A Measurement of the CMB ⟨EE⟩ Spectrum from the 2003 Flight of BOOMERANG

By T. Montroy, 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 report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R.A. = 82.°5, decl. = -45°. The observations were made using four pairs of polarization-sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a nonzero ⟨EE⟩ signal in the range 201 < l < 1000 with a significance of 4.8 σ, a 2 σ upper limit of 8.6 μK2 for any ⟨BB⟩ contribution, and a 2 σ upper limit of 7.0 μK2 for the ⟨EB⟩ spectrum. Estimates of foreground intensity fluctuations and the nondetection of ⟨BB⟩ and ⟨EB⟩ signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a ΛCDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d4f0a050ffaffb4f2b11aadaf8a0335d6863309c

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Citations in the corpus

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).”
A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND B-MODE POLARIZATION POWER SPECTRUM AT SUB-DEGREE SCALES WITH POLARBEAR (2014, background): “These measurements are consistent with a single source for both the temperature and E-mode signals – the adiabatic density fluctuations in the primordial universe (Barkats et al. 2014; Leitch et al. 2005; Montroy et al. 2006; Brown et al. 2009; quiet Collaboration 2011, 2012; Bennett et al. 2013).”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, unknown): “…Imager (CBI; Mason et al. 2003; Pearson et al. 2003), the Arcminute Cosmology Bolometer Array Receiver (ACBAR; Kuo et al. 2003) and BOOMERanG (Jones et al. 2006; Montroy et al. 2006; Piacentini et al. 2005), as incorporated into the current version of the CosmoMC code (Lewis & Bridle 2002).”
Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, background): “…Cosmic Background Imager (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…”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: ANGULAR POWER SPECTRA (2008, result): “The 5-year high-ℓ EE spectrum is shown in Figure 10, along with recent results from ground-based experiments (Leitch et al. 2005; Montroy et al. 2006; Sievers et al. 2007).”
Detection of B-mode polarization at degree angular scales by BICEP2. (2014, background): “…the EE power spectrum, including CAPMAP (Barkats et al. 2005; Bischoff et al. 2008), CBI (Readhead et al. 2004; Sievers et al. 2007), BOOMERANG03 (Montroy et al. 2006), WMAP (Page et al. 2007; Bennett et al. 2013), MAXIPOL (Wu et al. 2007), QUAD (Pryke et al. 2009; Brown et al. 2009), BICEP1…”
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).”
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…”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, unknown): “…al. 2003, 2007; Pearson 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…”
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).”