Details

Autor(en) / Beteiligte

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

Titel

Small Aperture Telescopes for the Simons Observatory

Ist Teil von

• Journal of low temperature physics, 2020, Vol.200 (5-6), p.461-471

Ort / Verlag

Goddard Space Flight Center: Springer

Erscheinungsjahr

2020

Quelle

Alma/SFX Local Collection

Beschreibungen/Notizen

• 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.