Author: "Teply, Grant" - Searchworks@Jio Institute Digital Library Search Results

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217 results on '"Teply, Grant"'

1. The Simons Observatory: Design, integration, and testing of the small aperture telescopes

Author: Galitzki, Nicholas, Tsan, Tran, Spisak, Jake, Randall, Michael, Silva-Feaver, Max, Seibert, Joseph, Lashner, Jacob, Adachi, Shunsuke, Adkins, Sean M., Alford, Thomas, Arnold, Kam, Ashton, Peter C., Austermann, Jason E., Baccigalupi, Carlo, Bazarko, Andrew, Beall, James A., Bhimani, Sanah, Bixler, Bryce, Coppi, Gabriele, Corbett, Lance, Crowley, Kevin D., Crowley, Kevin T., Day-Weiss, Samuel, Dicker, Simon, Dow, Peter N., Duell, Cody J., Duff, Shannon M., Gerras, Remington G., Groh, John C., Gudmundsson, Jon E., Harrington, Kathleen, Hasegawa, Masaya, Healy, Erin, Henderson, Shawn W., Hubmayr, Johannes, Iuliano, Jeffrey, Johnson, Bradley R., Keating, Brian, Keller, Ben, Kiuchi, Kenji, Kofman, Anna M., Koopman, Brian J., Kusaka, Akito, Lee, Adrian T., Lew, Richard A., Lin, Lawrence T., Link, Michael J, Lucas, Tammy J., Lungu, Marius, Mangu, Aashrita, McMahon, Jeffrey J, Miller, Amber D., Moore, Jenna E., Morshed, Magdy, Nakata, Hironobu, Nati, Federico, Newburgh, Laura B., Nguyen, David V., Niemack, Michael D., Page, Lyman A., Sakaguri, Kana, Sakurai, Yuki, Rao, Mayuri Sathyanarayana, Saunders, Lauren J., Shroyer, Jordan E., Sugiyama, Junna, Tajima, Osamu, Takeuchi, Atsuto, Bua, Refilwe Tanah, Teply, Grant, Terasaki, Tomoki, Ullom, Joel N., Van Lanen, Jeffrey L., Vavagiakis, Eve M., Vissers, Michael R, Walters, Liam, Wang, Yuhan, Xu, Zhilei, Yamada, Kyohei, and Zheng, Kaiwen
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Simons Observatory (SO) is a cosmic microwave background (CMB) survey experiment that includes small-aperture telescopes (SATs) observing from an altitude of 5,200 m in the Atacama Desert in Chile. The SO SATs will cover six spectral bands between 27 and 280 GHz to search for primordial B-modes to a sensitivity of $\sigma(r)=0.002$, with quantified systematic errors well below this value. Each SAT is a self-contained cryogenic telescope with a 35$^\circ$ field of view, 42 cm diameter optical aperture, 40 K half-wave plate, 1 K refractive optics, and $<0.1$ K focal plane that holds $>12,000$ TES detectors. We describe the nominal design of the SATs and present details about the integration and testing for one operating at 93 and 145 GHz.
Published: 2024

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

Author: Adachi, Shunsuke, Adkins, Tylor, Baccigalupi, Carlo, Chinone, Yuji, Crowley, Kevin T., Errard, Josquin, Fabbian, Giulio, Feng, Chang, Fujino, Takuro, Hasegawa, Masaya, Hazumi, Masashi, Jeong, Oliver, Kaneko, Daisuke, Keating, Brian, Kusaka, Akito, Lee, Adrian T., Lonappan, Anto I., Minami, Yuto, Murata, Masaaki, Piccirillo, Lucio, Reichardt, Christian L., Siritanasak, Praween, Spisak, Jacob, Takakura, Satoru, Teply, Grant P., and Yamada, Kyohei
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Crab Nebula, also known as Tau A, is a polarized astronomical source at millimeter wavelengths. It has been used as a stable light source for polarization angle calibration in millimeter-wave astronomy. However, it is known that its intensity and polarization vary as a function of time at a variety of wavelengths. Thus, it is of interest to verify the stability of the millimeter-wave polarization. If detected, polarization variability may be used to better understand the dynamics of Tau~A, and for understanding the validity of Tau~A as a calibrator. One intriguing application of such observation is to use it for the search of axion-like particles (ALPs). Ultralight ALPs couple to photons through a Chern-Simons term, and induce a temporal oscillation in the polarization angle of linearly polarized sources. After assessing a number of systematic errors and testing for internal consistency, we evaluate the variability of the polarization angle of the Crab Nebula using 2015 and 2016 observations with the 150 GHz POLARBEAR instrument. We place a median 95% upper bound of polarization oscillation amplitude $A < 0.065^\circ$ over the oscillation frequencies from $0.75~\mathrm{year}^{-1}$ to $0.66~\mathrm{hour}^{-1}$. Assuming that no sources other than ALP are causing Tau A's polarization angle variation, that the ALP constitutes all the dark matter, and that the ALP field is a stochastic Gaussian field, this bound translates into a median 95% upper bound of ALP-photon coupling $g_{a\gamma\gamma} < 2.16\times10^{-12}\,\mathrm{GeV}^{-1}\times(m_a/10^{-21} \mathrm{eV})$ in the mass range from $9.9\times10^{-23} \mathrm{eV}$ to $7.7\times10^{-19} \mathrm{eV}$. This demonstrates that this type of analysis using bright polarized sources is as competitive as those using the polarization of cosmic microwave background in constraining ALPs., Comment: 24 pages, 19 figures, 5 tables
Published: 2024
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3. The Simons Observatory: Beam characterization for the Small Aperture Telescopes

Author: Dachlythra, Nadia, Duivenvoorden, Adriaan J., Gudmundsson, Jon E., Hasselfield, Matthew, Coppi, Gabriele, Adler, Alexandre E., Alonso, David, Azzoni, Susanna, Chesmore, Grace E., Fabbian, Giulio, Ganga, Ken, Gerras, Remington G., Jaffe, Andrew H., Johnson, Bradley R., Keating, Brian, Keskitalo, Reijo, Kisner, Theodore S., Krachmalnicoff, Nicoletta, Lungu, Marius, Matsuda, Frederick, Naess, Sigurd, Page, Lyman, Puddu, Roberto, Puglisi, Giuseppe, Simon, Sara M., Teply, Grant, Tsan, Tran, Wollack, Edward J., Wolz, Kevin, and Xu, Zhilei
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a map maker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the map maker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions and input beams. We additionally show the reconstruction quality as function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within a ~1.5% error for a multipole range l = 30 - 700 and an ~0.5% error for a multipole range l = 50 - 200. We conclude by using a harmonic-domain component separation algorithm to verify that the beam reconstruction errors and biases observed in our analysis do not significantly bias the Simons Observatory r-measurement., Comment: 23 pages, 21 figures, published in ApJ
Published: 2023
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4. 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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5. 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

6. 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

7. The Simons Observatory: Design and Measured Performance of a Carbon Fiber Strut for a Cryogenic Truss

Author: Crowley, Kevin D., Dow, Peter, Shroyer, Jordan E., Groh, John C., Dober, Bradley, Spisak, Jacob, Galitzki, Nicholas, Bhandarkar, Tanay, Devlin, Mark J., Dicker, Simon, Gallardo, Patricio A., Harrington, Kathleen, Johnson, Bradley R., Johnson, Delwin, Kofman, Anna M., Kusaka, Akito, Lee, Adrian, Limon, Michele, Iuliano, Jeffrey, Nati, Federico, Orlowski-Scherer, John, Page, Lyman, Randall, Michael, Teply, Grant, Tsan, Tran, Wollack, Edward J., Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: We present the design and measured performance of a new carbon fiber strut design that is used in a cryogenically cooled truss for the Simons Observatory Small Aperture Telescope (SAT). The truss consists of two aluminum 6061 rings separated by 24 struts. Each strut consists of a central carbon fiber tube fitted with two aluminum end caps. We tested the performance of the strut and truss by (i) cryogenically cycling and destructively pull-testing strut samples, (ii) non-destructively pull-testing the final truss, and (iii) measuring the thermal conductivity of the carbon fiber tubes. We found that the strut strength is limited by the mounting fasteners and the strut end caps, not the epoxy adhesive or the carbon fiber tube. This result is consistent with our numerical predictions. Our thermal measurements suggest that the conductive heat load through the struts (from 4 K to 1 K) will be less than 1 mW. This strut design may be a promising candidate for use in other cryogenic support structures.
Published: 2022
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8. The Simons Observatory: Constraining inflationary gravitational waves with multi-tracer B-mode delensing

Author: Namikawa, Toshiya, Lizancos, Anton Baleato, Robertson, Naomi, Sherwin, Blake D., Challinor, Anthony, Alonso, David, Azzoni, Susanna, Baccigalupi, Carlo, Calabrese, Erminia, Carron, Julien, Chinone, Yuji, Chluba, Jens, Coppi, Gabriele, Errard, Josquin, Fabbian, Giulio, Ferraro, Simone, Kalaja, Alba, Lewis, Antony, Madhavacheril, Mathew S., Meerburg, P. Daniel, Meyers, Joel, Nati, Federico, Orlando, Giorgio, Poletti, Davide, Puglisi, Giuseppe, Remazeilles, Mathieu, Sehgal, Neelima, Tajima, Osamu, Teply, Grant, van Engelen, Alexander, Wollack, Edward J., Xu, Zhilei, Yu, Byeonghee, Zhu, Ningfeng, and Zonca, Andrea
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We introduce and validate a delensing framework for the Simons Observatory (SO), which will be used to improve constraints on inflationary gravitational waves (IGWs) by reducing the lensing noise in measurements of the $B$-modes in CMB polarization. SO will initially observe CMB by using three small aperture telescopes and one large-aperture telescope. While polarization maps from small-aperture telescopes will be used to constrain IGWs, the internal CMB lensing maps used to delens will be reconstructed from data from the large-aperture telescope. Since lensing maps obtained from the SO data will be noise-dominated on sub-degree scales, the SO lensing framework constructs a template for lensing-induced $B$-modes by combining internal CMB lensing maps with maps of the cosmic infrared background from Planck as well as galaxy density maps from the LSST survey. We construct a likelihood for constraining the tensor-to-scalar ratio $r$ that contains auto- and cross-spectra between observed $B$-modes and the lensing $B$-mode template. We test our delensing analysis pipeline on map-based simulations containing survey non-idealities, but that, for this initial exploration, does not include contamination from Galactic and extragalactic foregrounds. We find that the SO survey masking and inhomogeneous and atmospheric noise have very little impact on the delensing performance, and the $r$ constraint becomes $\sigma(r)\approx 0.0015$ which is close to that obtained from the idealized forecasts in the absence of the Galactic foreground and is nearly a factor of two tighter than without delensing. We also find that uncertainties in the external large-scale structure tracers used in our multi-tracer delensing pipeline lead to bias much smaller than the $1\,\sigma$ statistical uncertainties., Comment: 22 pages, 14 figures
Published: 2021
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9. Simons Observatory: Constraining inflationary gravitational waves with multitracer B-mode delensing

Author: Namikawa, Toshiya, Lizancos, Anton Baleato, Robertson, Naomi, Sherwin, Blake D, Challinor, Anthony, Alonso, David, Azzoni, Susanna, Baccigalupi, Carlo, Calabrese, Erminia, Carron, Julien, Chinone, Yuji, Chluba, Jens, Coppi, Gabriele, Errard, Josquin, Fabbian, Giulio, Ferraro, Simone, Kalaja, Alba, Lewis, Antony, Madhavacheril, Mathew S, Meerburg, P Daniel, Meyers, Joel, Nati, Federico, Orlando, Giorgio, Poletti, Davide, Puglisi, Giuseppe, Remazeilles, Mathieu, Sehgal, Neelima, Tajima, Osamu, Teply, Grant, van Engelen, Alexander, Wollack, Edward J, Xu, Zhilei, Yu, Byeonghee, Zhu, Ningfeng, and Zonca, Andrea
Subjects: Astronomical Sciences, Physical Sciences, 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 introduce and validate a delensing framework for the Simons Observatory (SO), which will be used to improve constraints on inflationary gravitational waves by reducing the lensing noise in measurements of the B modes in CMB polarization. SO will initially observe CMB by using three small aperture telescopes and one large-aperture telescope. While polarization maps from small-aperture telescopes will be used to constrain inflationary gravitational waves, the internal CMB lensing maps used to delens will be reconstructed from data from the large-aperture telescope. Since lensing maps obtained from the SO data will be noise dominated on subdegree scales, the SO lensing framework constructs a template for lensing-induced B modes by combining internal CMB lensing maps with maps of the cosmic infrared background from Planck as well as galaxy density maps from the LSST survey. We construct a likelihood for constraining the tensor-to-scalar ratio r that contains auto and cross spectra between observed B modes and the lensing B-mode template. We test our delensing analysis pipeline on map-based simulations containing survey nonidealities, but that, for this initial exploration, does not include contamination from Galactic and extragalactic foregrounds. We find that the SO survey masking and inhomogeneous and atmospheric noise have very little impact on the delensing performance, and the r constraint becomes σ(r)≈0.0015 which is close to that obtained from the idealized forecasts in the absence of the Galactic foreground and is nearly a factor of 2 tighter than without delensing. We also find that uncertainties in the external large-scale structure tracers used in our multitracer delensing pipeline lead to bias much smaller than the 1σ statistical uncertainties.
Published: 2022

10. The Simons Observatory: the Large Aperture Telescope (LAT)

Author: Xu, Zhilei, Adachi, Shunsuke, Ade, Peter, Beall, J. A., Bhandarkar, Tanay, Bond, J. Richard, Chesmore, Grace E., Chinone, Yuji, Choi, Steve K., Connors, Jake A., Coppi, Gabriele, Cothard, Nicholas F., Crowley, Kevin D., Devlin, Mark, Dicker, Simon, Dober, Bradley, Duff, Shannon M., Galitzki, Nicholas, Gallardo, Patricio A., Golec, Joseph E., Gudmundsson, Jon E., Haridas, Saianeesh K., Harrington, Kathleen, Hervias-Caimapo, Carlos, Ho, Shuay-Pwu Patty, Huber, Zachary B., Hubmayr, Johannes, Iuliano, Jeffrey, Kaneko, Daisuke, Kofman, Anna M., Koopman, Brian J., Lashner, Jack, Limon, Michele, Link, Michael J., Lucas, Tammy J., Matsuda, Frederick, McCarrick, Heather, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Piccirillo, Lucio, Sarmiento, Karen Perez, Schaan, Emmanuel, Silva-Feaver, Maximiliano, Sonka, Rita, Sutariya, Shreya, Tajima, Osamu, Teply, Grant P., Terasaki, Tomoki, Thornton, Robert, Tucker, Carole, Ullom, Joel, Vavagiakis, Eve M., Vissers, Michael R., Walker, Samantha, Whipps, Zachary, Wollack, Edward J., Zannoni, Mario, Zhu, Ningfeng, and Zonca, Andrea
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Simons Observatory (SO) is a Cosmic Microwave Background (CMB) experiment to observe the microwave sky in six frequency bands from 30GHz to 290GHz. The Observatory -- at $\sim$5200m altitude -- comprises three Small Aperture Telescopes (SATs) and one Large Aperture Telescope (LAT) at the Atacama Desert, Chile. This research note describes the design and current status of the LAT along with its future timeline., Comment: 4 pages, 1 figure
Published: 2021
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11. The Simons Observatory Large Aperture Telescope Receiver

Author: Zhu, Ningfeng, Bhandarkar, Tanay, Coppi, Gabriele, Kofman, Anna M., Orlowski-Scherer, John L., Xu, Zhilei, Adachi, Shunsuke, Ade, Peter, Aiola, Simone, Austermann, Jason, Bazarko, Andrew O., Beall, James A., Bhimani, Sanah, Bond, J. Richard, Chesmore, Grace E., Choi, Steve K., Connors, Jake, Cothard, Nicholas F., Devlin, Mark, Dicker, Simon, Dober, Bradley, Duell, Cody J., Duff, Shannon M., Dünner, Rolando, Fabbian, Giulio, Galitzki, Nicholas, Gallardo, Patricio A., Golec, Joseph E., Haridas, Saianeesh K., Harrington, Kathleen, Healy, Erin, Ho, Shuay-Pwu Patty, Huber, Zachary B., Hubmayr, Johannes, Iuliano, Jeffrey, Johnson, Bradley R., Keatin, Brian, Kiuchi, Kenji, Koopman, Brian J., Lashner, Jack, Lee, Adrian T., Li, Yaqiong, Limon, Michele, Link, Michael, Lucas, Tammy J, McCarrick, Heather, Moore, Jenna, Nati, Federico, Newburgh, Laura B., Niemack, Michael D., Pierpaoli, Elena, Randall, Michael J., Sarmiento, Karen Perez, Saunders, Lauren J., Seibert, Joseph, Sierra, Carlos, Sonka, Rita, Spisak, Jacob, Sutariya, Shreya, Tajima, Osamu, Teply, Grant P., Thornton, Robert J., Tsan, Tran, Tucker, Carole, Ullom, Joel, Vavagiakis, Eve M., Vissers, Michael R., Walker, Samantha, Westbrook, Benjamin, Wollack, Edward J., and Zannoni, Mario
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Simons Observatory (SO) Large Aperture Telescope Receiver (LATR) will be coupled to the Large Aperture Telescope located at an elevation of 5,200 m on Cerro Toco in Chile. The resulting instrument will produce arcminute-resolution millimeter-wave maps of half the sky with unprecedented precision. The LATR is the largest cryogenic millimeter-wave camera built to date with a diameter of 2.4 m and a length of 2.6 m. It cools 1200 kg of material to 4 K and 200 kg to 100 mk, the operating temperature of the bolometric detectors with bands centered around 27, 39, 93, 145, 225, and 280 GHz. Ultimately, the LATR will accommodate 13 40 cm diameter optics tubes, each with three detector wafers and a total of 62,000 detectors. The LATR design must simultaneously maintain the optical alignment of the system, control stray light, provide cryogenic isolation, limit thermal gradients, and minimize the time to cool the system from room temperature to 100 mK. The interplay between these competing factors poses unique challenges. We discuss the trade studies involved with the design, the final optimization, the construction, and ultimate performance of the system.
Published: 2021
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12. Simons Observatory Small Aperture Telescope overview

Author: Kiuchi, Kenji, Adachi, Shunsuke, Ali, Aamir M., Arnold, Kam, Ashton, Peter, Austermann, Jason E., Bazako, Andrew, Beall, James A., Chinone, Yuji, Coppi, Gabriele, Crowley, Kevin D., Crowley, Kevin T., Dicker, Simon, Dober, Bradley, Duff, Shannon M., Fabbian, Giulio, Galitzki, Nicholas, Golec, Joseph E., Gudmundsson, Jon E., Harrington, Kathleen, Hasegawa, Masaya, Hattori, Makoto, Hill, Charles A., Ho, Shuay-Pwu Patty, Hubmayr, Johannes, Johnson, Bradley R., Kaneko, Daisuke, Katayama, Nobuhiko, Keating, Brian, Kusaka, Akito, Lashner, Jack, Lee, Adrian T., Matsuda, Frederick, McCarrick, Heather, Murata, Masaaki, Nati, Federico, Nishinomiya, Yume, Page, Lyman, Rao, Mayuri Sathyanarayana, Reichardt, Christian L., Sakaguri, Kana, Sakurai, Yuki, Seibert, Joseph, Spisak, Jacob, Tajima, Osamu, Teply, Grant P., Terasaki, Tomoki, Tsan, Tran, Walker, Samantha, Wollack, Edward J., Xu, Zhilei, Yamada, Kyohei, Zannoni, Mario, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Simons Observatory (SO) is a cosmic microwave background (CMB) experiment from the Atacama Desert in Chile comprising three small-aperture telescopes (SATs) and one large-aperture telescope (LAT). In total, SO will field over 60,000 transition-edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities. In this work, we focus on the SATs which are optimized to search for primordial gravitational waves that are detected as parity-odd polarization patterns called a B-modes on degree scales in the CMB. Each SAT employs a single optics tube with TES arrays operating at 100 mK. The high throughput optics system has a 42 cm aperture and a 35-degree field of view coupled to a 36 cm diameter focal plane. The optics consist of three metamaterial anti-re ection coated silicon lenses. Cryogenic ring baffles with engineered blackbody absorbers are installed in the optics tube to minimize the stray light. The entire optics tube is cooled to 1 K. A cryogenic continuously rotating half-wave plate near the sky side of the aperture stop helps to minimize the effect of atmospheric uctuations. The telescope warm baffling consists of a forebaffle, an elevation stage mounted co-moving shield, and a fixed ground shield that together control the far side-lobes and mitigates ground-synchronous systematics. We present the status of the SAT development., Comment: 8 pages, 6 figures
Published: 2021
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13. 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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14. The Simons Observatory: Metamaterial Microwave Absorber (MMA) and its Cryogenic Applications

Author: Xu, Zhilei, Chesmore, Grace E., Adachi, Shunsuke, Ali, Aamir M., Bazarko, Andrew, Coppi, Gabriele, Devlin, Mark, Devlin, Tom, Dicker, Simon R., Gallardo, Patricio A., Golec, Joseph E., Gudmundsson, Jon E., Harrington, Kathleen, Hattori, Makoto, Kofman, Anna, Kiuchi, Kenji, Kusaka, Akito, Limon, Michele, Matsuda, Frederick, McMahon, Jeff, Nati, Federico, Niemack, Michael D., Sutariya, Shreya, Suzuki, Aritoki, Teply, Grant P., Thornton, Robert J., Wollack, Edward J., Zannoni, Mario, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Controlling stray light at millimeter wavelengths requires special optical design and selection of absorptive materials that should be compatible with cryogenic operating environments. While a wide selection of absorptive materials exists, these typically exhibit high indices of refraction and reflect/scatter a significant fraction of light before absorption. For many lower index materials such as commercial microwave absorbers, their applications in cryogenic environments are challenging. In this paper, we present a new tool to control stray light: metamaterial microwave absorber tiles. These tiles comprise an outer metamaterial layer that approximates a lossy gradient index anti-reflection coating. They are fabricated via injection molding commercially available carbon-loaded polyurethane (25\% by mass). The injection molding technology enables mass production at low cost. The design of these tiles is presented, along with thermal tests to 1 K. Room temperature optical measurements verify their control of reflectance to less than 1\% up to 65$\circ$ angles of incidence, and control of wide angle scattering below 0.01\%. The dielectric properties of the bulk carbon-loaded material used in the tiles is also measured at different temperatures, confirming that the material maintains similar dielectric properties down to 3 K., Comment: 10 pages, 11 figures, published in Applied Optics, selected as "Editor's pick"
Published: 2020
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15. The Simons Observatory: Modeling Optical Systematics in the Large Aperture Telescope

Author: Gudmundsson, Jon E., Gallardo, Patricio A., Puddu, Roberto, Dicker, Simon R., Adler, Alexandre E., Ali, Aamir M., Bazarko, Andrew, Chesmore, Grace E., Coppi, Gabriele, Cothard, Nicholas F., Dachlythra, Nadia, Devlin, Mark, Dünner, Rolando, Fabbian, Giulio, Galitzki, Nicholas, Golec, Joseph E., Ho, Shuay-Pwu Patty, Hargrave, Peter C., Kofman, Anna M., Lee, Adrian T., Limon, Michele, Matsuda, Frederick T., Mauskopf, Philip D., Moodley, Kavilan, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Page, Lyman A., Partridge, Bruce, Puglisi, Giuseppe, Reichardt, Christian L., Sierra, Carlos E., Simon, Sara M., Teply, Grant P., Tucker, Carole, Wollack, Edward J., Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present geometrical and physical optics simulation results for the Simons Observatory Large Aperture Telescope. This work was developed as part of the general design process for the telescope; allowing us to evaluate the impact of various design choices on performance metrics and potential systematic effects. The primary goal of the simulations was to evaluate the final design of the reflectors and the cold optics which are now being built. We describe non-sequential ray tracing used to inform the design of the cold optics, including absorbers internal to each optics tube. We discuss ray tracing simulations of the telescope structure that allow us to determine geometries that minimize detector loading and mitigate spurious near-field effects that have not been resolved by the internal baffling. We also describe physical optics simulations, performed over a range of frequencies and field locations, that produce estimates of monochromatic far field beam patterns which in turn are used to gauge general optical performance. Finally, we describe simulations that shed light on beam sidelobes from panel gap diffraction., Comment: 15 pages, 13 figures
Published: 2020
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16. 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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17. Simons Observatory Microwave SQUID Multiplexing Readout -- Cryogenic RF Amplifier and Coaxial Chain Design

Author: Rao, Mayuri Sathyanarayana, Silva-Feaver, Maximiliano, Ali, Aamir, Arnold, Kam, Ashton, Peter, Dober, Bradley J., Duell, Cody J., Duff, Shannon M., Galitzki, Nicholas, Healy, Erin, Henderson, Shawn, Ho, Shuay-Pwu Patty, Hoh, Jonathan, Kofman, Anna M., Kusaka, Akito, Lee, Adrian T., Mangu, Aashrita, Mathewson, Justin, Mauskopf, Philip, McCarrick, Heather, Moore, Jenna, Niemack, Michael D., Raum, Christopher, Salatino, Maria, Sasse, Trevor, Seibert, Joseph, Simon, Sara M., Staggs, Suzanne, Stevens, Jason R., Teply, Grant, Thornton, Robert, Ullom, Joel, Vavagiakis, Eve M., Westbrook, Benjamin, Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: The Simons Observatory (SO) is an upcoming polarization-sensitive Cosmic Microwave Background (CMB) experiment on the Cerro Toco Plateau (Chile) with large overlap with other optical and infrared surveys (e.g., DESI, LSST, HSC). To enable the readout of \bigO(10,000) detectors in each of the four telescopes of SO, we will employ the microwave SQUID multiplexing technology. With a targeted multiplexing factor of \bigO{(1,000)}, microwave SQUID multiplexing has never been deployed on the scale needed for SO. Here we present the design of the cryogenic coaxial cable and RF component chain that connects room temperature readout electronics to superconducting resonators that are coupled to Transition Edge Sensor bolometers operating at sub-Kelvin temperatures. We describe design considerations including cryogenic RF component selection, system linearity, noise, and thermal power dissipation., Comment: 10 pages, 2 figures
Published: 2020
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18. Small Aperture Telescopes for the Simons Observatory

Author: Ali, Aamir M., Adachi, Shunsuke, Arnold, Kam, Ashton, Peter, Bazarko, Andrew, Chinone, Yuji, Coppi, Gabriele, Corbett, Lance, Crowley, Kevin D, Crowley, Kevin T, Devlin, Mark, Dicker, Simon, Duff, Shannon, Ellis, Chris, Galitzki, Nicholas, Goeckner-Wald, Neil, Harrington, Kathleen, Healy, Erin, Hill, Charles A, Ho, Shuay-Pwu Patty, Hubmayr, Johannes, Keating, Brian, Kiuchi, Kenji, Kusaka, Akito, Lee, Adrian T, Ludlam, Michael, Mangu, Aashrita, Matsuda, Frederick, McCarrick, Heather, Nati, Federico, Niemack, Michael D., Nishino, Haruki, Orlowski-Scherer, John, Rao, Mayuri Sathyanarayana, Raum, Christopher, Sakurai, Yuki, Salatino, Maria, Sasse, Trevor, Seibert, Joseph, Sierra, Carlos, Silva-Feaver, Maximiliano, Spisak, Jacob, Simon, Sara M, Staggs, Suzanne, Tajima, Osamu, Teply, Grant, Tsan, Tran, Wollack, Edward, Westbrook, Bejamin, Xu, Zhilei, Zannoni, Mario, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Simons Observatory (SO) is an upcoming cosmic microwave background (CMB) experiment located on Cerro Toco, Chile, that will map the microwave sky in temperature and polarization in six frequency bands spanning 27 to 285 GHz. SO will consist of one 6-meter Large Aperture Telescope (LAT) fielding $\sim$30,000 detectors and an array of three 0.42-meter Small Aperture Telescopes (SATs) fielding an additional 30,000 detectors. This synergy will allow for the extremely sensitive characterization of the CMB over angular scales ranging from an arcmin to tens of degrees, enabling a wide range of scientific output. Here we focus on the SATs targeting degree angular scales with successive dichroic instruments observing at Mid-Frequency (MF: 93/145 GHz), Ultra-High-Frequency (UHF: 225/285 GHz), and Low-Frequency (LF: 27/39 GHz). The three SATs will be able to map $\sim$10% of the sky to a noise level of 2 $\mu$K-arcmin when combining 93 and 145 GHz. The multiple frequency bands will allow the CMB to be separated from galactic foregrounds (primarily synchrotron and dust), with the primary science goal of characterizing the primordial tensor-to-scalar ratio, $r$, at a target level of $\sigma \left(r\right) \approx 0.003$.
Published: 2020
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19. 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

20. 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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21. 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

22. 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

23. 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

24. Standard-Model Extension Constraints on Lorentz and CPT Violation From Optical Polarimetry of Active Galactic Nuclei

Author: Friedman, Andrew S., Leon, David, Gerasimov, Roman, Crowley, Kevin D., Broudy, Isaac, Melkani, Yash, Stevens, Walker, Johnson, Delwin, Teply, Grant, Tytler, David, Keating, Brian G., and Cole, Gary M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, High Energy Physics - Theory
Abstract: Vacuum birefringence from Lorentz and CPT violation in the Standard-Model Extension can be constrained using ground-based optical polarimetry of extragalactic sources. We describe results from a pilot program with an automated system that can perform simultaneous optical polarimetry in multiple passbands on different telescopes with an effective 0.45 m aperture. Despite the limited collecting area, our polarization measurements of AGN using a wider effective optical passband than previous studies yielded individual line-of-sight constraints for Standard-Model Extension mass dimension $d = 5$ operators within a factor of about one to ten of comparable broadband polarimetric bounds obtained using data from a 3.6 m telescope with roughly 64 times the collecting area. Constraining more general anisotropic Standard-Model Extension coefficients at higher $d$ would require more AGN along different lines of sight. This motivates a future dedicated ground-based, multi-band, optical polarimetry AGN survey with $\gtrsim 1$ m-class telescopes, to obtain state-of-the-art anisotropic Standard-Model Extension $d = 4, 5, 6$ constraints, while also using complementary archival polarimetry. This could happen more quickly and cost-effectively than via spectropolarimetry and long before more competitive constraints from space- or balloon-based x-ray/$\gamma$-ray polarization measurements., Comment: Presented at the Eighth Meeting on CPT and Lorentz Symmetry, Bloomington, Indiana, May 12-16, 2019; typo in one author name changed from v1
Published: 2019

25. Removal of Galactic foregrounds for the Simons Observatory primordial gravitational wave search

Author: Thorne, Ben, Dunkley, Jo, Alonso, David, Abitbol, Maximilian H., Errard, Josquin, Hill, J. Colin, Keating, Brian, Teply, Grant, and Wollack, Edward J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Upcoming observations from the Simons Observatory have been projected to constrain the tensor-to-scalar ratio, $r$, at the level of $\sigma(r)=$0.003. Here we describe one of the forecasting algorithms for the Simons Observatory in more detail, based on cleaning CMB polarization maps using a parametric model. We present a new code to perform this end-to-end forecast, and explore the assumptions in greater detail. If spatial uniformity of the spectral energy distribution of synchrotron radiation and thermal dust emission is assumed over the region planned for observations, covering almost a fifth of the sky, a bias of order 1--3$\sigma$ in $r$ is projected for foreground models consistent with current data. We find that by masking the most contaminated regions of sky, or by adopting more parameters to describe the spatial variation in spectral index for synchrotron and dust, such a bias can be mitigated for the foreground models we consider. We also explore strategies for testing whether the cleaned CMB polarization maps contain residual foreground contamination, including cross-correlating with maps tracing the foregrounds. This method also has applications for other CMB polarization experiments., Comment: 13 pages, 9 figures
Published: 2019

26. 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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27. Development of Calibration Strategies for the Simons Observatory

Author: Bryan, Sean A., Simon, Sara M., Gerbino, Martina, Teply}, Grant, Ali, Aamir, Chinone, Yuji, Crowley, Kevin, Fabbian, Giulio, Gallardo, Patricio A., Goeckner-Wald, Neil, Keating, Brian, Koopman, Brian, Kusaka, Akito, Matsuda, Frederick, Mauskopf, Philip, McMahon, Jeff, Nati, Federico, Puglisi, Giuseppe, Reichardt, Christian L, Salatino, Maria, Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Simons Observatory (SO) is a set of cosmic microwave background instruments that will be deployed in the Atacama Desert in Chile. The key science goals include setting new constraints on cosmic inflation, measuring large scale structure with gravitational lensing, and constraining neutrino masses. Meeting these science goals with SO requires high sensitivity and improved calibration techniques. In this paper, we highlight a few of the most important instrument calibrations, including spectral response, gain stability, and polarization angle calibrations. We present their requirements for SO and experimental techniques that can be employed to reach those requirements., Comment: 13 pages, 4 figures, SPIE Astronomical Telescopes and Instrumentation 2018
Published: 2018
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28. Constraints on Lorentz Invariance and CPT Violation using Optical Photometry and Polarimetry of Active Galaxies BL Lacertae and S5 B0716+714

Author: Friedman, Andrew S., Leon, David, Crowley, Kevin D., Johnson, Delwin, Teply, Grant, Tytler, David, Keating, Brian G., and Cole, Gary M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology
Abstract: Various quantum gravity approaches that extend beyond the standard model predict Lorentz Invariance and Charge-Parity-Time Violation at energies approaching the Planck scale. These models frequently predict a wavelength dependent speed of light, which would result in time delays between promptly emitted photons at different energies, as well as a wavelength-dependent rotation of the plane of linear polarization for photons resulting from vacuum birefringence. Here, we describe a pilot program with an automated system of small telescopes that can simultaneously conduct high cadence optical photometry and polarimetry of Active Galactic Nuclei (AGN) in multiple passbands. We use these observations as a proof-of-principle to demonstrate how such data can be used to test various Lorentz Violation models, including special cases of the Standard Model Extension (SME). In our initial campaign with this system, the Array Photo Polarimeter, we observed two AGN sources, including BL Lacertae at redshift z = 0.069, and S5 B0716+714 at z = 0.31. We demonstrate that optical polarimetry with a broadband Luminance filter combined with simultaneous $I_c$-band observations yields SME parameter constraints that are up to ~10 and ~30 times more sensitive than with a standard $I_c$-band filter, for SME models with mass dimension d = 5 and d = 6, respectively. Using only a small system of telescopes with an effective 0.45-m aperture, we further demonstrate d = 5 constraints for individual lines of sight that are within a factor of ~1-10 in sensitivity to comparable constraints from optical polarimetry with a 3.6-m telescope. Such an approach could significantly improve existing SME constraints via a polarimetric all-sky survey of AGN with multiple 1-meter class telescopes., Comment: 25 pages, 16 figures
Published: 2018
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29. 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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30. Studies of Systematic Uncertainties for Simons Observatory: Detector Array Effects

Author: Crowley, Kevin T., Simon, Sara M., Silva-Feaver, Max, Goeckner-Wald, Neil, Ali, Aamir, Austermann, Jason, Brown, Michael L., Chinone, Yuji, Cukierman, Ari, Dober, Bradley, Duff, Shannon M., Dunkley, Jo, Errard, Josquin, Fabbian, Giulio, Gallardo, Patricio A., Ho, Shuay-Pwu Patty, Hubmayr, Johannes, Keating, Brian, Kusaka, Akito, McCallum, Nialh, McMahon, Jeff, Nati, Federico, Niemack, Michael D., Puglisi, Giuseppe, Rao, Mayuri Sathyanarayana, Reichardt, Christian L., Salatino, Maria, Siritanasak, Praween, Staggs, Suzanne, Suzuki, Aritoki, Teply, Grant, Thomas, Daniel B., Ullom, Joel N., Vergès, Clara, Vissers, Michael R., Westbrook, Benjamin, Wollack, Edward J., Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In this proceeding, we present studies of instrumental systematic effects for the Simons Obsevatory (SO) that are associated with the detector system and its interaction with the full SO experimental systems. SO will measure the Cosmic Microwave Background (CMB) temperature and polarization anisotropies over a wide range of angular scales in six bands with bandcenters spanning from 27 GHz to 270 GHz. We explore effects including intensity-to-polarization leakage due to coupling optics, bolometer nonlinearity, uncalibrated gain variations of bolometers, and readout crosstalk. We model the level of signal contamination, discuss proposed mitigation schemes, and present instrument requirements to inform the design of SO and future CMB projects., Comment: Proceeding from SPIE Astronomical Telescopes+Instrumentation 2018 (27 pages, 13 figures) v2: Added HEALPix reference
Published: 2018
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31. Cooldown Strategies and Transient Thermal Simulations for the Simons Observatory

Author: Coppi, Gabriele, Xu, Zhilei, Ali, Aamir, Devlin, Mark J., Dicker, Simon, Galitzki, Nicholas, Gallardo, Patricio A., Keating, Brian, Limon, Michele, Longu, Marius, May, Andrew J., McMahon, Jeff, Niemack, Michael D., Orlowski-Scherer, Jack L., Piccirillo, Lucio, Puglisi, Giuseppe, Salatino, Maria, Simon, Sara M., Teply, Grant, Thornton, Robert, Vavagiakis, Eve M., and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Simons Observatory (SO) will provide precision polarimetry of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales from arc-minutes to tens of degrees, contain over 60,000 detectors, and observe in frequency bands between 27 GHz and 270 GHz. SO will consist of a six-meter-aperture telescope initially coupled to ~35,000 detectors along with an array of 0.5m aperture refractive cameras, coupled to an additional 30,000+ detectors. The large aperture telescope receiver (LATR) is coupled to a six-meter crossed Dragone telescope and will be 2.4m in diameter, weigh over 3 tons, and have five cryogenic stages (80 K, 40 K, 4 K, 1 K and 100 mK). The LATR is coupled to the telescope via 13 independent optics tubes containing cryogenic optical elements and detectors. The cryostat will be cooled by by two Cryomech PT90 (80 K) and three Cryomech PT420 (40 K and 4 K) pulse tube cryocoolers, with cooling of the 1 K and 100 mK stages by a commercial dilution refrigerator system. The second component, the small aperture telescope (SAT), is a single optics tube refractive cameras of 42cm diameter. Cooling of the SAT stages will be provided by two Cryomech PT420, one of which is dedicated to the dilution refrigeration system which will cool the focal plane to 100 mK. SO will deploy a total of three SATs. In order to estimate the cool down time of the camera systems given their size and complexity, a finite difference code based on an implicit solver has been written to simulate the transient thermal behavior of both cryostats. The result from the simulations presented here predict a 35 day cool down for the LATR. The simulations suggest additional heat switches between stages would be effective in distribution cool down power and reducing the time it takes for the LATR to cool. The SAT is predicted to cool down in one week, which meets the SO design goals.
Published: 2018
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32. Studies of Systematic Uncertainties for Simons Observatory: Polarization Modulator Related Effects

Author: Salatino, Maria, Lashner, Jacob, Gerbino, Martina, Simon, Sara M., Didier, Joy, Ali, Aamir, Ashton, Peter C., Bryan, Sean, Chinone, Yuji, Coughlin, Kevin, Crowley, Kevin T., Fabbian, Giulio, Galitzki, Nicholas, Goeckner-Wald, Neil, Golec, Joseph E., Gudmundsson, Jon E., Hill, Charles A., Keating, Brian, Kusaka, Akito, Lee, Adrian T., McMahon, Jeffrey, Miller, Amber D., Puglisi, Giuseppe, Reichardt, Christian L., Teply, Grant, Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Simons Observatory (SO) will observe the temperature and polarization anisotropies of the cosmic microwave background (CMB) over a wide range of frequencies (27 to 270 GHz) and angular scales by using both small (0.5 m) and large (6 m) aperture telescopes. The SO small aperture telescopes will target degree angular scales where the primordial B-mode polarization signal is expected to peak. The incoming polarization signal of the small aperture telescopes will be modulated by a cryogenic, continuously-rotating half-wave plate (CRHWP) to mitigate systematic effects arising from slowly varying noise and detector pair-differencing. In this paper, we present an assessment of some systematic effects arising from using a CRHWP in the SO small aperture systems. We focus on systematic effects associated with structural properties of the HWP and effects arising when operating a HWP, including the amplitude of the HWP synchronous signal (HWPSS), and I -> P (intensity to polarization) leakage that arises from detector non-linearity in the presence of a large HWPSS. We demonstrate our ability to simulate the impact of the aforementioned systematic effects in the time domain. This important step will inform mitigation strategies and design decisions to ensure that SO will meet its science goals., Comment: 22 pages, 10 figures. Submitted to the Proceedings of SPIE: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX
Published: 2018

33. 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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34. Designs for next generation CMB survey strategies from Chile

Author: Stevens, Jason R., Goeckner-Wald, Neil, Keskitalo, Reijo, McCallum, Nialh, Ali, Aamir, Borrill, Julian, Brown, Michael L., Chinone, Yuji, Gallardo, Patricio A., Kusaka, Akito, Lee, Adrian T., McMahon, Jeff, Niemack, Michael D., Page, Lyman, Puglisi, Giuseppe, Salatino, Maria, Mak, Suet Ying D., Teply, Grant, Thomas, Daniel B., Vavagiakis, Eve M., Wollack, Edward J., Xu, Zhilei, and Zhu, Ningfeng
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: New telescopes are being built to measure the Cosmic Microwave Background (CMB) with unprecedented sensitivity, including Simons Observatory (SO), CCAT-prime, the BICEP Array, SPT-3G, and CMB Stage-4. We present observing strategies for telescopes located in Chile that are informed by the tools used to develop recent Atacama Cosmology Telescope (ACT) and Polarbear surveys. As with ACT and Polarbear, these strategies are composed of scans that sweep in azimuth at constant elevation. We explore observing strategies for both small (0.42 m) aperture telescopes (SAT) and a large (6 m) aperture telescope (LAT). We study strategies focused on small sky areas to search for inflationary gravitational waves as well as strategies spanning roughly half the low-foreground sky to constrain the effective number of relativistic species and measure the sum of neutrino masses via the gravitational lensing signal due to large scale structure. We present these strategies specifically considering the telescope hardware and science goals of the SO, located at 23 degrees South latitude, 67.8 degrees West longitude. Observations close to the Sun and the Moon can introduce additional systematics by applying additional power to the instrument through telescope sidelobes. Significant side lobe contamination in the data can occur even at tens of degrees or more from bright sources. Therefore, we present several strategies that implement Sun and Moon avoidance constraints into the telescope scheduling. Strategies for resolving conflicts between simultaneously visible fields are discussed. We focus on maximizing telescope time spent on science observations. It will also be necessary to schedule calibration measurements, however that is beyond the scope of this work. The outputs of this study are algorithms that can generate specific schedule commands for the Simons Observatory instruments., Comment: 15 pages, 9 figures, 3 tables, SPIE Astronomical Telescopes + Instrumentation 2018
Published: 2018
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35. 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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36. Design and characterization of the POLARBEAR-2b and POLARBEAR-2c cosmic microwave background cryogenic receivers

Author: Howe, Logan, Tsai, Calvin, Lowry, Lindsay, Arnold, Kam, Coppi, Gabriele, Groh, John, Guo, Xiaoyu, Keating, Brian, Lee, Adrian, May, Andrew J., Piccirillo, Lucio, Stebor, Nathan, and Teply, Grant
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The POLARBEAR-2/Simons Array Cosmic Microwave Background (CMB) polarization experiment is an upgrade and expansion of the existing POLARBEAR-1 (PB-1) experiment, located in the Atacama desert in Chile. Along with the CMB temperature and $E$-mode polarization anisotropies, PB-1 and the Simons Array study the CMB $B$-mode polarization anisotropies produced at large angular scales by inflationary gravitational waves, and at small angular scales by gravitational lensing. These measurements provide constraints on various cosmological and particle physics parameters, such as the tensor-to-scalar ratio $r$, and the sum of the neutrino masses. The Simons Array consists of three 3.5 m diameter telescopes with upgraded POLARBEAR-2 (PB-2) cryogenic receivers, named PB-2a, -2b, and -2c. PB-2a and -2b will observe the CMB over multiple bands centered at 95 GHz and 150 GHz, while PB-2c will observe at 220 GHz and 270 GHz, which will enable enhanced foreground separation and de-lensing. Each Simons Array receiver consists of two cryostats which share the same vacuum space: an optics tube containing the cold reimaging lenses and Lyot stop, infrared-blocking filters, and cryogenic half-wave plate; and a backend which contains the focal plane detector array, cold readout components, and millikelvin refrigerator. Each PB-2 focal plane array is comprised of 7,588 dual-polarization, multi-chroic, lenslet- and antenna-coupled, Transition Edge Sensor (TES) bolometers which are cooled to 250 mK and read out using Superconducting Quantum Interference Devices (SQUIDs) through a digital frequency division multiplexing scheme with a multiplexing factor of 40. In this work we describe progress towards commissioning the PB-2b and -2c receivers including cryogenic design, characterization, and performance of both the PB-2b and -2c backend cryostats., Comment: 20 pages
Published: 2018

37. 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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38. POLOCALC: a Novel Method to Measure the Absolute Polarization Orientation of the Cosmic Microwave Background

Author: Nati, Federico, Devlin, Mark J., Gerbino, Martina, Johnson, Bradley R., Keating, Brian, Pagano, Luca, and Teply, Grant
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We describe a novel method to measure the absolute orientation of the polarization plane of the CMB with arcsecond accuracy, enabling unprecedented measurements for cosmology and fundamental physics. Existing and planned CMB polarization instruments looking for primordial B-mode signals need an independent, experimental method for systematics control on the absolute polarization orientation. The lack of such a method limits the accuracy of the detection of inflationary gravitational waves, the constraining power on the neutrino sector through measurements of gravitational lensing of the CMB, the possibility of detecting Cosmic Birefringence, and the ability to measure primordial magnetic fields. Sky signals used for calibration and direct measurements of the detector orientation cannot provide an accuracy better than 1 deg. Self-calibration methods provide better accuracy, but may be affected by foreground signals and rely heavily on model assumptions. The POLarization Orientation CALibrator for Cosmology, POLOCALC, will dramatically improve instrumental accuracy by means of an artificial calibration source flying on balloons and aerial drones. A balloon-borne calibrator will provide far-field source for larger telescopes, while a drone will be used for tests and smaller polarimeters. POLOCALC will also allow a unique method to measure the telescopes' polarized beam. It will use microwave emitters between 40 and 150 GHz coupled to precise polarizing filters. The orientation of the source polarization plane will be registered to sky coordinates by star cameras and gyroscopes with arcsecond accuracy. This project can become a rung in the calibration ladder for the field: any existing or future CMB polarization experiment observing our polarization calibrator will enable measurements of the polarization angle for each detector with respect to absolute sky coordinates., Comment: 15 pages, 5 figures, Accepted by Journal of Astronomical Instrumentation
Published: 2017
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39. 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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40. 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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41. The effects of inclination on a two stage pulse tube cryocooler for use with a ground based observatory

Author: Tsan, Tran, Galitzki, Nicholas, Ali, Aamir M., Arnold, Kam, Coppi, Gabriele, Ervin, Tamar, Foote, Logan, Keating, Brian, Lashner, Jack, Orlowski-Scherer, John, Randall, Michael J., Seibert, Joseph, Spisak, Jacob, Teply, Grant P., Xu, Zhilei, and Zhu, Ningfeng
Published: 2021
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42. 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

43. The Simons Observatory : Beam Characterization for the Small Aperture Telescopes

Author: Dachlythra, Nadia, Duivenvoorden, Adriaan J., Gudmundsson, Jón E., Hasselfield, Matthew, Coppi, Gabriele, Adler, Alexandre E., Alonso, David, Azzoni, Susanna, Chesmore, Grace E., Fabbian, Giulio, Ganga, Ken, Gerras, Remington G., Jaffe, Andrew H., Johnson, Bradley R., Keating, Brian, Keskitalo, Reijo, Kisner, Theodore S., Krachmalnicoff, Nicoletta, Lungu, Marius, Matsuda, Frederick, Naess, Sigurd, Page, Lyman, Puddu, Roberto, Puglisi, Giuseppe, Simon, Sara M., Teply, Grant, Tsan, Tran, Wollack, Edward J., Wolz, Kevin, Xu, Zhilei, Dachlythra, Nadia, Duivenvoorden, Adriaan J., Gudmundsson, Jón E., Hasselfield, Matthew, Coppi, Gabriele, Adler, Alexandre E., Alonso, David, Azzoni, Susanna, Chesmore, Grace E., Fabbian, Giulio, Ganga, Ken, Gerras, Remington G., Jaffe, Andrew H., Johnson, Bradley R., Keating, Brian, Keskitalo, Reijo, Kisner, Theodore S., Krachmalnicoff, Nicoletta, Lungu, Marius, Matsuda, Frederick, Naess, Sigurd, Page, Lyman, Puddu, Roberto, Puglisi, Giuseppe, Simon, Sara M., Teply, Grant, Tsan, Tran, Wollack, Edward J., Wolz, Kevin, and Xu, Zhilei
Abstract: We use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a mapmaker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the mapmaker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions, and input beams. We additionally show the reconstruction quality as a function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within an ∼1.5% error for a multipole range ℓ = 30–700 and an ∼0.5% error for a multipole range ℓ = 50–200. We conclude by using a harmonic-domain component separation algorithm to verify that the beam reconstruction errors and biases observed in our analysis do not significantly bias the Simons Observatory r-measurement
Published: 2024
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44. The Simons Observatory: Beam Characterization for the Small Aperture Telescopes

Author: Dachlythra, N, Duivenvoorden, A, Gudmundsson, J, Hasselfield, M, Coppi, G, Adler, A, Alonso, D, Azzoni, S, Chesmore, G, Fabbian, G, Ganga, K, Gerras, R, Jaffe, A, Johnson, B, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Lungu, M, Matsuda, F, Naess, S, Page, L, Puddu, R, Puglisi, G, Simon, S, Teply, G, Tsan, T, Wollack, E, Wolz, K, Xu, Z, Dachlythra, Nadia, Duivenvoorden, Adriaan J., Gudmundsson, Jon E., Hasselfield, Matthew, Coppi, Gabriele, Adler, Alexandre E., Alonso, David, Azzoni, Susanna, Chesmore, Grace E., Fabbian, Giulio, Ganga, Ken, Gerras, Remington G., Jaffe, Andrew H., Johnson, Bradley R., Keating, Brian, Keskitalo, Reijo, Kisner, Theodore S., Krachmalnicoff, Nicoletta, Lungu, Marius, Matsuda, Frederick, Naess, Sigurd, Page, Lyman, Puddu, Roberto, Puglisi, Giuseppe, Simon, Sara M., Teply, Grant, Tsan, Tran, Wollack, Edward J., Wolz, Kevin, Xu, Zhilei, Dachlythra, N, Duivenvoorden, A, Gudmundsson, J, Hasselfield, M, Coppi, G, Adler, A, Alonso, D, Azzoni, S, Chesmore, G, Fabbian, G, Ganga, K, Gerras, R, Jaffe, A, Johnson, B, Keating, B, Keskitalo, R, Kisner, T, Krachmalnicoff, N, Lungu, M, Matsuda, F, Naess, S, Page, L, Puddu, R, Puglisi, G, Simon, S, Teply, G, Tsan, T, Wollack, E, Wolz, K, Xu, Z, Dachlythra, Nadia, Duivenvoorden, Adriaan J., Gudmundsson, Jon E., Hasselfield, Matthew, Coppi, Gabriele, Adler, Alexandre E., Alonso, David, Azzoni, Susanna, Chesmore, Grace E., Fabbian, Giulio, Ganga, Ken, Gerras, Remington G., Jaffe, Andrew H., Johnson, Bradley R., Keating, Brian, Keskitalo, Reijo, Kisner, Theodore S., Krachmalnicoff, Nicoletta, Lungu, Marius, Matsuda, Frederick, Naess, Sigurd, Page, Lyman, Puddu, Roberto, Puglisi, Giuseppe, Simon, Sara M., Teply, Grant, Tsan, Tran, Wollack, Edward J., Wolz, Kevin, and Xu, Zhilei
Abstract: We use time-domain simulations of Jupiter observations to test and develop a beam reconstruction pipeline for the Simons Observatory Small Aperture Telescopes. The method relies on a mapmaker that estimates and subtracts correlated atmospheric noise and a beam fitting code designed to compensate for the bias caused by the mapmaker. We test our reconstruction performance for four different frequency bands against various algorithmic parameters, atmospheric conditions, and input beams. We additionally show the reconstruction quality as a function of the number of available observations and investigate how different calibration strategies affect the beam uncertainty. For all of the cases considered, we find good agreement between the fitted results and the input beam model within an ∼1.5% error for a multipole range l = 30-700 and an ∼0.5% error for a multipole range l = 50-200. We conclude by using a harmonic-domain component separation algorithm to verify that the beam reconstruction errors and biases observed in our analysis do not significantly bias the Simons Observatory r-measurement
Published: 2024

45. The Simons Observatory: Beam Characterization for the Small Aperture Telescopes

Author: Dachlythra, Nadia, primary, Duivenvoorden, Adriaan J., additional, Gudmundsson, Jon E., additional, Hasselfield, Matthew, additional, Coppi, Gabriele, additional, Adler, Alexandre E., additional, Alonso, David, additional, Azzoni, Susanna, additional, Chesmore, Grace E., additional, Fabbian, Giulio, additional, Ganga, Ken, additional, Gerras, Remington G., additional, Jaffe, Andrew H., additional, Johnson, Bradley R., additional, Keating, Brian, additional, Keskitalo, Reijo, additional, Kisner, Theodore S., additional, Krachmalnicoff, Nicoletta, additional, Lungu, Marius, additional, Matsuda, Frederick, additional, Naess, Sigurd, additional, Page, Lyman, additional, Puddu, Roberto, additional, Puglisi, Giuseppe, additional, Simon, Sara M., additional, Teply, Grant, additional, Tsan, Tran, additional, Wollack, Edward J., additional, Wolz, Kevin, additional, and Xu, Zhilei, additional
Published: 2024
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46. Simons Observatory Microwave SQUID Multiplexing Readout: Cryogenic RF Amplifier and Coaxial Chain Design

Author: Sathyanarayana Rao, Mayuri, Silva-Feaver, Maximiliano, Ali, Aamir, Arnold, Kam, Ashton, Peter, Dober, Bradley J., Duell, Cody J., Duff, Shannon M., Galitzki, Nicholas, Healy, Erin, Henderson, Shawn, Ho, Shuay-Pwu Patty, Hoh, Jonathan, Kofman, Anna M., Kusaka, Akito, Lee, Adrian T., Mangu, Aashrita, Mathewson, Justin, Mauskopf, Philip, McCarrick, Heather, Moore, Jenna, Niemack, Michael D., Raum, Christopher, Salatino, Maria, Sasse, Trevor, Seibert, Joseph, Simon, Sara M., Staggs, Suzanne, Stevens, Jason R., Teply, Grant, Thornton, Robert, Ullom, Joel, Vavagiakis, Eve M., Westbrook, Benjamin, Xu, Zhilei, and Zhu, Ningfeng
Published: 2020
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47. 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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48. 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

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

Author: Crowley, Kevin D., primary, Dow, Peter, additional, Shroyer, Jordan E., additional, Groh, John C., additional, Dober, Bradley, additional, Spisak, Jacob, additional, Galitzki, Nicholas, additional, Bhandarkar, Tanay, additional, Devlin, Mark J., additional, Dicker, Simon, additional, Gallardo, Patricio A., additional, Harrington, Kathleen, additional, Iuliano, Jeffrey, additional, Johnson, Bradley R., additional, Johnson, Delwin, additional, Kofman, Anna M., additional, Kusaka, Akito, additional, Lee, Adrian, additional, Limon, Michele, additional, Nati, Federico, additional, Orlowski-Scherer, John, additional, Page, Lyman, additional, Randall, Michael, additional, Teply, Grant, additional, Tsan, Tran, additional, Wollack, Edward J., additional, Xu, Zhilei, additional, and Zhu, Ningfeng, additional
Published: 2022
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50. CMB-S4

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, 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, Zonca, Andrea, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CMB-S4, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11), Apollo - University of Cambridge Repository, Van Swinderen Institute for Particle Physics and G, Cosmic Frontier, Abazajian, K, Addison, G, Adshead, P, Ahmed, Z, Akerib, D, Ali, A, Allen, S, Alonso, D, Alvarez, M, Amin, M, Anderson, A, Arnold, K, Ashton, P, Baccigalupi, C, Bard, D, Barkats, D, Barron, D, Barry, P, Bartlett, J, Basu Thakur, R, Battaglia, N, Bean, R, Bebek, C, Bender, A, Benson, B, Bianchini, F, Bischoff, C, Bleem, L, Bock, J, Bocquet, S, Boddy, K, Richard Bond, J, Borrill, J, Bouchet, F, Brinckmann, T, Brown, M, Bryan, S, Buza, V, Byrum, K, Hervias Caimapo, C, Calabrese, E, Calafut, V, Caldwell, R, Carlstrom, J, Carron, J, Cecil, T, Challinor, A, Chang, C, Chinone, Y, Sherry Cho, H, Cooray, A, Coulton, W, Crawford, T, Crites, A, Cukierman, A, Cyr-Racine, F, De Haan, T, Delabrouille, J, Devlin, M, Di Valentino, E, Dierickx, M, Dobbs, M, Duff, S, Dvorkin, C, Eimer, J, Elleflot, T, Errard, J, Essinger-Hileman, T, Fabbian, G, Feng, C, Ferraro, S, Filippini, J, Flauger, R, Flaugher, B, Fraisse, A, Frolov, A, Galitzki, N, Gallardo, P, Galli, S, Ganga, K, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Green, D, Grin, D, Grohs, E, Gualtieri, R, Gudmundsson, J, Gullett, I, Gupta, N, Habib, S, Halpern, M, Halverson, N, Hanany, S, Harrington, K, Hasegawa, M, Hasselfield, M, Hazumi, M, Heitmann, K, Henderson, S, Hensley, B, Hill, C, Colin Hill, J, Hlozek, R, Patty Ho, S, Hoang, T, Holder, G, Holzapfel, W, Hood, J, Hubmayr, J, Huffenberger, K, Hui, H, Irwin, K, Jeong, O, Johnson, B, Jones, W, Hwan Kang, J, Karkare, K, Katayama, N, Keskitalo, R, Kisner, T, Knox, L, Koopman, B, Kosowsky, A, Kovac, J, Kovetz, E, Kuhlmann, S, Kuo, C, Kusaka, A, Lahteenmaki, A, Lawrence, C, Lee, A, Lewis, A, Li, D, Linder, E, Loverde, M, Lowitz, A, Lubin, P, Madhavacheril, M, Mantz, A, Marques, G, Matsuda, F, Mauskopf, P, Mccarrick, H, Mcmahon, J, Daniel Meerburg, P, Melin, J, Menanteau, F, Meyers, J, Millea, M, Mohr, J, Moncelsi, L, Monzani, M, Mroczkowski, T, Mukherjee, S, Nagy, J, Namikawa, T, Nati, F, Natoli, T, Newburgh, L, Niemack, M, Nishino, H, Nord, B, Novosad, V, O'Brient, R, Padin, S, Palladino, S, Partridge, B, Petravick, D, Pierpaoli, E, Pogosian, L, Prabhu, K, Pryke, C, Puglisi, G, Racine, B, Rahlin, A, Sathyanarayana Rao, M, Raveri, M, Reichardt, C, Remazeilles, M, Rocha, G, Roe, N, Roy, A, Ruhl, J, Salatino, M, Saliwanchik, B, Schaan, E, Schillaci, A, Schmitt, B, Schmittfull, M, Scott, D, Sehgal, N, Shandera, S, Sherwin, B, Shirokoff, E, Simon, S, Slosar, A, Spergel, D, S, T, Staggs, S, Stark, A, Starkman, G, Stompor, R, Stoughton, C, Suzuki, A, Tajima, O, Teply, G, Thompson, K, Thorne, B, Timbie, P, Tomasi, M, Tristram, M, Tucker, G, Umilta, C, Van Engelen, A, Vavagiakis, E, Vieira, J, Vieregg, A, Wagoner, K, Wallisch, B, Wang, G, Watson, S, Westbrook, B, Whitehorn, N, Wollack, E, Kimmy Wu, W, Xu, Z, Eric Yang, H, Yasini, S, Yefremenko, V, Won Yoon, K, Young, E, Yu, C, Zonca, A, University of California Irvine, Johns Hopkins University, University of Illinois at Urbana-Champaign, SLAC National Accelerator Laboratory, University of California Berkeley, Stanford University, University of Oxford, Rice University, Fermi National Accelerator Laboratory, University of California San Diego, International School for Advanced Studies, Lawrence Berkeley National Laboratory, Harvard University, University of New Mexico, Argonne National Laboratory, Université Paris-Diderot, California Institute of Technology, Cornell University, University of Melbourne, University of Cincinnati, Ludwig Maximilian University of Munich, University of Toronto, UMR7095, Stony Brook University, University of Manchester, Arizona State University, Florida State University, Cardiff University, Dartmouth College, University of Geneva, University of Cambridge, The University of Tokyo, University of Groningen, University of Chicago, University of Pennsylvania, McGill University, National Institute of Standards and Technology, NASA Goddard Space Flight Center, University of Sussex, Princeton University, Simon Fraser University, National Institute for Nuclear Physics, Haverford College, Stockholm University, Case Western Reserve University, University of British Columbia, University of Colorado Boulder, University of Minnesota Twin Cities, University of Michigan, Ann Arbor, Simons Foundation, Columbia University, University of Virginia, University of California Davis, Yale University, University of Pittsburgh, Ben-Gurion University of the Negev, Department of Electronics and Nanoengineering, Jet Propulsion Laboratory, University of California Santa Barbara, Perimeter Institute for Theoretical Physics, Service d'Astrophysique CEA, European Southern Observatory, Washington University St. Louis, University of Milan - Bicocca, University of Southern California, Institute for Advanced Studies, Pennsylvania State University, Brookhaven National Laboratory, Kyoto University, University of Wisconsin-Madison, University of Milano, Université Paris-Saclay, Brown University, Syracuse University, University of California Los Angeles, Aalto-yliopisto, and Aalto University
Subjects: Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology, CMB, Settore FIS/05, Space and Planetary Science, astro-ph.CO, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies and Cosmology, 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 $5��$, or, in the absence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL., 24 pages, 8 figures, 9 tables, submitted to ApJ. arXiv admin note: text overlap with arXiv:1907.04473
Published: 2022

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