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1. CONCERTO: instrument and status

Author: Fasano, Alessandro, Ade, Peter, Aravena, Manuel, Barria, Emilio, Beelen, Alexandre, Benoît, Alain, Béthermin, Matthieu, Bounmy, Julien, Bourrion, Olivier, Bres, Guillaume, Calvo, Martino, Catalano, Andrea, De Breuck, Carlos, Désert, François-Xavier, Durán, Carlos, Fenouillet, Thomas, Garcia, Jose, Garde, Gregory, Goupy, Johannes, Groppi, Christopher, Hoarau, Christophe, Hu, Wenkai, Lagache, Guilaine, Lambert, Jean-Charles, Leggeri, Jean-Paul, Levy-Bertrand, Florence, Lundgren, Andreas, Macías-Pérez, Juan, Mani, Hamdi, Marpaud, Julien, Mauskopf, Philip, Monfardini, Alessandro, Pisano, Giampaolo, Ponthieu, Nicolas, Prieur, Leo, Roni, Samuel, Roudier, Sebastien, Tourres, Damien, and Tucker, Carol
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: CONCERTO (CarbON CII line in post-rEionization and ReionizaTiOn) is a low-resolution Fourier transform spectrometer dedicated to the study of star-forming galaxies and clusters of galaxies in the transparent millimeter windows from the ground. It is characterized by a wide instantaneous 18.6 arcmin field of view, operates at 130-310 GHz, and was installed on the 12-meter Atacama Pathfinder Experiment (APEX) telescope at 5100 m above sea level. CONCERTO's double focal planes host two arrays of 2152 kinetic inductance detectors and represent a pioneering instrument to meet a state-of-the-art scientific challenge. This paper introduces the CONCERTO instrument and explains its status, shows the first CONCERTO spectral maps of Orion, and describes the perspectives of the project., Comment: 6 pages, 2 figures, to appear in Proc. of the mm Universe 2023 conference, Grenoble (France), June 2023, published by F. Mayet et al. (Eds), EPJ Web of conferences, EDP Sciences
Published: 2023
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2. A Cryogenic Wideband (2.5-14 GHz) Receiver system for the Arecibo 12m Telescope

Author: Roshi, D. Anish, Perillat, Phil, Fernandez, Felix, Mani, Hamdi, Perera, Benetge, Manoharan, P. K., Quintero, Luis, and Venkataraman, Arun
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: In this paper we present details of the construction of a wideband, cryogenic receiver and its successful commissioning on the Arecibo 12m telescope. The cryogenic receiver works in the 2.5-14 GHz frequency range. The telescope is operated by the Arecibo Observatory, and is located within the premises of the Observatory. We upgraded the current narrow band, room temperature receivers of the telescope with the new wideband receiver. The current receiver is built around a Quadruple-Ridged Flared Horn (QRHF) developed by Akgiray et al. (2013). To mitigate strong radio frequency interference (RFI) below 2.7 GHz, we installed a highpass filter before the first stage low noise amplifier (LNA). The QRHF, highpass filter, noise coupler and LNA are located inside a cryostat and are cooled to 15 K. The measured receiver temperature is 25 K (median value) over 2.5 GHz to 14 GHz. The system temperature measured at zenith is about 40 K near 3.1 and 8.6 GHz and the zenith antenna gains are 0.025 and 0.018 K/Jy at the two frequencies respectively. In the next stage of the development, we plan to upgrade the highpass filter in order to achieve better RFI rejection near 2.5 GHz, improve the aperture efficiency at 8.6 GHz and upgrade the IF system to increase the upper frequency of operation from 12 GHz to 14 GHz., Comment: 13 pages, 7 figures, 1 table (submitted for publication)
Published: 2023

3. CONCERTO: a breakthrough in wide field-of-view spectroscopy at millimeter wavelengths

Author: Fasano, Alessandro, Beelen, Alexandre, Benoit, Alain, Lundgren, Andreas, Ade, Peter, Aravena, Manuel, Barria, Emilio, Béthermin, Matthieu, Bounmy, Julien, Bourrion, Olivier, Bres, Guillaume, Calvo, Martino, Catalano, Andrea, Désert, François-Xavier, De Breuck, Carlos, Durán, Carlos, Fenouillet, Thomas, Garcia, Jose, Garde, Gregory, Goupy, Johannes, Groppi, Christopher, Hoarau, Christophe, Hu, Wenkai, Lagache, Guilaine, Lambert, Jean-Charles, Leggeri, Jean-Paul, Levy-Bertrand, Florence, Macias-Pérez, Juan-Francisco, Mani, Hamdi, Marpaud, Julien, Mauskopf, Philip, Monfardini, Alessandro, Pisano, Giampaolo, Ponthieu, Nicolas, Prieur, Leo, Roni, Samuel, Roudier, Sebastien, Tourres, Damien, Tucker, Carol, and Van Cuyck, Mathilde
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: CarbON CII line in post-rEionization and ReionizaTiOn (CONCERTO) is a low-resolution spectrometer with an instantaneous field-of-view of 18.6 arcmin, operating in the 130-310 GHz transparent atmospheric window. It is installed on the 12-meter Atacama Pathfinder Experiment (APEX) telescope at 5100 m above sea level. The Fourier transform spectrometer (FTS) contains two focal planes hosting a total of 4304 kinetic inductance detectors. The FTS interferometric pattern is recorded on the fly while continuously scanning the sky. One of the goals of CONCERTO is to characterize the large-scale structure of the Universe by observing the integrated emission from unresolved galaxies. This methodology is an innovative technique and is called line intensity mapping. In this paper, we describe the CONCERTO instrument, the effect of the vibration of the FTS beamsplitter, and the status of the CONCERTO main survey., Comment: 9 pages, 7 figures, to appear in the Proceedings of SPIE Astronomical Telescopes + Instrumentation 2022
Published: 2022

4. Search for axion-like dark matter using solid-state nuclear magnetic resonance

Author: Aybas, Deniz, Adam, Janos, Blumenthal, Emmy, Gramolin, Alexander V., Johnson, Dorian, Kleyheeg, Annalies, Afach, Samer, Blanchard, John W., Centers, Gary P., Garcon, Antoine, Engler, Martin, Figueroa, Nataniel L., Sendra, Marina Gil, Wickenbrock, Arne, Lawson, Matthew, Wang, Tao, Wu, Teng, Luo, Haosu, Mani, Hamdi, Mauskopf, Philip, Graham, Peter W., Rajendran, Surjeet, Kimball, Derek F. Jackson, Budker, Dmitry, and Sushkov, Alexander O.
Subjects: High Energy Physics - Experiment, Condensed Matter - Other Condensed Matter, Physics - Instrumentation and Detectors
Abstract: We report the results of an experimental search for ultralight axion-like dark matter in the mass range 162 neV to 166 neV. The detection scheme of our Cosmic Axion Spin Precession Experiment (CASPEr) is based on a precision measurement of $^{207}$Pb solid-state nuclear magnetic resonance in a polarized ferroelectric crystal. Axion-like dark matter can exert an oscillating torque on $^{207}$Pb nuclear spins via the electric-dipole moment coupling $g_d$, or via the gradient coupling $g_{\text{aNN}}$. We calibrated the detector and characterized the excitation spectrum and relaxation parameters of the nuclear spin ensemble with pulsed magnetic resonance measurements in a 4.4 T magnetic field. We swept the magnetic field near this value and searched for axion-like dark matter with Compton frequency within a 1 MHz band centered at 39.65 MHz. Our measurements place the upper bounds $|g_d|<9.5\times10^{-4}\,\text{GeV}^{-2}$ and $|g_{\text{aNN}}|<2.8\times10^{-1}\,\text{GeV}^{-1}$ (95% confidence level) in this frequency range. The constraint on $g_d$ corresponds to an upper bound of $1.0\times 10^{-21}\,\text{e}\cdot\text{cm}$ on the amplitude of oscillations of the neutron electric dipole moment, and $4.3\times 10^{-6}$ on the amplitude of oscillations of CP-violating $\theta$ parameter of quantum chromodynamics. Our results demonstrate the feasibility of using solid-state nuclear magnetic resonance to search for axion-like dark matter in the nano-electronvolt mass range.
Published: 2021
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5. Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver

Author: Lowe, Ian, Ade, Peter A. R., Ashton, Peter C., Austermann, Jason E., Coppi, Gabriele, Cox, Erin G., Devlin, Mark J., Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas, Gao, Jiansong, Gordon, Samuel, Groppi, Christopher E., Hilton, Gene C., Hubmayr, Johannes, Klein, Jeffrey, Li, Dale, Lourie, Nathan P., Mani, Hamdi, Mauskopf, Philip, McKenney, Christopher, Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, L. Javier, Soler, Juan D., Sinclair, Adrian, Tucker, Carole, Ullom, Joel, Vissers, Michael, Wheeler, Caleb, and Williams, Paul A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID pixels, respectively. The pixels are formed from two orthogonally oriented, crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to sub 300mK temperatures and stabilized via a closed cycle $^3$He sorption fridge in combination with a $^4$He vacuum pot. The detectors are read out through a combination of the second-generation Reconfigurable Open Architecture Computing Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The firmware and software designed to readout and characterize these detectors was built from scratch by the BLAST team around these detectors, and has been adapted for use by other MKID instruments such as TolTEC and OLIMPO. We present an overview of these systems as well as in-depth methodology of the ground-based characterization and the measured in-flight performance., Comment: Presented at SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X, December 13-18, 2020
Published: 2020
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6. In-flight performance of the BLAST-TNG telescope platform

Author: Coppi, Gabriele, Ade, Peter A. R., Ashton, Peter C., Austermann, Jason E., Cox, Erin G., Devlin, Mark J., Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas, Gao, Jiansong, Gordon, Samuel, Groppi, Christopher E., Hilton, Gene C., Hubmayr, Johannes, Klein, Jeffrey, Li, Dale, Lourie, Nathan P., Lowe, Ian, Mani, Hamdi, Mauskopf, Philip, McKenney, Christopher, Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, L. Javier, Sinclair, Adrian, Soler, Juan D., Tucker, Carole, Ullom, Joel, Vissers, Michael, Wheeler, Caleb, and Williams, Paul A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Next Generation Balloon-Borne Large Aperture Submillimeter Telescope (BLAST-TNG) was a unique instrument for characterizing the polarized submillimeter sky at high-angular resolution. BLAST-TNG flew from the Long Duration Balloon Facility in Antarctica in January 2020. Despite the short flight duration, the instrument worked very well and is providing significant information about each subsystem that will be invaluable for future balloon missions. In this contribution, we discuss the performance of telescope and gondola., Comment: Submitted to SPIE Astronomical Telescopes + Instrumentation, Ground-based and Airborne Telescopes VIII
Published: 2020
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7. 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

8. CONCERTO: Instrument and status

Author: Fasano Alessandro, Ade Peter, Aravena Manuel, Barria Emilio, Beelen Alexandre, Benoît Alain, Béthermin Matthieu, Bounmy Julien, Bourrion Olivier, Bres Guillaume, Calvo Martino, Catalano Andrea, De Breuck Carlos, Désert François-Xavier, Durán Carlos, Fenouillet Thomas, Garcia Jose, Garde Gregory, Goupy Johannes, Groppi Christopher, Hoarau Christophe, Hu Wenkai, Lagache Guilaine, Lambert Jean-Charles, Leggeri Jean-Paul, Levy-Bertrand Florence, Lundgren Andreas, Macías-Pérez Juan, Mani Hamdi, Marpaud Julien, Mauskopf Philip, Monfardini Alessandro, Pisano Giampaolo, Ponthieu Nicolas, Prieur Leo, Roni Samuel, Roudier Sebastien, Tourres Damien, and Tucker Carol
Subjects: Physics, QC1-999
Abstract: CONCERTO (CarbON CII line in post-rEionization and ReionizaTiOn) is a low-resolution Fourier transform spectrometer dedicated to the study of star-forming galaxies and clusters of galaxies in the transparent millimeter windows from the ground. It is characterized by a wide instantaneous 18.6 arcmin field of view, operates at 130–310 GHz, and was installed on the 12-meter Atacama Pathfinder Experiment (APEX) telescope at 5 100m above sea level. CONCERTO’s double focal planes host two arrays of 2 152 kinetic inductance detectors and represent a pioneering instrument to meet a state-of-the-art scientific challenge. This paper introduces the CONCERTO instrument and explains its status, shows the first CONCERTO spectral maps of Orion, and describes the perspectives of the project.
Published: 2024
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9. Preflight Characterization of the BLAST-TNG Receiver and Detector Arrays

Author: Lourie, Nathan P., Ade, Peter A. R., Angile, Francisco E., Ashton, Peter C., Austermann, Jason E., Devlin, Mark J., Dober, Bradley, Galitzki, Nicholas, Gao, Jiansong, Gordon, Sam, Groppi, Christopher E., Klein, Jeffrey, Hilton, Gene C., Hubmayr, Johannes, Li, Dale, Lowe, Ian, Mani, Hamdi, Mauskopf, Philip, McKenney, Christopher M., Nati, Federico, Novak, Giles, Pascale, Enzo, Pisano, Giampaolo, Sinclair, Adrian, Soler, Juan D., Tucker, Carole, Ullom, Joel, Vissers, Michael, and Williams, Paul A.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter mapping experiment planned for a 28 day long-duration balloon (LDB) flight from McMurdo Station, Antarctica during the 2018-2019 season. BLAST-TNG will detect submillimeter polarized interstellar dust emission, tracing magnetic fields in galactic molecular clouds. BLAST-TNG will be the first polarimeter with the sensitivity and resolution to probe the $\sim$0.1 parsec-scale features that are critical to understanding the origin of structures in the interstellar medium. BLAST-TNG features three detector arrays operating at wavelengths of 250, 350, and 500 $\mu$m (1200, 857, and 600 GHz) comprised of 918, 469, and 272 dual-polarization pixels, respectively. Each pixel is made up of two crossed microwave kinetic inductance detectors (MKIDs). These arrays are cooled to 275 mK in a cryogenic receiver. Each MKID has a different resonant frequency, allowing hundreds of resonators to be read out on a single transmission line. This inherent ability to be frequency-domain multiplexed simplifies the cryogenic readout hardware, but requires careful optical testing to map out the physical location of each resonator on the focal plane. Receiver-level optical testing was carried out using both a cryogenic source mounted to a movable xy-stage with a shutter, and a beam-filling, heated blackbody source able to provide a 10-50 $^\circ$C temperature chop. The focal plane array noise properties, responsivity, polarization efficiency, instrumental polarization were measured. We present the preflight characterization of the BLAST-TNG cryogenic system and array-level optical testing of the MKID detector arrays in the flight receiver., Comment: 15 pages, 7 figures, SPIE Astronomical Telescopes and Instrumentation Conference
Published: 2018
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10. 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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11. Operation of a superconducting nanowire in two detection modes: KID and SPD

Author: Schroeder, Edward, Mauskopf, Philip, Mani, Hamdi, Bryan, Sean, Berggren, Karl K., and Zhu, Di
Subjects: Physics - Instrumentation and Detectors
Abstract: We present the performance of a superconducting nanowire that can be operated in two detection modes: i) as a kinetic inductance detector (KID) or ii) as a single-photon detector (SPD). Two superconducting nanowires developed for use as single-photon detectors (SNSPDs) are embedded as the inductive (L) component in resonant inductor/capacitor (LC) circuits coupled to a microwave transmission line. The capacitors are low loss commercial chip capacitors and limit the internal quality factor of the resonators to approximately $Q_i = 170$. The resonator quality factor, $Q_r \simeq 23$, is dominated by the coupling to the feedline and limits the detection bandwidth to on the order of 1MHz. When operated in KID mode, the detectors are AC biased with tones at their resonant frequencies of 45.85 and 91.81MHz. In the low-bias, standard KID mode, a single photon produces a hot spot that does not turn an entire section of the line normal but only increases the kinetic inductance. In the high-bias, critical KID mode, a photon event turns a section of the line normal and the resonance is destroyed until the normal region is dissipated. When operated as an SPD in Geiger mode, the resonators are DC biased through cryogenic bias tees and each photon produces a sharp voltage step followed by a ringdown signal at the resonant frequency of the detector which is converted to a standard pulse with an envelop detector. We show that AC biasing in the critical KID mode is inferior to the sensitivity achieved in DC-biased SPD mode due to the small fraction of time spent near the critical current with an AC bias., Comment: 7 pages, 9 figures, submitted to Journal of Low Temperature Physics
Published: 2017
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12. A Superconducting Phase Shifter and Traveling Wave Kinetic Inductance Parametric Amplifier for W-Band Astronomy

Author: Che, George, Gordon, Samuel, Day, Peter, Groppi, Christopher, Jackson, Rebecca, Mani, Hamdi, Mauskopf, Philip, Surdi, Harshad, Trichopoulos, Georgios, and Underhill, Matthew
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The W-Band ($75-110\; \mathrm{GHz}$) sky contains a plethora of information about star formation, galaxy evolution and the cosmic microwave background. We have designed and fabricated a dual-purpose superconducting circuit to facilitate the next generation of astronomical observations in this regime by providing proof-of-concept for both a millimeter-wave low-loss phase shifter, which can operate as an on-chip Fourier transform spectrometer (FTS) and a traveling wave kinetic inductance parametric amplifier (TKIP). Superconducting transmission lines have a propagation speed that depends on the inductance in the line which is a combination of geometric inductance and kinetic inductance in the superconductor. The kinetic inductance has a non-linear component with a characteristic current, $I_*$, and can be modulated by applying a DC current, changing the propagation speed and effective path length. Our test circuit is designed to measure the path length difference or phase shift, $\Delta \phi$, between two symmetric transmission lines when one line is biased with a DC current. To provide a measurement of $\Delta\phi$, a key parameter for optimizing a high gain W-Band TKIP, and modulate signal path length in FTS operation, our $3.6 \times 2.5\; \mathrm{cm}$ chip employs a pair of $503\; \mathrm{mm}$ long NbTiN inverted microstrip lines coupled to circular waveguide ports through radial probes. For a line of width $3\; \mathrm{\mu m}$ and film thickness $20\; \mathrm{nm}$, we predict $\Delta\phi\approx1767\; \mathrm{rad}$ at $90\; \mathrm{GHz}$ when biased at close to $I_*$. We have fabricated a prototype with $200\; \mathrm{nm}$ thick Nb film and the same line length and width. The predicted phase shift for our prototype is $\Delta\phi\approx30\; \mathrm{rad}$ at $90\; \mathrm{GHz}$ when biased at close to $I_*$ for Nb., Comment: 8 pages, 3 figures, submitted to Journal of Low Temperature Physics
Published: 2017

13. Instrumental performance and results from testing of the BLAST-TNG receiver, submillimeter optics, and MKID arrays

Author: Galitzki, Nicholas, Ade, Peter, Angile, Francesco E., Ashton, Peter, Austermann, Jason, Billings, Tashalee, Che, George, Cho, Hsiao-Mei, Davis, Kristina, Devlin, Mark, Dicker, Simon, Dober, Bradley J., Fissel, Laura M., Fukui, Yasuo, Gao, Jiansong, Gordon, Samuel, Groppi, Christopher E., Hillbrand, Seth, Hilton, Gene C., Hubmayr, Johannes, Irwin, Kent D., Klein, Jeffrey, Li, Dale, Li, Zhi-Yun, Lourie, Nathan P., Lowe, Ian, Mani, Hamdi, Martin, Peter G., Mauskopf, Philip, McKenney, Christopher, Nati, Federico, Novak, Giles, Pascale, Enzo, Pisano, Giampaolo, Santos, Fabio P., Scott, Douglas, Sinclair, Adrian, Soler, Juan D., Tucker, Carole, Underhill, Matthew, Vissers, Michael, and Williams, Paul
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Polarized thermal emission from interstellar dust grains can be used to map magnetic fields in star forming molecular clouds and the diffuse interstellar medium (ISM). The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) flew from Antarctica in 2010 and 2012 and produced degree-scale polarization maps of several nearby molecular clouds with arcminute resolution. The success of BLASTPol has motivated a next-generation instrument, BLAST-TNG, which will use more than 3000 linear polarization sensitive microwave kinetic inductance detectors (MKIDs) combined with a 2.5m diameter carbon fiber primary mirror to make diffraction-limited observations at 250, 350, and 500 $\mu$m. With 16 times the mapping speed of BLASTPol, sub-arcminute resolution, and a longer flight time, BLAST-TNG will be able to examine nearby molecular clouds and the diffuse galactic dust polarization spectrum in unprecedented detail. The 250 $\mu$m detector array has been integrated into the new cryogenic receiver, and is undergoing testing to establish the optical and polarization characteristics of the instrument. BLAST-TNG will demonstrate the effectiveness of kilo-pixel MKID arrays for applications in submillimeter astronomy. BLAST-TNG is scheduled to fly from Antarctica in December 2017 for 28 days and will be the first balloon-borne telescope to offer a quarter of the flight for "shared risk" observing by the community., Comment: Presented at SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, June 29th, 2016
Published: 2016
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14. The Next Generation BLAST Experiment

Author: Galitzki, Nicholas, Ade, Peter A. R., Angilè, Francesco E., Ashton, Peter, Beall, James A., Becker, Dan, Bradford, Kristi J., Che, George, Cho, Hsiao-Mei, Devlin, Mark J., Dober, Bradley J., Fissel, Laura M., Fukui, Yasuo, Gao, Jiansong, Groppi, Christopher E., Hillbrand, Seth, Hilton, Gene C., Hubmayr, Johannes, Irwin, Kent D., Klein, Jeffrey, Van Lanen, Jeff, Li, Dale, Li, Zhi-Yun, Lourie, Nathan P., Mani, Hamdi, Martin, Peter G., Mauskopf, Philip, Nakamura, Fumitaka, Novak, Giles, Pappas, David P., Pascale, Enzo, Pisano, Giampaolo, Santos, Fabio P., Savini, Giorgio, Scott, Douglas, Stanchfield, Sara, Tucker, Carole, Ullom, Joel N., Underhill, Matthew, Vissers, Michael R., and Ward-Thompson, Derek
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) was a suborbital experiment designed to map magnetic fields in order to study their role in star formation processes. BLASTPol made detailed polarization maps of a number of molecular clouds during its successful flights from Antarctica in 2010 and 2012. We present the next-generation BLASTPol instrument (BLAST-TNG) that will build off the success of the previous experiment and continue its role as a unique instrument and a test bed for new technologies. With a 16-fold increase in mapping speed, BLAST-TNG will make larger and deeper maps. Major improvements include a 2.5 m carbon fiber mirror that is 40% wider than the BLASTPol mirror and ~3000 polarization sensitive detectors. BLAST-TNG will observe in three bands at 250, 350, and 500 microns. The telescope will serve as a pathfinder project for microwave kinetic inductance detector (MKID) technology, as applied to feedhorn coupled submillimeter detector arrays. The liquid helium cooled cryostat will have a 28-day hold time and will utilize a closed-cycle $^3$He refrigerator to cool the detector arrays to 270 mK. This will enable a detailed mapping of more targets with higher polarization resolution than any other submillimeter experiment to date. BLAST-TNG will also be the first balloon-borne telescope to offer shared risk observing time to the community. This paper outlines the motivation for the project and the instrumental design.
Published: 2014
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15. The next-generation BLASTPol experiment

Author: Dober, Bradley, Ade, Peter A. R., Ashton, Peter, Angilè, Francesco E., Beall, James A., Becker, Dan, Bradford, Kristi J., Che, George, Cho, Hsiao-Mei, Devlin, Mark J., Fissel, Laura M., Fukui, Yasuo, Galitzki, Nicholas, Gao, Jiansong, Groppi, Christopher E., Hillbrand, Seth, Hilton, Gene C., Hubmayr, Johannes, Irwin, Kent D., Klein, Jeffrey, Van Lanen, Jeff, Li, Dale, Li, Zhi-Yun, Lourie, Nathan P., Mani, Hamdi, Martin, Peter G., Mauskopf, Philip, Nakamura, Fumitaka, Novak, Giles, Pappas, David P., Pascale, Enzo, Santos, Fabio P., Savini, Giorgio, Scott, Douglas, Stanchfield, Sara, Ullom, Joel N., Underhill, Matthew, Vissers, Michael R., and Ward-Thompson, Derek
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) is a suborbital mapping experiment designed to study the role magnetic fields play in star formation. BLASTPol has had two science flights from McMurdo Station, Antarctica in 2010 and 2012. These flights have produced thousands of polarization vectors at 250, 350 and 500 microns in several molecular cloud targets. We present the design, specifications, and progress towards the next-generation BLASTPol experiment (BLAST-TNG). BLAST-TNG will fly a 40% larger diameter primary mirror, with almost 8 times the number of polarization-sensitive detectors resulting in a factor of 16 increase in mapping speed. With a spatial resolution of 22 arcseconds and four times the field of view of BLASTPol, BLAST-TNG will bridge the angular scales between Planck's low resolution all-sky maps and ALMA's ultra-high resolution narrow fields. The new receiver has a larger cryogenics volume, allowing for a 28 day hold time. BLAST-TNG employs three arrays of Microwave Kinetic Inductance Detectors (MKIDs) with 30% fractional bandwidth at 250, 350 and 500 microns. In this paper, we will present the new BLAST-TNG instrument and science objectives., Comment: 12 pages, 6 figures. Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145
Published: 2014
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16. SuperCam, a 64-pixel heterodyne imaging array for the 870 micron atmospheric window

Author: Groppi, Christopher, Walker, Christopher, Kulesa, Craig, Puetz, Patrick, Golish, Dathon, Gensheimer, Paul, Hedden, Abigail, Bussmann, Shane, Weinreb, Sander, Kuiper, Thomas, Kooi, Jacob, Jones, Glenn, Bardin, Joseph, Mani, Hamdi, Lichtenberger, Arthur, and Narayanan, Gopal
Subjects: Astrophysics
Abstract: We report on the development of SuperCam, a 64 pixel, superheterodyne camera designed for operation in the astrophysically important 870 micron atmospheric window. SuperCam will be used to answer fundamental questions about the physics and chemistry of molecular clouds in the Galaxy and their direct relation to star and planet formation. The advent of such a system will provide an order of magnitude increase in mapping speed over what is now available and revolutionize how observational astronomy is performed in this important wavelength regime. Unlike the situation with bolometric detectors, heterodyne receiver systems are coherent, retaining information about both the amplitude and phase of the incident photon stream. From this information a high resolution spectrum of the incident light can be obtained without multiplexing. SuperCam will be constructed by stacking eight, 1x8 rows of fixed tuned, SIS mixers. The IF output of each mixer will be connected to a low-noise, broadband MMIC amplifier integrated into the mixer block. The instantaneous IF bandwidth of each pixel will be ~2 GHz, with a center frequency of 5 GHz. A spectrum of the central 500 MHz of each IF band will be provided by the array spectrometer. Local oscillator power is provided by a frequency multiplier whose output is divided between the pixels by using a matrix of waveguide power dividers. The mixer array will be cooled to 4K by a closed-cycle refrigeration system. SuperCam will reside at the Cassegrain focus of the 10m Heinrich Hertz telescope (HHT). A prototype single row of the array will be tested on the HHT in 2006, with the first engineering run of the full array in late 2007. The array is designed and constructed so that it may be readily scaled to higher frequencies., Comment: 12 pages, 14 figures, to be published in the Proceedings of SPIE Vol. 6275, "Astronomical Telescopes and Instrumentation, Millimeter and Submillimeter Detectors and Instrumentation for Astronomy III"
Published: 2006
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17. Operation of a Superconducting Nanowire in Two Detection Modes: KID and SPD

Author: Schroeder, Edward, Mauskopf, Philip, Mani, Hamdi, Bryan, Sean, Berggren, Karl K., and Zhu, Di
Published: 2019
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18. A Cryogenic Wideband (2.5–14 GHz) Receiver System for the Arecibo Observatory 12 m Telescope.

Author: Roshi, D. Anish, Perillat, Phil, Fernandez, Felix, Mani, Hamdi, Perera, Benetge, Manoharan, Periasamy K., Quintero, Luis, and Venkataraman, Arun
Subjects: RADIO interference, LOW noise amplifiers, HIGHPASS electric filters, OBSERVATORIES, VERY large array telescopes, TELESCOPES, PHOSPHORIMETRY
Abstract: In this paper we present details of the construction of a wideband, cryogenic receiver and its successful commissioning on the Arecibo Observatory 12 m telescope. The cryogenic receiver works in the 2.5–14 GHz frequency range. We upgraded the current narrow band, room temperature receivers of the telescope with the new wideband receiver. The current receiver is built around a Quadruple‐Ridged Flared Horn (QRFH) developed by Akgiray et al. (2013, https://doi.org/10.1109/tap.2012.2229953). To mitigate strong radio frequency interference (RFI) below 2.7 GHz, we installed a highpass filter before the first stage low noise amplifier (LNA). The QRFH, highpass filter, noise coupler and LNA are located inside a cryostat and are cooled to 15 K. The measured receiver temperature is 25 K (median value) over 2.5–14 GHz. The system temperature measured at zenith is about 40 K near 3.1 and 8.6 GHz and the zenith antenna gains are 0.025 and 0.018 K/Jy at the two frequencies respectively. We recommend the following improvements to the telescope system: (a) Upgrade the highpass filter to achieve better RFI rejection near 2.5 GHz; (b) Improve aperture efficiency at 8.6 GHz; (c) Upgrade the intermediate frequency system to increase the upper frequency of operation from 12 to 14 GHz. Key Points: Successful commissioning of a wideband, cryogenic receiver for the 12 m telescope at the Arecibo ObservatoryAchieved system temperature of 40 K and gains of 0.025 K/Jy and 0.018 K/Jy at frequencies 3.1 and 8.6 GHz respectively [ABSTRACT FROM AUTHOR]
Published: 2024
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19. 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

20. CONCERTO: a breakthrough in wide field-of-view spectroscopy at millimeter wavelengths

Author: Fasano, Alessandro, primary, Beelen, Alexandre, additional, Benoit, Alain, additional, Lundgren, Andreas, additional, Ade, Peter, additional, Aravena, Manuel, additional, Barria, Emilio, additional, Béthermin, Matthieu, additional, Boumy, Julien, additional, Bourrion, Olivier, additional, Bres, Guillaume, additional, Calvo, Martino, additional, Catalano, Andrea, additional, Désert, François-Xavier, additional, De Breuck, Carlos, additional, Duran, Carlos, additional, Fenouillet, Thomas, additional, Garcia, Jose, additional, Garde, Gregory, additional, Goupy, Johannes, additional, Groppi, Christian, additional, Hoarau, Christophe, additional, Hu, Wenkai, additional, Lagache, Guilaine, additional, Lambert, Jean-Charles, additional, Leggeri, Jean-Paul, additional, Levy-Bertrand, Florence, additional, Macias-Perez, Juan, additional, Mani, Hamdi, additional, Marpaud, Julien, additional, Mauskopf, Philip, additional, Monfardini, Alessandro, additional, Pisano, Giampaolo, additional, Ponthieu, Nicola, additional, Prieur, Leo, additional, Roni, Samuel, additional, Roudier, Sebastien, additional, Tourres, Damien, additional, Tucker, Carol, additional, and Cuyck, Mathilde V., additional
Published: 2022
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21. A 4.2-9.2GHz Cryogenic Transformer Feedback Low Noise Amplifier with 4.5K Noise Temperature and Noise-Power Matching in 22nm CMOS FDSOI

Author: Lin, Boce, primary, Mani, Hamdi, additional, Marsh, Phil, additional, Hadi, Richard Al, additional, and Wang, Hua, additional
Published: 2022
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22. Current Status of the Ali CMB Polarization Telescope Focal Plane Camera

Author: Salatino, Maria, primary, Austermann, Jason, additional, Meinke, Jeremy, additional, Sinclair, Adrian K., additional, Walker, Samantha, additional, Bai, Xiran, additional, Beall, James, additional, Connors, Jake, additional, Dober, Bradley, additional, Duff, Shannon M., additional, Givhan, Richard C., additional, Hilton, Gene, additional, Hubmayr, Johannes, additional, Karpel, Ethan D., additional, Kuo, Chao-Lin, additional, Mani, Hamdi, additional, Mates, John A.B., additional, Mathewson, Justin, additional, Mauskopf, Philip, additional, Montana-Lopez, Jordi A., additional, Stephenson, Ryan, additional, Thompson, Keith L., additional, Ullom, Joel, additional, van Lanen, Jeff, additional, Yoon, Ki Won, additional, Weeks, Eric L., additional, Wu, Yi-Han, additional, and Zhang, Xinmin, additional
Published: 2021
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23. Cryogenic Noise-Parameter Measurements: Recent Research and a Fully Automated Measurement Application

Author: Sheldon, Alexander, primary, Belostotski, Leonid, additional, Mani, Hamdi, additional, Groppi, Christopher E., additional, and Warnick, Karl F., additional
Published: 2021
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24. Search for Axionlike Dark Matter Using Solid-State Nuclear Magnetic Resonance

Author: Aybas, Deniz, Adam, Janos, Blumenthal, Emmy, Gramolin, Alexander, V, Johnson, Dorian, Kleyheeg, Annalies, Afach, Samer, Blanchard, John W., Centers, Gary P., Garcon, Antoine, Engler, Martin, Figueroa, Nataniel L., Sendra, Marina Gil, Wickenbrock, Arne, Lawson, Matthew, Wang, Tao, Wu, Teng, Luo, Haosu, Mani, Hamdi, Mauskopf, Philip, Graham, Peter W., Rajendran, Surjeet, Kimball, Derek F. Jackson, Budker, Dmitry, Sushkov, Alexander O., Aybas, Deniz, Adam, Janos, Blumenthal, Emmy, Gramolin, Alexander, V, Johnson, Dorian, Kleyheeg, Annalies, Afach, Samer, Blanchard, John W., Centers, Gary P., Garcon, Antoine, Engler, Martin, Figueroa, Nataniel L., Sendra, Marina Gil, Wickenbrock, Arne, Lawson, Matthew, Wang, Tao, Wu, Teng, Luo, Haosu, Mani, Hamdi, Mauskopf, Philip, Graham, Peter W., Rajendran, Surjeet, Kimball, Derek F. Jackson, Budker, Dmitry, and Sushkov, Alexander O.
Abstract: We report the results of an experimental search for ultralight axionlike dark matter in the mass range 162-166 neV. The detection scheme of our Cosmic Axion Spin Precession Experiment is based on a precision measurement of Pb-207 solid-state nuclear magnetic resonance in a polarized ferroelectric crystal. Axionlike dark matter can exert an oscillating torque on Pb-20(7) nuclear spins via the electric dipole moment coupling g(d) or via the gradient coupling g(aNN). We calibrate the detector and characterize the excitation spectrum and relaxation parameters of the nuclear spin ensemble with pulsed magnetic resonance measurements in a 4.4 T magnetic field. We sweep the magnetic field near this value and search for axionlike dark matter with Compton frequency within a 1 MHz band centered at 39.65 MHz. Our measurements place the upper bounds vertical bar g(d)vertical bar < 9.5 x 10(-4) GeV-2 and vertical bar g(aNN)vertical bar( )< 2.8 x 10(-1) GeV-1 (95% confidence level) in this frequency range. The constraint on g d corresponds to an upper bound of 1.0 x 10(-21) e cm on the amplitude of oscillations of the neutron electric dipole moment and 4.3 x 10(-6) on the amplitude of oscillations of CP-violating theta parameter of quantum chromodynamics. Our results demonstrate the feasibility of using solid-state nuclear magnetic resonance to search for axionlike dark matter in the neV mass range., QC 20210611
Published: 2021
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25. Automated Noise-Parameter Measurements of Cryogenic LNAs

Author: Sheldon, Alexander, primary, Belostotski, Leonid, additional, Mani, Hamdi, additional, Groppi, Christopher E., additional, and Warnick, Karl F., additional
Published: 2021
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26. Search for Axionlike Dark Matter Using Solid-State Nuclear Magnetic Resonance

Author: Aybas, Deniz, primary, Adam, Janos, additional, Blumenthal, Emmy, additional, Gramolin, Alexander V., additional, Johnson, Dorian, additional, Kleyheeg, Annalies, additional, Afach, Samer, additional, Blanchard, John W., additional, Centers, Gary P., additional, Garcon, Antoine, additional, Engler, Martin, additional, Figueroa, Nataniel L., additional, Sendra, Marina Gil, additional, Wickenbrock, Arne, additional, Lawson, Matthew, additional, Wang, Tao, additional, Wu, Teng, additional, Luo, Haosu, additional, Mani, Hamdi, additional, Mauskopf, Philip, additional, Graham, Peter W., additional, Rajendran, Surjeet, additional, Kimball, Derek F. Jackson, additional, Budker, Dmitry, additional, and Sushkov, Alexander O., additional
Published: 2021
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27. Design of cryogenic SiGe low-noise amplifiers

Author: Weinreb, Sander, Bardin, Joseph C., and Mani, Hamdi
Subjects: Microwave amplifiers -- Design and construction, Silicon compounds -- Properties, Germanium -- Properties, Business, Computers, Electronics, Electronics and electrical industries
Abstract: This paper describes a method for designing cryogenic silicon--germanium (SiGe) transistor low-noise amplifiers and reports record microwave noise temperature, i.e., 2 K, measured at the module connector interface with a 50-[OMEGA] generator. A theory for the relevant noise sources in the transistor is derived from first principles to give the minimum possible noise temperature and optimum generator impedance in terms of dc measured current gain and transconductance. These measured dc quantities are then reported for an IBM SiGe BiCMOS-8HP transistor at temperatures from 295 to 15 K. The measured and modeled noise and gain for both a single- and two-transistor cascode amplifier in the 0.2-3-GHz range are then presented. The noise model is then combined with the transistor equivalent-circuit elements in a circuit simulator and the noise in the frequency range up to 20 GHz is compared with that of a typical InP HEMT. Index Terms--Cascode, cryogenic, low-noise amplifier (LNA), noise parameters, silicon--germanium (SiGe).
Published: 2007

28. In-flight performance of the BLAST-TNG telescope platform

Author: Marshall, HK, Spyromilio, J, Usuda, T, Coppi, G, Ade, P, Ashton, P, Austermann, J, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lowe, I, Lourie, N, Mckinney, C, Mani, H, Mauskopf, P, Nati, F, Novak, G, Pisano, G, Romualdez, J, Sinclair, A, Soler, J, Tucker, C, Ullom, J, Visser, M, Wheeler, C, Williams, P, Coppi, Gabriele, Ade, Peter A., Ashton, Peter C., Austermann, Jason E., Cox, Erin G., Devlin, Mark J., Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas B., Gao, Jiansong, Gordon, Samuel, Groppi, Christopher E., Hilton, Gene C., Hubmayr, Johannes, Klein, Jeffrey, Li, Dale, Lowe, Ian, Lourie, Nathan P., Mckinney, Christopher, Mani, Hamdi, Mauskopf, Philip D., Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, Javier L., Sinclair, Adrian K., Soler, Juan D., Tucker, Carole, Ullom, Joel, Visser, Michael, Wheeler, Caleb H., Williams, Paul A., Marshall, HK, Spyromilio, J, Usuda, T, Coppi, G, Ade, P, Ashton, P, Austermann, J, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lowe, I, Lourie, N, Mckinney, C, Mani, H, Mauskopf, P, Nati, F, Novak, G, Pisano, G, Romualdez, J, Sinclair, A, Soler, J, Tucker, C, Ullom, J, Visser, M, Wheeler, C, Williams, P, Coppi, Gabriele, Ade, Peter A., Ashton, Peter C., Austermann, Jason E., Cox, Erin G., Devlin, Mark J., Dober, Bradley J., Fanfani, Valentina, Fissel, Laura M., Galitzki, Nicholas B., Gao, Jiansong, Gordon, Samuel, Groppi, Christopher E., Hilton, Gene C., Hubmayr, Johannes, Klein, Jeffrey, Li, Dale, Lowe, Ian, Lourie, Nathan P., Mckinney, Christopher, Mani, Hamdi, Mauskopf, Philip D., Nati, Federico, Novak, Giles, Pisano, Giampaolo, Romualdez, Javier L., Sinclair, Adrian K., Soler, Juan D., Tucker, Carole, Ullom, Joel, Visser, Michael, Wheeler, Caleb H., and Williams, Paul A.
Abstract: The Next Generation Balloon-Borne Large Aperture Submillimeter Telescope (BLAST-TNG) was a unique instrument for characterizing the polarized submillimeter sky at high-angular resolution. BLAST-TNG flew from the Long Duration Balloon Facility in Antarctica in January 2020. Despite the short flight duration, the instrument worked very well and is providing significant information about each subsystem that will be invaluable for future balloon missions. In this contribution, we discuss the performance of telescope and gondola.
Published: 2020

29. Operation of a Superconducting Nanowire in Two Detection Modes: KID and SPD

Author: Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Schroeder, Edward, Mauskopf, Philip, Mani, Hamdi, Bryan, Sean, Berggren, Karl K., Zhu, Di, Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Schroeder, Edward, Mauskopf, Philip, Mani, Hamdi, Bryan, Sean, Berggren, Karl K., and Zhu, Di
Abstract: We present the performance of a superconducting nanowire that can be operated in two detection modes: (i) as a kinetic inductance detector (KID) or (ii) as a single-photon detector (SPD). Two superconducting nanowires developed for use as single-photon detectors (SNSPDs) are embedded as the inductive (L) component in resonant inductor/capacitor (LC) circuits coupled to a microwave transmission line. The capacitors are low loss commercial chip capacitors and limit the internal quality factor of the resonators to approximately Q i = 170. The resonator quality factor, Q r ≃ 23 , is dominated by the coupling to the feedline and limits the detection bandwidth to on the order of 1 MHz. When operated in KID mode, the detectors are AC biased with tones at their resonant frequencies of 45.85 and 91.81 MHz. In the low-bias, standard KID mode, a single photon produces a hot spot that does not turn an entire section of the line normal but only increases the kinetic inductance. In the high-bias, critical KID mode, a photon event turns a section of the line normal and the resonance is destroyed until the normal region is dissipated. When operated as an SPD in Geiger mode, the resonators are DC biased through cryogenic bias tees and each photon produces a sharp voltage step followed by a ringdown signal at the resonant frequency of the detector which is converted to a standard pulse with an envelope detector. We show that AC biasing in the critical KID mode is inferior to the sensitivity achieved in DC-biased SPD mode due to the small fraction of time spent near the critical current with an AC bias. ©2018, Springer Science+Business Media, LLC, part of Springer Nature., NSF (AST ATI Grant: 1509078)
Published: 2020

30. The TolTEC camera: an overview of the instrument and in-lab testing results

Author: Wilson, Grant W., primary, Abi-saad, Sophia, additional, Ade, Peter, additional, Aretxaga, Itziar, additional, Austermann, Jason E., additional, Ban, Yvonne, additional, Bardin, Joseph, additional, Beall, James A., additional, Berthoud, Marc, additional, Bryan, Sean A., additional, Bussan, John, additional, Castillo-Domínguez, Edgar, additional, Chavez, Miguel, additional, Contente, Reid, additional, DeNigris, Natalie W., additional, Dober, Bradley, additional, Eiben, Miranda, additional, Ferrusca, Daniel, additional, Fissel, Laura, additional, Gao, Jiansong, additional, Golec, Joey, additional, Golina, Robert, additional, Gomez, Arturo, additional, Gordon, Sam, additional, Gutermuth, Robert, additional, Hilton, Gene, additional, Hosseini, Mohsen, additional, Hubmayr, Johannes, additional, Hughes, David, additional, Kuczarski, Stephen W., additional, Lee, Dennis, additional, Lunde, Emily, additional, Ma, Zhiyuan, additional, Mani, Hamdi, additional, Mauskopf, Philip, additional, McCrackan, Michael, additional, McKenney, Christopher, additional, McMahon, Jeffrey, additional, Novak, Giles, additional, Pisano, Giampaolo, additional, Pope, Alexandra, additional, Ralston, Amy, additional, Rodriguez, Ivan, additional, Sánchez-Argüelles, David, additional, Schloerb, F. Peter, additional, Simon, Sara M., additional, Sinclair, Adrian, additional, Souccar, Kamal, additional, Torres Campos, Ana, additional, Tucker, Carole, additional, Ullom, Joel, additional, Van Camp, Eric, additional, Van Lanen, Jeff, additional, Velazquez, Miguel, additional, Vissers, Michael, additional, Weeks, Eric, additional, and Yun, Min S., additional
Published: 2020
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31. Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver

Author: Lowe, Ian N., primary, Ade, Peter, additional, Ashton, Peter, additional, Austermann, Jason, additional, Coppi, Gabriele, additional, Cox, Erin G., additional, Devlin, Mark, additional, Dober, Bradley, additional, Fanfani, Valentina, additional, Fissel, Laura, additional, Galitzki, Nicholas, additional, Gao, Jiansong, additional, Gordon, Samuel, additional, Groppi, Christopher, additional, Hilton, Gene, additional, Hubmayr, Johannes, additional, Klein, Jeff, additional, Li, Dale, additional, Lourie, Nathan P., additional, Mani, Hamdi, additional, Mauskopf, Philip, additional, McKenney, Christopher, additional, Nati, Federico, additional, Novak, Giles, additional, Pisano, Giampaolo, additional, Romualdez, Javier, additional, Soler, Juan D., additional, Sinclair, Adrian, additional, Tucker, Carole, additional, Ullom, Joel, additional, Vissers, Michael, additional, Wheeler, Caleb, additional, and Williams, Paul, additional
Published: 2020
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32. In-flight performance of the BLAST-TNG telescope platform

Author: Coppi, Gabriele, primary, Ade, Peter A., additional, Ashton, Peter C., additional, Austermann, Jason E., additional, Cox, Erin G., additional, Devlin, Mark J., additional, Dober, Bradley J., additional, Fanfani, Valentina, additional, Fissel, Laura M., additional, Galitzki, Nicholas B., additional, Gao, Jiansong, additional, Gordon, Samuel, additional, Groppi, Christopher E., additional, Hilton, Gene C., additional, Hubmayr, Johannes, additional, Klein, Jeffrey, additional, Li, Dale, additional, Lowe, Ian, additional, Lourie, Nathan P., additional, Mckinney, Christopher, additional, Mani, Hamdi, additional, Mauskopf, Philip D., additional, Nati, Federico, additional, Novak, Giles, additional, Pisano, Giampaolo, additional, Romualdez, Javier L., additional, Sinclair, Adrian K., additional, Soler, Juan D., additional, Tucker, Carole, additional, Ullom, Joel, additional, Visser, Michael, additional, Wheeler, Caleb H., additional, and Williams, Paul A., additional
Published: 2020
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33. CONCERTO: a breakthrough in wide field-of-view spectroscopy at millimeter wavelengths

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, Fasano, Alessandro, Beelen, Alexandre, Benoît, Alain, Lundgren, Andreas, Ade, Peter, Aravena, Manuel, Barria, Emilio, Béthermin, Matthieu, Bounmy, Julien, Bourrion, Olivier, Bres, Guillaume, Calvo, Martino, Catalano, Andrea, Désert, François-Xavier, De Breuck, Carlos, Durán, Carlos, Fenouillet, Thomas, Garcia, Jose, Garde, Gregory, Goupy, Johannes, Groppi, Christopher, Hoarau, Christophe, Hu, Wenkai, Lagache, Guilaine, Lambert, Jean-Charles, Leggeri, Jean-Paul, Levy-Bertrand, Florence, Macías-Pérez, Juan, Mani, Hamdi, Marpaud, Julien, Mauskopf, Philip, Monfardini, Alessandro, Pisano, Giampaolo, Ponthieu, Nicolas, Prieur, Leo, Roni, Samuel, Roudier, Sebastien, Tourres, Damien, Tucker, Carol, and Cuyck, Mathilde Van
Published: 2022
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34. The Simons Observatory : science goals and forecasts

Author: Ade, Peter, Aguirre, James, Ahmed, Zeeshan, Aiola, Simone, Ali, Aamir, Alonso, David, Alvarez, Marcelo A., Arnold, Kam, Ashton, Peter, Austermann, Jason, Awan, Humna, Baccigalupi, Carlo, Baildon, Taylor, Barron, Darcy, Battaglia, Nick, Battye, Richard, Baxter, Eric, Bazarko, Andrew, Beall, James A., Bean, Rachel, Beck, Dominic, Beckman, Shawn, Beringue, Benjamin, Bianchini, Federico, Boada, Steven, Boettger, David, Bond, J. Richard, Borrill, Julian, Brown, Michael L., Bruno, Sarah Marie, Bryan, Sean, Calabrese, Erminia, Calafut, Victoria, Calisse, Paolo, Carron, Julien, Challinor, Anthony, Chesmore, Grace, Chinone, Yuji, Chluba, Jens, Cho, Hsiao-Mei Sherry, Choi, Steve, Coppi, Gabriele, Cothard, Nicholas F., Coughlin, Kevin, Crichton, Devin, Crowley, Kevin D., Crowley, Kevin T., Cukierman, Ari, D'Ewart, John M., Dunner, 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, Fluxa, 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, Hlozek, Renee, 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, Loic, 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, 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, Sakurail, 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., Verges, 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, Zhu, Ningfeng, 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., Dunner, 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, Fluxa, 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, Hlozek, Renee, 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, Loic, 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, 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, Sakurail, 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., Verges, 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
Abstract: The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial con figuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping approximate to 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 large aperture telescope will map approximate to 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 Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and
Published: 2019
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35. The Simons Observatory: science goals and forecasts

Author: Ade, P, Aguirre, J, Ahmed, Z, Aiola, S, Ali, A, Alonso, D, Alvarez, M, Arnold, K, Ashton, P, Austermann, J, Awan, H, Baccigalupi, C, Baildon, T, Barron, D, Battaglia, N, Battye, R, Baxter, E, Bazarko, A, Beall, J, Bean, R, Beck, D, Beckman, S, Beringue, B, Bianchini, F, Boada, S, Boettger, D, Bond, J, Borrill, J, Brown, M, Bruno, S, Bryan, S, Calabrese, E, Calafut, V, Calisse, P, Carron, J, Challinor, A, Chesmore, G, Chinone, Y, Chluba, J, Cho, H, Choi, S, Coppi, G, Cothard, N, Coughlin, K, Crichton, D, Crowley, K, Cukierman, A, D'Ewart, J, Dünner, R, de Haan, T, Devlin, M, Dicker, S, Didier, J, Dobbs, M, Dober, B, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dusatko, J, Errard, J, Fabbian, G, Feeney, S, Ferraro, S, Fluxà, P, Freese, K, Frisch, J, Frolov, A, Fuller, G, Fuzia, B, Galitzki, N, Gallardo, P, Ghersi, J, Gao, J, Gawiser, E, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Golec, J, Gordon, S, Gralla, M, Green, D, Grigorian, A, Groh, J, Groppi, C, Guan, Y, Gudmundsson, J, Han, D, Hargrave, P, Hasegawa, M, Hasselfield, M, Hattori, M, Haynes, V, Hazumi, M, He, Y, Healy, E, Henderson, S, Hervias-Caimapo, C, Hill, C, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hinshaw, G, Hložek, R, Ho, S, Howe, L, Huang, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Ijjas, A, Ikape, M, Irwin, K, Jaffe, A, Jain, B, Jeong, O, Kaneko, D, Karpel, E, Katayama, N, Keating, B, Kernasovskiy, S, Keskitalo, R, Kisner, T, Kiuchi, K, Klein, J, Knowles, K, Koopman, B, Kosowsky, A, Krachmalnicoff, N, Kuenstner, S, Kuo, C, Kusaka, A, Lashner, J, Lee, A, Lee, E, Leon, D, Leung, J, Lewis, A, Li, Y, Li, Z, Limon, M, Linder, E, Lopez-Caraballo, C, Louis, T, Lowry, L, Lungu, M, Madhavacheril, M, Mak, D, Maldonado, F, Mani, H, Mates, B, Matsuda, F, Maurin, L, Mauskopf, P, May, A, Mccallum, N, Mckenney, C, Mcmahon, J, Meerburg, P, Meyers, J, Miller, A, Mirmelstein, M, Moodley, K, Munchmeyer, M, Munson, C, Naess, S, Nati, F, Navaroli, M, Newburgh, L, Nguyen, H, Niemack, M, Nishino, H, Orlowski-Scherer, J, Page, L, Partridge, B, Peloton, J, Perrotta, F, Piccirillo, L, Pisano, G, Poletti, D, Puddu, R, Puglisi, G, Raum, C, Reichardt, C, Remazeilles, M, Rephaeli, Y, Riechers, D, Rojas, F, Roy, A, Sadeh, S, Sakurai, Y, Salatino, M, Rao, M, Schaan, E, Schmittfull, M, Sehgal, N, Seibert, J, Seljak, U, Sherwin, B, Shimon, M, Sierra, C, Sievers, J, Sikhosana, P, Silva-Feaver, M, Simon, S, Sinclair, A, Siritanasak, P, Smith, K, Smith, S, Spergel, D, Staggs, S, Stein, G, Stevens, J, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Teply, G, Thomas, D, Thorne, B, Thornton, R, Trac, H, Tsai, C, Tucker, C, Ullom, J, Vagnozzi, S, Engelen, A, Lanen, J, Winkle, D, Vavagiakis, E, Vergès, C, Vissers, M, Wagoner, K, Walker, S, Ward, J, Westbrook, B, Whitehorn, N, Williams, J, Wollack, E, Xu, Z, Yu, B, Yu, C, Zago, F, Zhang, H, Zhu, N, 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, Engelen, Alexander van, Lanen, Jeff Van, Winkle, Daniel D. Van, 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, Zhu, Ningfeng, Ade, P, Aguirre, J, Ahmed, Z, Aiola, S, Ali, A, Alonso, D, Alvarez, M, Arnold, K, Ashton, P, Austermann, J, Awan, H, Baccigalupi, C, Baildon, T, Barron, D, Battaglia, N, Battye, R, Baxter, E, Bazarko, A, Beall, J, Bean, R, Beck, D, Beckman, S, Beringue, B, Bianchini, F, Boada, S, Boettger, D, Bond, J, Borrill, J, Brown, M, Bruno, S, Bryan, S, Calabrese, E, Calafut, V, Calisse, P, Carron, J, Challinor, A, Chesmore, G, Chinone, Y, Chluba, J, Cho, H, Choi, S, Coppi, G, Cothard, N, Coughlin, K, Crichton, D, Crowley, K, Cukierman, A, D'Ewart, J, Dünner, R, de Haan, T, Devlin, M, Dicker, S, Didier, J, Dobbs, M, Dober, B, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dusatko, J, Errard, J, Fabbian, G, Feeney, S, Ferraro, S, Fluxà, P, Freese, K, Frisch, J, Frolov, A, Fuller, G, Fuzia, B, Galitzki, N, Gallardo, P, Ghersi, J, Gao, J, Gawiser, E, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Golec, J, Gordon, S, Gralla, M, Green, D, Grigorian, A, Groh, J, Groppi, C, Guan, Y, Gudmundsson, J, Han, D, Hargrave, P, Hasegawa, M, Hasselfield, M, Hattori, M, Haynes, V, Hazumi, M, He, Y, Healy, E, Henderson, S, Hervias-Caimapo, C, Hill, C, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hinshaw, G, Hložek, R, Ho, S, Howe, L, Huang, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Ijjas, A, Ikape, M, Irwin, K, Jaffe, A, Jain, B, Jeong, O, Kaneko, D, Karpel, E, Katayama, N, Keating, B, Kernasovskiy, S, Keskitalo, R, Kisner, T, Kiuchi, K, Klein, J, Knowles, K, Koopman, B, Kosowsky, A, Krachmalnicoff, N, Kuenstner, S, Kuo, C, Kusaka, A, Lashner, J, Lee, A, Lee, E, Leon, D, Leung, J, Lewis, A, Li, Y, Li, Z, Limon, M, Linder, E, Lopez-Caraballo, C, Louis, T, Lowry, L, Lungu, M, Madhavacheril, M, Mak, D, Maldonado, F, Mani, H, Mates, B, Matsuda, F, Maurin, L, Mauskopf, P, May, A, Mccallum, N, Mckenney, C, Mcmahon, J, Meerburg, P, Meyers, J, Miller, A, Mirmelstein, M, Moodley, K, Munchmeyer, M, Munson, C, Naess, S, Nati, F, Navaroli, M, Newburgh, L, Nguyen, H, Niemack, M, Nishino, H, Orlowski-Scherer, J, Page, L, Partridge, B, Peloton, J, Perrotta, F, Piccirillo, L, Pisano, G, Poletti, D, Puddu, R, Puglisi, G, Raum, C, Reichardt, C, Remazeilles, M, Rephaeli, Y, Riechers, D, Rojas, F, Roy, A, Sadeh, S, Sakurai, Y, Salatino, M, Rao, M, Schaan, E, Schmittfull, M, Sehgal, N, Seibert, J, Seljak, U, Sherwin, B, Shimon, M, Sierra, C, Sievers, J, Sikhosana, P, Silva-Feaver, M, Simon, S, Sinclair, A, Siritanasak, P, Smith, K, Smith, S, Spergel, D, Staggs, S, Stein, G, Stevens, J, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Teply, G, Thomas, D, Thorne, B, Thornton, R, Trac, H, Tsai, C, Tucker, C, Ullom, J, Vagnozzi, S, Engelen, A, Lanen, J, Winkle, D, Vavagiakis, E, Vergès, C, Vissers, M, Wagoner, K, Walker, S, Ward, J, Westbrook, B, Whitehorn, N, Williams, J, Wollack, E, Xu, Z, Yu, B, Yu, C, Zago, F, Zhang, H, Zhu, N, 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, Engelen, Alexander van, Lanen, Jeff Van, Winkle, Daniel D. Van, 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
Abstract: The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial con figuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping approximate to 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 large aperture telescope will map approximate to 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 Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and
Published: 2019

36. Cryogenic high-linearity and dynamic range C-band low-noise amplifier for uMUX TES and CMB readout systems

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, Mathewson, Justin L. H., Weeks, Eric L., Scott, Richard M., Zheng, Kaiwen, Groppi, Chris, Mauskopf, Philip, and Mani, Hamdi
Published: 2024
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37. A customizable, five-stage, intermediate frequency, low-noise amplifier and readout chain for the Astrophysics Stratospheric Telescope for High-spectral Resolution Observations at Submillimeter-wavelengths (ASTHROS)

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, Mathewson, Justin L. H., Rodriguez, Ricardo R., Weeks, Eric L., Horton, Paul, Roberson, Cody, Hedges, Madison, Thompson, Christian, Kawamura, Jonathan H., Siles, Jose V., Mani, Hamdi, Mauskopf, Philip, and Groppi, Chris
Published: 2024
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38. The Simons Observatory: science goals and forecasts

Author: Ade, Peter, primary, Aguirre, James, additional, Ahmed, Zeeshan, additional, Aiola, Simone, additional, Ali, Aamir, additional, Alonso, David, additional, Alvarez, Marcelo A., additional, Arnold, Kam, additional, Ashton, Peter, additional, Austermann, Jason, additional, Awan, Humna, additional, Baccigalupi, Carlo, additional, Baildon, Taylor, additional, Barron, Darcy, additional, Battaglia, Nick, additional, Battye, Richard, additional, Baxter, Eric, additional, Bazarko, Andrew, additional, Beall, James A., additional, Bean, Rachel, additional, Beck, Dominic, additional, Beckman, Shawn, additional, Beringue, Benjamin, additional, Bianchini, Federico, additional, Boada, Steven, additional, Boettger, David, additional, Bond, J. Richard, additional, Borrill, Julian, additional, Brown, Michael L., additional, Bruno, Sarah Marie, additional, Bryan, Sean, additional, Calabrese, Erminia, additional, Calafut, Victoria, additional, Calisse, Paolo, additional, Carron, Julien, additional, Challinor, Anthony, additional, Chesmore, Grace, additional, Chinone, Yuji, additional, Chluba, Jens, additional, Cho, Hsiao-Mei Sherry, additional, Choi, Steve, additional, Coppi, Gabriele, additional, Cothard, Nicholas F., additional, Coughlin, Kevin, additional, Crichton, Devin, additional, Crowley, Kevin D., additional, Crowley, Kevin T., additional, Cukierman, Ari, additional, D'Ewart, John M., additional, Dünner, Rolando, additional, de Haan, Tijmen, additional, Devlin, Mark, additional, Dicker, Simon, additional, Didier, Joy, additional, Dobbs, Matt, additional, Dober, Bradley, additional, Duell, Cody J., additional, Duff, Shannon, additional, Duivenvoorden, Adri, additional, Dunkley, Jo, additional, Dusatko, John, additional, Errard, Josquin, additional, Fabbian, Giulio, additional, Feeney, Stephen, additional, Ferraro, Simone, additional, Fluxà, Pedro, additional, Freese, Katherine, additional, Frisch, Josef C., additional, Frolov, Andrei, additional, Fuller, George, additional, Fuzia, Brittany, additional, Galitzki, Nicholas, additional, Gallardo, Patricio A., additional, Ghersi, Jose Tomas Galvez, additional, Gao, Jiansong, additional, Gawiser, Eric, additional, Gerbino, Martina, additional, Gluscevic, Vera, additional, Goeckner-Wald, Neil, additional, Golec, Joseph, additional, Gordon, Sam, additional, Gralla, Megan, additional, Green, Daniel, additional, Grigorian, Arpi, additional, Groh, John, additional, Groppi, Chris, additional, Guan, Yilun, additional, Gudmundsson, Jon E., additional, Han, Dongwon, additional, Hargrave, Peter, additional, Hasegawa, Masaya, additional, Hasselfield, Matthew, additional, Hattori, Makoto, additional, Haynes, Victor, additional, Hazumi, Masashi, additional, He, Yizhou, additional, Healy, Erin, additional, Henderson, Shawn W., additional, Hervias-Caimapo, Carlos, additional, Hill, Charles A., additional, Hill, J. Colin, additional, Hilton, Gene, additional, Hilton, Matt, additional, Hincks, Adam D., additional, Hinshaw, Gary, additional, Hložek, Renée, additional, Ho, Shirley, additional, Ho, Shuay-Pwu Patty, additional, Howe, Logan, additional, Huang, Zhiqi, additional, Hubmayr, Johannes, additional, Huffenberger, Kevin, additional, Hughes, John P., additional, Ijjas, Anna, additional, Ikape, Margaret, additional, Irwin, Kent, additional, Jaffe, Andrew H., additional, Jain, Bhuvnesh, additional, Jeong, Oliver, additional, Kaneko, Daisuke, additional, Karpel, Ethan D., additional, Katayama, Nobuhiko, additional, Keating, Brian, additional, Kernasovskiy, Sarah S., additional, Keskitalo, Reijo, additional, Kisner, Theodore, additional, Kiuchi, Kenji, additional, Klein, Jeff, additional, Knowles, Kenda, additional, Koopman, Brian, additional, Kosowsky, Arthur, additional, Krachmalnicoff, Nicoletta, additional, Kuenstner, Stephen E., additional, Kuo, Chao-Lin, additional, Kusaka, Akito, additional, Lashner, Jacob, additional, Lee, Adrian, additional, Lee, Eunseong, additional, Leon, David, additional, Leung, Jason S.-Y., additional, Lewis, Antony, additional, Li, Yaqiong, additional, Li, Zack, additional, Limon, Michele, additional, Linder, Eric, additional, Lopez-Caraballo, Carlos, additional, Louis, Thibaut, additional, Lowry, Lindsay, additional, Lungu, Marius, additional, Madhavacheril, Mathew, additional, Mak, Daisy, additional, Maldonado, Felipe, additional, Mani, Hamdi, additional, Mates, Ben, additional, Matsuda, Frederick, additional, Maurin, Loïc, additional, Mauskopf, Phil, additional, May, Andrew, additional, McCallum, Nialh, additional, McKenney, Chris, additional, McMahon, Jeff, additional, Meerburg, P. Daniel, additional, Meyers, Joel, additional, Miller, Amber, additional, Mirmelstein, Mark, additional, Moodley, Kavilan, additional, Munchmeyer, Moritz, additional, Munson, Charles, additional, Naess, Sigurd, additional, Nati, Federico, additional, Navaroli, Martin, additional, Newburgh, Laura, additional, Nguyen, Ho Nam, additional, Niemack, Michael, additional, Nishino, Haruki, additional, Orlowski-Scherer, John, additional, Page, Lyman, additional, Partridge, Bruce, additional, Peloton, Julien, additional, Perrotta, Francesca, additional, Piccirillo, Lucio, additional, Pisano, Giampaolo, additional, Poletti, Davide, additional, Puddu, Roberto, additional, Puglisi, Giuseppe, additional, Raum, Chris, additional, Reichardt, Christian L., additional, Remazeilles, Mathieu, additional, Rephaeli, Yoel, additional, Riechers, Dominik, additional, Rojas, Felipe, additional, Roy, Anirban, additional, Sadeh, Sharon, additional, Sakurai, Yuki, additional, Salatino, Maria, additional, Rao, Mayuri Sathyanarayana, additional, Schaan, Emmanuel, additional, Schmittfull, Marcel, additional, Sehgal, Neelima, additional, Seibert, Joseph, additional, Seljak, Uros, additional, Sherwin, Blake, additional, Shimon, Meir, additional, Sierra, Carlos, additional, Sievers, Jonathan, additional, Sikhosana, Precious, additional, Silva-Feaver, Maximiliano, additional, Simon, Sara M., additional, Sinclair, Adrian, additional, Siritanasak, Praween, additional, Smith, Kendrick, additional, Smith, Stephen R., additional, Spergel, David, additional, Staggs, Suzanne T., additional, Stein, George, additional, Stevens, Jason R., additional, Stompor, Radek, additional, Suzuki, Aritoki, additional, Tajima, Osamu, additional, Takakura, Satoru, additional, Teply, Grant, additional, Thomas, Daniel B., additional, Thorne, Ben, additional, Thornton, Robert, additional, Trac, Hy, additional, Tsai, Calvin, additional, Tucker, Carole, additional, Ullom, Joel, additional, Vagnozzi, Sunny, additional, Engelen, Alexander van, additional, Lanen, Jeff Van, additional, Winkle, Daniel D. Van, additional, Vavagiakis, Eve M., additional, Vergès, Clara, additional, Vissers, Michael, additional, Wagoner, Kasey, additional, Walker, Samantha, additional, Ward, Jon, additional, Westbrook, Ben, additional, Whitehorn, Nathan, additional, Williams, Jason, additional, Williams, Joel, additional, Wollack, Edward J., additional, Xu, Zhilei, additional, Yu, Byeonghee, additional, Yu, Cyndia, additional, Zago, Fernando, additional, Zhang, Hezi, additional, and Zhu, Ningfeng, additional
Published: 2019
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39. Cryogenic 1.2 to 116 GHz receiver for large arrays

Author: Weinreb, Sander, Mani, Hamdi, Zhong, Weiye, Flygare, Jonas, Billade, Bushan, Akgiray, Ahmed, Dong, Li, Weinreb, Sander, Mani, Hamdi, Zhong, Weiye, Flygare, Jonas, Billade, Bushan, Akgiray, Ahmed, and Dong, Li
Abstract: Current and future large arrays for radio astronomy are compared and the Next Generation Very Large Array, ngVLA, is introduced. Receiver requirements are described and a 4-feed system covering 1.2 to 116 GHz, in a single vacuum cryogenic enclosure is presented followed by description of the reflector optics, the wide-band feeds, and the expected system performance.
Published: 2018

40. Operation of a Superconducting Nanowire in Two Detection Modes: KID and SPD

Author: Schroeder, Edward, primary, Mauskopf, Philip, additional, Mani, Hamdi, additional, Bryan, Sean, additional, Berggren, Karl K., additional, and Zhu, Di, additional
Published: 2018
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41. IF system design for the Galactic/Extragalactic ULDB Spectroscopic Terahertz Observatory (GUSTO)

Author: Neric, Marko, primary, Groppi, Christopher E., primary, Mani, Hamdi, primary, Mathewson, Justin, primary, Davis, Kristina, primary, Underhill, Matthew, primary, Kulesa, Craig, primary, Walker, Christopher, primary, Mozdzen, Thomas, primary, and Young, Abram, primary
Published: 2018
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42. The TolTEC project: a millimeter wavelength imaging polarimeter (Conference Presentation)

Author: Wilson, Grant W., primary, Ade, Peter A. R., additional, Aretxaga, Itziar, additional, Austermann, Jason E., additional, Bardin, Joseph, additional, Barry, Peter S., additional, Beall, James, additional, Berthoud, Marc, additional, Braeley, Alan, additional, Bryan, Sean A., additional, Burkott, Alexandra, additional, Bussan, John, additional, Castillo-Domínguez, Edgar, additional, Chavez, Miguel, additional, DeNigris, Natalie, additional, Doyle, Simon M., additional, Eiben, Miranda, additional, Ferrusca, Daniel, additional, Fissel, Laura M., additional, Gao, Jiansong, additional, Gear, Walter, additional, Gómez, Victor, additional, Gordon, Samuel, additional, Groppi, Christopher E., additional, Gutermuth, Robert, additional, Heyer, Mark, additional, Kuczarski, Stephen, additional, Hosseini, Mohsen, additional, Offner, Stella, additional, Pope, Alexandra, additional, Schloerb, F. Peter, additional, Souccar, Kamal, additional, Tang, Yuping, additional, Wallace, Gary, additional, Yun, Min S., additional, Mauskopf, Phillip, additional, Kelso, Rhys, additional, Knapp, Jacob, additional, Lunde, Emily, additional, Mani, Hamdi, additional, Mathewson, Justin, additional, Scannapieco, Evan, additional, Underhill, Matthew, additional, Hubmayr, Johannes, additional, Vissers, Michael, additional, Hughes, David H., additional, Rodriguez Montoya, Ivan, additional, Sanchez, David, additional, Velazquez, Miguel, additional, Ventura, Salvador, additional, Pascale, Enzo, additional, Rowe, Sam, additional, Tucker, Carole, additional, Novak, Giles, additional, McMahon, Jeffrey J., additional, and Simon, Sara M., additional
Published: 2018
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43. Preflight characterization of the BLAST-TNG receiver and detector arrays

Author: Lourie, Nathan P., primary, Galitzki, Nicholas, primary, Ade, Peter A. R., primary, Angile, Francisco E., primary, Ashton, Peter C., primary, Austermann, Jason E., primary, Devlin, Mark, primary, Dober, Bradley, primary, Gao, Jiansong, primary, Gordon, Samuel, primary, Groppi, Christopher E., primary, Hilton, Gene C., primary, Hubmayr, Johannes, primary, Klein, Jeffrey, primary, Li, Dale, primary, Lowe, Ian, primary, Mani, Hamdi, primary, Mauskopf, Philip, primary, McKenney, Christopher M., primary, Nati, Federico, primary, Novak, Giles, primary, Pascale, Enzo, primary, Pisano, Giampaolo, primary, Sinclair, Adrian, primary, Soler, Juan D., primary, Tucker, Carole, primary, Vissers, Michael, primary, Williams, Paul, primary, and Ullom, Joel N., primary
Published: 2018
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44. On the measurement of intensity correlations from laboratory and astronomical sources with SPADs and SNSPDs

Author: Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Smith, Nathan B., Berggren, Karl K, Zhu, Di, Schroeder, Edward, Mauskopf, Philip, Pilyavsky, Genady, Sinclair, Adrian, Bryan, Sean, Mani, Hamdi, Morozov, Dmitry, Smirnov, Konstantin, Vakhtomin, Yuriy, Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Smith, Nathan B., Berggren, Karl K, Zhu, Di, Schroeder, Edward, Mauskopf, Philip, Pilyavsky, Genady, Sinclair, Adrian, Bryan, Sean, Mani, Hamdi, Morozov, Dmitry, Smirnov, Konstantin, and Vakhtomin, Yuriy
Abstract: We describe the performance of detector modules containing silicon single photon avalanche photodiodes (SPADs) and superconducting nanowire single photon detectors (SNSPDs) to be used for intensity interferometry. The SPADs are mounted in fiber-coupled and free-space coupled packages. The SNSPDs are mounted in a small liquid helium cryostat coupled to single mode fiber optic cables which pass through a hermetic feed-through. The detectors are read out with microwave amplifiers and FPGA-based coincidence electronics. We present progress on measurements of intensity correlations from incoherent sources including gas-discharge lamps and stars with these detectors. From the measured laboratory performance of the correlation system, we estimate the sensitivity to intensity correlations from stars using commercial telescopes and larger existing research telescopes. © (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Published: 2017

45. SPIE Proceedings: IF System Design for the Galactic/Extragalactic ULDB Spectroscopic Terahertz Observatory (GUSTO).

Author: Neric, Marko, Groppi, Christopher, Mani, Hamdi, Mathewson, Justin, Davis, Kristina, Underhill, Matthew, Mozdzen, Thomas, Kulesa, Craig, Young, Abram, and Walker, Christopher
Published: 2018
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46. Results of using permanent magnets to suppress Josephson noise in the KAPPa SIS receiver

Author: Holland, Wayne S., Zmuidzinas, Jonas, Wheeler, Caleb H., Neric, Marko, Groppi, Christopher E., Underhill, Matthew, Mani, Hamdi, Weinreb, Sander, Russell, Damon S., Kooi, Jacob W., Lichtenberger, Arthur W., Walker, Christopher K., Kulesa, Craig, Holland, Wayne S., Zmuidzinas, Jonas, Wheeler, Caleb H., Neric, Marko, Groppi, Christopher E., Underhill, Matthew, Mani, Hamdi, Weinreb, Sander, Russell, Damon S., Kooi, Jacob W., Lichtenberger, Arthur W., Walker, Christopher K., and Kulesa, Craig
Abstract: We present the results from the magnetic field generation within the Kilopixel Array Pathfinder Project (KAPPa) instrument. The KAPPa instrument is a terahertz heterodyne receiver using a Superconducting-Insulating- Superconducting (SIS) mixers. To improve performance, SIS mixers require a magnetic field to suppress Josephson noise. The KAPPa test receiver can house a tunable electromagnet used to optimize the applied magnetic field. The receiver is also capable of accommodating a permanent magnet that applies a fixed field. Our permanent magnet design uses off-the-shelf neodymium permanent magnets and then reshapes the magnetic field using machined steel concentrators. These concentrators allow the use of an unmachined permanent magnet in the back of the detector block while two small posts provide the required magnetic field across the SIS junction in the detector cavity. The KAPPa test receiver is uniquely suited to compare the permanent magnet and electromagnet receiver performance. The current work includes our design of a ‘U’ shaped permanent magnet, the testing and calibration procedure for the permanent magnet, and the overall results of the performance comparison between the electromagnet and the permanent magnet counterpart.
Published: 2016

47. On the measurement of intensity correlations from laboratory and astronomical sources with SPADs and SNSPDs

Author: Schroeder, Edward, additional, Mauskopf, Philip, additional, Pilyavsky, Genady, additional, Sinclair, Adrian, additional, Smith, Nathan, additional, Bryan, Sean, additional, Mani, Hamdi, additional, Morozov, Dmitry, additional, Berggren, Karl, additional, Zhu, Di, additional, Smirnov, Konstantin, additional, and Vakhtomin, Yuriy, additional
Published: 2016
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48. Results of using permanent magnets to suppress Josephson noise in the KAPPa SIS receiver

Author: Wheeler, Caleb H., additional, Neric, Marko, additional, Groppi, Christopher E., additional, Underhill, Matthew, additional, Mani, Hamdi, additional, Weinreb, Sander, additional, Russell, Damon S., additional, Kooi, Jacob W., additional, Lichtenberger, Arthur W., additional, Walker, Christopher K., additional, and Kulesa, Craig, additional
Published: 2016
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49. Instrumental performance and results from testing of the BLAST-TNG receiver, submillimeter optics, and MKID detector arrays

Author: Galitzki, Nicholas, additional, Ade, Peter, additional, Angilè, Francesco E., additional, Ashton, Peter, additional, Austermann, Jason, additional, Billings, Tashalee, additional, Che, George, additional, Cho, Hsiao-Mei, additional, Davis, Kristina, additional, Devlin, Mark, additional, Dicker, Simon, additional, Dober, Bradley J., additional, Fissel, Laura M., additional, Fukui, Yasuo, additional, Gao, Jiansong, additional, Gordon, Samuel, additional, Groppi, Christopher E., additional, Hillbrand, Seth, additional, Hilton, Gene C., additional, Hubmayr, Johannes, additional, Irwin, Kent D., additional, Klein, Jeffrey, additional, Li, Dale, additional, Li, Zhi-Yun, additional, Lourie, Nathan P., additional, Lowe, Ian, additional, Mani, Hamdi, additional, Martin, Peter G., additional, Mauskopf, Philip, additional, McKenney, Christopher, additional, Nati, Federico, additional, Novak, Giles, additional, Pascale, Enzo, additional, Pisano, Giampaolo, additional, Santos, Fabio P., additional, Scott, Douglas, additional, Sinclair, Adrian, additional, Soler, Juan D., additional, Tucker, Carole, additional, Underhill, Matthew, additional, Vissers, Michael, additional, and Williams, Paul, additional
Published: 2016
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50. 10 Meter sub-orbital large balloon reflector (LBR)

Author: Lesser, David, primary, Walker, Christopher K., additional, Smith, I. Steve, additional, Goldsmith, Paul F., additional, Cortes, German, additional, Dougherty, Stefan, additional, Swift, Brandon, additional, Kloosterman, Jenna, additional, Honniball, Casey, additional, Young, Abram, additional, Peters, William, additional, Kulesa, Craig, additional, Perry, William, additional, Noll, James, additional, Bernasconi, Pietro, additional, Groppi, Christopher, additional, Mani, Hamdi, additional, and Duffy, Brian, additional
Published: 2015
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