The Simons Observatory microwave SQUID multiplexing detector module design

McCarrick, Heather; Healy, Erin; Ahmed, Zeeshan; Arnold, Kam; Atkins, Zachary; Austermann, Jason E.; Bhandarkar, Tanay; Beall, Jim A.; Bruno, Sarah Marie; Choi, Steve K.; Connors, Jake; Cothard, Nicholas F.; Crowley, Kevin D.; Dicker, Simon; Dober, Bradley; Duell, Cody J.; Duff, Shannon M.; Dutcher, Daniel; Frisch, Josef C.; Galitzki, Nicholas; Gralla, Megan B.; Gudmundsson, Jon E.; Henderson, Shawn W.; Hilton, Gene C.; Ho, Shuay-Pwu Patty; Huber, Zachary B.; Hubmayr, Johannes; Iuliano, Jeffrey; Johnson, Bradley R.; Kofman, Anna M.; Kusaka, Akito; Lashner, Jack; Lee, Adrian T.; Li, Yaqiong; Link, Michael J.; Lucas, Tammy J.; Lungu, Marius; Mates, J. A. B.; McMahon, Jeffrey J.; Niemack, Michael D.; Orlowski-Scherer, John; Seibert, Joseph; Silva-Feaver, Maximiliano; Simon, Sara M.; Staggs, Suzanne; Suzuki, Aritoki; Terasaki, Tomoki; Ullom, Joel N.; Vavagiakis, Eve M.; Vale, Leila R.; Van Lanen, Jeff; Vissers, Michael R.; Wang, Yuhan; Wollack, Edward J.; Xu, Zhilei; Young, Edward; Yu, Cyndia; Zheng, Kaiwen; Zhu, Ningfeng

doi:10.48550/arxiv.2106.14797

Cited by 2 publications

(3 citation statements)

References 26 publications

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“…The expected noise from TES in superconducting stage and normal stage comes from the readout noise and Johnson noise as described in [Ref. 3 ]. With a higher Johnson noise, the TES noise in the superconducting stage will be higher than the noise in normal stage (when biased at high voltage) and is confirmed by results shown in Figure 3.…”

Section: Resultsmentioning

confidence: 99%

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Simons Observatory Focal-Plane Module: In-lab Testing and Characterization Program

Wang¹,

Zheng²,

Atkins³

et al. 2021

Preprint

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The Simons Observatory (SO) is a ground-based cosmic microwave background instrument to be sited in the Atacama Desert in Chile. SO will deploy 60,000 transitionedge sensor bolometers in 49 separate focal-plane modules across a suite of four telescopes covering three dichroic bands termed low frequency (LF), mid frequency (MF) and ultrahigh frequency (UHF). Each MF and UHF focal-plane module packages 1720 optical detectors and corresponding 100 mK microwave SQUID multiplexing readout components. In this paper we describe the testing program we have developed for high-throughput validation of the modules after they are assembled. The validation requires measurements of the yield, saturation powers, time constants, noise properties and optical efficiencies. Additional measurements will be performed for further characterizations as needed. We describe the methods developed and demonstrate preliminary results from initial testing of prototype modules.

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Section: Resultsmentioning

confidence: 99%

“…Each MF and UHF focal-plane module packages 1728 optical detectors and 36 dark bolometers. Further details of SO focal plane model can be found in McCarrick, et al (2021) 3 .…”

Section: Introductionmentioning

confidence: 99%

Simons Observatory Focal-Plane Module: In-lab Testing and Characterization Program

Wang¹,

Zheng²,

Atkins³

et al. 2021

Preprint

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“…Simons Observatory is packaging all of the cold readout technology into a common universal microwave-multiplexing module (UMM) that can be used with all detector arrays regardless of frequency across all of the SO telescopes [5]. Each UMM is composed of µmux chips containing the resonator-coupled SQUIDs, a silicon wafer that both connects the µmux chips in series and contains the TES bias circuitry, and an enclosing copper frame.…”

Section: Introductionmentioning

confidence: 99%

The Simons Observatory: Magnetic Shielding Measurements for the Universal Multiplexing Module

Huber,

Li,

Vavagiakis

et al. 2021

Preprint

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The Simons Observatory (SO) includes four telescopes that will measure the temperature and polarization of the cosmic microwave background using over 60,000 highly sensitive transition-edge bolometers (TES). These multichroic TES bolometers are read out by a microwave RF SQUID multiplexing system with a multiplexing factor of 910. Given that both TESes and SQUIDs are susceptible to magnetic field pickup and that it is hard to predict how they will respond to such fields, it is important to characterize the magnetic response of these systems empirically. This information can then be used to limit spurious signals by informing magnetic shielding designs for the detectors and readout. This paper focuses on measurements of magnetic pickup with different magnetic shielding configurations for the SO universal multiplexing module (UMM), which contains the SQUIDs, associated resonators, and TES bias circuit. The magnetic pickup of a prototype UMM was tested under three shielding configurations: no shielding (copper packaging), aluminum packaging for the UMM, and a tin/lead-plated shield surrounding the entire dilution refrigerator 100 mK cold stage. The measurements show that the aluminum packaging outperforms the copper packaging by a shielding factor of 8-10, and adding the tin/lead-plated 1K shield further increases the relative shielding factor in the aluminum configuration by 1-2 orders of magnitude.

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The Simons Observatory microwave SQUID multiplexing detector module design

Cited by 2 publications

References 26 publications

Simons Observatory Focal-Plane Module: In-lab Testing and Characterization Program

Simons Observatory Focal-Plane Module: In-lab Testing and Characterization Program

The Simons Observatory: Magnetic Shielding Measurements for the Universal Multiplexing Module

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