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1. A Method of Measuring TES Complex ETF Response in Frequency-domain Multiplexed Readout by Single Sideband Power Modulation

Author

Zhou, Yu, de Haan, Tijmen, Akamatsu, Hiroki, Kaneko, Daisuke, Hazumi, Masashi, Hasegawa, Masaya, Suzuki, Aritoki, and Lee, Adrian T.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

The digital frequency domain multiplexing (DfMux) technique is widely used for astrophysical instruments with large detector arrays. Detailed detector characterization is required for instrument calibration and systematics control. We conduct the TES complex electrothermal-feedback (ETF) response measurement with the DfMux readout system as follows. By injecting a single sideband signal, we induce modulation in TES power dissipation over a frequency range encompassing the detector response. The modulated current signal induced by TES heating effect is measured, allowing for the ETF response characterization of the detector. With the injection of an upper sideband, the TES readout current shows both an upper and a lower sideband. We model the upper and lower sideband complex ETF response and verify the model by fitting to experimental data. The model not only can fit for certain physical parameters of the detector, such as loop gain, temperature sensitivity, current sensitivity, and time constant, but also enables us to estimate the systematic effect introduced by the multiplexed readout. The method is therefore useful for in-situ detector calibration and for estimating systematic effects during astronomical telescope observations, such as those performed by the upcoming LiteBIRD satellite., Comment: 9 pages, 4 figures, accepted to Journal of Low Temperature Physics

Published
2024

2. Do food cinemagraphs evoke stronger appetitive responses than stills?

Author

Toet, Alexander, van Schaik, Martin G., Kaneko, Daisuke, and van Erp, Jan B. F.

Subjects
Visual arts, N1-9211, Hospitality industry. Hotels, clubs, restaurants, etc. Food service, TX901-946.5
Abstract

Viewing images of food triggers the desire to eat and this effect increases when images represent food in a more vivid way. Cinemagraphs are a new medium that is intermediate between photographs and videos: most of the frame is static, while some details are animated in a seamless loop, resulting in a vivid viewing experience. On social media cinemagraphs are increasingly used for food-related communication. Given their vivid appearance we hypothesized that food cinemagraphs may evoke stronger appetitive responses than their static counterparts (stills). This would make them a promising medium for food advertisements on the Internet or on digital menu boards. In this study we measured the ‘wanting’ (appetitive) and ‘liking’ (affective) responses to both cinemagraph and stills representing a wide range of different food products. Our results show that food cinemagraphs slightly increase ‘wanting’ scores while not affecting ‘liking’ scores, compared to similar stills. Although we found no overall main effect of image dynamics on ‘liking’, we did observe a significant effect for some individual food items. The effects of image dynamics on ‘wanting’ and ‘liking’ appear to be product specific: while dynamic images were scored higher on ‘wanting’ or ‘liking’ for some products, static images were scored higher on these factors for other products. Observer responses to a free association task indicate that image dynamics can affect the appeal of a food product in two ways: by emphasizing its hedonic qualities (lusciousness, freshness) and by enhancing the observers’ awareness of their own core affect (‘liking’) for the product. We conclude that the effective use of cinemagraphs in food advertisements therefore requires a careful consideration of the characteristics (hedonic aspects) of the food product that are to be highlighted through image motion and the inherent preferences (core liking) of the target group.

Published
2019
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3. Exploration of the polarization angle variability of the Crab Nebula with POLARBEAR and its application to the search for axion-like particles

Author

Adachi, Shunsuke, Adkins, Tylor, Baccigalupi, Carlo, Chinone, Yuji, Crowley, Kevin T., Errard, Josquin, Fabbian, Giulio, Feng, Chang, Fujino, Takuro, Hasegawa, Masaya, Hazumi, Masashi, Jeong, Oliver, Kaneko, Daisuke, Keating, Brian, Kusaka, Akito, Lee, Adrian T., Lonappan, Anto I., Minami, Yuto, Murata, Masaaki, Piccirillo, Lucio, Reichardt, Christian L., Siritanasak, Praween, Spisak, Jake, Takakura, Satoru, Teply, Grant P., and Yamada, Kyohei

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Crab Nebula, also known as Tau A, is a polarized astronomical source at millimeter wavelengths. It has been used as a stable light source for polarization angle calibration in millimeter-wave astronomy. However, it is known that its intensity and polarization vary as a function of time at a variety of wavelengths. Thus, it is of interest to verify the stability of the millimeter-wave polarization. If detected, polarization variability may be used to better understand the dynamics of Tau A, and for understanding the validity of Tau~A as a calibrator. One intriguing application of such observation is to use it for the search of axion-light particles (ALPs). Ultralight ALPs couple to photons through a Chern-Simons term, and induce a temporal oscillation in the polarization angle of linearly polarized sources. After assessing a number of systematic errors and testing for internal consistency, we evaluate the variability of the polarization angle of the Crab Nebula using 2015 and 2016 observations with the 150 GHz POLARBEAR instrument. We place a median 95% upper bound of polarization oscillation amplitude $A < 0.065^\circ$ over the oscillation frequencies from $0.75~\mathrm{year}^{-1}$ to $0.66~\mathrm{hour}^{-1}$. Assuming that no sources other than ALP are causing Tau A's polarization angle variation, that the ALP constitutes all the dark matter, and that the ALP field is a stochastic Gaussian field, this bound translates into a median 95% upper bound of ALP-photon coupling $g_{a\gamma\gamma} < 2.16\times10^{-12}\,\mathrm{GeV}^{-1}\times(m_a/10^{-21} \mathrm{eV})$ in the mass range from $9.9\times10^{-23} \mathrm{eV}$ to $7.7\times10^{-19} \mathrm{eV}$. This demonstrates that this type of analysis using bright polarized sources is as competitive as those using the polarization of cosmic microwave background in constraining ALPs., Comment: 24 pages, 19 figures, 5 tables. Submitted to PRD

Published
2024

4. Constraints on axionlike polarization oscillations in the cosmic microwave background with POLARBEAR

Author

Adachi, Shunsuke, Adkins, Tylor, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Cheung, Kolen, Chinone, Yuji, Crowley, Kevin T, Errard, Josquin, Fabbian, Giulio, Feng, Chang, Flauger, Raphael, Fujino, Takuro, Green, Daniel, Hasegawa, Masaya, Hazumi, Masashi, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Kusaka, Akito, Lee, Adrian T, Minami, Yuto, Nishino, Haruki, Reichardt, Christian L, Siritanasak, Praween, Spisak, Jacob, Tajima, Osamu, Takakura, Satoru, Takatori, Sayuri, Teply, Grant Paul, and Yamada, Kyohei

Subjects
Particle and High Energy Physics, Physical Sciences
Abstract

Very light pseudoscalar fields, often referred to as axions, are compelling dark matter candidates and can potentially be detected through their coupling to the electromagnetic field. Recently a novel detection technique using the cosmic microwave background (CMB) was proposed, which relies on the fact that the axion field oscillates at a frequency equal to its mass in appropriate units, leading to a time-dependent birefringence. For appropriate oscillation periods this allows the axion field at the telescope to be detected via the induced sinusoidal oscillation of the CMB linear polarization. We search for this effect in two years of POLARBEAR data. We do not detect a signal, and place a median 95% upper limit of 0.65° on the sinusoid amplitude for oscillation frequencies between 0.02 days-1 and 0.45 days-1, which corresponds to axion masses between 9.6×10-22 eV and 2.2×10-20 eV. Under the assumptions that (1) the axion constitutes all the dark matter and (2) the axion field amplitude is a Rayleigh-distributed stochastic variable, this translates to a limit on the axion-photon coupling gφγ

Published
2023

5. Constraints on axion-like polarization oscillations in the cosmic microwave background with POLARBEAR

Author

The POLARBEAR Collaboration, Adachi, Shunsuke, Adkins, Tylor, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Cheung, Kolen, Chinone, Yuji, Crowley, Kevin T., Errard, Josquin, Fabbian, Giulio, Feng, Chang, Flauger, Raphael, Fujino, Takuro, Green, Daniel, Hasegawa, Masaya, Hazumi, Masashi, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Kusaka, Akito, Lee, Adrian T., Minami, Yuto, Nishino, Haruki, Reichardt, Christian L., Siritanasak, Praween, Spisak, Jacob, Tajima, Osamu, Takakura, Satoru, Takatori, Sayuri, Teply, Grant Paul, and Yamada, Kyohei

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Very light pseudoscalar fields, often referred to as axions, are compelling dark matter candidates and can potentially be detected through their coupling to the electromagnetic field. Recently a novel detection technique using the cosmic microwave background (CMB) was proposed, which relies on the fact that the axion field oscillates at a frequency equal to its mass in appropriate units, leading to a time-dependent birefringence. For appropriate oscillation periods this allows the axion field at the telescope to be detected via the induced sinusoidal oscillation of the CMB linear polarization. We search for this effect in two years of POLARBEAR data. We do not detect a signal, and place a median $95 \%$ upper limit of $0.65 ^\circ$ on the sinusoid amplitude for oscillation frequencies between $0.02\,\text{days}^{-1}$ and $0.45\,\text{days}^{-1}$, which corresponds to axion masses between $9.6 \times 10^{-22} \, \text{eV}$ and $2.2\times 10^{-20} \,\text{eV}$. Under the assumptions that 1) the axion constitutes all the dark matter and 2) the axion field amplitude is a Rayleigh-distributed stochastic variable, this translates to a limit on the axion-photon coupling $g_{\phi \gamma} < 2.4 \times 10^{-11} \,\text{GeV}^{-1} \times ({m_\phi}/{10^{-21} \, \text{eV}})$., Comment: 17 pages, 5 figures, 2 tables. Published in Physical Review D

Published
2023
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6. The Simons Observatory: the Large Aperture Telescope (LAT)

Author

Xu, Zhilei, Adachi, Shunsuke, Ade, Peter, Beall, J. A., Bhandarkar, Tanay, Bond, J. Richard, Chesmore, Grace E., Chinone, Yuji, Choi, Steve K., Connors, Jake A., Coppi, Gabriele, Cothard, Nicholas F., Crowley, Kevin D., Devlin, Mark, Dicker, Simon, Dober, Bradley, Duff, Shannon M., Galitzki, Nicholas, Gallardo, Patricio A., Golec, Joseph E., Gudmundsson, Jon E., Haridas, Saianeesh K., Harrington, Kathleen, Hervias-Caimapo, Carlos, Ho, Shuay-Pwu Patty, Huber, Zachary B., Hubmayr, Johannes, Iuliano, Jeffrey, Kaneko, Daisuke, Kofman, Anna M., Koopman, Brian J., Lashner, Jack, Limon, Michele, Link, Michael J., Lucas, Tammy J., Matsuda, Frederick, McCarrick, Heather, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Piccirillo, Lucio, Sarmiento, Karen Perez, Schaan, Emmanuel, Silva-Feaver, Maximiliano, Sonka, Rita, Sutariya, Shreya, Tajima, Osamu, Teply, Grant P., Terasaki, Tomoki, Thornton, Robert, Tucker, Carole, Ullom, Joel, Vavagiakis, Eve M., Vissers, Michael R., Walker, Samantha, Whipps, Zachary, Wollack, Edward J., Zannoni, Mario, Zhu, Ningfeng, and Zonca, Andrea

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Simons Observatory (SO) is a Cosmic Microwave Background (CMB) experiment to observe the microwave sky in six frequency bands from 30GHz to 290GHz. The Observatory -- at $\sim$5200m altitude -- comprises three Small Aperture Telescopes (SATs) and one Large Aperture Telescope (LAT) at the Atacama Desert, Chile. This research note describes the design and current status of the LAT along with its future timeline., Comment: 4 pages, 1 figure

Published
2021
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7. Trends of Checklist Survey of Computer Operational Skills for First-Year Students: Over the Past Four Years

Author

Kaneko, Daisuke, Ishida, Yukiya, Omata, Masaki, Yoshikawa, Masanobu, Koga, Takaaki, Rannenberg, Kai, Editor-in-Chief, Soares Barbosa, Luís, Editorial Board Member, Goedicke, Michael, Editorial Board Member, Tatnall, Arthur, Editorial Board Member, Neuhold, Erich J., Editorial Board Member, Stiller, Burkhard, Editorial Board Member, Stettner, Lukasz, Editorial Board Member, Pries-Heje, Jan, Editorial Board Member, Kreps, David, Editorial Board Member, Rettberg, Achim, Editorial Board Member, Furnell, Steven, Editorial Board Member, Mercier-Laurent, Eunika, Editorial Board Member, Winckler, Marco, Editorial Board Member, Malaka, Rainer, Editorial Board Member, Keane, Therese, editor, Lewin, Cathy, editor, Brinda, Torsten, editor, and Bottino, Rosa, editor

Published
2023
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8. Simons Observatory Small Aperture Telescope overview

Author

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

Subjects
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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9. The Simons Observatory: Astro2020 Decadal Project Whitepaper

Author

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

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile that promises to provide breakthrough discoveries in fundamental physics, cosmology, and astrophysics. Supported by the Simons Foundation, the Heising-Simons Foundation, and with contributions from collaborating institutions, SO will see first light in 2021 and start a five year survey in 2022. SO has 287 collaborators from 12 countries and 53 institutions, including 85 students and 90 postdocs. The SO experiment in its currently funded form ('SO-Nominal') consists of three 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT). Optimized for minimizing systematic errors in polarization measurements at large angular scales, the SATs will perform a deep, degree-scale survey of 10% of the sky to search for the signature of primordial gravitational waves. The LAT will survey 40% of the sky with arc-minute resolution. These observations will measure (or limit) the sum of neutrino masses, search for light relics, measure the early behavior of Dark Energy, and refine our understanding of the intergalactic medium, clusters and the role of feedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution of the Planck satellite, and roughly an order of magnitude increase in mapping speed over currently operating ("Stage 3") experiments, SO will measure the CMB temperature and polarization fluctuations to exquisite precision in six frequency bands from 27 to 280 GHz. SO will rapidly advance CMB science while informing the design of future observatories such as CMB-S4., Comment: Astro2020 Decadal Project Whitepaper. arXiv admin note: text overlap with arXiv:1808.07445

Published
2019

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

Author

Matsuda, Frederick, Lowry, Lindsay, Suzuki, Aritoki, Faundez, Mario Aguilar, Arnold, Kam, Barron, Darcy, Bianchini, Federico, Cheung, Kolen, Chinone, Yuji, Elleflot, Tucker, Fabbian, Giulio, Goeckner-Wald, Neil, Hasegawa, Masaya, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Lee, Adrian, Navaroli, Martin, Nishino, Haruki, Paar, Hans, Puglisi, Giuseppe, Richards, Paul, Seibert, Joseph, Siritanasak, Praween, Tajima, Osamu, Takatori, Sayuri, Tsai, Calvin, and Westbrook, Ben

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

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

Published
2019
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11. Evidence for the Cross-correlation between Cosmic Microwave Background Polarization Lensing from POLARBEAR and Cosmic Shear from Subaru Hyper Suprime-Cam

Author

Namikawa, Toshiya, Chinone, Yuji, Miyatake, Hironao, Oguri, Masamune, Takahashi, Ryuichi, Kusaka, Akito, Katayama, Nobuhiko, Adachi, Shunsuke, Aguilar, Mario, Aihara, Hiroaki, Ali, Aamir, Armstrong, Robert, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beck, Dominic, Beckman, Shawn, Bianchini, Federico, Boettger, David, Borrill, Julian, Cheung, Kolen, Corbett, Lance, Crowley, Kevin T., Bouhargani, Hamza El, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feng, Chang, Galitzki, Nicholas, Goeckner-Wald, Neil, Groh, John, Hamada, Takaho, Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Jeong, Oliver, Kaneko, Daisuke, Keating, Brian, Lee, Adrian T., Leon, David, Linder, Eric, Lowry, Lindsay Ng, Mangu, Aashrita, Matsuda, Frederick, Minami, Yuto, Miyazaki, Satoshi, Murayama, Hitoshi, Navaroli, Martin, Nishino, Haruki, Nishizawa, Atsushi J., Pham, Anh Thi Phuong, Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Sherwin, Blake D., Silva-Feaver, Maximiliano, Siritanasak, Praween, Speagle, Joshua S., Stompor, Radek, Suzuki, Aritoki, Tait, Philip J., Tajima, Osamu, Takada, Masahiro, Takakura, Satoru, Takatori, Sayuri, Tanabe, Daiki, Tanaka, Masayuki, Teply, Grant P., Tsai, Calvin, Verges, Clara, Westbrook, Ben, Zhou, Yuyang, Collaboration, The POLARBEAR, and Collaboration, the Subaru HSC SSP

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the first measurement of cross-correlation between the lensing potential, reconstructed from cosmic microwave background (CMB) {\it polarization} data, and the cosmic shear field from galaxy shapes. This measurement is made using data from the POLARBEAR CMB experiment and the Subaru Hyper Suprime-Cam (HSC) survey. By analyzing an 11~deg$^2$ overlapping region, we reject the null hypothesis at 3.5$\sigma$\ and constrain the amplitude of the {\bf cross-spectrum} to $\widehat{A}_{\rm lens}=1.70\pm 0.48$, where $\widehat{A}_{\rm lens}$ is the amplitude normalized with respect to the Planck~2018{} prediction, based on the flat $\Lambda$ cold dark matter cosmology. The first measurement of this {\bf cross-spectrum} without relying on CMB temperature measurements is possible due to the deep POLARBEAR map with a noise level of ${\sim}$6\,$\mu$K-arcmin, as well as the deep HSC data with a high galaxy number density of $n_g=23\,{\rm arcmin^{-2}}$. We present a detailed study of the systematics budget to show that residual systematics in our results are negligibly small, which demonstrates the future potential of this cross-correlation technique., Comment: 16 pages, 5 figures, Accepted for publication in ApJ

Published
2019
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13. Measurements of tropospheric ice clouds with a ground-based CMB polarization experiment, POLARBEAR

Author

Takakura, Satoru, Aguilar-Faúndez, Mario A. O., Akiba, Yoshiki, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beck, Dominic, Bianchini, Federico, Boettger, David, Borrill, Julian, Cheung, Kolen, Chinone, Yuji, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feng, Chang, Goeckner-Wald, Neil, Hamada, Takaho, Hasegawa, Masaya, Hazumi, Masashi, Howe, Logan, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Krachmalnicoff, Nicoletta, Kusaka, Akito, Lee, Adrian T., Lowry, Lindsay N., Matsuda, Frederick T., May, Andrew J., Minami, Yuto, Navaroli, Martin, Nishino, Haruki, Piccirillo, Lucio, Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Segawa, Yuuko, Silva-Feaver, Maximiliano, Siritanasak, Praween, Suzuki, Aritoki, Tajima, Osamu, Takatori, Sayuri, Tanabe, Daiki, Teply, Grant P., and Tsai, Calvin

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract

The polarization of the atmosphere has been a long-standing concern for ground-based experiments targeting cosmic microwave background (CMB) polarization. Ice crystals in upper tropospheric clouds scatter thermal radiation from the ground and produce a horizontally-polarized signal. We report the detailed analysis of the cloud signal using a ground-based CMB experiment, POLARBEAR, located at the Atacama desert in Chile and observing at 150 GHz. We observe horizontally-polarized temporal increases of low-frequency fluctuations ("polarized bursts," hereafter) of $\lesssim$0.1 K when clouds appear in a webcam monitoring the telescope and the sky. The hypothesis of no correlation between polarized bursts and clouds is rejected with $>$24$\sigma$ statistical significance using three years of data. We consider many other possibilities including instrumental and environmental effects, and find no other reasons other than clouds that can explain the data better. We also discuss the impact of the cloud polarization on future ground-based CMB polarization experiments., Comment: 14 pages, 12 figures, 1 table, Submitted to ApJ

Published
2018
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14. The Simons Observatory: Science goals and forecasts

Author

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

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
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: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes (SATs) and one large-aperture 6-m telescope (LAT), 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 SATs will target the largest angular scales observable from Chile, mapping ~10% of the sky to a white noise level of 2 $\mu$K-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, $r$, at a target level of $\sigma(r)=0.003$. The LAT will map ~40% of the sky at arcminute angular resolution to an expected white noise level of 6 $\mu$K-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the LSST sky region and partially with DESI. 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., Comment: This paper presents an overview of the Simons Observatory science goals, details about the instrument will be presented in a companion paper. The author contribution to this paper is available at https://simonsobservatory.org/publications.php (Abstract abridged) -- matching version published in JCAP

Published
2018
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16. Performance of a continuously rotating half-wave plate on the POLARBEAR telescope

Author

Takakura, Satoru, Aguilar, Mario, Akiba, Yoshiki, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Fujino, Takuro, Galitzki, Nicholas, Goeckner-Wald, Neil, Halverson, Nils W., Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Krachmalnicoff, Nicoletta, Kusaka, Akito, Lee, Adrian T., Leon, David, Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Navaroli, Martin, Nishino, Haruki, Paar, Hans, Peloton, Julien, Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Suzuki, Aritoki, Tajima, Osamu, Takatori, Sayuri, and Teply, Grant

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Physics - Instrumentation and Detectors
Abstract

A continuously rotating half-wave plate (CRHWP) is a promising tool to improve the sensitivity to large angular scales in cosmic microwave background (CMB) polarization measurements. With a CRHWP, single detectors can measure three of the Stokes parameters, $I$, $Q$ and $U$, thereby avoiding the set of systematic errors that can be introduced by mismatches in the properties of orthogonal detector pairs. We focus on the implementation of CRHWPs in large aperture telescopes (i.e. the primary mirror is larger than the current maximum half-wave plate diameter of $\sim$0.5 m), where the CRHWP can be placed between the primary mirror and focal plane. In this configuration, one needs to address the intensity to polarization ($I{\rightarrow}P$) leakage of the optics, which becomes a source of 1/f noise and also causes differential gain systematics that arise from CMB temperature fluctuations. In this paper, we present the performance of a CRHWP installed in the POLARBEAR experiment, which employs a Gregorian telescope with a 2.5 m primary illumination pattern. The CRHWP is placed near the prime focus between the primary and secondary mirrors. We find that the $I{\rightarrow}P$ leakage is larger than the expectation from the physical properties of our primary mirror, resulting in a 1/f knee of 100 mHz. The excess leakage could be due to imperfections in the detector system, i.e. detector non-linearity in the responsivity and time-constant. We demonstrate, however, that by subtracting the leakage correlated with the intensity signal, the 1/f noise knee frequency is reduced to 32 mHz ($\ell \sim$39 for our scan strategy), which is very promising to probe the primordial B-mode signal. We also discuss methods for further noise subtraction in future projects where the precise temperature control of instrumental components and the leakage reduction will play a key role., Comment: 27 pages, 5 figures, 3 tables, published version in JCAP. Includes some minor corrections

Published
2017
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18. Sequential dependency for affective appraisal of food images

Author

Van der Burg, Erik, Toet, Alexander, Abbasi, Zahra, Brouwer, Anne-Marie, Van Erp, Jan B. F., Kallen, Victor L., Kaneko, Daisuke, Kim, Youjin (Eugene), Kinnear, Marise, de Kock, Henriëtte L., Kusbiantari, Dyah, Lee, Tzong-Ru, Liu, Yingxuan, Luhovyy, Bohdan L., MacEachern, Emily, Mezgebe, Abadi Gebre, Nikolova, Rouja, Olatunde, Ganiyat, Srisayekti, Wilis, Tahir, Muhammad Rizwan, Ushiama, Shota, and Yürek, Merve Aslıhan

Published
2021
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19. Deployment of Polarbear-2A

Author

Kaneko, Daisuke, Adachi, S., Ade, P. A. R., Aguilar Faúndez, 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., Dűnner, R., El-Bouhargani, H., Elleflot, T., Errard, J., Fabbian, G., Feeney, S. M., Feng, C., Fujino, T., Galitzki, N., Gilbert, A., Goeckner-Wald, N., Groh, J., Hall, G., Halverson, N. W., Hamada, T., Hasegawa, M., Hazumi, M., Hill, C. A., Howe, L., Inoue, Y., Jaehnig, G., Jeong, O., Katayama, N., Keating, B., Keskitalo, R., Kikuchi, S., Kisner, T., Krachmalnicoff, N., Kusaka, A., Lee, A. T., Leon, D., Linder, E., Lowry, L. N., Mangu, A., Matsuda, F., Minami, Y., Navaroli, M., Nishino, H., Peloton, J., Pham, A. T. P., Poletti, D., Puglisi, G., Reichardt, C. L., 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. P., Tomaru, T., Tsai, C., Verges, C., Westbrook, B., and Zhou, Y.

Published
2020
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20. Astro2020 APC White Paper Project: The Simons Observatory

Author

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

Subjects
Astrophysics
Abstract

The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile that promises to provide breakthrough discoveries in fundamental physics, cosmology, and astrophysics. Supported by the Simons Foundation, the Heising-Simons Foundation, and with contributions from collaborating institutions, SO will see first light in 2021 and start a five year survey in 2022. SO has 287 collaborators from 12 countries and 53 institutions, including 85 students and 90 postdocs. The SO experiment in its currently funded form (‘SO-Nominal’) consists of three 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT). Optimized for minimizing systematic errors in polarization measurements at large angular scales, the SATs will perform a deep, degree-scale survey of 10% of the sky to search for the signature of primordial gravitational waves. The LAT will survey 40% of the sky with arc-minute resolution. These observations will measure (or limit) the sum of neutrino masses, search for light relics, measure the early behavior of Dark Energy, and refine our understanding of the intergalactic medium, clusters and the role of feedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution of the Planck satellite, and roughly an order of magnitude increase in mapping speed over currently operating (“Stage 3”) experiments, SO will measure the CMB temperature and polarization fluctuations to exquisite precision in six frequency bands from 27 to 280 GHz. SO will rapidly advance CMB science while informing the design of future observatories such as CMB-S4. Construction of SO-Nominal is fully funded, and operations and data analysis are funded for part of the planned five-year observations. We will seek federal funding to complete the observations and analysis of SO-Nominal, at the $25M level. The SO has a low risk and cost efficient upgrade path – the 6 m LAT can accommodate almost twice the baseline number of detectors and the SATs can be duplicated at low cost. We will seek funding at the $75M level for an expansion of the SO (‘SO-Enhanced’) that fills the remaining focal plane in the LAT, adds three SATs, and extends operations by five years, substantially improving our science return. By this time SO may be operating as part of the larger CMB-S4 project. This white paper summarizes and extends material presented in, which describes the science goals of SO-Nominal, and which describe the instrument design.

Published
2019

23. On-site detector noise characterization of the POLARBEAR-2a receiver

Author

Farias, Nicole, primary, Russell, Megan, additional, Kaneko, Daisuke, additional, Takatori, Sayuri, additional, Lee, Adrian T., additional, Arnold, Kam, additional, Adkins, Tylor, additional, Barron, Darcy R., additional, Crowley, Kevin T., additional, Elleflot, Tucker, additional, Fujino, Takuro, additional, Hasegawa, Masaya, additional, Ito, Jennifer, additional, Lowry, Lindsay N., additional, Nishinomiya, Yume, additional, Raum, Christopher, additional, Siritanasak, Praween, additional, Westbrook, Benjamin, additional, and Yamada, Kyohei, additional

Published
2022
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27. Methods to assess food-evoked emotions across cultures

Author

Kaneko, Daisuke, van Erp, Jan B., Human Media Interaction, and Digital Society Institute

Subjects
digestive, oral, and skin physiology
Abstract

Traditionally, consumer science groups and food companies use self-report measures, in which people indicate how much they like a certain food after having tasted it, to predict consumers’ future buying behaviors. However, it has been suggested that food-evoked emotion may improve prediction of individuals’ food choice. It may reveal previously unknown product attributes that go beyond traditional sensory and acceptability measurements, and can be a valuable source of information for product development and marketing. Although many research groups acknowledge that the evaluation of food-evoked emotions is probably important to predict food choice behavior, and although many different emotion-association questionnaires and measures have been developed and used, it is still unclear how to best assess food-evoked emotions. This thesis investigated what (type of) measures are used to evaluate food-evoked emotions and to what extent these measures are able to capture food-evoked emotions. Also, we explored the added value of the different measures and their combination, all of these specifically in a cross-cultural context, where the same foods can be either novel or familiar, and where measures other than explicit, verbal measures are expected to be especially valuable. A new cross-cultural food image database and pictorial emotional response tool were developed. This thesis contributed to the methodology to more comprehensively and reliably measure food related emotions in crosscultural contexts. To achieve the goals, this thesis consists of two sections, ‘Measures to evaluate food-evoked emotion’ and ‘Measures of food-evoked emotion in cross-cultural context’.

Published
2022

32. The Influence of Alloy Composition and Heat-Treatments on the Shape Memory Properties in a Cu-Sn-X Alloy

Author

Muramatsu Naokuni, Kaneko Daisuke, Mahoto Takeda, and Nakajima Takanari

Subjects
Materials science, Stress induced martensite, Three point flexural test, Mechanical Engineering, Alloy, Shape-memory alloy, engineering.material, Condensed Matter Physics, Alloy composition, Microstructure, Mechanics of Materials, X-ray crystallography, engineering, General Materials Science, Composite material, Thermal analysis
Abstract

We have focused on shape-memory properties of Cu-Sn based ternary alloys in this study. We have attempted to suppress degradation at room temperature aging and to improve the amount of shape recovery by adding the third element to a binary Cu-Sn alloy. The attempt has successfully conducted in Cu-Sn-Mn alloy, the degradation due to aging at room temperature was suppressed and the thermal stability was improved. Furthermore, the present study revealed that Cu-Sn-Mn alloy exhibited a large super elastic recovery in three point bending tests. We have also investigated the shape-memory properties of Cu-Sn-Si alloys and revealed that the ternary alloy has achieved super-elastic recovery better than the Cu-Sn-Mn alloy in the three-point bending tests.

Published
2018

37. The Simons Observatory: The Large Aperture Telescope (LAT)

Author

Xu, Zhilei, primary, Adachi, Shunsuke, additional, Ade, Peter, additional, Beall, J. A., additional, Bhandarkar, Tanay, additional, Bond, J. Richard, additional, Chesmore, Grace E., additional, Chinone, Yuji, additional, Choi, Steve K., additional, Connors, Jake A., additional, Coppi, Gabriele, additional, Cothard, Nicholas F., additional, Crowley, Kevin D., additional, Devlin, Mark, additional, Dicker, Simon, additional, Dober, Bradley, additional, Duff, Shannon M., additional, Galitzki, Nicholas, additional, Gallardo, Patricio A., additional, Golec, Joseph E., additional, Gudmundsson, Jon E., additional, Haridas, Saianeesh K., additional, Harrington, Kathleen, additional, Hervias-Caimapo, Carlos, additional, Patty Ho, Shuay-Pwu, additional, Huber, Zachary B., additional, Hubmayr, Johannes, additional, Iuliano, Jeffrey, additional, Kaneko, Daisuke, additional, Kofman, Anna M., additional, Koopman, Brian J., additional, Lashner, Jack, additional, Limon, Michele, additional, Link, Michael J., additional, Lucas, Tammy J., additional, Matsuda, Frederick, additional, McCarrick, Heather, additional, Nati, Federico, additional, Niemack, Michael D., additional, Orlowski-Scherer, John, additional, Piccirillo, Lucio, additional, Sarmiento, Karen Perez, additional, Schaan, Emmanuel, additional, Silva-Feaver, Maximiliano, additional, Sonka, Rita, additional, Sutariya, Shreya, additional, Tajima, Osamu, additional, Teply, Grant P., additional, Terasaki, Tomoki, additional, Thornton, Robert, additional, Tucker, Carole, additional, Ullom, Joel, additional, Vavagiakis, Eve M., additional, Vissers, Michael R., additional, Walker, Samantha, additional, Whipps, Zachary, additional, Wollack, Edward J., additional, Zannoni, Mario, additional, Zhu, Ningfeng, additional, and Zonca, Andrea, additional

Published
2021
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42. Method for rapid performance validation of large TES bolometer array for POLARBEAR-2A using a coherent millimeter-wave source

Author

Segawa, Yuuko, primary, Hirose, Haruaki, additional, Kaneko, Daisuke, additional, Hasegawa, Masaya, additional, Adachi, Shunsuke, additional, Ade, Peter, additional, Faúndez, Mario Andrés Osvaldo Aguilar, additional, Akiba, Yoshiki, additional, Arnold, Kam, additional, Avva, Jessica, additional, Baccigalupi, Carlo, additional, Barron, Darcy, additional, Beck, Dominic, additional, Beckman, Shawn, additional, Bianchini, Federico, additional, Boettger, David, additional, Borrill, Julian, additional, Carron, Julien, additional, Chapman, Scott, additional, Cheung, Kolen, additional, Chinone, Yuji, additional, Crowley, Kevin, additional, Cukierman, Ari, additional, de Haan, Tijmen, additional, Dobbs, Matt, additional, Dunner, Rolando, additional, Bouhargani, Hamza El, additional, Elleflot, Tucker, additional, Errard, Josquin, additional, Fabbian, Giulio, additional, Feeney, Stephen, additional, Feng, Chang, additional, Fujino, Takuro, additional, Galitzki, Nicholas, additional, Goeckner-Wald, Neil, additional, Groh, John, additional, Hall, Grantland, additional, Halverson, Nils, additional, Hamada, Takaho, additional, Hazumi, Masashi, additional, Hill, Charles, additional, Howe, Logan, additional, Inoue, Yuki, additional, Ito, Jennifer, additional, Jaehnig, Greg, additional, Jeong, Oliver, additional, Katayama, Nobuhiko, additional, Keating, Brian, additional, Keskitalo, Reijo, additional, Kikuchi, Shuhei, additional, Kisner, Theodore, additional, Krachmalnicoff, Nicoletta, additional, Kusaka, Akito, additional, Lee, Adrian T., additional, Leon, David, additional, Linder, Eric, additional, Lowry, Lindsay Ng, additional, Mangu, Aashrita, additional, Matsuda, Frederick, additional, Minami, Yuto, additional, Montgomery, Josh, additional, Navaroli, Martin, additional, Nishino, Haruki, additional, Peloton, Julien, additional, Pham, Anh Thi Phuong, additional, Poletti, Davide, additional, Puglisi, Giuseppe, additional, Raum, Christopher, additional, Reichardt, Christian L., additional, Ross, Colin, additional, Silva-Feaver, Maximiliano, additional, Siritanasak, Praween, additional, Stompor, Radek, additional, Suzuki, Aritoki, additional, Tajima, Osamu, additional, Takakura, Satoru, additional, Takatori, Sayuri, additional, Tanabe, Daiki, additional, Teply, Grant P., additional, Tsai, Calvin, additional, Verges, Clara, additional, Westbrook, Ben, additional, and Zhou, Yuyang, additional

Published
2021
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45. The Simons Observatory Small Aperture Telescope overview

Author

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

Published
2020
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46. Data acquisition and management system for the CMB polarization experiment: Simons Array

Author

Nishino, Haruki, primary, Barron, Darcy, additional, Bender, Amy N., additional, Chinone, Yuji, additional, Crowley, Kevin T., additional, Elleflot, Tucker, additional, Groh, John, additional, Hasegawa, Masaya, additional, Hazumi, Masashi, additional, Hill, Charles A., additional, Hirose, Haruaki, additional, Howe, Logan, additional, Kaneko, Daisuke, additional, Kikuchi, Shuhei, additional, Kisner, Theodore, additional, Kusaka, Akito, additional, Montgomery, Joshua, additional, Rahlin, Alexandra S., additional, Siritanasak, Praween, additional, Smecher, Graeme, additional, Takakura, Satoru, additional, Takatori, Sayuri, additional, Tanabe, Daiki, additional, Westbrook, Benjamin, additional, Whitehorn, Nathan, additional, Zahn, Alex, additional, and Zhou, Yuyang, additional

Published
2020
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49. Double-Stranded RNA of Intestinal Commensal but Not Pathogenic Bacteria Triggers Production of Protective Interferon-β

Author

Kawashima, Tadaomi, Kosaka, Akemi, Yan, Huimin, Guo, Zijin, Uchiyama, Ryosuke, Fukui, Ryutaro, Kaneko, Daisuke, Kumagai, Yutaro, You, Dong-Ju, Carreras, Joaquim, Uematsu, Satoshi, Jang, Myoung Ho, Takeuchi, Osamu, Kaisho, Tsuneyasu, Akira, Shizuo, Miyake, Kensuke, Tsutsui, Hiroko, Saito, Takashi, Nishimura, Ikuko, and Tsuji, Noriko M.

Published
2013
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50. On-site detector noise characterization of the POLARBEAR-2A receiver

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Farias, Nicole, Russell, Megan, Kaneko, Daisuke, Takatori, Sayuri, Lee, Adrian T., Arnold, Kam, Adkins, Tylor, Barron, Darcy R., Crowley, Kevin T., Elleflot, Tucker, Fujino, Takuro, Hasegawa, Masaya, Ito, Jennifer, Lowry, Lindsay N., Nishinomiya, Yume, Raum, Christopher, Siritanasak, Praween, Westbrook, Benjamin, and Yamada, Kyohei

Published
2022
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