Transition-edge sensor: Difference between revisions

Revision as of 22:12, 23 October 2020

Revision as of 12:56, 30 October 2024

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==Applications==

TES arrays are becoming increasingly common in physics and astronomy experiments such as [[James Clerk Maxwell Telescope#SCUBA-2|SCUBA-2]], the HAWC+ instrument on the [[Stratospheric Observatory for Infrared Astronomy]], the [[Atacama Cosmology Telescope]], the [[Cryogenic Dark Matter Search]], the [[Cryogenic Observatory for Signatures Seen in Next-Generation Underground Searches]], the [[Cryogenic Rare Event Search with Superconducting Thermometers]], [[the E and B Experiment]], the [[South Pole Telescope]], the [[Spider (polarimeter)|Spider polarimeter]], the X-IFU instrument of the [[Advanced Telescope for High Energy Astrophysics]] satellite, the future [https://link.springer.com/article/10.1007/s10909-019-02329-w LiteBIRD] Cosmic Microwave Background polarization experiment, the [[Simons Observatory]], and the CMB Stage-IV Experiment.

==See also==