Search

Your search keyword '"Aashrita Mangu"' showing total 12 results
Start Over Author "Aashrita Mangu"
12 results on '"Aashrita Mangu"'

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

Author

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

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

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

Published
2024
Full Text
View/download PDF

2. Small Aperture Telescopes for the Simons Observatory

Author

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

Subjects
Instrumentation And Photography
Abstract

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

Published
2020
Full Text
View/download PDF

3. Assembly and Integration Process of the High-Density Detector Array Readout Modules for the Simons Observatory

Author

Yaqlong Li, Kam Arnold, Zachary Atkins, Sarah Marie Bruno, Nicholas F. Cothard, Bradley Dober, Cody J. Duell, Shannon M. Duff, Patricio A. Gallardo, Erin Healy, Shuay‑Pwu Patty Ho, Johannes Hubmayr, Brian Keating, Adrian T Lee, Aashrita Mangu, Heather McCarrick, Michael D. Niemack, Laura Newburgh, Christopher Raum, Maria Salatino, Trevor Sasse, Maximiliano Silva‑Feaver, Sara M. Simon, Suzanne Staggs, Aritoki Suzuki, Joel Ullom, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Benjamin Westbrook, Edward J Wollack, Zhilei Xu, Kaiwen Zheng, and Ningfeng Zhu

Subjects
Astronomy, Instrumentation And Photography
Abstract

The Simons Observatory will measure the cosmic microwave background tempera-ture and polarization using a suite of new telescopes in the Atacama Desert in Chile. The Simons Observatory will use dichroic transition edge sensor (TES) bolometer arrays spanning six frequency bands from 27 to 280 GHz. The Simons Observa-tory will pioneer the use of a densely packed multiplexing architecture based on the microwave SQUID multiplexer ( 𝜇mux), housing ∼2000 microwave resonators, each coupled to a TES. The Simons Observatory aims to multiplex each array of ∼2000 detectors with a single pair of coaxial cables and requires a multiplexing factor of ∼1000 . The Simons Observatory cryogenic readout system is called the universal microwave multiplexing module (UMM). The UMM couples to both horn and lenslet-coupled detector arrays and is integrated into the universal focal-plane module (UFM) after being independently characterized. We present processes we have developed for highly repeatable and automated integration methods of UMMs, which will be needed for the production of the 49 UFMs required for the first stage of the Simons Observatory.

Published
2020
Full Text
View/download PDF

4. Machine Learning in High Energy Physics Community White Paper.

Author

Kim Albertsson, Piero Altoe, Dustin Anderson, Michael Andrews, Juan Pedro Araque Espinosa, Adam Aurisano, Laurent Basara, Adrian Bevan, Wahid Bhimji, Daniele Bonacorsi, Paolo Calafiura, Mario Campanelli, Louis Capps, Federico Carminati, Stefano Carrazza, Taylor Childers, Elias Coniavitis, Kyle Cranmer, Claire David, Douglas Davis, Javier M. Duarte, Martin Erdmann, Jonas Eschle, Amir Farbin, Matthew Feickert, Nuno Filipe Castro, Conor Fitzpatrick, Michele Floris, Alessandra Forti, Jordi Garra-Tico, Jochen Gemmler, Maria Girone, Paul Glaysher, Sergei Gleyzer, Vladimir V. Gligorov, Tobias Golling, Jonas Graw, Lindsey Gray, Dick Greenwood, Thomas Hacker, John Harvey, Benedikt Hegner, Lukas Heinrich, Ben Hooberman, Johannes Junggeburth, Michael Kagan, Meghan Kane, Konstantin Kanishchev, Przemyslaw Karpinski, Zahari Kassabov, Gaurav Kaul, Dorian Kcira, Thomas Keck, Alexei Klimentov, Jim Kowalkowski, Luke Kreczko, Alexander Kurepin, Rob Kutschke, Valentin Kuznetsov, Nicolas Köhler, Igor Lakomov, Kevin Lannon, Mario Lassnig, Antonio Limosani, Gilles Louppe, Aashrita Mangu, Pere Mato, Narain Meenakshi, Helge Meinhard, Dario Menasce, Lorenzo Moneta, Seth Moortgat, Mark S. Neubauer, Harvey B. Newman, Hans Pabst, Michela Paganini, Manfred Paulini, Gabriel N. Perdue, Uzziel Perez, Attilio Picazio, Jim Pivarski, Harrison Prosper, Fernanda Psihas, Alexander Radovic, Ryan Reece, Aurelius Rinkevicius, Eduardo Rodrigues, Jamal Rorie, David Rousseau, Aaron Sauers, Steven Schramm, Ariel Schwartzman, Horst Severini, Paul Seyfert, Filip Siroky, Konstantin Skazytkin, Mike Sokoloff, Graeme Andrew Stewart, Bob Stienen, Ian Stockdale, Giles Chatham Strong, Savannah Thais, Karen Tomko, Eli Upfal, Emanuele Usai, Andrey Ustyuzhanin, Martin Vala, Sofia Vallecorsa, Mauro Verzetti, Xavier Vilasís-Cardona, Jean-Roch Vlimant, Ilija Vukotic, Sean-Jiun Wang, Gordon Watts, Michael Williams, Wenjing Wu, Stefan Wunsch, and Omar Zapata

Published
2018

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

Author

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

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

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

Published
2020
Full Text
View/download PDF

6. Assembly and Integration Process of the High-Density Detector Array Readout Modules for the Simons Observatory

Author

Zhilei Xu, Aritoki Suzuki, Maximiliano Silva-Feaver, Kaiwen Zheng, Maria Salatino, Laura Newburgh, Kam Arnold, Michael D. Niemack, Trevor Sasse, Shannon M. Duff, Sara M. Simon, Ningfeng Zhu, Christopher Raum, Nicholas F. Cothard, Heather McCarrick, Brian Keating, Shuay-Pwu Patty Ho, Erin Healy, Suzanne T. Staggs, B. Dober, Sarah Marie Bruno, Yuhan Wang, Aashrita Mangu, Zachary Atkins, Adrian T. Lee, Michael R. Vissers, Johannes Hubmayr, Yaqiong Li, Cody J. Duell, Eve M. Vavagiakis, Patricio A. Gallardo, Benjamin Westbrook, Joel N. Ullom, and Edward J. Wollack

Subjects
Physics, business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Dichroic glass, 01 natural sciences, Multiplexer, Multiplexing, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, law.invention, Optics, Observatory, law, 0103 physical sciences, General Materials Science, Transition edge sensor, 010306 general physics, business, Microwave
Abstract

The Simons Observatory will measure the cosmic microwave background temperature and polarization using a suite of new telescopes in the Atacama Desert in Chile. The Simons Observatory will use dichroic transition edge sensor (TES) bolometer arrays spanning six frequency bands from 27 to 280 GHz. The Simons Observatory will pioneer the use of a densely packed multiplexing architecture based on the microwave SQUID multiplexer ($$\mu $$mux), housing $$\sim \! 2000$$ microwave resonators, each coupled to a TES. The Simons Observatory aims to multiplex each array of $$\sim \! 2000$$ detectors with a single pair of coaxial cables and requires a multiplexing factor of $$\sim \! 1000$$. The Simons Observatory cryogenic readout system is called the universal microwave multiplexing module (UMM). The UMM couples to both horn and lenslet-coupled detector arrays and is integrated into the universal focal-plane module (UFM) after being independently characterized. We present processes we have developed for highly repeatable and automated integration methods of UMMs, which will be needed for the production of the 49 UFMs required for the first stage of the Simons Observatory.

Published
2020
Full Text
View/download PDF

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

Author

Peter A. R. Ade, Davide Poletti, C. Verges, Shunsuke Adachi, Kam Arnold, Yuji Chinone, A. Suzuki, Yuto Minami, Chang Feng, J. Peloton, Nathan Whitehorn, Oliver Jeong, N. W. Halverson, Yuki Inoue, T. Hamada, Akito Kusaka, Y. Zhou, A. Zahn, A. Cukierman, M. Aguilar, Carole Tucker, D. Beck, Nicoletta Krachmalnicoff, Rolando Dünner, Brian Keating, Paul L. Richards, Stephen M. Feeney, J. C. Groh, Julian Borrill, C. Tsai, Joshua Montgomery, Darcy Barron, Theodore Kisner, R. Stompor, G. Hall, D. Boettger, Tucker Elleflot, Josquin Errard, Frederick Matsuda, L. N. Lowry, D. Leon, Takayuki Tomaru, Reijo Keskitalo, Benjamin Westbrook, M. Navaroli, D. Kaneko, K. Cheung, Osamu Tajima, A. T. P. Pham, Eric V. Linder, Giulio Fabbian, A. J. Gilbert, L. Howe, Neil Goeckner-Wald, H. El-Bouhargani, Max Silva-Feaver, Hans P. Paar, M. A. Dobbs, S. Takatori, Federico Bianchini, Colin Ross, Christian L. Reichardt, John Groh, Praween Siritanasak, Julien Carron, Tomotake Matsumura, T. Fujino, Y. Akiba, H. Nishino, G. Jaehnig, Giuseppe Puglisi, Charles A. Hill, D. Tanabe, Andrew H. Jaffe, Masashi Hazumi, Nicholas Galitzki, Blake D. Sherwin, S. Kikuchi, Carlo Baccigalupi, E. M. Leitch, S. Beckman, N. Katayama, Grant Teply, A. Ducout, Aashrita Mangu, M. LeJeune, Adrian T. Lee, Nathan Stebor, Masaya Hasegawa, S. Takakura, Y. Segawa, Scott Chapman, Kevin T. Crowley, Chinone, Y, Adachi, S, Ade, P, Aguilar, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Elbouhargani, H, Carron, J, Chapman, S, Cheung, K, Crowley, K, Cukierman, A, Dunner, R, Dobbs, M, Ducout, A, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Lejeune, M, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leitch, E, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Matsumura, T, Minami, Y, Montgomery, J, Navaroli, M, Nishino, H, Paar, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Richards, P, Ross, C, Segawa, Y, Sherwin, B, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Tucker, C, Verges, C, Westbrook, B, Whitehorn, N, Zahn, A, Zhou, Y, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), POLARBEAR, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
History, satellite: Planck, Cosmic microwave background, gravitational lensing, cosmic background radiation: polarization, detector: noise, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravity waves, power spectrum, 01 natural sciences, Education, Primary mirror, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, Polarization, 0103 physical sciences, Planck, mirror, 010303 astronomy & astrophysics, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Gravitational wave, Settore FIS/05, POLARBEAR experiment, Gravitational effects, gravitational radiation: primordial, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Galaxy, Computer Science Applications, Gravitational lens, B-mode, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy
Abstract

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

Published
2020
Full Text
View/download PDF

8. Small Aperture Telescopes for the Simons Observatory

Author

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

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

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

Published
2020

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

Author

Julien Carron, M. A. Dobbs, C. Tsai, Dominic Beck, D. Leon, Ted Kisner, Aashrita Mangu, D. Boettger, Christian L. Reichardt, A. T. P. Pham, Kam Arnold, Akito Kusaka, Nicoletta Krachmalnicoff, T. Hamada, John Groh, S. Beckman, Josquin Errard, Ben Westbrook, Nathan Stebor, Neil Goeckner-Wald, Reijo Keskitalo, Daisuke Kaneko, Greg Jaehnig, Kevin T. Crowley, S. Takatori, Masaya Hasegawa, D. Tanabe, Tucker Elleflot, Giulio Fabbian, L. Howe, A. Cukierman, T. Fujino, Y. Zhou, S. Takakura, Eric V. Linder, Julian Borrill, N. Katayama, Yuki Inoue, Davide Poletti, Praween Siritanasak, Haruki Nishino, Yuto Minami, Yuji Chinone, Y. Segawa, H. El Bouhargani, Osamu Tajima, Aritoki Suzuki, N. W. Halverson, Darcy Barron, Masashi Hazumi, L. N. Lowry, G. Hall, Frederick Matsuda, Federico Bianchini, Scott Chapman, M. Navaroli, R. Stompor, Nicholas Galitzki, Clara Vergès, Maximiliano Silva-Feaver, Oliver Jeong, M. A. O. Aguilar Faúndez, Grant Teply, Brian Keating, Shunsuke Adachi, S. Kikuchi, K. Cheung, Adrian T. Lee, Giuseppe Puglisi, Charles A. Hill, Chang Feng, C. Baccigalupi, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), POLARBEAR, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Adachi, S, Aguilar Faundez, M, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feng, C, Fujino, T, Galitzki, N, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Kaneko, D, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

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

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

Published
2019
Full Text
View/download PDF

10. Deployment of Polarbear-2A

Author

Chang Feng, Radek Stompor, Takayuki Tomaru, Rolando Dünner, Josquin Errard, D. Tanabe, Praween Siritanasak, N. Stebor, Julien Carron, D. Leon, Davide Poletti, K. Cheung, C. Tsai, S. Takakura, Grant Teply, Yuto Minami, Yuki Inoue, Stephen M. Feeney, Yuji Chinone, Frederick Matsuda, D. Beck, Akito Kusaka, Y. Akiba, A. Suzuki, Nicoletta Krachmalnicoff, Adrian T. Lee, M. Aguilar Faúndez, J. Peloton, Colin Ross, Osamu Tajima, D. Boettger, B. Westbrook, A. T. P. Pham, M. Navaroli, N. W. Halverson, Y. Zhou, Federico Bianchini, A. Cukierman, Aashrita Mangu, Nobuhiko Katayama, T. Hamada, Tucker Elleflot, Y. Segawa, Masaya Hasegawa, G. Hall, Julian Borrill, Peter A. R. Ade, Eric V. Linder, Giulio Fabbian, H. Nishino, G. Jaehnig, Giuseppe Puglisi, Charles A. Hill, Shunsuke Adachi, S. Takatori, L. Howe, A. J. Gilbert, H. El-Bouhargani, Christian L. Reichardt, Kam Arnold, John Groh, Masashi Hazumi, Neil Goeckner-Wald, Nicholas Galitzki, S. Beckman, Brian Keating, M. A. Dobbs, Carlo Baccigalupi, Clara Vergès, Theodore Kisner, Reijo Keskitalo, Daisuke Kaneko, T. Fujino, S. Kikuchi, Darcy Barron, L. N. Lowry, Scott Chapman, Maximiliano Silva-Feaver, Oliver Jeong, Kevin T. Crowley, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Kaneko, D, Adachi, S, Ade, P, Aguilar Faundez, M, Akiba, Y, Arnold, K, Baccigalupi, C, Barron, D, Beck, D, Beckman, S, Bianchini, F, Boettger, D, Borrill, J, Carron, J, Chapman, S, Cheung, K, Chinone, Y, Crowley, K, Cukierman, A, Dobbs, M, Dunner, R, El-Bouhargani, H, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Fujino, T, Galitzki, N, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hamada, T, Hasegawa, M, Hazumi, M, Hill, C, Howe, L, Inoue, Y, Jaehnig, G, Jeong, O, Katayama, N, Keating, B, Keskitalo, R, Kikuchi, S, Kisner, T, Krachmalnicoff, N, Kusaka, A, Lee, A, Leon, D, Linder, E, Lowry, L, Mangu, A, Matsuda, F, Minami, Y, Navaroli, M, Nishino, H, Peloton, J, Pham, A, Poletti, D, Puglisi, G, Reichardt, C, Ross, C, Segawa, Y, Silva-Feaver, M, Siritanasak, P, Stebor, N, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Takatori, S, Tanabe, D, Teply, G, Tomaru, T, Tsai, C, Verges, C, Westbrook, B, Zhou, Y, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS]Physics [physics], Settore FIS/05, Gravitational wave, Cosmic microwave background, Millimeter wave, First light, CMB, Condensed Matter Physics, 7. Clean energy, 01 natural sciences, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, Microwave emission, Settore FIS/05 - Astronomia e Astrofisica, TES bolometer, Planet, Software deployment, 0103 physical sciences, Extremely high frequency, B-mode polarization, General Materials Science, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Remote sensing
Abstract

International audience; Polarbear-2A is the first of three receivers in the Simons array, a cosmic microwave background experiment located on the Atacama Plateau in Chile. Polarbear-2A was deployed and achieved the first light in January 2019 by mapping the microwave emission from planet observations. Commissioning work is underway to prepare the receiver for science observations.

Published
2019
Full Text
View/download PDF

11. Characterization of Transition Edge Sensors for the Simons Observatory

Author

Shannon M. Duff, Michael D. Niemack, Christopher Raum, Nicholas F. Cothard, Sara M. Simon, Gene C. Hilton, Jason E. Austermann, Steve K. Choi, Maria Salatino, Edward J. Wollack, Johannes Hubmayr, Zhilei Xu, Trevor Sasse, Mario Renzullo, Aashrita Mangu, Joel N. Ullom, Suzanne T. Staggs, Thuong D. Hoang, Eve M. Vavagiakis, Aamir Ali, John Vivalda, Benjamin Westbrook, Federico Nati, Shuay-Pwu Patty Ho, Adrian T. Lee, Bradley Dober, Cody J. Duell, Kam Arnold, Daniel Yohannes, Michael R. Vissers, Samantha Walker, Aritoki Suzuki, Jason R. Stevens, Patrick Truitt, Stevens, J, Cothard, N, Vavagiakis, E, Ali, A, Arnold, K, Austermann, J, Choi, S, Dober, B, Duell, C, Duff, S, Hilton, G, Ho, S, Hoang, T, Hubmayr, J, Lee, A, Mangu, A, Nati, F, Niemack, M, Raum, C, Renzullo, M, Salatino, M, Sasse, T, Simon, S, Staggs, S, Suzuki, A, Truitt, P, Ullom, J, Vivalda, J, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Xu, Z, and Yohannes, D

Subjects
Simons Observatory, Aperture, Physics::Instrumentation and Detectors, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Noise (electronics), 010305 fluids & plasmas, law.invention, Optics, Observatory, law, 0103 physical sciences, General Materials Science, Dilution refrigerator, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, SQUID, NIST, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business, TES
Abstract

The Simons Observatory is building both large (6 m) and small (0.5 m) aperture telescopes in the Atacama desert in Chile to observe the cosmic microwave background (CMB) radiation with unprecedented sensitivity. Simons Observatory telescopes in total will use over 60,000 transition edge sensor (TES) detectors spanning center frequencies between 27 and 285 GHz and operating near 100 mK. TES devices have been fabricated for the Simons Observatory by NIST, Berkeley, and HYPRES/SeeQC corporation. Iterations of these devices have been tested cryogenically in order to inform the fabrication of further devices, which will culminate in the final TES designs to be deployed in the field. The detailed design specifications have been independently iterated at each fabrication facility for particular detector frequencies. We present test results for prototype devices, with emphasis on NIST high frequency detectors. A dilution refrigerator was used to achieve the required temperatures. Measurements were made both with 4-lead resistance measurements and with a time domain Superconducting Quantum Interference Device (SQUID) multiplexer system. The SQUID readout measurements include analysis of current vs voltage (IV) curves at various temperatures, square wave bias step measurements, and detector noise measurements. Normal resistance, superconducting critical temperature, saturation power, thermal and natural time constants, and thermal properties of the devices are extracted from these measurements., Comment: 9 Pages, 5 figures, Low Temperature Detectors 19

Published
2019
Full Text
View/download PDF

12. Precision Timing Detectors with Cadmium Telluride Sensors

Author

Cristian Pena, Aashrita Mangu, Maria Spiropulu, Si Xie, A. Bornheim, Jiajing Mao, Zhicai Zhang, and Dustin Anderson

Subjects
Materials science, Large Hadron Collider, Luminosity (scattering theory), Calorimeter (particle physics), Physics::Instrumentation and Detectors, business.industry, Detector, Calorimetry, Particle detector, Cadmium telluride photovoltaics, Optics, Cathode ray, High Energy Physics::Experiment, business
Abstract

Precision timing properties of high energy physics detectors in high luminosity colliders has become an important requirement for the success of particle detection, of which new calorimeter with timing precision of few tens of ps is the main interest. In this paper, we presented the first calorimetry and timing performance measurement of Cadmium-Telluride (CdTe) as the active material of sampling calorimeter, using 2 GeV to 200 GeV electron beam from CERN beamlines. A good energy performance is achieved due to the better sensitivity of CdTe to X ray photons in the secondary shower than other semi-conducting sensors such as silicon. The timing resolution of the tested CdTe sensor is measured to be down to 21 ps under the best conditions.

Published
2017
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results