, Kofman, A, Kusaka, A, Lee, A, Limon, M, Nati, F, Orlowski-Scherer, J, Page, L, Randall, M, Teply, G, Tsan, T, Wollack, E, Xu, Z, and Zhu, N

Subjects
Instrumentation, CMB, cosmology, telescopes
Abstract

We present the design and measured performance of a new carbon fiber strut design that is used in a cryogenically cooled truss for the Simons Observatory small aperture telescope. The truss consists of two aluminum 6061 rings separated by 24 struts. Each strut consists of a central carbon fiber tube fitted with two aluminum end caps. We tested the performance of the strut and truss by (i) cryogenically cycling and destructively pull-testing strut samples, (ii) non-destructively pull-testing the final truss, and (iii) measuring the thermal conductivity of the carbon fiber tubes. We found that the strut strength is limited by the mounting fasteners and the strut end caps, not the epoxy adhesive or the carbon fiber tube. This result is consistent with our numerical predictions. Our thermal measurements suggest that the conductive heat load through the struts (from 4 to 1 K) will be less than 1 mW. This strut design may be a promising candidate for use in other cryogenic support structures.

Published
2022

19. Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment

Author

Peter A. R. Ade, Davide Poletti, C. Verges, Shunsuke Adachi, Kam Arnold, Yuji Chinone, A. Suzuki, Yuto Minami, Chang Feng, J. Peloton, Nathan Whitehorn, Oliver Jeong, N. W. Halverson, Yuki Inoue, T. Hamada, Akito Kusaka, Y. Zhou, A. Zahn, A. Cukierman, M. Aguilar, Carole Tucker, D. Beck, Nicoletta Krachmalnicoff, Rolando Dünner, Brian Keating, Paul L. Richards, Stephen M. Feeney, J. C. Groh, Julian Borrill, C. Tsai, Joshua Montgomery, Darcy Barron, Theodore Kisner, R. Stompor, G. Hall, D. Boettger, Tucker Elleflot, Josquin Errard, Frederick Matsuda, L. N. Lowry, D. Leon, Takayuki Tomaru, Reijo Keskitalo, Benjamin Westbrook, M. Navaroli, D. Kaneko, K. Cheung, Osamu Tajima, A. T. P. Pham, Eric V. Linder, Giulio Fabbian, A. J. Gilbert, L. Howe, Neil Goeckner-Wald, H. El-Bouhargani, Max Silva-Feaver, Hans P. Paar, M. A. Dobbs, S. Takatori, Federico Bianchini, Colin Ross, Christian L. Reichardt, John Groh, Praween Siritanasak, Julien Carron, Tomotake Matsumura, T. Fujino, Y. Akiba, H. Nishino, G. Jaehnig, Giuseppe Puglisi, Charles A. Hill, D. Tanabe, Andrew H. Jaffe, Masashi Hazumi, Nicholas Galitzki, Blake D. Sherwin, S. Kikuchi, Carlo Baccigalupi, E. M. Leitch, S. Beckman, N. Katayama, Grant Teply, A. Ducout, Aashrita Mangu, M. LeJeune, Adrian T. Lee, Nathan Stebor, Masaya Hasegawa, S. Takakura, Y. Segawa, Scott Chapman, Kevin T. Crowley, Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, 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, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, 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, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, 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), POLARBEAR, 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
History, satellite: Planck, Cosmic microwave background, gravitational lensing, cosmic background radiation: polarization, detector: noise, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravity waves, power spectrum, 01 natural sciences, Education, Primary mirror, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, Polarization, 0103 physical sciences, Planck, mirror, 010303 astronomy & astrophysics, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Gravitational wave, Settore FIS/05, POLARBEAR experiment, Gravitational effects, gravitational radiation: primordial, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Galaxy, Computer Science Applications, Gravitational lens, B-mode, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy
Abstract

POLARBEAR is a Cosmic Microwave Background radiation (CMB) polarization experiment that is located in the Atacama Desert in Chile. The scientific goals of the experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for B-mode signals created by primordial gravitational waves (PGWs). Polarbear started observations in 2012 and has published a series of results. These include the first measurement of a nonzero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In addition, we have achieved the first measurement of crosscorrelation between the lensing potential, which was reconstructed from the CMB polarization data alone by Polarbear, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. In 2014, we installed a continuously rotating half-wave plate (CRHWP) at the focus of the primary mirror to search for PGWs and demonstrated the control of low-frequency noise. We have found that the low-frequency B-mode power in the combined dataset with the Planck high-frequency maps is consistent with Galactic dust foreground, thus placing an upper limit on the tensor-to-scalar ratio of r < 0.90 at the 95% confidence level after marginalizing over the foregrounds.

Published
2020

20. The cross correlation of the ABS and ACT maps

Author

Johannes Hubmayr, Mathew S. Madhavacheril, Shannon M. Duff, Sigurd Naess, Emilie Storer, Lucas Parker, Edward J. Wollack, Jonathan Sievers, Suzanne T. Staggs, Akito Kusaka, Patricio A. Gallardo, Thibaut Louis, Lyman A. Page, Sara M. Simon, Maria Salatino, Simone Aiola, Joseph W. Fowler, Joanna Dunkley, David Alonso, Thomas Essinger-Hileman, John W. Appel, Jeff McMahon, Kevin T. Crowley, Bruce Partridge, Shuay-Pwu Patty Ho, Michael D. Niemack, Cristóbal Sifón, J. Richard Bond, Zack Li, Erminia Calabrese, Steve K. Choi, Federico Nati, 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), Li, Z, Naess, S, Aiola, S, Alonso, D, Appel, J, Bond, J, Calabrese, E, Choi, S, Crowley, K, Essinger-Hileman, T, Duff, S, Dunkley, J, Fowler, J, Gallardo, P, Ho, S, Hubmayr, J, Kusaka, A, Louis, T, Madhavacheril, M, Mcmahon, J, Nati, F, Niemack, M, Page, L, Parker, L, Partridge, B, Salatino, M, Sievers, J, Sifon, C, Simon, S, Staggs, S, Storer, E, Wollack, E, 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Spectral line, symbols.namesake, 0103 physical sciences, Planck, 010306 general physics, 010303 astronomy & astrophysics, CMBR polarization, Physics, Cross-correlation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Polarization (waves), Atacama Cosmology Telescope, symbols, CMBR experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio), CMBR detector, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

One of the most important checks for systematic errors in CMB studies is the cross correlation of maps made by independent experiments. In this paper we report on the cross correlation between maps from the Atacama B-mode Search (ABS) and Atacama Cosmology Telescope (ACT) experiments in both temperature and polarization. These completely different measurements have a clear correlation with each other and with the Planck satellite in both the EE and TE spectra at $\ell, Comment: 7 pages, 5 figures. For an interactive demonstration of the methods, see https://colab.research.google.com/drive/1CnMGLn-J3pySv8A9ffNWDSlXlJWMrp2W

Published
2020

21. Small Aperture Telescopes for the Simons Observatory

Author

Osamu Tajima, Johannes Hubmayr, Suzanne T. Staggs, Aamir Ali, Bejamin Westbrook, Kam Arnold, Trevor Sasse, Charles A. Hill, Frederick Matsuda, Tran Tsan, Kenji Kiuchi, Grant Teply, Andrew Bazarko, Federico Nati, Yuji Chinone, Joseph Seibert, Carlos Sierra, Nicholas Galitzki, Zhilei Xu, Peter Ashton, Ningfeng Zhu, Erin Healy, Haruki Nishino, Sara M. Simon, Shannon M. Duff, Kevin D. Crowley, Mario Zannoni, Edward J. Wollack, Jacob Spisak, Michael D. Niemack, John Orlowski-Scherer, Christopher Raum, Lance Corbett, Adrian T. Lee, Aashrita Mangu, Kathleen Harrington, Michael Ludlam, Yuki Sakurai, Shunsuke Adachi, Gabriele Coppi, Maria Salatino, Neil Goeckner-Wald, Mayuri Sathyanarayana Rao, Maximiliano Silva-Feaver, Mark J. Devlin, Christopher G. Ellis, Heather McCarrick, Kevin T. Crowley, Shuay-Pwu Patty Ho, Akito Kusaka, Brian Keating, Simon Dicker, Ali, A, Adachi, S, Arnold, K, Ashton, P, Bazarko, A, Chinone, Y, Coppi, G, Corbett, L, Crowley, K, Devlin, M, Dicker, S, Duff, S, Ellis, C, Galitzki, N, Goeckner-Wald, N, Harrington, K, Healy, E, Hill, C, Ho, S, Hubmayr, J, Keating, B, Kiuchi, K, Kusaka, A, Lee, A, Ludlam, M, Mangu, A, Matsuda, F, Mccarrick, H, Nati, F, Niemack, M, Nishino, H, Orlowski-Scherer, J, Sathyanarayana Rao, M, Raum, C, Sakurai, Y, Salatino, M, Sasse, T, Seibert, J, Sierra, C, Silva-Feaver, M, Spisak, J, Simon, S, Staggs, S, Tajima, O, Teply, G, Tsan, T, Wollack, E, Westbrook, B, Xu, Z, Zannoni, M, and Zhu, N

Subjects
Small aperture telescope, TES, Refractor, Simons Observatory, Cosmic microwave background, CMB, Inflation, Cosmology, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Radio spectrum, 010305 fluids & plasmas, law.invention, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, law, Observatory, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, media_common, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Sky, Refracting telescope, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Simons Observatory (SO) is an upcoming cosmic microwave background (CMB) experiment located on Cerro Toco, Chile, that will map the microwave sky in temperature and polarization in six frequency bands spanning 27 to 285 GHz. SO will consist of one 6-m large aperture telescope fielding $$\sim$$ 30,000 detectors and an array of three 0.42-m small aperture telescopes (SATs) fielding an additional 30,000 detectors. This synergy will allow for the extremely sensitive characterization of the CMB over angular scales ranging from an arcmin to tens of degrees, enabling a wide range of scientific output. Here we focus on the SATs targeting degree angular scales with successive dichroic instruments observing at mid-frequency (MF: 93/145 GHz), ultra-high-frequency (UHF: 225/285 GHz), and low-frequency (LF: 27/39 GHz). The three SATs will be able to map $$\sim$$ 10% of the sky to a noise level of $$\sim$$ $$2\,\upmu {\hbox {K}}$$ -arcmin when combining 93 and 145 GHz. The multiple frequency bands will allow the CMB to be separated from galactic foregrounds (primarily synchrotron and dust), with the primary science goal of characterizing the primordial tensor-to-scalar ratio, r, at a target level of $$\sigma (r) \approx 0.003$$ .

Published
2020

22. A measurement of the CMB E-mode angular power spectrum at subdegree scales from 670 square degrees of POLARBEAR data

Author

Osamu Tajima, T. Fujino, Andrew H. Jaffe, Scott Chapman, Eric V. Linder, S. Kikuchi, N. Katayama, D. Leon, Masashi Hazumi, Oliver Jeong, D. Tanabe, Grant Teply, Nicholas Galitzki, Tucker Elleflot, S. Takakura, Christian L. Reichardt, Praween Siritanasak, Josquin Errard, Akito Kusaka, Giulio Fabbian, John Groh, Brian Keating, Federico Bianchini, Ben Westbrook, M. A. O. Aguilar Faúndez, Shunsuke Adachi, Ted Kisner, K. Cheung, Adrian T. Lee, Y. Zhou, C. Tsai, Neil Goeckner-Wald, Frederick Matsuda, Tomotake Matsumura, D. Beck, Kam Arnold, Masaya Hasegawa, S. Takatori, Darcy Barron, Carlo Baccigalupi, L. N. Lowry, Davide Poletti, Clara Vergès, Kevin D. Crowley, G. Hall, M. Navaroli, Haruki Nishino, Yuto Minami, Haruaki Hirose, A. T. P. Pham, Chang Feng, Yuji Chinone, H. El Bouhargani, Y. Segawa, M. A. Dobbs, Daisuke Kaneko, 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), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Polarbear, Adachi, S, Aguilar Faundez, M, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Dobbs, M, El Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Hasegawa, M, Hazumi, M, Hirose, H, Jaffe, A, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Kikuchi, S, Kisner, T, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Minami, Y, Navaroli, M, Nishino, H, Pham, A, Poletti, D, Reichardt, C, Segawa, Y, Siritanasak, P, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, 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 de Paris (UP)

Subjects
cosmological model, 010504 meteorology & atmospheric sciences, Cosmic microwave background, cosmic background radiation: polarization, detector: noise, Astrophysics, cosmic background radiation, 01 natural sciences, Physical Chemistry, Atomic, expansion: multipole, Cosmology, Particle and Plasma Physics, Cosmic microwave background radiation, Big Bang nucleosynthesis, polarbear data, polarization: power spectrum, 010303 astronomy & astrophysics, helium: primordial, Physics, Hubble constant, symbols, astro-ph.CO, power spectrum: angular dependence, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics, satellite: Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), nucleosynthesis: big bang, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, statistical analysis, Nucleosynthesis, 0103 physical sciences, Nuclear, Planck, cosmic background radiation: power spectrum, 0105 earth and related environmental sciences, Spectral density, Molecular, Astronomy and Astrophysics, Abundance of the chemical elements, detector: sensitivity, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract

We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from July 2014 to December 2016 with the POLARBEAR experiment. We reach an effective polarization map noise level of $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range $500 \leq \ell, Comment: 15 pages, 5 figures, submitted to ApJ

Published
2020
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23. Commercialization of Micro-fabrication of Antenna-Coupled Transition Edge Sensor Bolometer Detectors for Studies of the Cosmic Microwave Background

Author

Aritoki Suzuki, Nicholas P. Palaio, Natalie A. Roe, Maurice Garcia-Sciveres, Adrian T. Lee, Chris Bebek, Stephen Holland, Leo Steinmetz, and Akito Kusaka

Subjects
General Physics, Fabrication, Physics::Instrumentation and Detectors, Classical Physics, Cosmic microwave background, Micro-fabrication, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Dichroic glass, 01 natural sciences, law.invention, Optics, law, Polarization, 0103 physical sciences, General Materials Science, Wafer, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Mathematical Physics, Physics, 010308 nuclear & particles physics, business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Inflation, Atomic and Molecular Physics, and Optics, TES bolometer, B-mode, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business, astro-ph.IM
Abstract

We report on the development of commercially fabricated multi-chroic antenna coupled Transition Edge Sensor (TES) bolometer arrays for Cosmic Microwave Background (CMB) polarimetry experiments. CMB polarimetry experiments have deployed instruments in stages. Stage-II experiments deployed with O(1,000) detectors and reported successful detection of B-mode (divergent free) polarization pattern in the CMB. Stage-III experiments have recently started observing with O(10,000) detectors with wider frequency coverage. A concept for a Stage-IV experiment, CMB-S4, is emerging to make a definitive measurement of CMB polarization from the ground with O(400,000) detectors. The orders of magnitude increase in detector count for CMB-S4 requires a new approach in detector fabrication to increase fabrication throughput.and reduce cost. We report on collaborative efforts with two commercial micro-fabrication foundries to fabricate antenna coupled TES bolometer detectors. The detector design is based on the sinuous antenna coupled dichroic detector from the POLARBEAR-2 experiment. The TES bolometers showed the expected I-V response and the RF performance agrees with simulation. We will discuss the motivation, design consideration, fabrication processes, test results, and how industrial detector fabrication could be a path to fabricate hundreds of detector wafers for future CMB polarimetry experiments., 5 pages 2 figures Journal of Low Temperature Physics - Special Edition - LTD17 Proceedings

Published
2018

24. Lithographed Superconducting Resonator Development for Next-Generation Frequency Multiplexing Readout of Transition-Edge Sensors

Author

Benjamin Westbrook, Aaron Lee, T. de Haan, Christopher Raum, Aritoki Suzuki, R. Plambeck, B. Neuhauser, Akito Kusaka, and F. Faramarzi

Subjects
Physics, Physics::Instrumentation and Detectors, business.industry, Detector, Bandwidth (signal processing), 02 engineering and technology, 021001 nanoscience & nanotechnology, Condensed Matter Physics, 01 natural sciences, Multiplexing, Atomic and Molecular Physics, and Optics, Frequency-division multiplexing, law.invention, Resonator, Capacitor, law, 0103 physical sciences, Optoelectronics, General Materials Science, Wafer, 010306 general physics, 0210 nano-technology, business, Order of magnitude
Abstract

Ground-based cosmic microwave background (CMB) experiments are undergoing a period of exponential growth. Current experiments are observing with 1000–10,000 detectors, and the next-generation experiment (CMB stage 4) is proposing to deploy approximately 500,000 detectors. This order of magnitude increase in detector count will require a new approach for readout electronics. We have developed superconducting resonators for next-generation frequency-domain multiplexing (fMUX) readout architecture. Our goal is to reduce the physical size of resonators, such that resonators and detectors can eventually be integrated on a single wafer. To reduce the size of these resonators, we have designed spiral inductors and interdigitated capacitors that resonate around 10–100 MHz, an order of magnitude higher frequency compared to current fMUX readout systems. The higher frequency leads to a wider bandwidth and would enable higher multiplexing factor than the current $$\sim $$ 50 detectors per readout channel. We will report on the simulation, fabrication method, characterization technique, and measurement of quality factor of these resonators.

Published
2018

25. The Simons Observatory Microwave SQUID Multiplexing Detector Module Design

Author

Shannon M. Duff, Sarah Marie Bruno, Kaiwen Zheng, Jason E. Austermann, Heather McCarrick, Suzanne T. Staggs, Zachary Atkins, Sara M. Simon, Michael D. Niemack, Megan Gralla, D. Dutcher, Johannes Hubmayr, John A. B. Mates, Bradley R. Johnson, Zachary B. Huber, Leila R. Vale, Nicholas F. Cothard, Jake Connors, A. M. Kofman, Steve K. Choi, Kam Arnold, Nicholas Galitzki, Tammy J. Lucas, Jeff Van Lanen, Kevin D. Crowley, Shawn W. Henderson, Aritoki Suzuki, Yuhan Wang, C. Yu, Edward D. Young, Simon Dicker, Edward J. Wollack, Akito Kusaka, Joel N. Ullom, Bradley Dober, Erin Healy, Zeeshan Ahmed, John Orlowski-Scherer, Adrian T. Lee, Jeffrey Iuliano, Cody J. Duell, Yaqiong Li, Joseph Seibert, Robert Thornton, Jon E. Gudmundsson, Josef Frisch, Ningfeng Zhu, Tomoki Terasaki, Zhilei Xu, Jack Lashner, Tanay Bhandarkar, James A. Beall, Michael J. Link, Shuay-Pwu Patty Ho, Eve M. Vavagiakis, Maximiliano Silva-Feaver, Michael R. Vissers, Gene C. Hilton, Marius Lungu, and Jeff McMahon

Subjects
Physics, Squid, Cosmology and Nongalactic Astrophysics (astro-ph.CO), biology, Physics::Instrumentation and Detectors, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Multiplexing, Optics, Space and Planetary Science, Observatory, biology.animal, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Advances in cosmic microwave background (CMB) science depend on increasing the number of sensitive detectors observing the sky. New instruments deploy large arrays of superconducting transition-edge sensor (TES) bolometers tiled densely into ever larger focal planes. High multiplexing factors reduce the thermal loading on the cryogenic receivers and simplify their design. We present the design of focal-plane modules with an order of magnitude higher multiplexing factor than has previously been achieved with TES bolometers. We focus on the novel cold readout component, which employs microwave SQUID multiplexing ($��$mux). Simons Observatory will use 49 modules containing 60,000 bolometers to make exquisitely sensitive measurements of the CMB. We validate the focal-plane module design, presenting measurements of the readout component with and without a prototype detector array of 1728 polarization-sensitive bolometers coupled to feedhorns. The readout component achieves a $95\%$ yield and a 910 multiplexing factor. The median white noise of each readout channel is 65 $\mathrm{pA/\sqrt{Hz}}$. This impacts the projected SO mapping speed by $< 8\%$, which is less than is assumed in the sensitivity projections. The results validate the full functionality of the module. We discuss the measured performance in the context of SO science requirements, which are exceeded., Accepted to The Astrophysical Journal

Published
2021

26. Internal delensing of cosmic microwave background polarization B-modes with the POLARBEAR experiment

Author

Kam Arnold, Grant Teply, D. Leon, R. Stompor, Neil Goeckner-Wald, Yuji Chinone, D. Beck, J. Borrill, H. El Bouhargani, Kevin T. Crowley, S. Takatori, Toshiya Namikawa, M. A. O. Aguilar Faúndez, Max Silva-Feaver, M. Navaroli, Christian L. Reichardt, J. Peloton, Tucker Elleflot, Josquin Errard, Darcy Barron, Davide Poletti, Osamu Tajima, K. Cheung, C. Verges, L. N. Lowry, N. Katayama, Federico Bianchini, Eric V. Linder, Giulio Fabbian, Praween Siritanasak, Yuto Minami, Brian Keating, Julien Carron, L. Howe, Shunsuke Adachi, Tomotake Matsumura, A. T. P. Pham, Y. Segawa, Carlo Baccigalupi, Aamir Ali, Akito Kusaka, Masaya Hasegawa, Frederick Matsuda, Aaron Lee, Chang Feng, Giuseppe Puglisi, Charles A. Hill, T. Fujino, Y. Akiba, D. Tanabe, S. Kikuchi, H. Nishino, Masashi Hazumi, Blake D. Sherwin, 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), 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), POLARBEAR, 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), 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), Adachi, S, Aguilar Faundez, M, Akiba, Y, Ali, A, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Bianchini, F, Borrill, J, Carron, J, Cheung, K, Chinone, Y, Crowley, K, El Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Goeckner-Wald, N, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Katayama, N, Keating, B, Kikuchi, S, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Minami, Y, Namikawa, T, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stompor, R, Tajima, O, Takatori, S, Tanabe, D, Teply, G, Verges, C, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic Microwave Background Polarization, Cosmic microwave background, FOS: Physical sciences, General Physics and Astronomy, cosmic background radiation: polarization, General Relativity and Quantum Cosmology (gr-qc), Gravitation and Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, B-mode: primordial, Settore FIS/05 - Astronomia e Astrofisica, QB0980, 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), QC, QB, Physics, Settore FIS/05, Polarization (waves), inflation: model, Computational physics, POLARBEAR Experiment, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Instrumentation and Methods for Astrophysics, Variance reduction, Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using only cosmic microwave background polarization data from the POLARBEAR experiment, we measure $B$-mode polarization delensing on subdegree scales at more than $5\sigma$ significance. We achieve a 14% $B$-mode power variance reduction, the highest to date for internal delensing, and improve this result to 2% by applying for the first time an iterative maximum a posteriori delensing method. Our analysis demonstrates the capability of internal delensing as a means of improving constraints on inflationary models, paving the way for the optimal analysis of next-generation primordial $B$-mode experiments., Comment: Matches version published in Physical Review Letters

Published
2019

27. A Measurement of the Degree Scale CMB B-mode Angular Power Spectrum with POLARBEAR

Author

Julien Carron, M. A. Dobbs, C. Tsai, Dominic Beck, D. Leon, Ted Kisner, Aashrita Mangu, D. Boettger, Christian L. Reichardt, A. T. P. Pham, Kam Arnold, Akito Kusaka, Nicoletta Krachmalnicoff, T. Hamada, John Groh, S. Beckman, Josquin Errard, Ben Westbrook, Nathan Stebor, Neil Goeckner-Wald, Reijo Keskitalo, Daisuke Kaneko, Greg Jaehnig, Kevin T. Crowley, S. Takatori, Masaya Hasegawa, D. Tanabe, Tucker Elleflot, Giulio Fabbian, L. Howe, A. Cukierman, T. Fujino, Y. Zhou, S. Takakura, Eric V. Linder, Julian Borrill, N. Katayama, Yuki Inoue, Davide Poletti, Praween Siritanasak, Haruki Nishino, Yuto Minami, Yuji Chinone, Y. Segawa, H. El Bouhargani, Osamu Tajima, Aritoki Suzuki, N. W. Halverson, Darcy Barron, Masashi Hazumi, L. N. Lowry, G. Hall, Frederick Matsuda, Federico Bianchini, Scott Chapman, M. Navaroli, R. Stompor, Nicholas Galitzki, Clara Vergès, Maximiliano Silva-Feaver, Oliver Jeong, M. A. O. Aguilar Faúndez, Grant Teply, Brian Keating, Shunsuke Adachi, S. Kikuchi, K. Cheung, Adrian T. Lee, Giuseppe Puglisi, Charles A. Hill, Chang Feng, C. Baccigalupi, 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), POLARBEAR, 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, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Adachi, S, Aguilar Faundez, M, 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, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, 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, Kaneko, D, 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, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmic microwave background radiation, Cosmic inflation, Cosmology, Observational cosmology, cosmological model, 010504 meteorology & atmospheric sciences, Cosmic microwave background, Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, Spectral line, thermal, Cosmic microwave background radiationCosmic inflationCosmologyObservational cosmology, Particle and Plasma Physics, polarization: power spectrum, 010303 astronomy & astrophysics, media_common, Physics, Settore FIS/05, Polarization (waves), symbols, astro-ph.CO, power spectrum: angular dependence, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics, data analysis method, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, frequency: high, cosmic background radiation: B-mode, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, statistical analysis, 0103 physical sciences, Nuclear, Planck, cosmic background radiation: power spectrum, inflation, 0105 earth and related environmental sciences, gravitational radiation: primordial, gravitational radiation, Spectral density, Molecular, Astronomy and Astrophysics, Square degree, detector: sensitivity, Space and Planetary Science, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present a measurement of the $B$-mode polarization power spectrum of the cosmic microwave background (CMB) using taken from July 2014 to December 2016 with the POLARBEAR experiment. The CMB power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of $\mathrm{NET}_\mathrm{array}=23\, \mu \mathrm{K} \sqrt{\mathrm{s}}$ on a 670 square degree patch of sky centered at (RA, Dec)=($+0^\mathrm{h}12^\mathrm{m}0^\mathrm{s},-59^\circ18^\prime$). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve $32\,\mu\mathrm{K}$-$\mathrm{arcmin}$ effective polarization map noise with a knee in sensitivity of $\ell = 90$, where the inflationary gravitational wave signal is expected to peak. The measured $B$-mode power spectrum is consistent with a $\Lambda$CDM lensing and single dust component foreground model over a range of multipoles $50 \leq \ell \leq 600$. The data disfavor zero $C_\ell^{BB}$ at $2.2\sigma$ using this $\ell$ range of POLARBEAR data alone. We cross-correlate our data with Planck high frequency maps and find the low-$\ell$ $B$-mode power in the combined dataset to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio $r < 0.90$ at 95% confidence level after marginalizing over foregrounds.

Published
2019

28. 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

29. 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 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

32. The Simons Observatory: gain, bandpass and polarization-angle calibration requirements for B-mode searches

Author

Valentina Fanfani, Mario Zannoni, Mark J. Devlin, J. Colin Hill, Josquin Errard, Aritoki Suzuki, Gabriele Coppi, Edward J. Wollack, Julien Carron, Adrian T. Lee, Thibaut Louis, Davide Poletti, Mathew S. Madhavacheril, Michael L. Brown, Baptiste Jost, Brian Keating, Federico Nati, P. Daniel Meerburg, S. Azzoni, Maximilian H. Abitbol, Haruki Nishino, Sara M. Simon, Michael J. Randall, Jacob Spisak, Lyman A. Page, Bradley R. Johnson, Jo Dunkley, Yuji Chinone, Aamir Ali, David Alonso, Grant Teply, Jeff McMahon, Carlo Baccigalupi, Clara Vergès, Jens Chluba, Aditya Rotti, Giuseppe Puglisi, Nicholas Galitzki, Kevin D. Crowley, Martina Gerbino, Zhilei Xu, Jack Lashner, Erminia Calabrese, Kevin T. Crowley, Darcy Barron, Akito Kusaka, Nicoletta Krachmalnicoff, Heather McCarrick, 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), 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), Van Swinderen Institute for Particle Physics and G, High-Energy Frontier, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ANR-17-CE31-0022,BxB,Champs B interstellaires et modes B de l'inflation(2017), ANR-17-CE23-0002,B3DCMB,Big Bang à partir de Big Data (du fond diffus cosmologique)(2017), Abitbol, M, Alonso, D, Simon, S, Lashner, J, Crowley, K, Ali, A, Azzoni, S, Baccigalupi, C, Barron, D, Brown, M, Calabrese, E, Carron, J, Chinone, Y, Chluba, J, Coppi, G, Devlin, M, Dunkley, J, Errard, J, Fanfani, V, Galitzki, N, Gerbino, M, Colin Hill, J, Johnson, B, Jost, B, Keating, B, Krachmalnicoff, N, Kusaka, A, Lee, A, Louis, T, Madhavacheril, M, Mccarrick, H, Mcmahon, J, Daniel Meerburg, P, Nati, F, Nishino, H, Page, L, Poletti, D, Puglisi, G, Randall, M, Rotti, A, Spisak, J, Suzuki, A, Teply, G, Vergès, C, Wollack, E, Xu, Z, and Zannoni, M

Subjects
CMBR polarisation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Calibration (statistics), Cosmic microwave background, FOS: Physical sciences, Parameter space, Residual, Atomic, 01 natural sciences, Particle and Plasma Physics, Settore FIS/05 - Astronomia e Astrofisica, Band-pass filter, Observatory, 0103 physical sciences, CMBR experiments, Nuclear, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, CMBR polarization, Physics, Settore FIS/05, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, cosmological parameters from CMBR, Molecular, Astronomy and Astrophysics, Polarization (waves), Nuclear & Particles Physics, gravitational waves and CMBR polarization, Computational physics, astro-ph.CO, CMBR experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Focus (optics), Astronomical and Space Sciences, astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We quantify the calibration requirements for systematic uncertainties for next-generation ground-based observatories targeting the large-angle $B$-mode polarization of the Cosmic Microwave Background, with a focus on the Simons Observatory (SO). We explore uncertainties on gain calibration, bandpass center frequencies, and polarization angles, including the frequency variation of the latter across the bandpass. We find that gain calibration and bandpass center frequencies must be known to percent levels or less to avoid biases on the tensor-to-scalar ratio $r$ on the order of $\Delta r\sim10^{-3}$, in line with previous findings. Polarization angles must be calibrated to the level of a few tenths of a degree, while their frequency variation between the edges of the band must be known to ${\cal O}(10)$ degrees. Given the tightness of these calibration requirements, we explore the level to which residual uncertainties on these systematics would affect the final constraints on $r$ if included in the data model and marginalized over. We find that the additional parameter freedom does not degrade the final constraints on $r$ significantly, broadening the error bar by ${\cal O}(10\%)$ at most. We validate these results by reanalyzing the latest publicly available data from the BICEP2/Keck collaboration within an extended parameter space covering both cosmological, foreground and systematic parameters. Finally, our results are discussed in light of the instrument design and calibration studies carried out within SO., Comment: 41 pages, 18 figures

Published
2021

33. Development of Readout Electronics for POLARBEAR-2 Cosmic Microwave Background Experiment

Author

Y. Hori, Kaja Rotermund, Aritoki Suzuki, Aaron Lee, Nathan Whitehorn, Kam Arnold, Masashi Hazumi, W. L. Holzapfel, Masaya Hasegawa, Y. Akiba, Brian Keating, Tucker Elleflot, Amy N. Bender, Kaori Hattori, I. Shirley, Darcy Barron, Akito Kusaka, M. A. Dobbs, T. de Haan, A. Cukierman, and Joshua Montgomery

Subjects
Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 02 engineering and technology, 01 natural sciences, Multiplexing, law.invention, Responsivity, law, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Equivalent series resistance, business.industry, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), 021001 nanoscience & nanotechnology, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Inductance, Capacitor, Frequency domain, Optoelectronics, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business
Abstract

The readout of transition-edge sensor (TES) bolometers with a large multiplexing factor is key for the next generation cosmic microwave background (CMB) experiment, Polarbear-2 (Suzuki in J Low Temp Phys 176:719, 2014), having 7588 TES bolometers. To enable the large arrays, we have been developing a readout system with a multiplexing factor of 40 in the frequency domain. Extending that architecture to 40 bolometers requires an increase in the bandwidth of the SQUID electronics, above 4 MHz. This paper focuses on cryogenic readout and shows how it affects cross talk and the responsivity of the TES bolometers. A series resistance, such as equivalent series resistance of capacitors for LC filters, leads to non-linear response of the bolometers. A wiring inductance modulates a voltage across the bolometers and causes cross talk. They should be controlled well to reduce systematic errors in CMB observations. We have been developing a cryogenic readout with a low series impedance and have tuned bolometers in the middle of their transition at a high frequency ( $$>$$ 3 MHz).

Published
2016

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. Systematic uncertainties in the Simons Observatory: optical effects and sensitivity considerations

Author

Federico Nati, Brian Keating, Simon Dicker, Zhilei Xu, Philip Daniel Mauskopf, C. L. Reichardt, Mark J. Devlin, Frederick Matsuda, Brian J. Koopman, Jeff McMahon, Giulio Fabbian, S. T. Staggs, S. Parshley, Jacob Lashner, Maria Salatino, Yuji Chinone, Edward J. Wollack, Jon E. Gudmundsson, Gabriele Coppi, Ningfeng Zhu, Sean Bryan, A. T. Lee, C. Hill, Akito Kusaka, Aamir Ali, Giuseppe Puglisi, Eve M. Vavagiakis, Aritoki Suzuki, Nicholas Galitzki, Michele Limon, J. Orlowski-Scherer, Patricio A. Gallardo, Sara M. Simon, Michael D. Niemack, and Nicholas F. Cothard

Subjects
Physics, Aperture, business.industry, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 02 engineering and technology, 021001 nanoscience & nanotechnology, Polarization (waves), 01 natural sciences, law.invention, 010309 optics, Telescope, Optics, Observatory, law, Sky, 0103 physical sciences, 0210 nano-technology, business, Focus (optics), Microwave, media_common
Abstract

The Simons Observatory (SO) is a new experiment that aims to measure the cosmic microwave background (CMB) in temperature and polarization. SO will measure the polarized sky over a large range of microwave frequencies and angular scales using a combination of small (~0.5 m) and large (~6 m) aperture telescopes and will be located in the Atacama Desert in Chile. This work is part of a series of papers studying calibration, sensitivity, and systematic errors for SO. In this paper, we discuss current efforts to model optical systematic effects, how these have been used to guide the design of the SO instrument, and how these studies can be used to inform instrument design of future experiments like CMB-S4. While optical systematics studies are underway for both the small aperture and large aperture telescopes, we limit the focus of this paper to the more mature large aperture telescope design for which our studies include: pointing errors, optical distortions, beam ellipticity, cross-polar response, instrumental polarization rotation and various forms of sidelobe pickup.

Published
2018

36. Towards the next generation of frequency-multipexed TES bolometer readout (Conference Presentation)

Author

Ari Cukierman, Tijmen de Haan, Akito Kusaka, Darcy Barron, Leo Steinmetz, and Aritoki Suzuki

Subjects
Physics::Instrumentation and Detectors, Computer science, business.industry, Detector, Cosmic microwave background, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Electrical engineering, Astrophysics::Cosmology and Extragalactic Astrophysics, Sense (electronics), Multiplexing, law.invention, law, Dark energy, Neutrino, business, Voltage
Abstract

The Cosmic Microwave Background (CMB) has provided an invaluable source of information about the universe we live in. However, much information is yet to be gained. For instance, information about the cosmological parameters of dark energy, inflation, and the neutrino sector is nearly guaranteed to provide revolutionary results in upcoming CMB experiments. The current most popular detector technology, TES bolometers, finds a challenge in its low-noise readout, which requires a per-detector strong voltage bias while being able to sense O(10 aW/rtHz) fluctations in incident power. Frequency-multiplexed (fMUX) readout has been demonstrated to great success with an O(10) multiplexing factor, and is currently being implemented with an O(100) multiplexing factor for SPT-3G and POLARBEAR-2. We are developing a series of improvements that will greatly simplify the fMUX readout architecture, improve performance, and increase the multiplexing factor. I will present results on a lossless method of fMUX detector bias that simplifies the readout architecture, as well as an effort to radically change and further simplify the readout architecture by moving the 4K DC SQUID to the sub-Kelvin stage.

Published
2018

37. 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

38. Cross-polarization systematics due to Mizuguchi-Dragone condition breaking by a continuously rotating half-wave plate at prime focus in the Huan Tran telescope

Author

Kam Arnold, Akito Kusaka, Masashi Hazumi, S. Takakura, Frederick Matsuda, Yuji Chinone, Adrian T. Lee, D. Boettger, and Brian Keating

Subjects
Physics, 010308 nuclear & particles physics, business.industry, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Physical optics, 01 natural sciences, Waveplate, law.invention, Telescope, Optics, Amplitude, Cardinal point, law, 0103 physical sciences, Mueller calculus, business, 010303 astronomy & astrophysics
Abstract

Polarization modulation using a continuously rotating half-wave plate (HWP) is a promising technique to reduce both low-frequency noise and instrumental systematics for Cosmic Microwave Background (CMB) polarization measurements targeting in ationary B-modes. Although a HWP is best placed sky-side of the telescope optics in order to minimize systematics, >0.5 meter aperture class telescopes must put the HWP elsewhere in the optics chain due to current fabrication limitations in the available HWP size. Polarbear is a ground-based CMB experiment installed on the 2.5m aperture off-axis Gregorian-Dragone type Huan Tran Telescope (HTT) designed to satisfy the Mizuguchi-Dragone condition. Polarbear-2 is a receiver that will be installed on a second HTT in 2018. Polarbear-2 is designed to have a larger field-of-view (FOV) and vastly increased sensitivity to the polarized CMB compared to Polarbear. From the third season of observations, Polarbear has installed a continuously rotating HWP at the spatially localized focus plane between the HTT primary and secondary re ectors which is an optimal location for minimizing the HWP diameter. The HWP's polarization angle re ection with respect to its birefringent axis will theoretically break the Mizuguchi-Dragone condition when placed between the two reflectors and increase cross-polarization systematics. In this study, we analyze how the Mizuguchi-Dragone condition is violated due to a HWP at this location. We then estimate the crosspolarization systematics of the HTT using physical optics simulations. We model an ideal HWP at various angles to estimate the effects of demodulation. We evaluate the increased cross-polarization as the Stokes Q-U mixing term using the Mueller Matrix formalism. It is calculated that this term creates a varying dipole beam pattern whose amplitude ranges from 1% at the center to 10% at the edge FOV pixels for Polarbear and potentially up to 20% for Polarbear-2. We also estimate the leakage of the E-mode into the B-mode angular power spectrum measurements due to this cross-polarization. We show that the cross-polarization systematic error leakage is sufficiently lower than the Polarbear-2 statistical uncertainty thanks to mitigations such as focal plane averaging and sky rotation. Currently for Polarbear-2 we are planning to place the HWP at Gregorian focus, but keeping the HWP at prime focus as a back-up solution in case that there are unforeseen telescope spatial and HWP material size constraints. Through this study we find that even though a HWP between the two reflectors will violate the Mizuguchi-Dragone condition, this HWP at prime focus will still have sufficiently low cross-polarization for Polarbear-2. The prime focus HWP is a potential configuration that can be applied to similar off-axis Gregorian-Dragone telescopes in order to minimize the required HWP diameter.

Published
2018

39. 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

40. 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

41. Development of calibration strategies for the Simons Observatory

Author

Frederick Matsuda, Giuseppe Puglisi, Grant Teply, Ningfeng Zhu, Zhilei Xu, Brian Keating, Christian L. Reichardt, Brian J. Koopman, Philip Daniel Mauskopf, Aamir Ali, Jeff McMahon, Neil Goeckner-Wald, Sean Bryan, Kevin D. Crowley, Giulio Fabbian, Martina Gerbino, Patricio A. Gallardo, Federico Nati, Maria Salatino, Akito Kusaka, Yuji Chinone, Sara M. Simon, 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)), 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), Zmuidzinas, J, Gao, JR, Zhu, N, Xu, Z, Salatino, M, Reichardt, C, Puglisi, G, Nati, F, Mcmahon, J, Mauskopf, P, Matsuda, F, Kusaka, A, Koopman, B, Keating, B, Goeckner-Wald, N, Gallardo, P, Fabbian, G, Crowley, K, Chinone, Y, Ali, A, Gerbino, M, Simon, S, Teply, G, Bryan, S, 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), 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 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Simons Observatory, Computer science, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Observatory, 0103 physical sciences, Calibration, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, 010306 general physics, Simons Observatory, cosmic microwave background, calibration, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Remote sensing, Inflation (cosmology), Spectrometer, Gravitational wave, Settore FIS/05, Astrophysics::Instrumentation and Methods for Astrophysics, neutrinos, calibration, Gravitational lens, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Simons Observatory (SO) is a set of cosmic microwave background instruments that will be deployed in the Atacama Desert in Chile. The key science goals include setting new constraints on cosmic inflation, measuring large scale structure with gravitational lensing, and constraining neutrino masses. Meeting these science goals with SO requires high sensitivity and improved calibration techniques. In this paper, we highlight a few of the most important instrument calibrations, including spectral response, gain stability, and polarization angle calibrations. We present their requirements for SO and experimental techniques that can be employed to reach those requirements., 13 pages, 4 figures, SPIE Astronomical Telescopes and Instrumentation 2018

Published
2018

42. Studies of systematic uncertainties for Simons Observatory: detector array effects

Author

Jason E. Austermann, Kevin T. Crowley, Shuay-Pwu Patty Ho, Joel N. Ullom, Jeff McMahon, Aritoki Suzuki, Ari Cukierman, Clara Vergès, Mayuri Sathyanarayana Rao, Michael R. Vissers, Zhilei Xu, Shannon M. Duff, Christian L. Reichardt, Giulio Fabbian, Daniel Thomas, Michael L. Brown, Suzanne T. Staggs, Sara M. Simon, Patricio A. Gallardo, Akito Kusaka, Bradley Dober, Federico Nati, Giuseppe Puglisi, Max Silva-Feaver, Maria Salatino, Grant Teply, Johannes Hubmayr, Praween Siritanasak, Jo Dunkley, Neil Goeckner-Wald, Josquin Errard, Yuji Chinone, Edward J. Wollack, Brian Keating, Aamir Ali, Benjamin Westbrook, Ningfeng Zhu, Nialh McCallum, Michael D. Niemack, 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 spatiale (IAS), 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), 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), Gao, JR, Crowley, K, Simon, S, Silva-Feaver, M, Goeckner-Wald, N, Ali, A, Austermann, J, Brown, M, Chinone, Y, Cukierman, A, Dober, B, Duff, S, Dunkley, J, Errard, J, Fabbian, G, Gallardo, P, Ho, S, Hubmayr, J, Keating, B, Kusaka, A, Mccallum, N, Mcmahon, J, Nati, F, Niemack, M, Puglisi, G, Sathyanarayana Rao, M, Reichardt, C, Salatino, M, Siritanasak, P, Staggs, S, Suzuki, A, Teply, G, Thomas, D, Ullom, J, Verges, C, Vissers, M, Westbrook, B, Wollack, E, Xu, Z, Zhu, N, 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
systematic effects, cosmic microwave background, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Simons Observatory, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, non-linearity, law.invention, detector array, optical coupling, gain variation, crosstalk, Optics, law, Observatory, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Anisotropy, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Leakage (electronics), Physics, 010308 nuclear & particles physics, Gravitational wave, business.industry, Settore FIS/05, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In this proceeding, we present studies of instrumental systematic effects for the Simons Obsevatory (SO) that are associated with the detector system and its interaction with the full SO experimental systems. SO will measure the Cosmic Microwave Background (CMB) temperature and polarization anisotropies over a wide range of angular scales in six bands with bandcenters spanning from 27 GHz to 270 GHz. We explore effects including intensity-to-polarization leakage due to coupling optics, bolometer nonlinearity, uncalibrated gain variations of bolometers, and readout crosstalk. We model the level of signal contamination, discuss proposed mitigation schemes, and present instrument requirements to inform the design of SO and future CMB projects., Proceeding from SPIE Astronomical Telescopes+Instrumentation 2018 (27 pages, 13 figures) v2: Added HEALPix reference

Published
2018

43. Quantum Sensing for High Energy Physics

Author

Cynthia Jenks, Vesna Mitrovic, Matthew Dietrich, Paul D. Lett, Petra Merkel, Kevin J. O'Brien, Volodymyr Yefremenko, Roger Rusack, Mattia Checchin, Ian Shipsey, Sae Woo Nam, Nicholas A. Peters, Alexander Romanenko, Malcolm Boshier, Michael V. Fazio, Tenzin Rabga, David Underwood, Larry Lurio, Karen Byrum, John Zasadzinski, Gensheng Wang, Benjamin J. Lawrie, Jonathan King, Hogan Nguyen, Eve Kovacs, Howard Nicholson, Jeffrey R. Guest, Robert Wagner, Xuedan Ma, Amr S. Helmy, Andrew Sonnenschein, U. Patel, Jason W. Henning, Xufeng Zhang, Valerie Taylor, Yuekun Heng, Geoffrey T. Bodwin, C. M. Posada, Andrei Nomerotski, Jessica Metcalfe, Hal Finkel, Patrick J. Fox, Yuri Alexeev, Keith Schwab, Derek F. Jackson Kimball, Nathan Woollett, Karl van Bibber, Joseph Heremans, Akito Kusaka, Harry Weerts, David Hume, Zeeshan Ahmed, Jonathan Lewis, Pavel Lougovski, Marcel Demarteau, Roger O'Brient, John F. Mitchell, Ranjan Dharmapalan, Vishnu Zutshi, Gustavo Cancelo, Przemyslaw Bienias, D. Braga, Richard Kriske, Junqi Xie, Ron Harnik, Giorgio Apollinari, Kent D. Irwin, Vladan Vuletic, Gianpaolo Carosi, R. Tschirhart, Erik Shirokoff, Zelimir Djurcic, James E. Fast, M. Crisler, Sergei Chekanov, Junjia Ding, Karl K. Berggren, Jason M. Hogan, Asimina Arvanitaki, Aaron S. Chou, Donna Kubik, Holger Mueller, Johannes Hubmayr, Andrei Gaponenko, Michael L. Norman, Raphael C. Pooser, Salman Habib, Konrad Lehnert, Nick Karonis, Aashish A. Clerk, Peter Fierlinger, Raj Kettimuthu, Monika Schleier-Smith, J. Segal, David D. Awschalom, D. Bowring, Ian C. Cloët, S. Rescia, Edward May, Misun Min, Tijana Rajh, Sandeep Miryala, Bjoern Penning, Phay J. Ho, Andrew Geraci, Gerald Gabrielse, Christopher George Tully, Supratik Guha, Maurice Garcia-Sciveres, Jie Zhang, Thomas Cecil, John M. Doyle, Sergey Perverzev, C. L. Chang, Jimmy Proudfoot, and Antonino Miceli

Subjects
Physics, Particle physics, Quantum sensor, Experimental methods, Domain (software engineering)
Abstract

Report of the first workshop to identify approaches and techniques in the domain of quantum sensing that can be utilized by future High Energy Physics applications to further the scientific goals of High Energy Physics.

Published
2018

44. A large-diameter cryogenic rotation stage for half-wave plate polarization modulation on the POLARBEAR-2 experiment

Author

Adrian T. Lee, B. Bixler, Akito Kusaka, Frederick Matsuda, Alex G. Droster, Danielle R. Sponseller, Charles A. Hill, Arian Jadbabaie, Oliver Jeong, Tomotake Matsumura, R. Tat, Aritoki Suzuki, Alex Madurowicz, Paul Barton, Mael Flament, Yuki Sakurai, S. Ganjam, and Adam Rutkowski

Subjects
Cryostat, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, Cosmic microwave background, FOS: Physical sciences, 7. Clean energy, 01 natural sciences, Waveplate, Optics, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010302 applied physics, Physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimeter, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Modulation, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the design of a cryogenic rotation stage (CRS) for use with the cryogenic half-wave plate (CHWP) polarization modulator on the POLARBEAR-2b and POLARBEAR-2c (PB2b/c) cosmic microwave background (CMB) experiments, the second and third installments of the Simons Array. Rapid modulation of the CMB polarization signal using a CHWP suppresses 1/f contamination due to atmospheric turbulence and allows a single polarimeter to measure both polarization states, mitigating systematic effects that arise when differencing orthogonal detectors. To modulate the full detector array while avoiding excess photon loading due to thermal emission, the CHWP must have a clear-aperture diameter of > 450 mm and be cooled to < 100 K. We have designed a 454-mm-clear-aperture, < 65 K CRS using a superconducting magnetic bearing driven by a synchronous magnetic motor. We present the specifications for the CRS, its interfacing to the PB2b/c receiver cryostat, its performance in a stand-alone test, and plans for future work., PREPRINT VERSION. Accepted to the Journal of Low Temperature Physics, Article JLTP-D-17-00265R1 See DOI link, supplied by Springer Publishing, for the fully-reviewed published article and citation information

Published
2018
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45. Results from the Atacama B-mode Search (ABS) Experiment

Author

Sara M. Simon, Norman Jarosik, Matthew Hasselfield, Steve K. Choi, S. P. Ho, K. W. Yoon, Gene C. Hilton, Gonzalo A. Palma, Kent D. Irwin, Michael R. Nolta, J. W. Appel, Hsiao-Mei Cho, Michael D. Niemack, Carl D. Reintsema, Jonathan Sievers, Akito Kusaka, Lucas Parker, Joseph W. Fowler, Suzanne T. Staggs, Luis E. Campusano, G. W. Nixon, Thomas Essinger-Hileman, James A. Beall, Kevin T. Crowley, Katerina Visnjic, Patricio A. Gallardo, Lyman A. Page, and Srinivasan Raghunathan

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Electromagnetic radiation, symbols.namesake, 0103 physical sciences, Atacama B-Mode Search, Planck, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Cosmic dust, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Polarization (waves), 13. Climate action, Sky, symbols, Astrophysics - Instrumentation and Methods for Astrophysics, Right ascension, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Atacama B-mode Search (ABS) is an experiment designed to measure cosmic microwave background (CMB) polarization at large angular scales ($\ell>40$). It operated from the ACT site at 5190~m elevation in northern Chile at 145 GHz with a net sensitivity (NEQ) of 41 $��$K$\sqrt{\rm s}$. It employed an ambient-temperature sapphire half-wave plate rotating at 2.55 Hz to modulate the incident polarization signal and reduce systematic effects. We report here on the analysis of data from a 2400 deg$^2$ patch of sky centered at declination $-42^\circ$ and right ascension $25^\circ$. We perform a blind analysis. After unblinding, we find agreement with the Planck TE and EE measurements on the same region of sky. We marginally detect polarized dust emission and give an upper limit on the tensor-to-scalar ratio of $r, 38 pages, 11 figures

Published
2018
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46. Studies of systematic uncertainties for Simons Observatory: polarization modulator related effects

Author

Amber Miller, Aamir Ali, Grant Teply, Ningfeng Zhu, Jeff McMahon, Kevin Coughlin, Joy Didier, Giulio Fabbian, Nicholas Galitzki, Yuji Chinone, Jon E. Gudmundsson, Peter Ashton, Sara M. Simon, Zhilei Xu, Jacob Lashner, Kevin T. Crowley, Christian L. Reichardt, Neil Goeckner-Wald, Brian Keating, Sean Bryan, Adrian T. Lee, Giuseppe Puglisi, Charles A. Hill, Akito Kusaka, Maria Salatino, and Martina Gerbino

Subjects
Sapphire, Simons Observatory, Cosmic microwave background, 01 natural sciences, Waveplate, Continuously Rotating Half-Wave Plate, Non Linearity, 010305 fluids & plasmas, 010309 optics, Optics, Observatory, 0103 physical sciences, Cosmic Microwave Background, Time domain, Physics, business.industry, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Systematic effects, Slant Incidence, Amplitude, Intensity to Polarization Leakage, Millimeter, business
Abstract

The Simons Observatory (SO) will observe the temperature and polarization anisotropies of the cosmic microwave background (CMB) over a wide range of frequencies (27 to 270 GHz) and angular scales by using both small (∼0.5 m) and large (∼6 m) aperture telescopes. The SO small aperture telescopes will target degree angular scales where the primordial B-mode polarization signal is expected to peak. The incoming polarization signal of the small aperture telescopes will be modulated by a cryogenic, continuously-rotating half-wave plate (CRHWP) to mitigate systematic effects arising from slowly varying noise and detector pair-differencing. In this paper, we present an assessment of some systematic effects arising from using a CRHWP in the SO small aperture systems. We focus on systematic effects associated with structural properties of the HWP and effects arising when operating a HWP, including the amplitude of the HWP synchronous signal (HWPSS), and I → P (intensity to polarization) leakage that arises from detector non-linearity in the presence of a large HWPSS. We demonstrate our ability to simulate the impact of the aforementioned systematic effects in the time domain. This important step will inform mitigation strategies and design decisions to ensure that SO will meet its science goals.

Published
2018

47. Designs for next generation CMB survey strategies from Chile

Author

Edward J. Wollack, Aamir Ali, Giuseppe Puglisi, Michael L. Brown, Michael D. Niemack, Neil Goeckner-Wald, Julian Borrill, Akito Kusaka, Zhilei Xu, Ningfeng Zhu, Yuji Chinone, Suet Ying D. Mak, Nialh McCallum, Daniel Thomas, Maria Salatino, Patricio A. Gallardo, Eve M. Vavagiakis, Lyman A. Page, Jeff McMahon, Reijo Keskitalo, Jason R. Stevens, Grant Teply, Adrian T. Lee, 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 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, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Simons Observatory, Computer science, Aperture, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Observing Strategy, law.invention, Telescope, Observatory, law, 0103 physical sciences, Cosmic Microwave Background, [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), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Gravitational wave, Settore FIS/05, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Gravitational lens, Sky, Atacama Cosmology Telescope, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

New telescopes are being built to measure the Cosmic Microwave Background (CMB) with unprecedented sensitivity, including Simons Observatory (SO), CCAT-prime, the BICEP Array, SPT-3G, and CMB Stage-4. We present observing strategies for telescopes located in Chile that are informed by the tools used to develop recent Atacama Cosmology Telescope (ACT) and Polarbear surveys. As with ACT and Polarbear, these strategies are composed of scans that sweep in azimuth at constant elevation. We explore observing strategies for both small (0.42 m) aperture telescopes (SAT) and a large (6 m) aperture telescope (LAT). We study strategies focused on small sky areas to search for inflationary gravitational waves as well as strategies spanning roughly half the low-foreground sky to constrain the effective number of relativistic species and measure the sum of neutrino masses via the gravitational lensing signal due to large scale structure. We present these strategies specifically considering the telescope hardware and science goals of the SO, located at 23 degrees South latitude, 67.8 degrees West longitude. Observations close to the Sun and the Moon can introduce additional systematics by applying additional power to the instrument through telescope sidelobes. Significant side lobe contamination in the data can occur even at tens of degrees or more from bright sources. Therefore, we present several strategies that implement Sun and Moon avoidance constraints into the telescope scheduling. Strategies for resolving conflicts between simultaneously visible fields are discussed. We focus on maximizing telescope time spent on science observations. It will also be necessary to schedule calibration measurements, however that is beyond the scope of this work. The outputs of this study are algorithms that can generate specific schedule commands for the Simons Observatory instruments., Comment: 15 pages, 9 figures, 3 tables, SPIE Astronomical Telescopes + Instrumentation 2018

Published
2018

48. Optimization Study for the Experimental Configuration of CMB-S4

Author

Julian Borril, Natalie A. Roe, Simone Ferraro, Stephen M. Feeney, Josquin Errard, Aritoki Suzuki, Adrian T. Lee, Blake D. Sherwin, Yuji Chinone, Reijo Keskitalo, Darcy Barron, Akito Kusaka, 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), and 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 )

Subjects
CMBR polarisation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Atomic, Cosmology, law.invention, Telescope, Particle and Plasma Physics, Conceptual design, law, 0103 physical sciences, CMBR experiments, Nuclear, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, media_common, Physics, Inflation (cosmology), COSMIC cancer database, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, cosmological parameters from CMBR, Molecular, Astronomy and Astrophysics, Nuclear & Particles Physics, Universe, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, gravitational waves and CMBR polarization, Algorithm, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

The CMB Stage 4 (CMB-S4) experiment is a next-generation, ground-based experiment that will measure the cosmic microwave background (CMB) polarization to unprecedented accuracy, probing the signature of inflation, the nature of cosmic neutrinos, relativistic thermal relics in the early universe, and the evolution of the universe. To advance the progress towards designing the instrument for CMB-S4, we have established a framework to optimize the instrumental configuration to maximize its scientific output. In this paper, we report our first results from this framework, using simplified instrumental and cost models. We have primarily studied two classes of instrumental configurations: arrays of large aperture telescopes with diameters ranging from 2-10 m, and hybrid arrays that combine small-aperture telescopes (0.5 m diameter) with large-aperture telescopes. We explore performance as a function of the telescope aperture size, the distribution of the detectors into different microwave frequencies, the survey strategy and survey area, the low-frequency noise performance, and the balance between small and large aperture telescopes for the hybrid configurations. We also examine the impact from the uncertainties of the instrumental model. There are several areas that deserve further improvement. In our forecasting framework, we adopt a simple two-component foregrounds model with spacially varying power-law spectral indices. We estimate delensing performance statistically and ignore possible non-idealities. Instrumental systematics, which is not accounted for in our study, may influence the design. Further study of the instrumental and cost models will be one of the main areas of study by the whole CMB-S4 community. We hope that our framework will be useful for estimating the influence of these improvement in future, and we will incorporate them in order to improve the optimization further., 42 pages, 23 figures; minor English/grammar corrections

Published
2018

49. 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

50. Concept Study of Optical Configurations for High-Frequency Telescope for LiteBIRD

Author

D. W. Curtis, M. Nakajima, T. Funaki, R. Takaku, Yoshinori Uzawa, Carlo Baccigalupi, Johannes Hubmayr, U. Fuskeland, Theodore Kisner, S. Beckman, Anna Mangilli, Erminia Calabrese, Neil Goeckner-Wald, Uroš Seljak, M. Nagai, N. Katayama, Jonathan Aumont, Carole Tucker, Suguru Takada, Shin Utsunomiya, Kazunori Kohri, R. Nagata, Kam Arnold, M. Bucher, A. Dominjon, N. Sato, M. A. Dobbs, Shin-ichiro Sakai, Darcy Barron, Gene C. Hilton, H. K. Eriksen, Yasuhiro Yamada, Oliver Jeong, Aritoki Suzuki, Atsushi Okamoto, Tadayasu Dotani, T. Tomida, D. Meilhan, L. Duband, S. A. Kernasovskiy, S. Takakura, S. Takatori, R. Stompor, A. Ducout, B. Thorne, Eiichiro Komatsu, Hajime Sugai, Keisuke Shinozaki, N. Tomita, J. Fischer, Yuji Chinone, C. L. Kuo, L. Montier, Akito Kusaka, Toshiaki Iida, Aaron Lee, Yuki Inoue, Makoto Sawada, Ingunn Kathrine Wehus, L. Hayes, Mitsuhiro Yoshida, K. L. Thompson, H. Nishino, Mathieu Remazeilles, Tomotake Matsumura, Shugo Oguri, K. Komatsu, Reijo Keskitalo, T. Yamashita, T. Kawasaki, Takahiro Okamura, Masashi Hazumi, Osamu Tajima, Takayuki Tomaru, G. Patanchon, M. Tristram, Giampaolo Pisano, Hirokazu Ishino, Masato Naruse, Jun-ichi Suzuki, H. M. Cho, Paul Turin, Toshiya Namikawa, Yuki Sakurai, Y. Kida, Blake D. Sherwin, J. Grain, Chiko Otani, Noriko Y. Yamasaki, N. W. Halverson, Shuji Matsuura, S. Uozumi, Takashi Noguchi, T. Nagasaki, H. Imada, M. Willer, Y. Sato, M. Inoue, J. M. Duval, Bruno Maffei, Toshifumi Shimizu, Yuto Minami, F. Boulanger, Tucker Elleflot, Charles A. Hill, Benjamin Westbrook, Shogo Nakamura, Peter A. R. Ade, Kaori Hattori, Paul L. Richards, Alex Lazarian, Y. Segawa, Julian Borrill, Ryo Yamamoto, Kiyotomo Ichiki, M. Maki, Satoru Mima, D. Tanabe, Jo Dunkley, Kazuhisa Mitsuda, Soumen Basak, Gabriel M. Rebeiz, Tom Nitta, T. de Haan, T. Hamada, H. Kanai, K. Ganga, Hideo Ogawa, D. Kaneko, A. Cukierman, Nathan Whitehorn, Eric V. Linder, Masaya Hasegawa, Josquin Errard, Kimihiro Kimura, Hiroyuki Sugita, David Alonso, T. Hasebe, Kent D. Irwin, E. Taylor, Norio Okada, N. Hidehira, Shingo Kashima, A. Kibayashi, Noah Kurinsky, T. Fujino, Y. Akiba, Makoto Hattori, Dale Li, Masahiro Tsujimoto, Yutaro Sekimoto, F. Vansyngel, 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 - 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 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), Laboratoire de l'Accélérateur Linéaire (LAL), 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), Laboratoire d'Electronique et des Technologies de l'Information (CEA-LETI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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)-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), 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)), 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), 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), 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), and Université Grenoble Alpes (UGA)-Direction de Recherche Technologique (CEA) (DRT (CEA))

Subjects
Cosmic microwave background radiation, Inflation, Satellite, Telescope, Silicon, Cosmic microwave background, chemistry.chemical_element, engineering.material, 01 natural sciences, law.invention, 010309 optics, Optics, Settore FIS/05 - Astronomia e Astrofisica, Coating, law, 0103 physical sciences, General Materials Science, Sensitivity (control systems), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Physics, business.industry, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Lens (optics), chemistry, engineering, Reflection (physics), business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
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): 長谷部, 孝; 堂谷, 忠靖; 羽澄, 昌史; 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: 2018-04-07, 資料番号: SA1180209000

Published
2017

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