Characterization and performance of the second-year SPT-3G focal plane
The third-generation instrument for the 10-meter South Pole Telescope, SPT-3G, was first installed in January 2017. In addition to completely new cryostats, secondary telescope optics, and readout electronics, the number of detectors in the focal plane has increased by an order of magnitude from pre...
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ftosti:oai:osti.gov:1478017 2023-07-30T04:06:54+02:00 Characterization and performance of the second-year SPT-3G focal plane Dutcher, D. 2022-02-02 application/pdf http://www.osti.gov/servlets/purl/1478017 https://www.osti.gov/biblio/1478017 https://doi.org/10.1117/12.2312451 unknown http://www.osti.gov/servlets/purl/1478017 https://www.osti.gov/biblio/1478017 https://doi.org/10.1117/12.2312451 doi:10.1117/12.2312451 79 ASTRONOMY AND ASTROPHYSICS 46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY 2022 ftosti https://doi.org/10.1117/12.2312451 2023-07-11T09:29:37Z The third-generation instrument for the 10-meter South Pole Telescope, SPT-3G, was first installed in January 2017. In addition to completely new cryostats, secondary telescope optics, and readout electronics, the number of detectors in the focal plane has increased by an order of magnitude from previous instruments to ~16,000. The SPT-3G focal plane consists of ten detector modules, each with an array of 269 trichroic, polarization-sensitive pixels on a six-inch silicon wafer. Within each pixel is a broadband, dual-polarization sinuous antenna; the signal from each orthogonal linear polarization is divided into three frequency bands centered at 95, 150, and 220 GHz by in-line lumped element filters and transmitted via superconducting microstrip to Ti/Au transition-edge sensor (TES) bolometers. Properties of the TES film, microstrip filters, and bolometer island must be tightly controlled to achieve optimal performance. For the second year of SPT-3G operation, we have replaced all ten wafers in the focal plane with new detector arrays tuned to increase mapping speed and improve overall performance. Here we discuss the TES superconducting transition temperature and normal resistance, detector saturation power, bandpasses, optical efficiency, and full array yield for the 2018 focal plane. Other/Unknown Material South pole SciTec Connect (Office of Scientific and Technical Information - OSTI, U.S. Department of Energy) South Pole Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX 69 |
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SciTec Connect (Office of Scientific and Technical Information - OSTI, U.S. Department of Energy) |
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79 ASTRONOMY AND ASTROPHYSICS 46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY |
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79 ASTRONOMY AND ASTROPHYSICS 46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY Dutcher, D. Characterization and performance of the second-year SPT-3G focal plane |
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79 ASTRONOMY AND ASTROPHYSICS 46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY |
description |
The third-generation instrument for the 10-meter South Pole Telescope, SPT-3G, was first installed in January 2017. In addition to completely new cryostats, secondary telescope optics, and readout electronics, the number of detectors in the focal plane has increased by an order of magnitude from previous instruments to ~16,000. The SPT-3G focal plane consists of ten detector modules, each with an array of 269 trichroic, polarization-sensitive pixels on a six-inch silicon wafer. Within each pixel is a broadband, dual-polarization sinuous antenna; the signal from each orthogonal linear polarization is divided into three frequency bands centered at 95, 150, and 220 GHz by in-line lumped element filters and transmitted via superconducting microstrip to Ti/Au transition-edge sensor (TES) bolometers. Properties of the TES film, microstrip filters, and bolometer island must be tightly controlled to achieve optimal performance. For the second year of SPT-3G operation, we have replaced all ten wafers in the focal plane with new detector arrays tuned to increase mapping speed and improve overall performance. Here we discuss the TES superconducting transition temperature and normal resistance, detector saturation power, bandpasses, optical efficiency, and full array yield for the 2018 focal plane. |
author |
Dutcher, D. |
author_facet |
Dutcher, D. |
author_sort |
Dutcher, D. |
title |
Characterization and performance of the second-year SPT-3G focal plane |
title_short |
Characterization and performance of the second-year SPT-3G focal plane |
title_full |
Characterization and performance of the second-year SPT-3G focal plane |
title_fullStr |
Characterization and performance of the second-year SPT-3G focal plane |
title_full_unstemmed |
Characterization and performance of the second-year SPT-3G focal plane |
title_sort |
characterization and performance of the second-year spt-3g focal plane |
publishDate |
2022 |
url |
http://www.osti.gov/servlets/purl/1478017 https://www.osti.gov/biblio/1478017 https://doi.org/10.1117/12.2312451 |
geographic |
South Pole |
geographic_facet |
South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
http://www.osti.gov/servlets/purl/1478017 https://www.osti.gov/biblio/1478017 https://doi.org/10.1117/12.2312451 doi:10.1117/12.2312451 |
op_doi |
https://doi.org/10.1117/12.2312451 |
container_title |
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX |
container_start_page |
69 |
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1772819851562188800 |