Journal
ASTROPHYSICAL JOURNAL
Volume 926, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ac397c
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Funding
- National Science Foundation Division of Astronomical Sciences [0959349, 1429236, 1636634, 1654494, 2034400]
- NASA [80NSSC19M0005, 80GSFC17M0002]
- NASA Postdoctoral Program at the NASA Goddard Space Flight Center
- NASA
- NASA-JHU [80NSSC19M005]
- CATA
- BASAL [AFB-170002]
- CONICYT-FONDECYT [1181620]
- Gordon and Betty Moore Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [2034400] Funding Source: National Science Foundation
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This study reports on the on-sky performance of the Cosmology Large Angular Scale Surveyor (CLASS), which aims to observe the polarized cosmic microwave background (CMB) to characterize primordial gravitational waves and cosmic reionization. By observing the Moon, Venus, and Jupiter, the researchers obtained power to antenna temperature calibrations and optical efficiencies for the telescopes. The measured noise-equivalent power of the detectors matches the expected noise model based on on-sky optical loading and lab-measured detector parameters.
The Cosmology Large Angular Scale Surveyor (CLASS) observes the polarized cosmic microwave background (CMB) over the angular scales of 1 degrees less than or similar to theta <= 90 degrees with the aim of characterizing primordial gravitational waves and cosmic reionization. We report on the on-sky performance of the CLASS Q-band (40 GHz), W-band (90 GHz), and dichroic G-band (150/220 GHz) receivers that have been operational at the CLASS site in the Atacama desert since 2016 June, 2018 May, and 2019 September, respectively. We show that the noise-equivalent power measured by the detectors matches the expected noise model based on on-sky optical loading and lab-measured detector parameters. Using Moon, Venus, and Jupiter observations, we obtain power to antenna temperature calibrations and optical efficiencies for the telescopes. From the CMB survey data, we compute instantaneous array noise-equivalent-temperature sensitivities of 22, 19, 23, and 71 mu K-cmp root s for the 40, 90, 150, and 220 GHz frequency bands, respectively. These noise temperatures refer to white noise amplitudes, which contribute to sky maps at all angular scales. Future papers will assess additional noise sources impacting larger angular scales.
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