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.
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Notes
For historical reasons, SO calls the highest detector frequency band the “ultra-high" frequency to distinguish it from Atacama Cosmology Telescope (ACT) high-frequency (HF) arrays.
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Acknowledgements
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.
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Healy, E., Dutcher, D., Atkins, Z. et al. The Simons Observatory 220 and 280 GHz Focal-Plane Module: Design and Initial Characterization. J Low Temp Phys 209, 815–823 (2022). https://doi.org/10.1007/s10909-022-02788-8
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DOI: https://doi.org/10.1007/s10909-022-02788-8