NINE-YEAR
                    <i>WILKINSON MICROWAVE ANISOTROPY PROBE</i>
                    (
                    <i>WMAP</i>
                    ) OBSERVATIONS: FINAL MAPS AND RESULTS

Bennett, C. L.; Larson, David; Weiland, J. L.; Jarosik, N.; Hinshaw, G.; Odegard, N.; Smith, Kendrick M.; Hill, Robert S.; Gold, B.; Halpern, M.; Komatsu, Eiichiro; Nolta, Michael R.; Page, Lyman A.; Spergel, David N.; Wollack, Edward J.; Dunkley, Joanna; Kogut, A.; Limon, M.; Meyer, S. S.; Tucker, Gregory S.; Wright, E. L.

doi:10.1088/0067-0049/208/2/20

Cited by 2,054 publications

(1,563 citation statements)

References 112 publications

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“…We use the following datasets: a) observations of type Ia supernovae from the Joint Lightcurve Analysis (JLA) of the Sloan Digital Sky Survey (SDSS-II) and the Supernova Legacy Survey (SNLS) samples [12]; b) observations of baryon acoustic oscillations in the SDSS DR7 [13] and SDSS DR9 [14], in the WiggleZ Survey [15] and in the 6dF Galaxy Survey (6dFGRS) [16]; c) measurements of cosmic microwave background temperature anisotropy from 2015 Planck [17] and WMAP9-year [18]; d) observations of the Hubble rate H(z) from [19][20][21][22][23][24]. In the following subsections, the statistical analysis used to deal with those observables is briefly described.…”

Section: Observational Datamentioning

confidence: 99%

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

Santos

Reis

Waga

2016

J. Cosmol. Astropart. Phys.

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Abstract. We revisit the kink-like parametrization of the deceleration parameter q(z) [1], which considers a transition, at redshift z t , from cosmic deceleration to acceleration. In this parametrization the initial, at z z t , value of the q-parameter is q i , its final, z = −1, value is q f and the duration of the transition is parametrized by τ . By assuming a flat space geometry we obtain constraints on the free parameters of the model using recent data from type Ia supernovae (SN Ia), baryon acoustic oscillations (BAO), cosmic microwave background (CMB) and the Hubble parameter H(z). The use of H(z) data introduces an explicit dependence of the combined likelihood on the present value of the Hubble parameter H 0 , allowing us to explore the influence of different priors when marginalizing over this parameter. We also study the importance of the CMB information in the results by considering data from WMAP7, WMAP9 (Wilkinson Microwave Anisotropy Probe -7 and 9 years) and Planck 2015. We show that the contours and best fit do not depend much on the different CMB data used and that the considered new BAO data is responsible for most of the improvement in the results. Assuming a flat space geometry, q i = 1/2 and expressing the present value of the deceleration parameter q 0 as a function of the other three free parameters, we obtain z t = 0.67 +0.10 −0.08 , τ = 0.26 +0.14 −0.10 and q 0 = −0.48 +0.11 −0.13 , at 68% of confidence level, with an uniform prior over H 0 . If in addition we fix q f = −1, as in flat ΛCDM, DGP and Chaplygin quartessence that are special models described by our parametrization, we get z t = 0.66 +0.03 −0.04 , τ = 0.33 +0.04 −0.04 and q 0 = −0.54 +0.05 −0.07 , in excellent agreement with flat ΛCDM for which τ = 1/3. We also obtain for flat wCDM, another dark energy model described by our parametrization, the constraint on the equation of state parameter −1.22 < w < −0.78 at more than 99% confidence level.

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Section: Observational Datamentioning

confidence: 99%

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

Santos

Reis

Waga

2016

J. Cosmol. Astropart. Phys.

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“…• For the CMB (temperature and polarization) as well as for the lensing map we adopt the WMAP 9-year point source catalogue mask (the one used by the WMAP team to exclude the Galactic plane and the Magellanic cloud regions when building the 9-year point source catalogues, Bennett et al 2013). …”

Section: Simulated Mapsmentioning

confidence: 99%

On the recovery of ISW fluctuations using large-scale structure tracers and CMB temperature and polarization anisotropies

Bonavera

Barreiro

Vielva

2016

Mon. Not. R. Astron. Soc.

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In this work we present a method to extract the signal induced by the integrated Sachs-Wolfe (ISW) effect in the cosmic microwave background (CMB). It makes use of the Linear Covariance-Based filter introduced by Barreiro et al., and combines CMB data with any number of large-scale structure (LSS) surveys and lensing information. It also exploits CMB polarization to reduce cosmic variance. The performance of the method has been thoroughly tested with simulations taking into account the impact of non-ideal conditions such as incomplete sky coverage or the presence of noise. In particular, three galaxy surveys are simulated, whose redshift distributions peak at low (z 0.3), intermediate (z 0.6) and high redshift (z 0.9). The contribution of each of the considered data sets as well as the effect of a mask and noise in the reconstructed ISW map is studied in detail. When combining all the considered data sets (CMB temperature and polarization, the three galaxy surveys and the lensing map), the proposed filter successfully reconstructs a map of the weak ISW signal, finding a perfect correlation with the input signal for the ideal case and around 80 per cent, on average, in the presence of noise and incomplete sky coverage. We find that including CMB polarization improves the correlation between input and reconstruction although only at a small level. Nonetheless, given the weakness of the ISW signal, even modest improvements can be of importance. In particular, in realistic situations, in which less information is available from the LSS tracers, the effect of including polarisation is larger. For instance, for the case in which the ISW signal is recovered from CMB plus only one survey, and taking into account the presence of noise and incomplete sky coverage, the improvement in the correlation coefficient can be as large as 10 per cent.

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“…For examples, the WMAP and Planck CMB data show the so-called large-scale anomalies, such as the low quadrupole, a hemispherical power asymmetry, and a remarkable alignment of the quadrupole and octupole, although the evidences for these anomalies are not statistically significant [5][6][7]. In addition, the combined Planck, BICEP2, and large-scale-structure data prefer, though not yet confirmed, a slightly negative running in the spectral index [4,8], which is unexpected in the standard slow-roll inflation model.…”

Section: Introductionmentioning

confidence: 99%

Inflaton fluctuations in the presence of cosmological defects

Cho

Wang

2014

J. Cosmol. Astropart. Phys.

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We study quantum fluctuations of a free massless scalar field during inflation in the presence of a point, line, or plane defect such as a black hole, cosmic string, or domain wall, using a perturbative expansion in powers of small defect parameters. We provide results for the scalar two-point correlation functions that show explicitly a small violation of translational invariance during inflation.

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NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE ( WMAP ) OBSERVATIONS: FINAL MAPS AND RESULTS

Cited by 2,054 publications

References 112 publications

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

Constraining the cosmic deceleration-acceleration transition with type Ia supernova, BAO/CMB and H(z) data

On the recovery of ISW fluctuations using large-scale structure tracers and CMB temperature and polarization anisotropies

Inflaton fluctuations in the presence of cosmological defects

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