Author: "Barron, Darcy" - Searchworks@Jio Institute Digital Library Search Results

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218 results on '"Barron, Darcy"'

1. A measurement of atmospheric circular polarization with POLARBEAR

Author: Fujino, Takuro, Takakura, Satoru, Arani, Shahed Shayan, Barron, Darcy, Baccigalupi, Carlo, Chinone, Yuji, Errard, Josquin, Fabbian, Giulio, Feng, Chang, Halverson, Nils W., Hasegawa, Masaya, Hazumi, Masashi, Jeong, Oliver, Kaneko, Daisuke, Keating, Brian, Kusaka, Akito, Lee, Adrian, Matsumura, Tomotake, Piccirillo, Lucio, Reichardt, Christian L., Sakaguri, Kana, Siritanasak, Praween, and Yamada, Kyohei
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: At millimeter wavelengths, the atmospheric emission is circularly polarized owing to the Zeeman splitting of molecular oxygen by the Earth's magnetic field. We report a measurement of the signal in the 150 GHz band using 3 years of observations of the \textsc{Polarbear} project. Although the detectors are sensitive to linear polarization, we can measure the circular polarization because a continuously rotating half-wave plate in the optics converts part of circular polarization into linear polarization. The atmospheric circular polarization signal appears as a modulated signal at twice the frequency of rotation of the half-wave plate. We reconstruct the azimuthal gradient of the circular polarization signal and measure the dependencies on the scanning azimuth and the detector bandpass. We compare the signal with a simulation based on atmospheric emission theory, the detector bandpass, and the half-wave plate leakage spectrum model. We find the ratio of the observed azimuthal slope to the simulated slope is $0.92 \pm 0.01\rm{(stat)} \pm 0.07\rm{(sys)}$, which demonstrates that our measurement is consistent with theoretical prediction. This result validates our understanding of the instrument and reinforces the feasibility of measuring the circular polarization using the imperfection of the half-wave plate. Quantifying atmospheric circular polarization is the first step toward conducting a search for cosmological circular polarization at these wavelengths., Comment: 22 pages, 11 figures
Published: 2024

2. The European Low Frequency Survey on the Simons Array

Author: Mennella, Aniello, Arnold, Kam, Azzoni, Susanna, Baccigalupi, Carlo, Banday, A. J., Barreiro, Rita Belén, Barron, Darcy, Bersanelli, Marco, Casas, Francisco J., Casey, Sean, de la Hoz, Elena, Franceschet, Cristian, Jones, Michael E., Genóva-Santos, Ricardo T., Hoyland, R., Lee, Adrian T., Martinez-Gonzalez, Enrique, Montonati, Filippo, Rubiño-Martín, José-Alberto, Taylor, Angela, and Vielva, Patricio
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In this paper we present the European Low Frequency Survey (ELFS), a project that will enable foregrounds-free measurements of the primordial $B$-mode polarization and a detection of the tensor-to-scalar ratio, $r$, to a level $\sigma(r) = 0.001$ by measuring the Galactic and extra-galactic emissions in the 5--120\,GHz frequency window. Indeed, the main difficulty in measuring the B-mode polarization comes from the fact that many other processes in the Universe also emit polarized microwaves, which obscure the faint Cosmic Microwave Background (CMB) signal. The first stage of this project is being carried out in synergy with the Simons Array (SA) collaboration, installing a 5.5--11\,GHz (X-band) coherent receiver at the focus of one of the three 3.5\,m SA telescopes in Atacama, Chile, followed by the installation of the QUIJOTE-MFI2 in the 10--20 GHz range. We designate this initial iteration of the ELFS program as ELFS-SA. The receivers are equipped with a fully digital back-end that will provide a frequency resolution of 1\,MHz across the band, allowing us to clean the scientific signal from unwanted radio frequency interference, particularly from low-Earth orbit satellite mega constellations. This paper reviews the scientific motivation for ELFS and its instrumental characteristics, and provides an update on the development of ELFS-SA., Comment: SPIE conference on Astronomical Telescopes + Instrumentation, Yokohama, 16-22 June 2024. New version with correction in Eq. (3) arXiv admin note: text overlap with arXiv:2310.16509
Published: 2024

3. End-to-End Modeling of the TDM Readout System for CMB-S4

Author: Goldfinger, David C., Ahmed, Zeeshan, Barron, Darcy R., Doriese, W. Bertrand, Durkin, Malcolm, Filippini, Jeffrey P., Haller, Gunther, Henderson, Shawn W., Herbst, Ryan, Hubmayr, Johannes, Irwin, Kent, Reese, Ben, Sapozhnikov, Leonid, Thompson, Keith L., Ullom, Joel, and Vissers, Michael R.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The CMB-S4 experiment is developing next-generation ground-based microwave telescopes to observe the Cosmic Microwave Background with unprecedented sensitivity. This will require an order of magnitude increase in the 100 mK detector count, which in turn increases the demands on the readout system. The CMB-S4 readout will use time division multiplexing (TDM), taking advantage of faster switches and amplifiers in order to achieve an increased multiplexing factor. To facilitate the design of the new readout system, we have developed a model that predicts the bandwidth and noise performance of this circuity and its interconnections. This is then used to set requirements on individual components in order to meet the performance necessary for the full system. We present an overview of this model and compare the model results to the performance of both legacy and prototype readout hardware., Comment: This manuscript was submitted to the Journal of Low Temperature Physics as part of the special issue "LTD20", supporting the conference contribution RP-005
Published: 2023

4. The European Low Frequency Survey

Author: Mennella, Aniello, Arnold, Kam, Azzoni, Susanna, Baccigalupi, Carlo, Banday, Anthony, Barreiro, R. Belen, Barron, Darcy, Bersanelli, Marco, Casey, Sean, Colombo, Loris, de la Hoz, Elena, Franceschet, Cristian, Jones, Michael E., Genova-Santos, Ricardo T., Hoyland, Roger J., Lee, Adrian T., Martinez-Gonzalez, Enrique, Montonati, Filippo, Rubino-Martin, Jose-Alberto, Taylor, Angela, and Vielva, Patricio
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: In this paper we present the European Low Frequency Survey (ELFS), a project that will enable foregrounds-free measurements of primordial $B$-mode polarization to a level 10$^{-3}$ by measuring the Galactic and extra-Galactic emissions in the 5--120\,GHz frequency window. Indeed, the main difficulty in measuring the B-mode polarization comes not just from its sheer faintness, but from the fact that many other objects in the Universe also emit polarized microwaves, which mask the faint CMB signal. The first stage of this project will be carried out in synergy with the Simons Array (SA) collaboration, installing a 5.5--11 GHz coherent receiver at the focus of one of the three 3.5\,m SA telescopes in Atacama, Chile ("ELFS on SA"). The receiver will be equipped with a fully digital back-end based on the latest Xilinx RF System-on-Chip devices that will provide frequency resolution of 1\,MHz across the whole observing band, allowing us to clean the scientific signal from unwanted radio frequency interference, particularly from low-Earth orbit satellite mega-constellations. This paper reviews the scientific motivation for ELFS and its instrumental characteristics, and provides an update on the development of ELFS on SA., Comment: to appear in Proc. of the mm Universe 2023 conference, Grenoble (France), June 2023, published by F. Mayet et al. (Eds), EPJ Web of conferences, EDP Sciences
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. 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

7. Review of Radio Frequency Interference and Potential Impacts on the CMB-S4 Cosmic Microwave Background Survey

Author: Barron, Darcy R., Bender, Amy N., Birdwell, Ian E., Carlstrom, John E., Delabrouille, Jacques, Guns, Sam, Kovac, John, Lawrence, Charles R., Paine, Scott, and Whitehorn, Nathan
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Physics and Society
Abstract: CMB-S4 will map the cosmic microwave background to unprecedented precision, while simultaneously surveying the millimeter-wave time-domain sky, in order to advance our understanding of cosmology and the universe. CMB-S4 will observe from two sites, the South Pole and the Atacama Desert of Chile. A combination of small- and large-aperture telescopes with hundreds of thousands of polarization-sensitive detectors will observe in several frequency bands from 20-300 GHz, surveying more than 50 percent of the sky to arcminute resolution with unprecedented sensitivity. CMB-S4 seeks to make a dramatic leap in sensitivity while observing across a broad range of largely unprotected spectrum which is increasingly being utilized for terrestrial and satellite transmissions. Fundamental aspects of CMB instrument technology leave them vulnerable to radio frequency interference (RFI) across a wide range of frequencies, including frequencies outside of their observing bands. Ground-based CMB instruments achieve their extraordinary sensitivities by deploying large focal planes of superconducting bolometers to extremely dry, high-altitude sites, with large fractional bandwidths, wide fields of view, and years of integration time. Suitable observing sites have historically offered significant protection from RFI, both naturally through their extremely remote locations as well as through restrictions on local emissions. Since the coupling mechanisms are complex, safe levels or frequencies of emission that would not interfere with CMB measurements cannot always be determined through straightforward calculations. We discuss models of interference for various types of RFI relevant to CMB-S4, mitigation strategies, and the potential impacts on survey sensitivity., Comment: Presented at and published in the proceedings of SPIE Astronomical Telescopes and Instrumentation 2022
Published: 2022

8. Snowmass2021 Cosmic Frontier: Cosmic Microwave Background Measurements White Paper

Author: Chang, Clarence L., Huffenberger, Kevin M., Benson, Bradford A., Bianchini, Federico, Chluba, Jens, Delabrouille, Jacques, Flauger, Raphael, Hanany, Shaul, Jones, William C., Kogut, Alan J., McMahon, Jeffrey J., Meyers, Joel, Sehgal, Neelima, Simon, Sara M., Umilta, Caterina, Abazajian, Kevork N., Ahmed, Zeeshan, Akrami, Yashar, Anderson, Adam J., Ansarinejad, Behzad, Austermann, Jason, Baccigalupi, Carlo, Barkats, Denis, Barron, Darcy, Barry, Peter S., Battaglia, Nicholas, Baxter, Eric, Beck, Dominic, Bender, Amy N., Bennett, Charles, Beringue, Benjamin, Bischoff, Colin, Bleem, Lindsey, Bock, James, Bolliet, Boris, Bond, J Richard, Borrill, Julian, Brinckmann, Thejs, Brown, Michael L., Calabrese, Erminia, Carlstrom, John, Challinor, Anthony, Chang, Chihway, Chinone, Yuji, Clark, Susan E., Coulton, William, Cukierman, Ari, Cyr-Racine, Francis-Yan, Duff, Shannon M., Dvorkin, Cora, van Engelen, Alexander, Errard, Josquin, Eskilt, Johannes R., Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey, Freese, Katherine, Galitzki, Nicholas, Gawiser, Eric, Grin, Daniel, Grohs, Evan, Gruppuso, Alessandro, Gudmundsson, Jon E., Halverson, Nils W., Hamilton, Jean-Christophe, Harrington, Kathleen, Henrot-Versillé, Sophie, Hensley, Brandon, Hill, J. Colin, Hincks, Adam D., Hlozek, Renee, Holzapfel, William, Hotinli, Selim C., Hui, Howard, Ibitoye, Ayodeji, Johnson, Matthew, Johnson, Bradley R., Kang, Jae Hwan, Karkare, Kirit S., Knox, Lloyd, Kovac, John, Lau, Kenny, Legrand, Louis, Loverde, Marilena, Lubin, Philip, Ma, Yin-Zhe, Mroczkowski, Tony, Mukherjee, Suvodip, Münchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Niemack, Michael, Novosad, Valentine, Omori, Yuuki, Orlando, Giorgio, Pan, Zhaodi, Perotto, Laurence, Petroff, Matthew A., Pogosian, Levon, Pryke, Clem, Rahlin, Alexandra, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rephaeli, Yoel, Ruhl, John, Schaan, Emmanuel, Shandera, Sarah, Shimon, Meir, Soliman, Ahmed, Stark, Antony A., Starkman, Glenn D., Stompor, Radek, Thakur, Ritoban Basu, Trendafilova, Cynthia, Tristram, Matthieu, Trivedi, Pranjal, Tucker, Gregory, Di Valentino, Eleonora, Vieira, Joaquin, Vieregg, Abigail, Wang, Gensheng, Watson, Scott, Wenzl, Lukas, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Zegeye, David, and Zhang, Cheng
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: This is a solicited whitepaper for the Snowmass 2021 community planning exercise. The paper focuses on measurements and science with the Cosmic Microwave Background (CMB). The CMB is foundational to our understanding of modern physics and continues to be a powerful tool driving our understanding of cosmology and particle physics. In this paper, we outline the broad and unique impact of CMB science for the High Energy Cosmic Frontier in the upcoming decade. We also describe the progression of ground-based CMB experiments, which shows that the community is prepared to develop the key capabilities and facilities needed to achieve these transformative CMB measurements., Comment: contribution to Snowmass 2021
Published: 2022

9. Snowmass 2021 CMB-S4 White Paper

Author: Abazajian, Kevork, Abdulghafour, Arwa, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Ajello, Marco, Akerib, Daniel, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Amiri, Mandana, Anderson, Adam, Ansarinejad, Behzad, Archipley, Melanie, Arnold, Kam S., Ashby, Matt, Aung, Han, Baccigalupi, Carlo, Baker, Carina, Bakshi, Abhishek, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Barton, Paul, Thakur, Ritoban Basu, Battaglia, Nicholas, Beall, Jim, Bean, Rachel, Beck, Dominic, Belkner, Sebastian, Benabed, Karim, Bender, Amy N., Benson, Bradford A., Besuner, Bobby, Bethermin, Matthieu, Bhimani, Sanah, Bianchini, Federico, Biquard, Simon, Birdwell, Ian, Bischoff, Colin A., Bleem, Lindsey, Bocaz, Paulina, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, Francois R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chan, Victor, Chang, Clarence L., Chapman, Scott, Charles, Eric, Chauvin, Eric, Cheng, Cheng, Chesmore, Grace, Cheung, Kolen, Chinone, Yuji, Chluba, Jens, Cho, Hsiao-Mei Sherry, Choi, Steve, Clancy, Justin, Clark, Susan, Cooray, Asantha, Coppi, Gabriele, Corlett, John, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, Dai, Wei-Ming, Daley, Cail, Dart, Eli, Daues, Gregorg, de Haan, Tijmen, Deaconu, Cosmin, Delabrouille, Jacques, Derylo, Greg, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dober, Brad, Doriese, Randy, Duff, Shannon, Dutcher, Daniel, Dvorkin, Cora, Dünner, Rolando, Eftekhari, Tarraneh, Eimer, Joseph, Bouhargani, Hamza El, Elleflot, Tucker, Emerson, Nick, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Fanfani, Valentina, Fasano, Alessandro, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frisch, Josef, Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Giannakopoulos, Christos, Gilchriese, Murdock, Gluscevic, Vera, Goeckner-Wald, Neil, Goldfinger, David, Green, Daniel, Grimes, Paul, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Vic, Gudmundsson, Jon E., Gullett, Ian, Guns, Sam, Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Hand, Emma, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Herbst, Ryan, Hervias-Caimapo, Carlos, Hill, J. Colin, Hills, Richard, Hivon, Eric, Hlozek, Renée, Ho, Anna, Holder, Gil, Hollister, Matt, Holzapfel, William, Hood, John, Hotinli, Selim, Hryciuk, Alec, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, nez, Roberto Ibá, Ibitoye, Ayodeji, Ikape, Margaret, Irwin, Kent, Jacobus, Cooper, Jeong, Oliver, Johnson, Bradley R., Johnstone, Doug, Jones, William C., Joseph, John, Jost, Baptiste, Kang, Jae Hwan, Kaplan, Ari, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, King, Cesiley, Kisner, Theodore, Klein, Matthias, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Krolewski, Alex, Kubik, Donna, Kuhlmann, Steve, Kuo, Chao-Lin, Kusaka, Akito, Lähteenmäki, Anne, Lau, Kenny, Lawrence, Charles R., Lee, Adrian T., Legrand, Louis, Leitner, Matthaeus, Leloup, Clément, Lewis, Antony, Li, Dale, Linder, Eric, Liodakis, Ioannis, Liu, Jia, Long, Kevin, Louis, Thibaut, Loverde, Marilena, Lowry, Lindsay, Lu, Chunyu, Lubin, Phil, Ma, Yin-Zhe, Maccarone, Thomas, Madhavacheril, Mathew S., Maldonado, Felipe, Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, May, Jared, McCarrick, Heather, McCracken, Ken, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Miranda, Vivian, Mitchell, Don, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria Elena, Moshed, Magdy, Mroczkowski, Tony, Mukherjee, Suvodip, Münchmeyer, Moritz, Nagai, Daisuke, Nagarajappa, Chandan, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Nerval, Simran, Newburgh, Laura, Nguyen, Hogan, Nichols, Erik, Nicola, Andrina, Niemack, Michael D., Nord, Brian, Norton, Tim, Novosad, Valentine, O'Brient, Roger, Omori, Yuuki, Orlando, Giorgio, Osherson, Benjamin, Osten, Rachel, Padin, Stephen, Paine, Scott, Partridge, Bruce, Patil, Sanjaykumar, Petravick, Don, Petroff, Matthew, Pierpaoli, Elena, Pilleux, Mauricio, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Raveri, Marco, Reese, Ben, Reichardt, Christian L., Remazeilles, Mathieu, Rizzieri, Arianna, Rocha, Graca, Roe, Natalie A., Rotermund, Kaja, Roy, Anirban, Ruhl, John E., Saba, Joe, Sailer, Noah, Salatino, Maria, Saliwanchik, Benjamin, Sapozhnikov, Leonid, Rao, Mayuri Sathyanarayana, Saunders, Lauren, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Shiu, Corwin, Simon, Sara M., Singari, Baibhav, Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony A., Starkman, Glenn D., Steinbach, Bryan, Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Tandoi, Chris, Teply, Grant P., Thayer, Gregg, Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Trendafilova, Cynthia, Tristram, Matthieu, Tucker, Carole, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, van Marrewijk, Joshiwa, Vavagiakis, Eve M., Vergès, Clara, Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Wang, Guo-Jian, Watson, Scott, Watts, Duncan, Weaver, Chris, Wenzl, Lukas, Westbrook, Ben, White, Martin, Whitehorn, Nathan, Wiedlea, Andrew, Williams, Paul, Wilson, Robert, Winch, Harrison, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yefremenko, Volodymyr G., Yu, Cyndia, Zegeye, David, Zivick, Jeff, and Zonca, Andrea
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract: This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. We provide an overview of the science case, the technical design, and project plan., Comment: Contribution to Snowmass 2021. arXiv admin note: substantial text overlap with arXiv:1908.01062, arXiv:1907.04473
Published: 2022

10. CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

Author: Abazajian, Kevork, Addison, Graeme E, Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W, Alonso, David, Alvarez, Marcelo, Amin, Mustafa A, Anderson, Adam, Arnold, Kam S, Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S, Bartlett, James G, Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N, Benson, Bradford A, Bianchini, Federico, Bischoff, Colin A, Bleem, Lindsey, Bock, James J, Bocquet, Sebastian, Boddy, Kimberly K, Bond, J Richard, Borrill, Julian, Bouchet, François R, Brinckmann, Thejs, Brown, Michael L, Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E, Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L, Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M, Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P, Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A, Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E, Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W, Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, and Henderson, Shawn
Subjects: Particle and High Energy Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: CMB-S4 - the next-generation ground-based cosmic microwave background (CMB) experiment - is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the universe. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semianalytic projection tool, targeted explicitly toward optimizing constraints on the tensor-to-scalar ratio, r, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2-3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments, given a desired scientific goal. To form a closed-loop process, we couple this semianalytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for r > 0.003 at greater than 5σ, or in the absence of a detection, of reaching an upper limit of r < 0.001 at 95% CL.
Published: 2022

11. Anomalous Frequency Noise from the Megahertz Channelizing Resonators in Frequency-Division Multiplexed Transition Edge Sensor Readout

Author: Groh, John, Arnold, Kam, Avva, Jessica, Barron, Darcy, Crowley, Kevin T., Dobbs, Matt, de Haan, Tijmen, Holzapfel, William, Lee, Adrian, Lowry, Lindsay Ng, Montgomery, Joshua, Silva-Feaver, Maximiliano, Suzuki, Aritoki, and Whitehorn, Nathan
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Condensed Matter - Superconductivity
Abstract: Superconducting lithographed resonators have a broad range of current and potential applications in the multiplexed readout of cryogenic detectors. Here, we focus on LC bandpass filters with resonances in the 1-5 MHz range used in the transition edge sensor (TES) bolometer readout of the Simons Array cosmic microwave background (CMB) experiment. In this readout scheme, each detector signal amplitude-modulates a sinusoidal carrier tone at the resonance frequency of the detector's accompanying LC filter. Many modulated signals are transmitted over the same wire pair, and quadrature demodulation recovers the complex detector signal. We observe a noise in the resonant frequencies of the LC filters, which presents primarily as a current-dependent noise in the quadrature component after demodulation. This noise has a rich phenomenology, bearing many similarities to that of two-level system (TLS) noise observed in similar resonators in the GHz regime. These similarities suggest a common physical origin, thereby offering a new regime in which the underlying physics might be probed. We further describe an observed non-orthogonality between this noise and the detector responsivities, and present laboratory measurements that bound the resulting sensitivity penalty expected in the Simons Array. From these results, we do not anticipate this noise to appreciably affect the overall Simons Array sensitivity, nor do we expect it to limit future implementations., Comment: 5 pages, 5 figures, accepted to IEEE Transactions on Applied Superconductivity
Published: 2020
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12. The Simons Observatory: gain, bandpass and polarization-angle calibration requirements for B-mode searches

Author: Abitbol, Maximilian H., Alonso, David, Simon, Sara M., Lashner, Jack, Crowley, Kevin T., Ali, Aamir M., Azzoni, Susanna, Baccigalupi, Carlo, Barron, Darcy, Brown, Michael L., Calabrese, Erminia, Carron, Julien, Chinone, Yuji, Chluba, Jens, Coppi, Gabriele, Crowley, Kevin D., Devlin, Mark, Dunkley, Jo, Errard, Josquin, Fanfani, Valentina, Galitzki, Nicholas, Gerbino, Martina, Hill, J. Colin, Johnson, Bradley R., Jost, Baptiste, Keating, Brian, Krachmalnicoff, Nicoletta, Kusaka, Akito, Lee, Adrian T., Louis, Thibaut, Madhavacheril, Mathew S., McCarrick, Heather, McMahon, Jeffrey, Meerburg, P. Daniel, Nati, Federico, Nishino, Haruki, Page, Lyman A., Poletti, Davide, Puglisi, Giuseppe, Randall, Michael J., Rotti, Aditya, Spisak, Jacob, Suzuki, Aritoki, Teply, Grant P., Vergès, Clara, Wollack, Edward J., Xu, Zhilei, and Zannoni, Mario
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for 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: 2020
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13. CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

Author: Collaboration, CMB-S4, Abazajian, Kevork, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Anderson, Adam, Arnold, Kam S., Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Bianchini, Federico, Bischoff, Colin A., Bleem, Lindsey, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E., Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Hill, Charles, Hill, J. Colin, Hlozek, Renée, Ho, Shuay-Pwu Patty, Hoang, Thuong, Holder, Gil, Holzapfel, William, Hood, John, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Jones, William C., Kang, Jae Hwan, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kusaka, Akito, Lähteenmäki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Lubin, Phil, Madhavacheril, Mathew S., Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, McCarrick, Heather, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria, Mroczkowski, Tony, Mukherjee, Suvodip, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nord, Brian, Novosad, Valentine, O'Brient, Roger, Padin, Stephen, Palladino, Steven, Partridge, Bruce, Petravick, Don, Pierpaoli, Elena, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Rahlin, Alexandra, Rao, Mayuri Sathyanarayana, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John E., Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony, Starkman, Glenn D., Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vavagiakis, Eve M., Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Watson, Scott, Westbrook, Ben, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yang, H. Y. Eric, Yasini, Siavash, Yefremenko, Volodymyr G., Yoon, Ki Won, Young, Edward, Yu, Cyndia, and Zonca, Andrea
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: CMB-S4---the next-generation ground-based cosmic microwave background (CMB) experiment---is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semi-analytic projection tool, targeted explicitly towards optimizing constraints on the tensor-to-scalar ratio, $r$, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2--3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments given a desired scientific goal. To form a closed-loop process, we couple this semi-analytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for $r > 0.003$ at greater than $5\sigma$, or, in the absence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL., Comment: 24 pages, 8 figures, 9 tables, submitted to ApJ. arXiv admin note: text overlap with arXiv:1907.04473
Published: 2020
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14. The Simons Observatory: gain, bandpass and polarization-angle calibration requirements for B-mode searches

Author: Abitbol, Maximilian H, Alonso, David, Simon, Sara M, Lashner, Jack, Crowley, Kevin T, Ali, Aamir M, Azzoni, Susanna, Baccigalupi, Carlo, Barron, Darcy, Brown, Michael L, Calabrese, Erminia, Carron, Julien, Chinone, Yuji, Chluba, Jens, Coppi, Gabriele, Crowley, Kevin D, Devlin, Mark, Dunkley, Jo, Errard, Josquin, Fanfani, Valentina, Galitzki, Nicholas, Gerbino, Martina, Hill, J Colin, Johnson, Bradley R, Jost, Baptiste, Keating, Brian, Krachmalnicoff, Nicoletta, Kusaka, Akito, Lee, Adrian T, Louis, Thibaut, Madhavacheril, Mathew S, McCarrick, Heather, McMahon, Jeffrey, Meerburg, P Daniel, Nati, Federico, Nishino, Haruki, Page, Lyman A, Poletti, Davide, Puglisi, Giuseppe, Randall, Michael J, Rotti, Aditya, Spisak, Jacob, Suzuki, Aritoki, Teply, Grant P, Vergès, Clara, Wollack, Edward J, Xu, Zhilei, and Zannoni, Mario
Subjects: Particle and High Energy Physics, Physical Sciences, CMBR experiments, CMBR polarisation, gravitational waves and CMBR polarization, cosmological parameters from CMBR, astro-ph.CO, astro-ph.IM, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Astronomical sciences, Particle and high energy physics
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 Δ r∼10-3, 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 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 O(10%) at most. We validate these results by reanalyzing the latest publicly available data from the 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.
Published: 2021

15. Measurement of the Cosmic Microwave Background Polarization Lensing Power Spectrum from Two Years of POLARBEAR Data

Author: Faúndez, Mario Aguilar, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beck, Dominic, Beckman, Shawn, Bianchini, Federico, Carron, Julien, Cheung, Kolen, Chinone, Yuji, Bouhargani, Hamza El, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feng, Chang, Fujino, Takuro, Goeckner-Wald, Neil, Hamada, Takaho, Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles A., Hirose, Haruaki, Jeong, Oliver, Katayama, Nobuhiko, Keating, Brian, Kikuchi, Shuhei, Kusaka, Akito, Lee, Adrian T., Leon, David, Linder, Eric, Lowry, Lindsay Ng, Matsuda, Frederick, Matsumura, Tomotake, Minami, Yuto, Navaroli, Martin, Nishino, Haruki, Pham, Anh Thi Phuong, Poletti, Davide, Puglisi, Giuseppe, Reichardt, Christian L, Segawa, Yuuko, Sherwin, Blake D, Silva-Feaver, Maximiliano, Siritanasak, Praween, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Takatori, Sayuri, Tanabe, Daiki, Teply, Grant P., and Tsai, Calvin
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a measurement of the gravitational lensing deflection power spectrum reconstructed with two seasons cosmic microwave background polarization data from the POLARBEAR experiment. Observations were taken at 150 GHz from 2012 to 2014 which survey three patches of sky totaling 30 square degrees. We test the consistency of the lensing spectrum with a Cold Dark Matter (CDM) cosmology and reject the no-lensing hypothesis at a confidence of 10.9 sigma including statistical and systematic uncertainties. We observe a value of A_L = 1.33 +/- 0.32 (statistical) +/- 0.02 (systematic) +/- 0.07 (foreground) using all polarization lensing estimators, which corresponds to a 24% accurate measurement of the lensing amplitude. Compared to the analysis of the first year data, we have improved the breadth of both the suite of null tests and the error terms included in the estimation of systematic contamination.
Published: 2019
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16. CMB-S4 Decadal Survey APC White Paper

Author: Abazajian, Kevork, Addison, Graeme, Adshead, Peter, Ahmed, Zeeshan, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Anderson, Adam, Arnold, Kam S., Baccigalupi, Carlo, Bailey, Kathy, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Baxter, Eric, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Berger, Edo, Bhimani, Sanah, Bischoff, Colin A., Bleem, Lindsey, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly, Bonato, Matteo, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brown, Michael L., Bryan, Sean, Burkhart, Blakesley, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, de Zotti, Gianfranco, Delabrouille, Jacques, Demarteau, Marcel, Devlin, Mark, Di Valentino, Eleonora, Dobbs, Matt, Duff, Shannon, Duivenvoorden, Adriaan, Dvorkin, Cora, Edwards, William, Eimer, Joseph, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gilchriese, Murdock, Gluscevic, Vera, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Victor, Gudmundsson, Jon E., Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Henning, Jason W., Hill, J. Colin, Hlozek, Renée, Holder, Gil, Holzapfel, William, Hubmayr, Johannes, Huffenberger, Kevin M., Huffer, Michael, Hui, Howard, Irwin, Kent, Johnson, Bradley R., Johnstone, Doug, Jones, William C., Karkare, Kirit, Katayama, Nobuhiko, Kerby, James, Kernovsky, Sarah, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kurita, Nadine, Kusaka, Akito, Lahteenmaki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Madhavacheril, Mathew S., Mantz, Adam, Matsuda, Frederick, Mauskopf, Philip, McMahon, Jeff, Meerburg, P. Daniel, Melin, Jean-Baptiste, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Mroczkowski, Tony, Mukherjee, Suvodip, Münchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Negrello, Mattia, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nordby, Martin, Novosad, Valentine, O'Connor, Paul, Obied, Georges, Padin, Stephen, Pandey, Shivam, Partridge, Bruce, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Rajagopalan, Srini, Raveri, Marco, Reichanadter, Mark, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John, Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sheehy, Christopher, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Somerville, Rachel, Staggs, Suzanne T., Stark, Antony, Stompor, Radek, Story, Kyle T., Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Timbie, Peter, Tomasi, Maurizio, Treu, Jesse I., Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vieira, Joaquin D., Vieregg, Abigail G., Vogelsberger, Mark, Wang, Gensheng, Watson, Scott, White, Martin, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yasini, Siavash, Yeck, James, Yoon, Ki Won, Young, Edward, and Zonca, Andrea
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies
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., Comment: Project White Paper submitted to the 2020 Decadal Survey, 10 pages plus references. arXiv admin note: substantial text overlap with arXiv:1907.04473
Published: 2019

17. 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

18. CMB-S4 Science Case, Reference Design, and Project Plan

Author: Abazajian, Kevork, Addison, Graeme, Adshead, Peter, Ahmed, Zeeshan, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Anderson, Adam, Arnold, Kam S., Baccigalupi, Carlo, Bailey, Kathy, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Baxter, Eric, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Berger, Edo, Bhimani, Sanah, Bischoff, Colin A., Bleem, Lindsey, Bocquet, Sebastian, Boddy, Kimberly, Bonato, Matteo, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brown, Michael L., Bryan, Sean, Burkhart, Blakesley, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, de Zotti, Gianfranco, Delabrouille, Jacques, Demarteau, Marcel, Devlin, Mark, Di Valentino, Eleonora, Dobbs, Matt, Duff, Shannon, Duivenvoorden, Adriaan, Dvorkin, Cora, Edwards, William, Eimer, Joseph, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gilchriese, Murdock, Gluscevic, Vera, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Victor, Gudmundsson, Jon E., Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Henning, Jason W., Hill, J. Colin, Hlozek, Renée, Holder, Gil, Holzapfel, William, Hubmayr, Johannes, Huffenberger, Kevin M., Huffer, Michael, Hui, Howard, Irwin, Kent, Johnson, Bradley R., Johnstone, Doug, Jones, William C., Karkare, Kirit, Katayama, Nobuhiko, Kerby, James, Kernovsky, Sarah, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kurita, Nadine, Kusaka, Akito, Lahteenmaki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Madhavacheril, Mathew S., Mantz, Adam, Matsuda, Frederick, Mauskopf, Philip, McMahon, Jeff, McQuinn, Matthew, Meerburg, P. Daniel, Melin, Jean-Baptiste, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Mroczkowski, Tony, Mukherjee, Suvodip, Münchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Negrello, Mattia, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nordby, Martin, Novosad, Valentine, O'Connor, Paul, Obied, Georges, Padin, Stephen, Pandey, Shivam, Partridge, Bruce, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Rajagopalan, Srini, Raveri, Marco, Reichanadter, Mark, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John, Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sheehy, Christopher, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Somerville, Rachel, Spergel, David, Staggs, Suzanne T., Stark, Antony, Stompor, Radek, Story, Kyle T., Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Timbie, Peter, Tomasi, Maurizio, Treu, Jesse I., Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vieira, Joaquin D., Vieregg, Abigail G., Vogelsberger, Mark, Wang, Gensheng, Watson, Scott, White, Martin, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yasini, Siavash, Yeck, James, Yoon, Ki Won, Young, Edward, and Zonca, Andrea
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Experiment
Abstract: We present the science case, reference design, and project plan for the Stage-4 ground-based cosmic microwave background experiment CMB-S4., Comment: 287 pages, 82 figures
Published: 2019

19. Astro2020 APC White Paper: The Early Career Perspective on the Coming Decade, Astrophysics Career Paths, and the Decadal Survey Process

Author: Moravec, Emily, Czekala, Ian, Follette, Kate, Ahmed, Zeeshan, Alpaslan, Mehmet, Amon, Alexandra, Armentrout, Will, Arney, Giada, Barron, Darcy, Bellm, Eric, Bender, Amy, Bridge, Joanna, Colon, Knicole, Datta, Rahul, DeRoo, Casey, Feng, Wanda, Florian, Michael, Gabriel, Travis, Hall, Kirsten, Hamden, Erika, Hathi, Nimish, Hawkins, Keith, Hoadley, Keri, Jensen-Clem, Rebecca, Kao, Melodie, Kara, Erin, Karkare, Kirit, Kiessling, Alina, Kimball, Amy, Kirkpatrick, Allison, La Plante, Paul, Leisenring, Jarron, Li, Miao, Lomax, Jamie, Lund, Michael B., McCleary, Jacqueline, Mills, Elisabeth, Montiel, Edward, Nelson, Nicholas, Nevin, Rebecca, Norris, Ryan, Ntampaka, Michelle, O'Donnell, Christine, Peretz, Eliad, Malagon, Andres Plazas, Prescod-Weinstein, Chanda, Pullen, Anthony, Rice, Jared, Roettenbacher, Rachael, Sanderson, Robyn, Simon, Jospeh, Smith, Krista Lynne, Stevenson, Kevin, Veach, Todd, Wetzel, Andrew, and Youngblood, Allison
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: In response to the need for the Astro2020 Decadal Survey to explicitly engage early career astronomers, the National Academies of Sciences, Engineering, and Medicine hosted the Early Career Astronomer and Astrophysicist Focus Session (ECFS) on October 8-9, 2018 under the auspices of Committee of Astronomy and Astrophysics. The meeting was attended by fifty six pre-tenure faculty, research scientists, postdoctoral scholars, and senior graduate students, as well as eight former decadal survey committee members, who acted as facilitators. The event was designed to educate early career astronomers about the decadal survey process, to solicit their feedback on the role that early career astronomers should play in Astro2020, and to provide a forum for the discussion of a wide range of topics regarding the astrophysics career path. This white paper presents highlights and themes that emerged during two days of discussion. In Section 1, we discuss concerns that emerged regarding the coming decade and the astrophysics career path, as well as specific recommendations from participants regarding how to address them. We have organized these concerns and suggestions into five broad themes. These include (sequentially): (1) adequately training astronomers in the statistical and computational techniques necessary in an era of "big data", (2) responses to the growth of collaborations and telescopes, (3) concerns about the adequacy of graduate and postdoctoral training, (4) the need for improvements in equity and inclusion in astronomy, and (5) smoothing and facilitating transitions between early career stages. Section 2 is focused on ideas regarding the decadal survey itself, including: incorporating early career voices, ensuring diverse input from a variety of stakeholders, and successfully and broadly disseminating the results of the survey., Comment: 9 pages; Astro2020 APC White Paper: State of the Profession Consideration
Published: 2019

20. 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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21. 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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22. Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

Author: Green, Daniel, Amin, Mustafa A., Meyers, Joel, Wallisch, Benjamin, Abazajian, Kevork N., Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Barron, Darcy, Battaglia, Nicholas, Baumann, Daniel, Bechtol, Keith, Bennett, Charles, Benson, Bradford, Beutler, Florian, Bischoff, Colin, Bleem, Lindsey, Bond, J. Richard, Borrill, Julian, Buckley-Geer, Elizabeth, Burgess, Cliff, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cooray, Asantha, Coulton, William, Craig, Nathaniel, Crawford, Thomas, Cyr-Racine, Francis-Yan, D'Amico, Guido, Demarteau, Marcel, Doré, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Ellison, John, van Engelen, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fabbian, Giulio, Filippini, Jeffrey, Flauger, Raphael, Foreman, Simon, Fuller, George, Garcia, Marcos A. G., García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Górski, Krzysztof M., Grin, Daniel, Grohs, Evan, Gudmundsson, Jon E., Hanany, Shaul, Handley, Will, Hill, J. Colin, Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Horiuchi, Shunsaku, Huterer, Dragan, Kadota, Kenji, Kamionkowski, Marc, Keeley, Ryan E., Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Lin, Tongyan, Loverde, Marilena, Madhavacheril, Mathew, Masui, Kiyoshi, McMahon, Jeff, McQuinn, Matthew, Meerburg, P. Daniel, Mirbabayi, Mehrdad, Motloch, Pavel, Mukherjee, Suvodip, Munõz, Julian B., Nagy, Johanna, Newburgh, Laura, Niemack, Michael D., Nomerotski, Andrei, Page, Lyman, Piacentni, Francesco, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Reichardt, Christian L., Rose, Benjamin, Rossi, Graziano, Ruhl, John, Schaan, Emmanuel, Schubnell, Michael, Schutz, Katelin, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Sherwin, Blake D., Simon, Sara, Slosar, Anže, Staggs, Suzanne, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Umiltà, Caterina, Di Valentino, Eleonora, Vargas-Magaña, M., Vieregg, Abigail, Watson, Scott, Weiler, Thomas, Whitehorn, Nathan, Wu, W. L. K., Xu, Weishuang, Xu, Zhilei, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zhu, Ningfeng, and Zuntz, Joe
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract: The hot dense environment of the early universe is known to have produced large numbers of baryons, photons, and neutrinos. These extreme conditions may have also produced other long-lived species, including new light particles (such as axions or sterile neutrinos) or gravitational waves. The gravitational effects of any such light relics can be observed through their unique imprint in the cosmic microwave background (CMB), the large-scale structure, and the primordial light element abundances, and are important in determining the initial conditions of the universe. We argue that future cosmological observations, in particular improved maps of the CMB on small angular scales, can be orders of magnitude more sensitive for probing the thermal history of the early universe than current experiments. These observations offer a unique and broad discovery space for new physics in the dark sector and beyond, even when its effects would not be visible in terrestrial experiments or in astrophysical environments. A detection of an excess light relic abundance would be a clear indication of new physics and would provide the first direct information about the universe between the times of reheating and neutrino decoupling one second later., Comment: 5 pages + references; 1 figure; science white paper submitted to the Astro2020 decadal survey
Published: 2019

23. Science from an Ultra-Deep, High-Resolution Millimeter-Wave Survey

Author: Sehgal, Neelima, Nguyen, Ho Nam, Meyers, Joel, Munchmeyer, Moritz, Mroczkowski, Tony, Di Mascolo, Luca, Baxter, Eric, Cyr-Racine, Francis-Yan, Madhavacheril, Mathew, Beringue, Benjamin, Holder, Gil, Nagai, Daisuke, Dicker, Simon, Dvorkin, Cora, Ferraro, Simone, Fuller, George M., Gluscevic, Vera, Han, Dongwon, Jain, Bhuvnesh, Johnson, Bradley, Klaassen, Pamela, Meerburg, Daan, Motloch, Pavel, Spergel, David N., van Engelen, Alexander, Adshead, Peter, Armstrong, Robert, Baccigalupi, Carlo, Barron, Darcy, Basu, Kaustuv, Benson, Bradford, Beutler, Florian, Bond, J. Richard, Borrill, Julian, Calabrese, Erminia, Darwish, Omar, Denny, S. Lucas, Douglass, Kelly A., Essinger-Hileman, Tom, Foreman, Simon, Frayer, David, Gerbino, Martina, Gontcho, Satya Gontcho A, Grohs, Evan B., Gupta, Nikhel, Hill, J. Colin, Hirata, Christopher M., Hotinli, Selim, Johnson, Matthew C., Kamionkowski, Marc, Kovetz, Ely D., Lau, Erwin T., Liguori, Michele, Namikawa, Toshiya, Newburgh, Laura, Partridge, Bruce, Piacentni, Francesco, Rose, Benjamin, Rossi, Graziano, Saliwanchik, Benjamin, Schaan, Emmanuel, Shan, Huanyuan, Simon, Sara, Slosar, Anže, Switzer, Eric R., Trac, Hy, Xu, Weishuang, Zaldarriaga, Matias, and Zemcov, Michael
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology
Abstract: Opening up a new window of millimeter-wave observations that span frequency bands in the range of 30 to 500 GHz, survey half the sky, and are both an order of magnitude deeper (about 0.5 uK-arcmin) and of higher-resolution (about 10 arcseconds) than currently funded surveys would yield an enormous gain in understanding of both fundamental physics and astrophysics. In particular, such a survey would allow for major advances in measuring the distribution of dark matter and gas on small-scales, and yield needed insight on 1.) dark matter particle properties, 2.) the evolution of gas and galaxies, 3.) new light particle species, 4.) the epoch of inflation, and 5.) the census of bodies orbiting in the outer Solar System., Comment: 5 pages + references; Submitted to the Astro2020 call for science white papers
Published: 2019

24. CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

Author: Collaboration, The CMB-S4, :, Abazajian, Kevork, Addison, Graeme E, Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W, Alonso, David, Alvarez, Marcelo, Amin, Mustafa A, Anderson, Adam, Arnold, Kam S, Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S, Bartlett, James G, Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N, Benson, Bradford A, Bianchini, Federico, Bischoff, Colin A, Bleem, Lindsey, Bock, James J, Bocquet, Sebastian, Boddy, Kimberly K, Bond, J Richard, Borrill, Julian, Bouchet, François R, Brinckmann, Thejs, Brown, Michael L, Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E, Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L, Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M, Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P, Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A, Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E, Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W, Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, and Hasselfield, Matthew
Subjects: astro-ph.CO
Abstract: CMB-S4---the next-generation ground-based cosmic microwave background (CMB)experiment---is set to significantly advance the sensitivity of CMBmeasurements and enhance our understanding of the origin and evolution of theUniverse, from the highest energies at the dawn of time through the growth ofstructure to the present day. Among the science cases pursued with CMB-S4, thequest for detecting primordial gravitational waves is a central driver of theexperimental design. This work details the development of a forecastingframework that includes a power-spectrum-based semi-analytic projection tool,targeted explicitly towards optimizing constraints on the tensor-to-scalarratio, $r$, in the presence of Galactic foregrounds and gravitational lensingof the CMB. This framework is unique in its direct use of information from theachieved performance of current Stage 2--3 CMB experiments to robustly forecastthe science reach of upcoming CMB-polarization endeavors. The methodologyallows for rapid iteration over experimental configurations and offers aflexible way to optimize the design of future experiments given a desiredscientific goal. To form a closed-loop process, we couple this semi-analytictool with map-based validation studies, which allow for the injection ofadditional complexity and verification of our forecasts with severalindependent analysis methods. We document multiple rounds of forecasts forCMB-S4 using this process and the resulting establishment of the currentreference design of the primordial gravitational-wave component of the Stage-4experiment, optimized to achieve our science goals of detecting primordialgravitational waves for $r > 0.003$ at greater than $5\sigma$, or, in theabsence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL.
Published: 2020

25. 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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26. 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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27. The Simons Observatory: Instrument Overview

Author: Galitzki, Nicholas, Ali, Aamir, Arnold, Kam S., Ashton, Peter C., Austermann, Jason E., Baccigalupi, Carlo, Baildon, Taylor, Barron, Darcy, Beall, James A., Beckman, Shawn, Bruno, Sarah Marie M., Bryan, Sean, Calisse, Paolo G., Chesmore, Grace E., Chinone, Yuji, Choi, Steve K., Coppi, Gabriele, Crowley, Kevin D., Crowley, Kevin T., Cukierman, Ari, Devlin, Mark J., Dicker, Simon, Dober, Bradley, Duff, Shannon M., Dunkley, Jo, Fabbian, Giulio, Gallardo, Patricio A., Gerbino, Martina, Goeckner-Wald, Neil, Golec, Joseph E., Gudmundsson, Jon E., Healy, Erin E., Henderson, Shawn, Hill, Charles A., Hilton, Gene C., Ho, Shuay-Pwu Patty, Howe, Logan A., Hubmayr, Johannes, Jeong, Oliver, Keating, Brian, Koopman, Brian J., Kuichi, Kenji, Kusaka, Akito, Lashner, Jacob, Lee, Adrian T., Li, Yaqiong, Limon, Michele, Lungu, Marius, Matsuda, Frederick, Mauskopf, Philip D., May, Andrew J., McCallum, Nialh, McMahon, Jeff, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John L., Parshley, Stephen C., Piccirillo, Lucio, Rao, Mayuri Sathyanarayana, Raum, Christopher, Salatino, Maria, Seibert, Joseph S., Sierra, Carlos, Silva-Feaver, Max, Simon, Sara M., Staggs, Suzanne T., Stevens, Jason R., Suzuki, Aritoki, Teply, Grant, Thornton, Robert, Tsai, Calvin, Ullom, Joel N., Vavagiakis, Eve M., Vissers, Michael R., Westbrook, Benjamin, Wollack, Edward J., Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Simons Observatory (SO) will make precise temperature and polarization measurements of the cosmic microwave background (CMB) using a set of telescopes which will cover angular scales between 1 arcminute and tens of degrees, contain over 60,000 detectors, and observe at frequencies between 27 and 270 GHz. SO will consist of a 6 m aperture telescope coupled to over 30,000 transition-edge sensor bolometers along with three 42 cm aperture refractive telescopes, coupled to an additional 30,000+ detectors, all of which will be located in the Atacama Desert at an altitude of 5190 m. The powerful combination of large and small apertures in a CMB observatory will allow us to sample a wide range of angular scales over a common survey area. SO will measure fundamental cosmological parameters of our universe, constrain primordial fluctuations, find high redshift clusters via the Sunyaev-Zel`dovich effect, constrain properties of neutrinos, and trace the density and velocity of the matter in the universe over cosmic time. The complex set of technical and science requirements for this experiment has led to innovative instrumentation solutions which we will discuss. The large aperture telescope will couple to a cryogenic receiver that is 2.4 m in diameter and nearly 3 m long, creating a number of technical challenges. Concurrently, we are designing the array of cryogenic receivers housing the 42 cm aperture telescopes. We will discuss the sensor technology SO will use and we will give an overview of the drivers for and designs of the SO telescopes and receivers, with their cold optical components and detector arrays.
Published: 2018
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28. BoloCalc: a sensitivity calculator for the design of Simons Observatory

Author: Hill, Charles A., Bruno, Sarah Marie M., Simon, Sara M., Ali, Aamir, Arnold, Kam S., Ashton, Peter C., Barron, Darcy, Bryan, Sean, Chinone, Yuji, Coppi, Gabriele, Crowley, Kevin T., Cukierman, Ari, Dicker, Simon, Dunkley, Jo, Fabbian, Giulio, Galitzki, Nicholas, Gallardo, Patricio A., Gudmundsson, Jon E., Hubmayr, Johannes, Keating, Brian, Kusaka, Akito, Lee, Adrian T., Matsuda, Frederick, Mauskopf, Philip D., McMahon, Jeffrey, Niemack, Michael D., Puglisi, Giuseppe, Rao, Mayuri Sathyanarayana, Salatino, Maria, Sierra, Carlos, Staggs, Suzanne, Suzuki, Aritoki, Teply, Grant, Ullom, Joel N., Westbrook, Benjamin, Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Simons Observatory (SO) is an upcoming experiment that will study temperature and polarization fluctuations in the cosmic microwave background (CMB) from the Atacama Desert in Chile. SO will field both a large aperture telescope (LAT) and an array of small aperture telescopes (SATs) that will observe in six bands with center frequencies spanning from 27 to 270~GHz. Key considerations during the SO design phase are vast, including the number of cameras per telescope, focal plane magnification and pixel density, in-band optical power and camera throughput, detector parameter tolerances, and scan strategy optimization. To inform the SO design in a rapid, organized, and traceable manner, we have created a Python-based sensitivity calculator with several state-of-the-art features, including detector-to-detector optical white-noise correlations, a handling of simulated and measured bandpasses, and propagation of low-level parameter uncertainties to uncertainty in on-sky noise performance. We discuss the mathematics of the sensitivity calculation, the calculator's object-oriented structure and key features, how it has informed the design of SO, and how it can enhance instrument design in the broader CMB community, particularly for CMB-S4., Comment: Submitted to the Proceedings of SPIE: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX
Published: 2018
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29. The Simons Observatory: Astro2020 Decadal Project Whitepaper

Author: Collaboration, The Simons Observatory, 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, 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, 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, and Gudmundsson, Jon E
Subjects: astro-ph.IM
Abstract: The Simons Observatory (SO) is a ground-based cosmic microwave background(CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile thatpromises to provide breakthrough discoveries in fundamental physics, cosmology,and astrophysics. Supported by the Simons Foundation, the Heising-SimonsFoundation, and with contributions from collaborating institutions, SO will seefirst light in 2021 and start a five year survey in 2022. SO has 287collaborators from 12 countries and 53 institutions, including 85 students and90 postdocs. The SO experiment in its currently funded form ('SO-Nominal') consists ofthree 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large ApertureTelescope (LAT). Optimized for minimizing systematic errors in polarizationmeasurements at large angular scales, the SATs will perform a deep,degree-scale survey of 10% of the sky to search for the signature of primordialgravitational waves. The LAT will survey 40% of the sky with arc-minuteresolution. These observations will measure (or limit) the sum of neutrinomasses, search for light relics, measure the early behavior of Dark Energy, andrefine our understanding of the intergalactic medium, clusters and the role offeedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution ofthe Planck satellite, and roughly an order of magnitude increase in mappingspeed over currently operating ("Stage 3") experiments, SO will measure the CMBtemperature and polarization fluctuations to exquisite precision in sixfrequency bands from 27 to 280 GHz. SO will rapidly advance CMB science whileinforming the design of future observatories such as CMB-S4.
Published: 2019

30. The Simons Observatory: science goals and forecasts

Author: 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, and Hill, Charles A
Subjects: Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Astronomical sciences, Particle and high energy physics
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

31. CMB-S4 Technology Book, First Edition

Author: Abitbol, Maximilian H., Ahmed, Zeeshan, Barron, Darcy, Thakur, Ritoban Basu, Bender, Amy N., Benson, Bradford A., Bischoff, Colin A., Bryan, Sean A., Carlstrom, John E., Chang, Clarence L., Chuss, David T., Crowley, Kevin T., Cukierman, Ari, de Haan, Tijmen, Dobbs, Matt, Essinger-Hileman, Tom, Filippini, Jeffrey P., Ganga, Ken, Gudmundsson, Jon E., Halverson, Nils W., Hanany, Shaul, Henderson, Shawn W., Hill, Charles A., Ho, Shuay-Pwu P., Hubmayr, Johannes, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Kernasovskiy, Sarah A., Kovac, John M., Kusaka, Akito, Lee, Adrian T., Maria, Salatino, Mauskopf, Philip, McMahon, Jeff J., Moncelsi, Lorenzo, Nadolski, Andrew W., Nagy, Johanna M., Niemack, Michael D., O'Brient, Roger C., Padin, Stephen, Parshley, Stephen C., Pryke, Clement, Roe, Natalie A., Rostem, Karwan, Ruhl, John, Simon, Sara M., Staggs, Suzanne T., Suzuki, Aritoki, Switzer, Eric R., Tajima, Osamu, Thompson, Keith L., Timbie, Peter, Tucker, Gregory S., Vieira, Joaquin D., Vieregg, Abigail G., Westbrook, Benjamin, Wollack, Edward J., Yoon, Ki Won, Young, Karl S., and Young, Edward Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: CMB-S4 is a proposed experiment to map the polarization of the Cosmic Microwave Background (CMB) to nearly the cosmic variance limit for angular scales that are accessible from the ground. The science goals and capabilities of CMB-S4 in illuminating cosmic inflation, measuring the sum of neutrino masses, searching for relativistic relics in the early universe, characterizing dark energy and dark matter, and mapping the matter distribution in the universe have been described in the CMB-S4 Science Book. This Technology Book is a companion volume to the Science Book. The ambitious science goals of CMB-S4, a "Stage-4" experiment, require a step forward in experimental capability from the current Stage=II experiments. To guide this process, we summarize the current state of CMB instrumentation technology, and identify R&D efforts necessary to advance it for use in CMB-S4. The book focuses on technical challenges in four broad areas: Telescope Design; Receiver Optics; Focal-Plane Optical Coupling; and Focal-Plane Sensor and Readout., Comment: 191 pages
Published: 2017

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

Author: Barron, Darcy, Chinone, Yuji, Kusaka, Akito, Borril, Julian, Errard, Josquin, Feeney, Stephen, Ferraro, Simone, Keskitalo, Reijo, Lee, Adrian T., Roe, Natalie A., Sherwin, Blake D., and Suzuki, Aritoki
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
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., Comment: 42 pages, 23 figures; minor English/grammar corrections
Published: 2017
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33. 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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34. Optimization study for the experimental configuration of CMB-S4

Author: Barron, Darcy, Chinone, Yuji, Kusaka, Akito, Borril, Julian, Errard, Josquin, Feeney, Stephen, Ferraro, Simone, Keskitalo, Reijo, Lee, Adrian T, Roe, Natalie A, Sherwin, Blake D, and Suzuki, Aritoki
Subjects: Particle and High Energy Physics, Physical Sciences, CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, gravitational waves and CMBR polarization, astro-ph.IM, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Astronomical sciences, Particle and high energy physics
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. CMB-S4 will consist of O(500,000) photon-noise-limited detectors that cover a wide range of angular scales in order to probe the cosmological signatures from both the early and late universe. It will measure a wide range of microwave frequencies to cleanly separate the CMB signals from galactic and extra-galactic foregrounds. 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. The framework combines cost and instrumental models with a cosmology forecasting tool, and evaluates the scientific sensitivity as a function of various instrumental parameters. The cost model also allows us to perform the analysis under a fixed-cost constraint, optimizing for the scientific output of the experiment given finite resources. 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 telescope aperture size, distribution of the detectors into different microwave frequencies, survey strategy and survey area, low-frequency noise performance, and balance between small and large aperture telescopes for hybrid configurations. Both types of configurations must cover both large (∼ degree) and small (∼ arcmin) angular scales, and the performance depends on assumptions for performance vs. angular scale. The configurations with large-aperture telescopes have a shallow optimum around 4-6 m in aperture diameter, assuming that large telescopes can achieve good performance for low-frequency noise. We explore some of the uncertainties of the instrumental model and cost parameters, and we find that the optimum has a weak dependence on these parameters. The hybrid configuration shows an even broader optimum, spanning a range of 4-10 m in aperture for the large telescopes. We also present two strawperson configurations as an outcome of this optimization study, and we discuss some ideas for improving our simple cost and instrumental models used here. There are several areas of this analysis that deserve further improvement. In our forecasting framework, we adopt a simple two-component foreground model with spatially varying power-law spectral indices. We estimate de-lensing performance statistically and ignore non-idealities such as anisotropic mode coverage, boundary effect, and possible foreground residual. Instrumental systematics, which is not accounted for in our analyses, may also influence the conceptual design. Further study of the instrumental and cost models will be one of the main areas of study by the entire CMB-S4 community. We hope that our framework will be useful for estimating the influence of these improvements in the future, and we will incorporate them in order to further improve the optimization.
Published: 2018

35. Making maps of Cosmic Microwave Background polarization for B-mode studies: the POLARBEAR example

Author: Poletti, Davide, Fabbian, Giulio, Jeune, Maude Le, Peloton, Julien, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Feeney, Stephen, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H., Jeong, Oliver, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Lee, Adrian T., Leon, David, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Navaroli, Martin, Paar, Hans, Puglisi, Giuseppe, Reichardt, Christian L., Ross, Colin, Siritanasak, Praween, Stebor, Nathan, Steinbach, Bryan, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant, and Whitehorn, Nathan
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Analysis of cosmic microwave background (CMB) datasets typically requires some filtering of the raw time-ordered data. Filtering is frequently used to minimize the impact of low frequency noise, atmospheric contributions and/or scan synchronous signals on the resulting maps. In this work we explicitly construct a general filtering operator, which can unambiguously remove any set of unwanted modes in the data, and then amend the map-making procedure in order to incorporate and correct for it. We show that such an approach is mathematically equivalent to the solution of a problem in which the sky signal and unwanted modes are estimated simultaneously and the latter are marginalized over. We investigate the conditions under which this amended map-making procedure can render an unbiased estimate of the sky signal in realistic circumstances. We then study the effects of time-domain filtering on the noise correlation structure in the map domain, as well as impact it may have on the performance of the popular pseudo-spectrum estimators. We conclude that although maps produced by the proposed estimators arguably provide the most faithful representation of the sky possible given the data, they may not straightforwardly lead to the best constraints on the power spectra of the underlying sky signal and special care may need to be taken to ensure this is the case. By contrast, simplified map-makers which do not explicitly correct for time-domain filtering, but leave it to subsequent steps in the data analysis, may perform equally well and be easier and faster to implement. We focus on polarization-sensitive measurements targeting the B-mode component of the CMB signal and apply the proposed methods to realistic simulations based on characteristics of an actual CMB polarization experiment, POLARBEAR., Comment: 26 pages
Published: 2016
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36. Making maps of cosmic microwave background polarization for B-mode studies: the POLARBEAR example

Author: Poletti, Davide, Fabbian, Giulio, Le Jeune, Maude, Peloton, Julien, Arnold, Kam, Baccigalupi, Carlo, Barron, Darcy, Beckman, Shawn, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Ducout, Anne, Elleflot, Tucker, Errard, Josquin, Feeney, Stephen, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Hasegawa, Masaya, Hazumi, Masashi, Hill, Charles, Howe, Logan, Inoue, Yuki, Jaffe, Andrew H, Jeong, Oliver, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Lee, Adrian T, Leon, David, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Navaroli, Martin, Paar, Hans, Puglisi, Giuseppe, Reichardt, Christian L, Ross, Colin, Siritanasak, Praween, Stebor, Nathan, Steinbach, Bryan, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant, and Whitehorn, Nathan
Subjects: Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, cosmic background radiation, cosmology: observations, astro-ph.IM, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: Analysis of cosmic microwave background (CMB) datasets typically requires some filtering of the raw time-ordered data. For instance, in the context of ground-based observations, filtering is frequently used to minimize the impact of low frequency noise, atmospheric contributions and/or scan synchronous signals on the resulting maps. In this work we have explicitly constructed a general filtering operator, which can unambiguously remove any set of unwanted modes in the data, and then amend the map-making procedure in order to incorporate and correct for it. We show that such an approach is mathematically equivalent to the solution of a problem in which the sky signal and unwanted modes are estimated simultaneously and the latter are marginalized over. We investigated the conditions under which this amended map-making procedure can render an unbiased estimate of the sky signal in realistic circumstances. We then discuss the potential implications of these observations on the choice of map-making and power spectrum estimation approaches in the context of B-mode polarization studies. Specifically, we have studied the effects of time-domain filtering on the noise correlation structure in the map domain, as well as impact it may haveon the performance of the popular pseudo-spectrum estimators. We conclude that although maps produced by the proposed estimators arguably provide the most faithful representation of the sky possible given the data, they may not straightforwardly lead to the best constraints on the power spectra of the underlying sky signal and special care may need to be taken to ensure this is the case. By contrast, simplified map-makers which do not explicitly correct for time-domain filtering, but leave it to subsequent steps in the data analysis, may perform equally well and be easier and faster to implement. We focused on polarization-sensitive measurements targeting the B-mode component of the CMB signal and apply the proposed methods to realistic simulations based on characteristics of an actual CMB polarization experiment, POLARBEAR. Our analysis and conclusions are however more generally applicable.
Published: 2017

37. POLARBEAR Constraints on Cosmic Birefringence and Primordial Magnetic Fields

Author: POLARBEAR Collaboration, Ade, Peter A. R., Arnold, Kam, Atlas, Matt, Baccigalupi, Carlo, Barron, Darcy, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Dobbs, Matt, Ducout, Anne, Dunner, Rolando, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feeney, Stephen, Feng, Chang, Gilbert, Adam, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Halverson, Nils W., Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Hill, Charles, Holzapfel, William L., Hori, Yasuto, Howe, Logan, Inoue, Yuki, Jaehnig, Gregory C., Jaffe, Andrew H., Jeong, Oliver, Katayama, Nobuhiko, Kaufman, Jonathan P., Keating, Brian, Kermish, Zigmund, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Jeune, Maude Le, Lee, Adrian T., Leitch, Erik M., Leon, David, Li, Yun, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Miller, Nathan, Montgomery, Josh, Myers, Michael J., Navaroli, Martin, Nishino, Haruki, Okamura, Takahiro, Paar, Hans, Peloton, Julien, Pogosian, Levon, Poletti, Davide, Puglisi, Giuseppe, Raum, Christopher, Rebeiz, Gabriel, Reichardt, Christian L., Richards, Paul L., Ross, Colin, Rotermund, Kaja M., Schenck, David E., Sherwin, Blake D., Shimon, Meir, Shirley, Ian, Siritanasak, Praween, Smecher, Graeme, Stebor, Nathan, Steinbach, Bryan, Suzuki, Aritoki, Suzuki, Jun-ichi, Tajima, Osamu, Takakura, Satoru, Tikhomirov, Alexei, Tomaru, Takayuki, Whitehorn, Nathan, Wilson, Brandon, Yadav, Amit, Zahn, Alex, and Zahn, Oliver
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We constrain anisotropic cosmic birefringence using four-point correlations of even-parity $E$-mode and odd-parity $B$-mode polarization in the cosmic microwave background measurements made by the POLARization of the Background Radiation (POLARBEAR) experiment in its first season of observations. We find that the anisotropic cosmic birefringence signal from any parity-violating processes is consistent with zero. The Faraday rotation from anisotropic cosmic birefringence can be compared with the equivalent quantity generated by primordial magnetic fields if they existed. The POLARBEAR nondetection translates into a 95% confidence level (C.L.) upper limit of 93 nanogauss (nG) on the amplitude of an equivalent primordial magnetic field inclusive of systematic uncertainties. This four-point correlation constraint on Faraday rotation is about 15 times tighter than the upper limit of 1380 nG inferred from constraining the contribution of Faraday rotation to two-point correlations of $B$-modes measured by Planck in 2015. Metric perturbations sourced by primordial magnetic fields would also contribute to the $B$-mode power spectrum. Using the POLARBEAR measurements of the $B$-mode power spectrum (two-point correlation), we set a 95% C.L. upper limit of 3.9 nG on primordial magnetic fields assuming a flat prior on the field amplitude. This limit is comparable to what was found in the Planck 2015 two-point correlation analysis with both temperature and polarization. We perform a set of systematic error tests and find no evidence for contamination. This work marks the first time that anisotropic cosmic birefringence or primordial magnetic fields have been constrained from the ground at subdegree scales., Comment: 10 pages, 5 figures. Phys. Rev. D Editors' Suggestion
Published: 2015
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38. POLARBEAR constraints on cosmic birefringence and primordial magnetic fields

Author: Ade, Peter AR, Arnold, Kam, Atlas, Matt, Baccigalupi, Carlo, Barron, Darcy, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Dobbs, Matt, Ducout, Anne, Dunner, Rolando, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feeney, Stephen, Feng, Chang, Gilbert, Adam, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Halverson, Nils W, Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Hill, Charles, Holzapfel, William L, Hori, Yasuto, Howe, Logan, Inoue, Yuki, Jaehnig, Gregory C, Jaffe, Andrew H, Jeong, Oliver, Katayama, Nobuhiko, Kaufman, Jonathan P, Keating, Brian, Kermish, Zigmund, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Le Jeune, Maude, Lee, Adrian T, Leitch, Erik M, Leon, David, Li, Yun, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Miller, Nathan, Montgomery, Josh, Myers, Michael J, Navaroli, Martin, Nishino, Haruki, Okamura, Takahiro, Paar, Hans, Peloton, Julien, Pogosian, Levon, Poletti, Davide, Puglisi, Giuseppe, Raum, Christopher, Rebeiz, Gabriel, Reichardt, Christian L, Richards, Paul L, Ross, Colin, Rotermund, Kaja M, Schenck, David E, Sherwin, Blake D, Shimon, Meir, Shirley, Ian, Siritanasak, Praween, Smecher, Graeme, Stebor, Nathan, Steinbach, Bryan, Suzuki, Aritoki, Suzuki, Jun-ichi, Tajima, Osamu, Takakura, Satoru, Tikhomirov, Alexei, Tomaru, Takayuki, Whitehorn, Nathan, Wilson, Brandon, Yadav, Amit, Zahn, Alex, and Zahn, Oliver
Subjects: Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Mathematical physics, Astronomical sciences, Particle and high energy physics
Abstract: We constrain anisotropic cosmic birefringence using four-point correlations of even-parity E-mode and odd-parity B-mode polarization in the cosmic microwave background measurements made by the POLARization of the Background Radiation (POLARBEAR) experiment in its first season of observations. We find that the anisotropic cosmic birefringence signal from any parity-violating processes is consistent with zero. The Faraday rotation from anisotropic cosmic birefringence can be compared with the equivalent quantity generated by primordial magnetic fields if they existed. The POLARBEAR nondetection translates into a 95% confidence level (C.L.) upper limit of 93 nanogauss (nG) on the amplitude of an equivalent primordial magnetic field inclusive of systematic uncertainties. This four-point correlation constraint on Faraday rotation is about 15 times tighter than the upper limit of 1380 nG inferred from constraining the contribution of Faraday rotation to two-point correlations of B-modes measured by Planck in 2015. Metric perturbations sourced by primordial magnetic fields would also contribute to the B-mode power spectrum. Using the POLARBEAR measurements of the B-mode power spectrum (two-point correlation), we set a 95% C.L. upper limit of 3.9 nG on primordial magnetic fields assuming a flat prior on the field amplitude. This limit is comparable to what was found in the Planck 2015 two-point correlation analysis with both temperature and polarization. We perform a set of systematic error tests and find no evidence for contamination. This work marks the first time that anisotropic cosmic birefringence or primordial magnetic fields have been constrained from the ground at subdegree scales.
Published: 2015

39. Adaptation of frequency-domain readout for Transition Edge Sensor bolometers for the POLARBEAR-2 Cosmic Microwave Background experiment

Author: Hattori, Kaori, Arnold, Kam, Barron, Darcy, Dobbs, Matt, de Haan, Tijmen, Harrington, Nicholas, Hasegawa, Masaya, Hazumi, Masashi, Holzapfel, William L., Keating, Brian, Lee, Adrian T., Morii, Hideki, Myers, Michael J., Smecher, Graeme, Suzuki, Aritoki, and Tomaru, Takayuki
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: The POLARBEAR-2 CosmicMicrowave Background (CMB) experiment aims to observe B-mode polarization with high sensitivity to explore gravitational lensing of CMB and inflationary gravitational waves. POLARBEAR-2 is an upgraded experiment based on POLARBEAR-1, which had first light in January 2012. For POLARBEAR-2, we will build a receiver that has 7,588 Transition Edge Sensor (TES) bolometers coupled to two-band (95 and 150 GHz) polarization-sensitive antennas. For the large array's readout, we employ digital frequency-domain multiplexing and multiplex 32 bolometers through a single superconducting quantum interference device (SQUID). An 8-bolometer frequency-domain multiplexing readout has been deployed on POLARBEAR-1 experiment. Extending that architecture to 32 bolometers requires an increase in the bandwidth of the SQUID electronics to 3 MHz. To achieve this increase in bandwidth, we use Digital Active Nulling (DAN) on the digital frequency multiplexing platform. In this paper, we present requirements and improvements on parasitic inductance and resistance of cryogenic wiring and capacitors used for modulating bolometers. These components are problematic above 1 MHz. We also show that our system is able to bias a bolometer in its superconducting transition at 3 MHz.
Published: 2013
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40. Performance of a 4 Kelvin pulse-tube cooled cryostat with dc SQUID amplifiers for bolometric detector testing

Author: Barron, Darcy, Atlas, Matt, Keating, Brian, Quillin, Ron, Stebor, Nathan, and Wilson, Brandon
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: The latest generation of cosmic microwave background (CMB) telescopes is searching for the undetected faint signature of gravitational waves from inflation in the polarized signal of the CMB. To achieve the unprecedented levels of sensitivity required, these experiments use arrays of superconducting Transition Edge Sensor (TES) bolometers that are cooled to sub-Kelvin temperatures for photon-noise limited performance. These TES detectors are read out using low- noise SQUID amplifiers. To rapidly test these detectors and similar devices in a laboratory setting, we constructed a cryogenic refrigeration chain consisting of a commercial two-stage pulse-tube cooler, with a base temperature of 3 K, and a closed-cycle 3He/4He/3He sorption cooler, with a base temperature of 220 mK. A commercial dc SQUID system, with sensors cooled to 4 K, was used as a highly-sensitive cryogenic ammeter. Due to the extreme sensitivity of SQUIDs to changing magnetic fields, there are several challenges involving cooling them with pulse-tube coolers. Here we describe the successful design and implementation of measures to reduce the vibration, electromagnetic interference, and other potential sources of noise associated with pulse-tube coolers., Comment: Published in the 17th International Cryocooler Conference proceedings
Published: 2013

41. Absolute polarization angle calibration using polarized diffuse Galactic emission observed by BICEP

Author: Matsumura, Tomotake, Ade, Peter, Barkats, Denis, Barron, Darcy, Battle, John O., Bierman, Evan M., Bock, James J., Chiang, H. Cynthia, Crill, Brendan P., Dowell, C. Darren, Duband, Lionel, Hivon, Eric F., Holzapfel, William L., Hristov, Viktor V., Jones, William C., Keating, Brian G., Kovac, John M., Kuo, Chao-Lin, Lange, Andrew E., Leitch, Erik M., Mason, Peter V., Nguyen, Hien T., Ponthieu, Nicolas, Pryke, Clem, Richter, Steffen, Rocha, Graca M., Takahashi, Yuki D., and Yoon, Ki Won
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a method of cross-calibrating the polarization angle of a polarimeter using BICEP Galactic observations. \bicep\ was a ground based experiment using an array of 49 pairs of polarization sensitive bolometers observing from the geographic South Pole at 100 and 150 GHz. The BICEP polarimeter is calibrated to +/-0.01 in cross-polarization and less than +/-0.7 degrees in absolute polarization orientation. BICEP observed the temperature and polarization of the Galactic plane (R.A= 100 degrees ~ 270 degrees and Dec. = -67 degrees ~ -48 degrees). We show that the statistical error in the 100 GHz BICEP Galaxy map can constrain the polarization angle offset of WMAP Wband to 0.6 degrees +\- 1.4 degrees. The expected 1 sigma errors on the polarization angle cross-calibration for Planck or EPIC are 1.3 degrees and 0.3 degrees at 100 and 150 GHz, respectively. We also discuss the expected improvement of the BICEP Galactic field observations with forthcoming BICEP2 and Keck observations., Comment: 13 pages, 10 figures and 2 tables. To appear in Proceedings of SPIE Astronomical Telescopes and Instrumentation 2010
Published: 2010
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42. End-to-End Modeling of the TDM Readout System for CMB-S4

Author: Goldfinger, David C., primary, Ahmed, Zeeshan, additional, Barron, Darcy R., additional, Doriese, W. Bertrand, additional, Durkin, Malcolm, additional, Filippini, Jeffery P., additional, Haller, Gunther, additional, Henderson, Shawn W., additional, Herbst, Ryan, additional, Hubmayr, Johannes, additional, Irwin, Kent, additional, Reese, Benjamin, additional, Sapozhnikov, Leonid, additional, Thompson, Keith L., additional, Ullom, Joel, additional, and Vissers, Michael R., additional
Published: 2023
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43. BoloCalc: a sensitivity calculator for the design of Simons Observatory (Erratum)

Author: Hill, Charles A., primary, Bruno, Sarah Marie, additional, Simon, Sara M., additional, Ali, Aamir, additional, Arnold, Kam S., additional, Ashton, Peter C., additional, Barron, Darcy, additional, Bryan, Sean, additional, Chinone, Yuji, additional, Coppi, Gabriele, additional, Crowley, Kevin T., additional, Cukierman, Ari J., additional, Dicker, Simon R., additional, Dunkley, Jo, additional, Fabbian, Giulio, additional, Galitzki, Nicholas, additional, Gallardo, Patricio A., additional, Gudmundsson, Jon E., additional, Hubmayr, Johannes, additional, Keating, Brian, additional, Kusaka, Akito, additional, Lee, Adrian T., additional, Matsuda, Frederick, additional, Mauskopf, Philip D., additional, McMahon, Jeffrey, additional, Niemack, Michael D., additional, Puglisi, Giuseppe, additional, Sathyanarayana Rao, Mayuri ., additional, Salatino, Maria, additional, Sierra, Carlos E., additional, Staggs, Suzanne, additional, Suzuki, Aritoki, additional, Teply, Grant, additional, Ullom, Joel N., additional, Westbrook, Benjamin, additional, Xu, Zhilei, additional, and Zhu, Ningfeng, additional
Published: 2023
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44. The POLARBEAR experiment

Author: Kermish, Zigmund D, Ade, Peter, Anthony, Aubra, Arnold, Kam, Barron, Darcy, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Dobbs, Matt A, Errard, Josquin, Fabbian, Giulio, Flanigan, Daniel, Fuller, George, Ghribi, Adnan, Grainger, Will, Halverson, Nils, Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Holzapfel, William L, Howard, Jacob, Hyland, Peter, Jaffe, Andrew, Keating, Brian, Kisner, Theodore, Lee, Adrian T, Le Jeune, Maude, Linder, Eric, Lungu, Marius, Matsuda, Frederick, Matsumura, Tomotake, Meng, Xiaofan, Miller, Nathan J, Morii, Hideki, Moyerman, Stephanie, Myers, Mike J, Nishino, Haruki, Paar, Hans, Quealy, Erin, Reichardt, Christian L, Richards, Paul L, Ross, Colin, Shimizu, Akie, Shimon, Meir, Shimmin, Chase, Sholl, Mike, Siritanasak, Praween, Spieler, Helmuth, Stebor, Nathan, Steinbach, Bryan, Stompor, Radek, Suzuki, Aritoki, Tomaru, Takayuki, Tucker, Carole, and Zahn, Oliver
Subjects: Cosmic Microwave Background, Inflation, Polarization, Bolometer, astro-ph.IM
Abstract: We present the design and characterization of the polarbear experiment. polarbear will measure the polarization of the cosmic microwave background (CMB) on angular scales ranging from the experiment's 3.5′ beam size to several degrees. The experiment utilizes a unique focal plane of 1,274 antenna-coupled, polarization sensitive TES bolometers cooled to 250 milliKelvin. Employing this focal plane along with stringent control over systematic errors, polarbear has the sensitivity to detect the expected small scale B-mode signal due to gravitational lensing and search for the large scale B-mode signal from inflationary gravitational waves. polarbear was assembled for an engineering run in the Inyo Mountains of California in 2010 and was deployed in late 2011 to the Atacama Desert in Chile. An overview of the instrument is presented along with characterization results from observations in Chile. © 2012 SPIE.
Published: 2012

45. Comparison of NIST SA13a and SA4b SQUID Array Amplifiers

Author: Silva-Feaver, Maximiliano, Arnold, Kam, Barron, Darcy, Denison, Edward V., Dobbs, Matt, Groh, John, Hilton, Gene, Hubmayr, Johannes, Irwin, Kent, Lee, Adrian, and Vale, Leila R.
Published: 2018
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46. 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

47. Conceptual design of the modular detector and readout system for the CMB-S4 survey experiment

Author: Barron, Darcy, primary, Ahmed, Zeeshan, additional, Aguilar, Jessica, additional, Anderson, Adam, additional, Baker, Carina, additional, Barry, Peter, additional, Beall, James, additional, Bender, Amy, additional, Benson, Bradford, additional, Besuner, Robert, additional, Cecil, Thomas, additional, Chang, Clarence, additional, Chapman, Scott, additional, Chesmore, Grace, additional, Derylo, Greg, additional, Doriese, W. Bertrand, additional, Duff, Shannon, additional, Elleflot, Tucker, additional, Filippini, Jeffrey, additional, Flaugher, Brenna, additional, Gomez, Jillian, additional, Grimes, Paul, additional, Gualtieri, Riccardo, additional, Gullett, Ian, additional, Haller, Gunther, additional, Henderson, Shawn, additional, Henke, Douglas, additional, Herbst, Ryan, additional, Huber, Anthony, additional, Hubmayr, Johannes, additional, Jonas, Michelle, additional, Joseph, John, additional, King, Cesiley, additional, Kovac, John, additional, Kubik, Donna, additional, Lisovenko, Marharyta, additional, McMahon, Jeffrey, additional, Moncelsi, Lorenzo, additional, Nagy, Johanna, additional, Osherson, Benjamin, additional, Reese, Benjamin, additional, Ruhl, John, additional, Sapozhnikov, Leonid, additional, Schillaci, Alessandro, additional, Simon, Sara, additional, Suzuki, Aritoki, additional, Wang, Gensheng, additional, Westbrook, Benjamin, additional, Yefremenko, Vladimir, additional, and Zhang, Jianjie, additional
Published: 2022
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48. 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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49. Review of radio frequency interference and potential impacts on the CMB-S4 cosmic microwave background survey

Author: Barron, Darcy, primary, Bender, Amy N., additional, Birdwell, Ian, additional, Carlstrom, John, additional, Delabrouille, Jacques, additional, Guns, Sam T., additional, Kovac, John M., additional, Lawrence, Charles R., additional, Paine, Scott N., additional, and Whitehorn, Nathan, additional
Published: 2022
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50. Correction to: Comparison of NIST SA13a and SA4b SQUID Array Amplifiers

Author: Silva-Feaver, Maximiliano, Arnold, Kam, Barron, Darcy, Denison, Edward, Dobbs, Matt, Groh, John, Hilton, Gene, Hubmayr, Johannes, Irwin, Kent, Lee, Adrian, and Vale, Leila
Published: 2019
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