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arxiv: 2405.05550 · v2 · pith:CDMFEOPJnew · submitted 2024-05-09 · 🌌 astro-ph.IM · astro-ph.CO

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

Nicholas Galitzki , Tran Tsan , Jake Spisak , Michael Randall , Max Silva-Feaver , Joseph Seibert , Jacob Lashner , Shunsuke Adachi
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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 Simon Dicker 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 Kaiwen Zheng
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classification 🌌 astro-ph.IM astro-ph.CO
keywords satsaperturedesignintegrationobservatorysimonstelescopestesting
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The Simons Observatory (SO) is a cosmic microwave background (CMB) survey experiment that includes small-aperture telescopes (SATs) observing from an altitude of 5,200 m in the Atacama Desert in Chile. The SO SATs will cover six spectral bands between 27 and 280 GHz to search for primordial B-modes to a sensitivity of $\sigma(r)=0.002$, with quantified systematic errors well below this value. Each SAT is a self-contained cryogenic telescope with a 35$^\circ$ field of view, 42 cm diameter optical aperture, 40 K half-wave plate, 1 K refractive optics, and $<0.1$ K focal plane that holds $>12,000$ TES detectors. We describe the nominal design of the SATs and present details about the integration and testing for one operating at 93 and 145 GHz.

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