A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG

By W. Jones, 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 on observations of the cosmic microwave background (CMB) obtained during the 2003 January flight of BOOMERANG. These results are derived from 195 hr of observation with four 145 GHz polarization-sensitive bolometer (PSB) pairs, identical in design to the four 143 GHz Planck High Frequency Instrument (HFI) polarized pixels. The data include 75 hr of observations distributed over 1.84% of the sky with an additional 120 hr concentrated on the central portion of the field, which represents 0.22% of the full sky. From these data we derive an estimate of the angular power spectrum of temperature fluctuations of the CMB in 24 bands over the multipole range 50 ≤ l ≤ 1500. A series of features, consistent with those expected from acoustic oscillations in the primordial photon-baryon fluid, are clearly evident in the power spectrum, as is the exponential damping of power on scales smaller than the photon mean free path at the epoch of last scattering (l ≳ 900). As a consistency check, the collaboration has performed two fully independent analyses of the time-ordered data, which are found to be in excellent agreement.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/aae0367bae11e44fe393988d31d18437ea094b7a

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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).”
THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008 POWER SPECTRUM (2010, unknown): “Measurements at higher resolution have been made by a set of complementary balloon and ground-based experiments (e.g., Jones et al. 2006; Brown et al. 2009; Reichardt et al. 2009; Sievers et al. 2009).”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “Recently, the BOOMERanG collaboration (Pagano et al. 2009) revisited a limit on ∆α from their 2003 flight (B2K), taking into account the effect of systematic errors rotating the polarization angle by −0.9◦ ± 0.7◦.”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…fluctuations has been gradually uncovered, culminating in the clear detection of three Doppler peaks due to acoustic oscillations in the photon-baryon fluid at the last scattering surface (de Bernardis et al. 2000; Hanany et al. 2000; Hinshaw et al. 2003; Jones et al. 2006; Hinshaw et al. 2006).”
HIGH-RESOLUTION CMB POWER SPECTRUM FROM THE COMPLETE ACBAR DATA SET (2008, methodology): “The CMB8 field (lower right corner) was targeted at the deep region of the B03 experiment as an alternative calibration path to the WMAP cross-calibration used for the results presented here. the amplitude of atmosphere-induced cross-channel correlations .”
Component separation methods for the PLANCK mission (2008, methodology): “The 145 GHz CMB maps were then used for the purpose of power spectrum estimation in both temperature and polarization, after masking away a handfulof compact sources (Jones et al. 2006).”
Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, methodology): “…I O N The acoustic peaks imprinted on the temperature power spectrum of the cosmic microwave background (CMB) have now been measured with impressive precision by a number of experiments (Lee et al. 2001; Bennet et al. 2003; Hinshaw et al. 2003, 2007, 2009; Jones et al. 2006; Reichardt et al. 2009).”
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).”