SECOND AND THIRD SEASON QUaD COSMIC MICROWAVE BACKGROUND TEMPERATURE AND POLARIZATION POWER SPECTRA

Pryke, C.; Ade, Peter A. R.; Bock, J. J.; Bowden, M.; Brown, Michael L.; Cahill, G.; Castro, Paulo Francisco de; Church, S.; Culverhouse, T.; Friedman, Robert; Ganga, K.; Gear, Walter Kieran; Gupta, S.; Hinderks, J.; Kovac, J. M.; Lange, A. E.; Leitch, E. M.; Melhuish, S. J.; Memari, Y.; Murphy, John A.; Orlando, A.; Schwarz, R.; Sullivan, Claire; Piccirillo, L.; Rajguru, N.; Rusholme, B.; Taylor, Andy; Thompson, K. L.; Turner, A. H.; Wu, Emily; Zemcov, Michael

doi:10.1088/0004-637x/692/2/1247

Cited by 100 publications

(93 citation statements)

References 31 publications

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“…We specifically use the CMB-only bandpowers given in Planck Collaboration XI (2016), adopting the same weighting scheme within each bin. Fitting for the positions and amplitudes of features in the bandpowers is a topic with a long history, with approaches becoming more sophisticated as the fidelity of the Pryke et al 2009). Following earlier approaches, we fit Gaussians to the peaks in C T T and C EE , but parabolas to the peaks in C T E .…”

Section: Peaks In the Power Spectramentioning

confidence: 99%

Planck2015 results

Adam

Ade

Aghanim

et al. 2016

A&A

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The European Space Agency's Planck satellite, which is dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013. In February 2015, ESA and the Planck Collaboration released the second set of cosmology products based on data from the entire Planck mission, including both temperature and polarization, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the main characteristics of the data and the data products in the release, as well as the associated cosmological and astrophysical science results and papers. The data products include maps of the cosmic microwave background (CMB), the thermal Sunyaev-Zeldovich effect, diffuse foregrounds in temperature and polarization, catalogues of compact Galactic and extragalactic sources (including separate catalogues of Corresponding author: C. R. Lawrence, e-mail: charles.lawrence@jpl.nasa.govArticle published by EDP Sciences A1, page 1 of 38 A&A 594, A1 (2016) Sunyaev-Zeldovich clusters and Galactic cold clumps), and extensive simulations of signals and noise used in assessing uncertainties and the performance of the analysis methods. The likelihood code used to assess cosmological models against the Planck data is described, along with a CMB lensing likelihood. Scientific results include cosmological parameters derived from CMB power spectra, gravitational lensing, and cluster counts, as well as constraints on inflation, non-Gaussianity, primordial magnetic fields, dark energy, and modified gravity, and new results on low-frequency Galactic foregrounds.

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Section: Peaks In the Power Spectramentioning

confidence: 99%

Planck2015 results

Adam

Ade

Aghanim

et al. 2016

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“…seven-year spectra, from the WMAP space mission (Larson et al 2011). In reality the current CMB bounds can be somewhat tightened if one includes results from other smaller scale CMB measurements, in particular the measurements of the temperature power spectrum from ACBAR (Reichardt et al 2009) and temperature and polarization spectra from QUaD (Pryke et al 2009). In addition, data from ACT (Das et al 2011) and SPT (Lueker et al 2010) could be added to the analysis, providing additional leverage on small scales 6 .…”

Section: Cmb Constraintsmentioning

confidence: 99%

WMAP7 and future CMB constraints on annihilating dark matter: implications for GeV-scale WIMPs

Hütsi

Chluba

Hektor

et al. 2011

A&A

120

154

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Aims. We calculate constraints from current and future cosmic microwave background (CMB) measurements on annihilating dark matter (DM) with masses below the electroweak scale: m DM = 5−100 GeV. In particular, we assume the S-wave annihilation mode to be dominant, and focus our attention on the lower end of this mass range, as DM particles with masses m DM ∼ 10 GeV have recently been claimed to be consistent with the CoGeNT and DAMA/LIBRA results, while also providing viable DM candidates to explain the measurements of Fermi and WMAP haze. We study the model (in)dependence of the CMB power spectra on particle physics DM models, large-scale structure formation and cosmological uncertainties. We attempt to find a simple and practical recipe for estimating current and future CMB bounds on a broad class of DM annihilation models. Methods. We use a model-independent description for DM annihilation into a wide set of Standard Model particles simulated by PYTHIA Monte Carlo. Our Markov chain Monte Carlo calculations used for finding model constraints involve realistic CMB likelihoods and assume a standard 6-parameter ΛCDM background cosmological model, which is extended by two additional DM annihilation parameters: m DM and σ A υ /m DM . Results. We show that in the studied DM mass range the CMB signal of DM annihilations is independent of the details of large-scale structure formation, distribution, and profile of DM halos and other cosmological uncertainties. All particle physics models of DM annihilation can be described with only one parameter, the fraction of energy carried away by neutrinos in DM annihilation. As the main result we provide a simple and rather generic fitting formula for calculating CMB constraints on the annihilation cross section of light WIMPs. We show that thermal relic DM in the CoGeNT, DAMA/LIBRA favored mass range is in a serious conflict with present CMB data for the annihilation channels with few neutrinos, and will definitely be tested by the Planck mission for all possible DM annihilation channels. Also, our findings strongly disfavor the claim that thermal relic DM annihilations with m DM ∼ 10 GeV and σ A υ ∼ 9 × 10 −25 cm 3 s −1 could be a cause of Fermi and WMAP haze.

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“…Over the past years, CMB polarization has been measured by several experiments and is being measured by the Planck surveyor Leitch et al 2002;Pryke et al 2002a,b Halverson et al 2002Leitch et al 2005;Ade & et al 2008;Pryke & et al 2009;Hinderks et al 2009;Brown & et al 2009;The Planck Collaboration 2006). CMB polarization pattern may be considered as the sum of gradient-like E mode and curllike B mode (Zaldarriaga & Seljak 1997;Kamionkowski et al 1997).…”

Section: Introductionmentioning

confidence: 99%

E/B decomposition of CMB polarization pattern of incomplete sky: a pixel space approach

Kim¹,

Naselsky²

2010

A&A

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CMB polarization pattern may be decomposed into gradient-like (E) and curl-like (B) mode, which provide invaluable information respectively. We have investigated E/B decomposition in pixel space. We find E/B mixing due to incomplete sky is localized in pixel-space, and negligible in the regions far away from the masked area. By estimating the expected local leakage power, we have diagnosed ambiguous pixels. Our criteria for ambiguous pixels (i.e. r c ) is associated with the tensor-to-scalar ratio of B mode power spectrum, which the leakage power is comparable to. By setting r c to a lower value, we may reduce leakage level, but reduce sky fraction at the same time. Therefore, we have solved ∂ΔC l /∂r c = 0, and obtained the optimal r c , which minimizes the estimation uncertainty, given a foreground mask and noise level. We have applied our method to a simulated map blocked by a foreground (diffuse + point source) mask. Our simulation shows leakage power is smaller than primordial (i.e. unlensed) B mode power spectrum of tensor-to-scalar ratio r ∼ 1 × 10 −3 at wide range of multipoles (50 l 2000), while allowing us to retain sky fraction ∼0.48.

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SECOND AND THIRD SEASON QUaD COSMIC MICROWAVE BACKGROUND TEMPERATURE AND POLARIZATION POWER SPECTRA

Cited by 100 publications

References 31 publications

Planck2015 results

Planck2015 results

WMAP7 and future CMB constraints on annihilating dark matter: implications for GeV-scale WIMPs

E/B decomposition of CMB polarization pattern of incomplete sky: a pixel space approach

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