Detection of polarization in the cosmic microwave background using DASI

By J. Kovac, E. Leitch, C. Pryke, J. Carlstrom, N. Halverson, W. Holzapfel. Nature, 2002

602 citations recorded by the source corpus.

The past several years have seen the emergence of a standard cosmological model, in which small temperature differences in the cosmic microwave background (CMB) radiation on angular scales of the order of a degree are understood to arise from acoustic oscillations in the hot plasma of the early Universe, arising from primordial density fluctuations. Within the context of this model, recent measurements of the temperature fluctuations have led to profound conclusions about the origin, evolution and composition of the Universe. Using the measured temperature fluctuations, the theoretical framework predicts the level of polarization of the CMB with essentially no free parameters. Therefore, a measurement of the polarization is a critical test of the theory and thus of the validity of the cosmological parameters derived from the CMB measurements. Here we report the detection of polarization of the CMB with the Degree Angular Scale Interferometer (DASI). The polarization is deteced with high confidence, and its level and spatial distribution are in excellent agreement with the predictions of the standard theory.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/48ef1279bb903bb3a5d82d502ac82b0c71e636ff

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Predictions for high-frequency radio surveys of extragalactic sources (2004, methodology): “Preliminary source counts at 30 GHz have been produced by the DASI (Kovac et al. 2002), VSA (Grainge et al. 2003), and CBI (Mason et al. 2003) CMB experiments.”
MEASUREMENT OF COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRA FROM TWO YEARS OF BICEP DATA (2009, methodology): “E-mode polarization was first detected by DASI (Kovac et al. 2002) and has since been measured by many other experiments (Leitch et al. 2005; Montroy et al. 2006; Sievers et al. 2007; Wu et al. 2007; Bischoff et al. 2008).”
Detection of B-mode polarization at degree angular scales by BICEP2. (2014, methodology): “They were first detected by the DASI experiment (Kovac et al. 2002).”
Three Year Wilkinson Microwave Anistropy Probe (WMAP) Observations: Polarization Analysis (2006, methodology): “In 2002, the DASI team announced a detection of CMB polarization at sub-degree angular scales based on 9 months of data from a 13 element 30 GHz interferometer (Kovac et al. 2002; Leitch et al. 2002).”
A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG (2005, methodology): “Previous detections of the temperature-polarization angular cross power spectrum have been obtained by the WMAP satellite (Kogut et al. 2003) and by the DASI (Kovac et al. 2002; Leitch et al. 2004) and CBI (Readhead et al. 2004) interferometers.”
Cosmological Parameters from the 2003 Flight of BOOMERANG (2005, methodology): “A mix of isocurvature and adiabatic modes can be designed to give acceptable fits to the CMB intensity power spectra (e.g., (Bucher et al. 2004; Kurki-Suonio et al. 2005)), and the polarization data, from B03 as well from DASI, CAPMAP and CBI are not yet at the point to clearly distinguish among the”
Radio and millimeter continuum surveys and their astrophysical implications (2009, methodology): “Counts at ∼ 30 GHz have been estimated from DASI data over the range 0.1 to 10 Jy (Kovac et al. 2002), from CBI maps in the range 5–50 mJy (Mason et al. 2003), and down to 1 mJy from the SZA blind cluster survey (Muchovej et al. 2009, in prep.).”
A Measurement of the CMB ⟨EE⟩ Spectrum from the 2003 Flight of BOOMERANG (2005, methodology): “To test how well particular models fit our data, we use the standard likelihood ratio technique in a manner similar to recent work done by DASI (Kovac et al. 2002; Leitch et al. 2004) and CBI (Readhead et al. 2004).”