A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG

By F. Piacentini, P. Ade, J. Bock, J. Richard Bond, J. Borrill, A. Boscaleri, P. Cabella, C. Contaldi, B. Crill, P. Bernardis and 27 more. 2005

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We present a measurement of the polarization-temperature angular cross power spectra, ⟨TE⟩ and ⟨TB⟩, of the cosmic microwave background. The result is based on ~200 hr of data from eight polarization-sensitive bolometers operating at 145 GHz during the 2003 flight of BOOMERANG. We detect a significant ⟨TE⟩ correlation in the l-range between 50 and 950 with a statistical significance of >3.5 σ. Contamination by polarized foreground emission and systematic effects are negligible in comparison with statistical uncertainties. The spectrum is consistent with previous detections and with the "concordance model" that assumes adiabatic initial conditions. This is the first measurement of polarization-temperature angular cross-power spectra using bolometric detectors.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/04b79f82a9c0df9605178c2445387c9e358fa9d2

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Citations in the corpus

Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, background): “…(CBI; Readhead et al. 2004) with 855 < < 1700, observations from the 2003 flight of BOOMERanG (Ruhl et al. 2003; Jones et al. 2006; Montroy et al. 2006; Piacentini et al. 2006) in the range 925 < < 1400 and the recent results for the temperature and polarization power spectra measurements…”
MEASUREMENT OF COSMIC MICROWAVE BACKGROUND POLARIZATION POWER SPECTRA FROM TWO YEARS OF BICEP DATA (2009, methodology): “The acoustic peaks in the polarization spectra have been measured to high precision in both the T E spectrum (Piacentini et al. 2006; Nolta et al. 2009) and, more recently, directly in the EE spectrum (Pryke et al. 2009; Brown et al. 2009), providing further support for our basic understanding of…”
Astrophysical Tests of Lorentz and CPT Violation with Photons (2008, methodology): “One involving BOOMERANG (B03) data (Montroy et al. 2006; Piacentini et al. 2006) alone yielded the possibility k (3) (V )00 = (12 ± 7) × 10−43 GeV (Kostelecký & Mewes 2007), while the result from another analysis combining B03 and WMAP 5-year data corresponds to k (3) (V )00 < (2.6 ± 1.9) × 10−43…”
Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology (2006, unknown): “…et al. 2005); improvements in small-scale CMB measurements ( Kuo et al. 2004; Readhead et al. 2004a, 2004b; Grainge et al. 2003; Leitch et al. 2005; Piacentini et al. 2006; Montroy et al. 2006; O'Dwyer et al. 2005); much larger samples of highredshift supernova (Riess et al. 2004; Astier et…”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “…0.25 +0.10(+0.15) −0.07(−0.17) at 68% CL (95% CL), which was obtained by Ichikawa et al. (2008) from the WMAP 5-year data combined with ACBAR (Reichardt et al. 2009), BOOMERanG (Jones et al. 2006; Piacentini et al. 2006; Montroy et al. 2006), and Cosmic Background Imager (CBI; Sievers et al. 2007).”
MultiNest: an efficient and robust Bayesian inference tool for cosmology and particle physics (2008, background): “…(ACBAR; Reichardt et al. 2008) + the Cosmic Background Imager (CBI; Readhead et al. 2004; Sievers J. L. et al. 2007; CBI Supplementary Data 2006) + Balloon Observations of Millimetric Extragalactic Radiation and Geophysics (BOOMERANG; Piacentini et al. 2006; Jones et al. 2006; Montroy et al. 2006).”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, unknown): “…et al. 2003; Readhead et al. 2004), VSA (Dickinson et al. 2004), ACBAR (Kuo et al. 2004, 2007), and BOOMERanG (Ruhl et al. 2003; Montroy et al. 2006; Piacentini et al. 2006), all of which go well beyond the WMAP angular resolution, so that their small-scale data are statistically independent of…”
HIGH-RESOLUTION CMB POWER SPECTRUM FROM THE COMPLETE ACBAR DATA SET (2008, unknown): “…et al. 2002 ); the DASI EE and TE band-powers (Leitch et al. 2005); the VSA final results (Dickinson et al. 2004); the MAXIMA 1998 flight results (Hanany et al. 2000); and the TT, TE, and EE results from the BOOMERANG 2003 flight (Jones et al. 2006; Piacentini et al. 2006; Montroy et al. 2006).”