The Simons Observatory Microwave SQUID Multiplexing Detector Module Design

被引：41

作者：

McCarrick, Heather ^{[1
]}

Healy, Erin ^{[1
]}

Ahmed, Zeeshan ^{[2
,3
]}

Arnold, Kam ^{[4
]}

Atkins, Zachary ^{[1
]}

Austermann, Jason E. ^{[5
]}

Bhandarkar, Tanay ^{[6
]}

Beall, James A. ^{[5
]}

Bruno, Sarah Marie ^{[1
]}

Choi, Steve K. ^{[7
,8
]}

Connors, Jake ^{[5
]}

Cothard, Nicholas F. ^{[9
]}

Crowley, Kevin D. ^{[1
]}

Dicker, Simon ^{[6
]}

Dober, Bradley ^{[5
,10
]}

Duell, Cody J. ^{[7
]}

Duff, Shannon M. ^{[5
]}

Dutcher, Daniel ^{[1
]}

Frisch, Josef C. ^{[3
]}

Galitzki, Nicholas ^{[4
]}

Gralla, Megan B. ^{[11
]}

Gudmundsson, Jon E. ^{[12
]}

Henderson, Shawn W. ^{[2
,3
]}

Hilton, Gene C. ^{[5
]}

Ho, Shuay-Pwu Patty ^{[13
]}

Huber, Zachary B. ^{[7
]}

Hubmayr, Johannes ^{[5
]}

Iuliano, Jeffrey ^{[6
]}

Johnson, Bradley R. ^{[14
]}

Kofman, Anna M. ^{[6
]}

Kusaka, Akito ^{[15
,16
,17
,18
]}

Lashner, Jack ^{[19
]}

Lee, Adrian T. ^{[15
,20
,21
]}

Li, Yaqiong ^{[7
,22
]}

Link, Michael J. ^{[5
]}

Lucas, Tammy J. ^{[5
]}

Lungu, Marius ^{[1
]}

Mates, J. A. B. ^{[5
]}

McMahon, Jeffrey J. ^{[23
,24
]}

Niemack, Michael D. ^{[7
,8
,22
]}

Orlowski-Scherer, John ^{[4
]}

Seibert, Joseph ^{[4
]}

Silva-Feaver, Maximiliano ^{[4
]}

Simon, Sara M. ^{[25
]}

Staggs, Suzanne ^{[1
]}

Suzuki, Aritoki ^{[15
]}

Terasaki, Tomoki ^{[16
]}

Ullom, Joel N. ^{[5
]}

Vavagiakis, Eve M. ^{[7
]}

Vale, Leila R. ^{[5
]}

机构：

[1] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA

[2] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA

[3] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[4] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA

[5] NIST, Boulder, CO 80305 USA

[6] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[7] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA

[8] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA

[9] Cornell Univ, Dept Appl & Engn Phys, Ithaca, NY 14853 USA

[10] Univ Colorado, Dept Phys, Boulder, CO 80309 USA

[11] Univ Arizona, Dept Astron, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA

[12] Stockholm Univ, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden

[13] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[14] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA

[15] Lawrence Berkeley Natl Lab, Phys Div, Berkeley, CA 94720 USA

[16] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan

[17] Univ Calif Berkeley, Kavli Inst Phys & Math Universe WPI, Berkeley Satellite, Berkeley, CA 94720 USA

[18] Univ Tokyo, Res Ctr Early Universe, Sch Sci, Tokyo 1130033, Japan

[19] Univ Southern Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA

[20] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[21] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA

[22] Cornell Univ, Kavli Inst Cornell Nanoscale Sci, Ithaca, NY 14853 USA

[23] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA

[24] Univ Chicago, USA Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA

[25] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[26] NASA, Goddard Space Flight Ctr, Code 916, Greenbelt, MD 20771 USA

[27] MIT, MIT Kavli Inst, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[28] Univ Penn, Dept Phys, W Chester, PA 19383 USA

来源：

ASTROPHYSICAL JOURNAL | 2021年 / 922卷 / 01期

关键词：

FOCAL-PLANE; ARRAYS; NOISE;

D O I：

10.3847/1538-4357/ac2232

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Advances in cosmic microwave background (CMB) science depend on increasing the number of sensitive detectors observing the sky. New instruments deploy large arrays of superconducting transition-edge sensor (TES) bolometers tiled densely into ever larger focal planes. High multiplexing factors reduce the thermal loading on the cryogenic receivers and simplify their design. We present the design of focal-plane modules with an order of magnitude higher multiplexing factor than has previously been achieved with TES bolometers. We focus on the novel cold readout component, which employs microwave SQUID multiplexing (mu mux). Simons Observatory will use 49 modules containing 70,000 bolometers to make exquisitely sensitive measurements of the CMB. We validate the focal-plane module design, presenting measurements of the readout component with and without a prototype detector array of 1728 polarization-sensitive bolometers coupled to feedhorns. The readout component achieves a 95% yield and a 910 multiplexing factor. The median white noise of each readout channel is 65 pA root Hz. This impacts the projected SO mapping speed by <8%, which is less than is assumed in the sensitivity projections. The results validate the full functionality of the module. We discuss the measured performance in the context of SO science requirements, which are exceeded.

引用

页数：10

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