A Measurement of the Cosmic Microwave Background B-Mode Polarization With Polarbear

Akiba, Y.; Anthony, A. E.; Arnold, K.; Atlas, M.; Barron, Darcy; Boettger, D.; Borrill, J.; Chapman, Scott; Chinone, Yuji; Dobbs, M.; Elleflot, T.; Errard, Josquin; Fabbian, Giulio; Feng, Chang; Flanigan, D.; Gilbert, A.; Grainger, W.; Halverson, N. W.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Holzapfel, W. L.; Hori, Y.; Howard, J.; Hyland, P.; Inoue, Yuki; Jaehnig, G.; Jaffe, A.H.; Keating, Brian; Kermish, Z.; Keskitalo, R.; Kisner, T. S.; Jeune, M. Le; Lee, A.T.; Leitch, E. M.; Linder, Eric V.; Lungu, Marius; Matsuda, Frederick; Matsumura, Tomotake; Meng, Xiaofan; Miller, Nathan J.; Morii, H.; Moyerman, S.; Myers, Michael J.; Navaroli, M.; Nishino, Haruki; Orlando, A.; Paar, H. P.; Peloton, J.; Poletti, D.; Quealy, E.; Rebeiz, Gabriel M.

doi:10.5303/pkas.2015.30.2.625

Cited by 11 publications

(14 citation statements)

References 22 publications

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“…PolarBear has published the first detection of auto-spectra of Bmodes at the arcminute scale. That was found consistent with predictions from cosmological gravitational lensing within the ΛCDM concordance model [264], and, to date, it represents the first detection of cosmological B-modes from one single experiment, at the auto-spectrum level. Immediately after, an excess on the degree angular scales, which could be ascribed to cosmological GWs, was announced by the BI-CEP2 collaboration [265].…”

Section: B-mode Observationssupporting

confidence: 73%

Gravitational wave astronomy: the current status

Blair

Zhao

et al. 2015

Sci. China Phys. Mech. Astron.

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In the centenary year of Einstein's General Theory of Relativity, this paper reviews the current status of gravitational wave astronomy across a spectrum which stretches from attohertz to kilohertz frequencies. Sect. 1 of this paper reviews the historical development of gravitational wave astronomy from Einstein's first prediction to our current understanding the spectrum. It is shown that detection of signals in the audio frequency spectrum can be expected very soon, and that a north-south pair of next generation detectors would provide large scientific benefits. Sect. 2 reviews the theory of gravitational waves and the principles of detection using laser interferometry. The state of the art Advanced LIGO detectors are then described. These detectors have a high chance of detecting the first events in the near future. Sect. 3 reviews the KAGRA detector currently under development in Japan, which will be the first laser interferometer detector to use cryogenic test masses. Sect. 4 of this paper reviews gravitational wave detection in the nanohertz frequency band using the technique of pulsar timing. Sect. 5 reviews the status of gravitational wave detection in the attohertz frequency band, detectable in the polarisation of the cosmic microwave background, and discusses the prospects for detection of primordial waves from the big bang. The techniques described in sects. 1-5 have already placed significant limits on the strength of gravitational wave sources. Sects. 6 and 7 review ambitious plans for future space based gravitational wave detectors in the millihertz frequency band. Sect. 6 presents a roadmap for development of space based gravitational wave detectors by China while sect. 7 discusses a key enabling technology for space interferometry known as time delay interferometry. gravitational waves, ground based detectors, pulsar timing, spaced based detectors, CMB PACS number(s): 04.80. Nn, 07.20.Mc,

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Section: B-mode Observationssupporting

confidence: 73%

Gravitational wave astronomy: the current status

Blair

Zhao

et al. 2015

Sci. China Phys. Mech. Astron.

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Section: H Y S I C a L R E V I E W L E T T E R S Week Ending 22 Januamentioning

confidence: 99%

“…[6]. Because of small gravitational deflections of the CMB photons in flight by intervening large scale structure, the initial purity of the E-mode pattern is disturbed and a small lensing B mode is produced at subdegree angular scales [7,8].IGWs are intrinsically quadrupolar distortions of the metric and produce both E-and B-mode polarization depending on their orientation with respect to our last scattering surface. However, due to the large ΛCDM E-mode signal, the most promising place to search for an IGW signal is in B modes.…”

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confidence: 99%

Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band

Ade¹,

Ahmed²,

Aikin³

et al. 2016

Phys. Rev. Lett.

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595

691

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We present results from an analysis of all data taken by the BICEP2 and Keck Array cosmic microwave background (CMB) polarization experiments up to and including the 2014 observing season. This includes the first Keck Array observations at 95 GHz. The maps reach a depth of 50 nK deg in Stokes Q and U in the 150 GHz band and 127 nK deg in the 95 GHz band. We take auto-and cross-spectra between these maps and publicly available maps from WMAP and Planck at frequencies from 23 to 353 GHz. An excess over lensed ΛCDM is detected at modest significance in the 95 × 150 BB spectrum, and is consistent with the dust contribution expected from our previous work. No significant evidence for synchrotron emission is found in spectra such as 23 × 95, or for correlation between the dust and synchrotron sky patterns in spectra such as 23 × 353. We take the likelihood of all the spectra for a multicomponent model including lensed ΛCDM, dust, synchrotron, and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r) using priors on the frequency spectral behaviors of dust and synchrotron emission from previous analyses of WMAP and Planck data in other regions of the sky. This analysis yields an upper limit r 0.05 < 0.09 at 95% confidence, which is robust to variations explored in analysis and priors. Combining these B-mode results with the (more model-dependent) constraints from Planck analysis of CMB temperature plus baryon acoustic oscillations and other data yields a combined limit r 0.05 < 0.07 at 95% confidence. These are the strongest constraints to date on inflationary gravitational waves. DOI: 10.1103/PhysRevLett.116.031302 PRL 116, 031302 (2016) P H Y S I C A L R E V I E W L E T T E R S week ending 22 JANUARY 20160031-9007=16=116(3)=031302 (9) 031302-1 © 2016 American Physical SocietyIntroduction.-Measurements of the cosmic microwave background (CMB) [1] are one of the observational pillars of the standard cosmological model (ΛCDM) and constrain its parameters to high precision (see most recently Ref. [2]). This model extrapolates the Universe back to very high temperatures (≫10 12 K) and early times (≪ 1 s). Observations indicate that conditions at these early times are described by an almost uniform plasma with a nearly scale invariant spectrum of adiabatic density perturbations. However, ΛCDM itself offers no explanation for how these conditions occurred. The theory of inflation is an extension to the standard model, which postulates a phase of exponential expansion at a still earlier epoch (∼10 −35 s) that precedes ΛCDM and produces the required initial conditions (see Ref.[3] for a recent review and citations to the original literature).There is widespread support for the claim that existing observations already indicate that some version of inflation probably did occur, but there are also skeptics [4,5]. As well as the specific form of the initial density perturbations, there is an additional relic which inflation predicts, and which one can attempt to detect....

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“…Ref. [9] for a review), which produces detectable levels of the bispectrum [6] and the B-mode polarization [10][11][12][13] even when they are primordially absent. Therefore, their contributions should be correctly taken into account to extract information on inflation from data.…”

Section: Introductionmentioning

confidence: 99%

Geodesiccurve-of-sight formulae for the cosmic microwave background: a unified treatment of redshift, time delay, and lensing

Saito

Naruko

Hiramatsu

et al. 2014

J. Cosmol. Astropart. Phys.

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Abstract. In this paper, we introduce a new approach to a treatment of the gravitational effects (redshift, time delay and lensing) on the observed cosmic microwave background (CMB) anisotropies based on the Boltzmann equation. From the Liouville's theorem in curved spacetime, the intensity of photons is conserved along a photon geodesic when non-gravitational scatterings are absent. Motivated by this fact, we derive a second-order line-of-sight formula by integrating the Boltzmann equation along a perturbed geodesic (curve) instead of a background geodesic (line). In this approach, the separation of the gravitational and intrinsic effects are manifest. This approach can be considered as a generalization of the remapping approach of CMB lensing, where all the gravitational effects can be treated on the same footing.

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A Measurement of the Cosmic Microwave Background B-Mode Polarization With Polarbear

Cited by 11 publications

References 22 publications

Gravitational wave astronomy: the current status

Gravitational wave astronomy: the current status

Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band

Geodesiccurve-of-sight formulae for the cosmic microwave background: a unified treatment of redshift, time delay, and lensing

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