The Simons Observatory 220 and 280 GHz Focal-Plane Module: Design and Initial Characterization
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10909_2022_2788_ReferencePDF.pdf
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7.76 MB
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Author(s)
Healy, Erin
Dutcher, Daniel
Atkins, Zachary
Austermann, Jason
Choi, Steve K.
Duell, Cody J.
Duff, Shannon
Galitzki, Nicholas
Huber, Zachary B.
Hubmayr, Johannes
Date Issued
July 21, 2022
Publisher
Springer US
Citation
Healy, Erin, Dutcher, Daniel, Atkins, Zachary, Austermann, Jason, Choi, Steve K. et al. 2022. "The Simons Observatory 220 and 280 GHz Focal-Plane Module: Design and Initial Characterization."
Version
Author's final manuscript
Abstract
Abstract
The Simons Observatory (SO) will detect and map the temperature and polarization of the millimeter-wavelength sky from Cerro Toco, Chile, across a range of angular scales, providing rich data sets for cosmological and astrophysical analysis. The SO focal planes will be tiled with compact hexagonal packages, called universal focal-plane modules (UFMs), in which the transition-edge sensor (TES) detectors are coupled to 100 mK microwave-multiplexing electronics. Three different types of dichroic TES detector arrays with bands centered at 30/40, 90/150, and 220/280 GHz will be implemented across the 49 planned UFMs. The 90/150 GHz and 220/280 GHz arrays each contain 1764 TESes, which are read out with two 910x multiplexer circuits. The modules contain a series of routed silicon chips, which are packaged together in a controlled electromagnetic environment and operated at 100 mK. Following an overview of the module design, we report on early results from the first 220/280 GHz UFM, including detector yield, as well as readout and detector noise levels.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
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DOI of Published Version
https://doi.org/10.1007/s10909-022-02788-8
