Measurement of Cosmic Microwave Background Polarization Power Spectra From Two Years of Bicep Data

Chiang, H. C.; Ade, Peter A. R.; Barkats, D.; Battle, John; Bierman, E. M.; Bock, J. J.; Dowell, C. D.; Duband, L.; Hivon, E.; Holzapfel, W. L.; Hristov, V. V.; Jones, W. C.; Keating, Brian; Kovac, J. M.; Kuo, Chao-Lin; Lange, A. E.; Leitch, E. M.; Mason, P.; Matsumura, Tomotake; Nguyen, Hien; Ponthieu, N.; Pryke, C.; Richter, Steffen; Rocha, G.; Sheehy, C. D.; Takahashi, Yuki; Tolan, J. E.; Yoon, K. W.

doi:10.1088/0004-637x/711/2/1123

Cited by 221 publications

(271 citation statements)

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“…The most direct way of testing for a tensor contribution is to search for a magnetic-type parity signature via a large-scale B-mode pattern in CMB polarization (Seljak 1997;Kamionkowski et al 1997). Direct B-mode measurements are challenging as the expected signal is small; upper limits measured by BICEP and QUIET give 95% upper limits of r 0.002 < 0.73 and r 0.002 < 2.8 respectively (Chiang et al 2010;QUIET Collaboration et al 2012) 37 .…”

Section: Tensor Fluctuationsmentioning

confidence: 99%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

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This paper presents the first cosmological results based on Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra. We find that the Planck spectra at high multipoles ( > ∼ 40) are extremely well described by the standard spatiallyflat six-parameter ΛCDM cosmology with a power-law spectrum of adiabatic scalar perturbations. Within the context of this cosmology, the Planck data determine the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be θ * = (1.04147 ± 0.00062) × 10 −2 , Ω b h 2 = 0.02205 ± 0.00028, Ω c h 2 = 0.1199 ± 0.0027, and n s = 0.9603 ± 0.0073, respectively (note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H 0 = (67.3 ± 1.2) km s −1 Mpc −1 , and a high value of the matter density parameter, Ω m = 0.315 ± 0.017. These values are in tension with recent direct measurements of H 0 and the magnituderedshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter ΛCDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured over the standard six-parameter ΛCDM cosmology. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r 0.002 < 0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. Using BAO and CMB data, we find N eff = 3.30 ± 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the sum of neutrino masses. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N eff = 3.046. We find no evidence for dynamical dark energy; using BAO and CMB data, the dark energy equation of state parameter is constrained to be w = −1.13 +0.13 −0.10 . We also use the Planck data to set limits on a possible variation of the fine-structure constant, dark matter annihilation and primordial magnetic fields. Despite the success of the six-parameter ΛCDM model in describing the Planck data at high multipoles, we note that this cosmology does not provide a good fit to the temperature power spectrum at low multipoles. T...

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Section: Tensor Fluctuationsmentioning

confidence: 99%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

Self Cite

5,014

163

2,253

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“…The first version of the experiment, BICEP1, observed at two frequencies: 100 GHz and 150 GHz. Collecting data from 2006 to 2008, it obtained the first significant upper limit on r from polarization measurements alone [136] r < 0.73 (95% limit) .…”

Section: Inflation After Bicep2mentioning

confidence: 99%

“…In practice, dN min is far more challenging to study than the related index density dI min , defined by 136) where (−1) F i is the sign of the determinant of the fermion mass matrix (see [44]). The integral of dI min over the moduli space is manifestly not the total number of vacua: it is instead a sum weighted by signs.…”

Section: Counting Vacuamentioning

confidence: 99%

Inflation and String Theory

2015

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“…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.…”

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confidence: 99%