TY - JOUR
T1 - The Simons Observatory 220 and 280 GHz Focal-Plane Module
T2 - Design and Initial Characterization
AU - Healy, Erin
AU - Dutcher, Daniel
AU - Atkins, Zachary
AU - Austermann, Jason
AU - Choi, Steve K.
AU - Duell, Cody J.
AU - Duff, Shannon
AU - Galitzki, Nicholas
AU - Huber, Zachary B.
AU - Hubmayr, Johannes
AU - Johnson, Bradley R.
AU - McCarrick, Heather
AU - Niemack, Michael D.
AU - Sonka, Rita
AU - Staggs, Suzanne T.
AU - Vavagiakis, Eve
AU - Wang, Yuhan
AU - Xu, Zhilei
AU - Zheng, Kaiwen
N1 - Funding Information:
This work was supported in part by a grant from the Simons Foundation (Award #457687, B.K.). ZBH acknowledges support from the NASA Space Technology Graduate Research Opportunities Award. SKC acknowledges support from NSF award AST-2001866. Zhilei Xu is supported by the Gordon and Betty Moore Foundation through grant GBMF5215 to the Massachusetts Institute of Technology.
Publisher Copyright:
© 2022, The Author(s), under exclusive licence to Springer Science+Business Media, LLC, part of Springer Nature.
PY - 2022/12
Y1 - 2022/12
N2 - 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.
AB - 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.
KW - Cosmic microwave background
KW - Microwave SQUID multiplexing
KW - Transition-edge sensor detectors
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U2 - 10.1007/s10909-022-02788-8
DO - 10.1007/s10909-022-02788-8
M3 - Article
AN - SCOPUS:85134628209
SN - 0022-2291
VL - 209
SP - 815
EP - 823
JO - Journal of Low Temperature Physics
JF - Journal of Low Temperature Physics
IS - 5-6
ER -