CLASS: the cosmology large angular scale surveyor

By T. Essinger-Hileman, Aamir Ali, M. Amiri, J. Appel, D. Araujo, C. Bennett, F. Boone, M. Chan, Hsiao-mei Cho, D. Chuss and 34 more. Astronomical Telescopes and Instrumentation, 2014

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The Cosmology Large Angular Scale Surveyor (CLASS) is an experiment to measure the signature of a gravitationalwave background from inflation in the polarization of the cosmic microwave background (CMB). CLASS is a multi-frequency array of four telescopes operating from a high-altitude site in the Atacama Desert in Chile. CLASS will survey 70% of the sky in four frequency bands centered at 38, 93, 148, and 217 GHz, which are chosen to straddle the Galactic-foreground minimum while avoiding strong atmospheric emission lines. This broad frequency coverage ensures that CLASS can distinguish Galactic emission from the CMB. The sky fraction of the CLASS survey will allow the full shape of the primordial B-mode power spectrum to be characterized, including the signal from reionization at low ɺ. Its unique combination of large sky coverage, control of systematic errors, and high sensitivity will allow CLASS to measure or place upper limits on the tensor-to-scalar ratio at a level of r = 0:01 and make a cosmic-variance-limited measurement of the optical depth to the surface of last scattering, Ƭ .

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3a4f19bea4f3c953cd9e4da1ad46b7b3c15ee085

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Citations in the corpus

The Simons Observatory: science goals and forecasts (2018, background): “CLASS (Essinger-Hileman et al. 2014) is a currently ongoing ground-based experiment aiming to measure large angular scale CMB from the ground at 98/148 GHz with a single dust channel at 217 GHz.”
The Quest for B Modes from Inflationary Gravitational Waves (2015, unknown): “The parameters sets {tobs,NETarray, fsky} used for the noise estimates for BICEP2, CLASS and CMB-S4 (assuming 105 detectors) are {590 days, 18.75µK √ sec, 0.01}, {3 yrs, 7µK √ sec, 0.7} and {2 yrs, 1.5µK √ sec, 0.75}, respectively.”
Robust forecasts on fundamental physics from the foreground-obscured, gravitationally-lensed CMB polarization (2015, background): “[80] frequencies [GHz] fractional bandpass [%] sensitivities [μK-arcmin] fsky [%] FWHM [arcmin] `min `max 38.”
PICO: Probe of Inflation and Cosmic Origins (2019, background): “Such next-generation US-based sub-orbital CMB experiments are collectively denoted as ‘Stage-3 (S3)’ [10–16].”
Early Dark Energy can Resolve the Hubble Tension. (2018, background): “Additionally, the pattern around the first peak (` ∼ 30−500) in the EE spectrum might be detectable in the future by large-scales E-mode measurements such as CLASS [61] or LiteBird [62].”