High-Resolution CMB Power Spectrum From the Complete Acbar Data Set

Abstract

In this paper, we present results from the complete set of cosmic microwave background (CMB) radiation temperature anisotropy observations made with the Arcminute Cosmology Bolometer Array Receiver (ACBAR) operating at 150 GHz. We include new data from the final 2005 observing season, expanding the number of detector-hours by 210% and the sky coverage by 490% over that used for the previous ACBAR release. As a result, the band-power uncertainties have been reduced by more than a factor of two on angular scales encompassing the third to fifth acoustic peaks as well as the damping tail of the CMB power spectrum. The calibration uncertainty has been reduced from 6% to 2.1% in temperature through a direct comparison of the CMB anisotropy measured by ACBAR with that of the dipole-calibrated WMAP5 experiment. The measured power spectrum is consistent with a spatially flat, ΛCDM cosmological model. We include the effects of weak lensing in the power spectrum model computations and find that this significantly improves the fits of the models to the combined ACBAR+WMAP5 power spectrum. The preferred strength of the lensing is consistent with theoretical expectations. On fine angular scales, there is weak evidence (1.1σ) for excess power above the level expected from primary anisotropies. We expect any excess power to be dominated by the combination of emission from dusty protogalaxies and the Sunyaev-Zel'dovich effect (SZE). However, the excess observed by ACBAR is significantly smaller than the excess power at ℓ > 2000 reported by the CBI experiment operating at 30 GHz. Therefore, while it is unlikely that the CBI excess has a primordial origin; the combined ACBAR and CBI results are consistent with the source of the CBI excess being either the SZE or radio source contamination.

Cosmic string parameter constraints and model analysis using small scale Cosmic Microwave Background data

“…Observations of the cosmic microwave background (CMB) radiation [2][3][4][5] and the large-scale distribution of galaxies [6] are consistent with the inflationary paradigm (see e.g. [7]) in which cosmic structure was seeded in the very early stages of the universe.…”

“…We then compare the above mentioned models to seven-year WMAP data [2] (ℓ 1000), and study the effect of adding ACBAR [3] (300 ℓ 3000) and QUAD data [4] (2000 ℓ 3000), and finally ACT data [5] (ℓ 10000).…”

Cosmology seeking friendship with sterile neutrinos

“…We use CMB data from WMAP after 7 years of observation [7], as well as from the ACBAR [37], BICEP [38], and QuAD [39] experiments. In addition, we use the halo power spectrum extracted from the SDSS-DR7 luminous In Figure 1, we show 2D confidence contours for the 3 + N s and N s + 3 cases.…”

SUSY SU(5)×S 4 GUT flavor model for fermion masses and mixings with adjoint, large θ 13 PMNS

“…The plot of the ratio |m 3 /m 2 | and sum of light neutrino mass k m k as function of the lightest neutrino mass m lightest , which is m 1 (m 3 ) for NH (IH) mass spectrum, are shown in figure 3(a) and figure 3(b), respectively. Note that the horizontal lines in figure 3(b) represents the cosmological bound at 0.19 eV (black), corresponding to the combined observational data from [113][114][115][116][117][118][119][120][121][122], and the upper bounds 0.23 eV from Planck [123]. The ratio tends to a degenerate mass spectrum in both cases as the value of m lightest → 0.1eV which is disfavoured in the model.…”