The Anisotropy of the Microwave Background to<i>l</i>= 3500: Mosaic Observations with the Cosmic Background Imager

Pearson, T. J.; Mason, B. S.; Readhead, A. C. S.; Shepherd, M. C.; Sievers, Jonathan; Udomprasert, P. S.; Cartwright, J. K.; Farmer, Alison J.; Padin, S.; Myers, Steven T.; Bond, J. R.; Contaldi, C. R.; Pen, Ue-Li; Prunet, S.; Pogosyan, D.; Carlstrom, J. E.; Kovac, J. M.; Leitch, E. M.; Pryke, C.; Halverson, N. W.; Holzapfel, W. L.; Altamirano, Pablo; Bronfman, L.; Casassus, S.; May, J.; Joy, M.

doi:10.1086/375508

Cited by 265 publications

(163 citation statements)

References 23 publications

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“…The observational results of CMB experiments correspond to a shift parameter of R = 1.716 ± 0.062 (given by WMAP, CBI, ACBAR) [5,69]. One of the advantages of using the parameter R is that it is independent of Hubble constant.…”

Section: Observational Constraints From the Background Evolutionmentioning

confidence: 94%

Observational Constraints with Recent Data on the DGP Modified Gravity

2008

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We study one of the simplest covariant modified-gravity models based on the Dvali-Gabadadze-Porrati (DGP) brane cosmology, a self-accelerating universe. In this model gravitational leakage into extra dimensions is responsible of late-time acceleration. We mainly focus on the effects of the model parameters on the geometry and the age of universe. Also we investigate the evolution of matter density perturbations in the modified gravity model, and obtain an analytical expression for the growth index, f . We show that increasing Ωr c leads to less growth of the density contrast δ, and also decreases the growth index. We give a fitting formula for the growth index at the present time and indicate that dominant term in this expression verifies the well-known approximation relation f ≃ Ω γ m . As the observational test, the new Supernova Type Ia (SNIa) Gold sample and Supernova Legacy Survey (SNLS) data, size of baryonic acoustic peak from Sloan Digital Sky Survey (SDSS), the position of the acoustic peak from the CMB observations and the Cluster Baryon Gas Mass Fraction (gas) are used to constrain the parameters of the DGP model. We also combine previous results with large scale structure formation (LSS) from the 2dFGRS survey. Finally to check the consistency of the DGP model, we compare the age of old cosmological objects with age of universe in this model.

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Section: Observational Constraints From the Background Evolutionmentioning

confidence: 94%

Observational Constraints with Recent Data on the DGP Modified Gravity

2008

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“…Recently, Spergel et al (2003) combined CMB measurements from the Wilkinson Microwave Anisotropy Probe (WMAP; Bennett et al 2003 and references therein), the Cosmic Background Imager (CBI; Pearson et al 2003), and the Arcminute Cosmology Bolometer Array Receiver (ACBAR; Kuo et al 2002), the galaxy power spectrum from the Two Degree Field (2dF) Galaxy Redshift Survey (Percival et al 2001;Verde et al 2002), and the measurements of the Lyman power spectrum (Croft et al 2002;Gnedin & Hamilton 2002) to find the best-fit cosmological model and obtained 8 ¼ 0:84 AE 0:04 (68% confidence). This result is in good agreement with our cosmic shear constraints.…”

Section: No 1 2003 Cosmic Shear Statistics With Suprime-cammentioning

confidence: 99%

Cosmic Shear Statistics in the Suprime‐Cam 2.1 Square Degree Field: Constraints on Ω_mand σ₈

Hamana¹,

Miyazaki²,

Shimasaku³

et al. 2003

ApJ

110

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We present measurements of the cosmic shear correlation in the shapes of galaxies in the Suprime-Cam 2.1 deg 2 R C -band imaging data. As an estimator of the shear correlation originating from the gravitational lensing, we adopt the aperture mass variance, which most naturally decomposes the correlation signal into E and B (non-gravitational lensing) modes. We detect a nonzero E mode variance on scales between ap ¼ 2 0 and 40 0 . We also detect a small but nonzero B-mode variance on scales larger than ap > 5 0 . We compare the measured E-mode variance to the model predictions in CDM cosmologies using maximum likelihood analysis. A four-dimensional space is explored, which examines 8 , m , C (the shape parameter of the CDM power spectrum), and " z z s (mean redshift of galaxies). We include three possible sources of error: statistical noise, the cosmic variance estimated using numerical experiments, and a residual systematic effect estimated from the B-mode variance. We derive joint constraints on two parameters by marginalizing over the two remaining parameters. We obtain an upper limit of À < 0:5 for " z z s > 0:9 (68% confidence). For a prior À 2 ½0:1; 0:4 and " z z s 2 ½0:6; 1:4 , we find 8 , we obtain a onedimensional confidence interval on 8 for the 95.4% level, 0:62 < 8 < 1:32 for " z z s 2 ½0:6; 1:4 . Information on the redshift distribution of galaxies is key to obtaining a correct cosmological constraint. An independent constraint on C from other observations is useful to tighten the constraint.

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“…Since the CMB is imprinted at a rather late time in our early cosmic history, at z > ∼ 10 5 , for comparing to the data, it suffices to consider a universe containing only baryons, CDM, photons, neutrinos and a cosmological constant Λ. This seems to be the minimal physics at the relevant energy scales required to account for the present observations.…”

Section: Introductionmentioning

confidence: 99%

“…These models may be compared to the WMAP data [1,2], extended to smaller angular scales by including data from the ACBAR [3], BOOMERANG [4], CBI [5] and VSA [6] experiments and LSS data from the 2dF galaxy redshift survey (2dFGRS), [7]. The analysis by the WMAP team indicates a good fit to a model of this sort with the following best-fit parameter choices: Ω Λ = 0.74, Ω b = 0.043, h = 0.73, τ = 0.15 [8].…”

Section: Introductionmentioning

confidence: 99%

Constraints on isocurvature models from the WMAP first-year data

et al. 2004

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We investigate the constraints imposed by the first-year WMAP CMB data extended to higher multipole by data from ACBAR, BOOMERANG, CBI and the VSA and by the LSS data from the 2dF galaxy redshift survey on the possible amplitude of primordial isocurvature modes. A flat universe with CDM and Λ is assumed, and the baryon, CDM (CI), and neutrino density (NID) and velocity (NIV) isocurvature modes are considered. Constraints on the allowed isocurvature contributions are established from the data for various combinations of the adiabatic mode and one, two, and three isocurvature modes, with intermode cross-correlations allowed. Since baryon and CDM isocurvature are observationally virtually indistinguishable, these modes are not considered separately. We find that when just a single isocurvature mode is added, the present data allows an isocurvature fraction as large as 13 ± 6, 7 ± 4, and 13 ± 7 percent for adiabatic plus the CI, NID, and NIV modes, respectively. When two isocurvature modes plus the adiabatic mode and crosscorrelations are allowed, these percentages rise to 47 ± 16, 34 ± 12, and 44 ± 12 for the combinations CI+NID, CI+NIV, and NID+NIV, respectively. Finally, when all three isocurvature modes and cross-correlations are allowed, the admissible isocurvature fraction rises to 57 ± 9 per cent. The sensitivity of the results to the choice of prior probability distribution is examined.

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The Anisotropy of the Microwave Background tol= 3500: Mosaic Observations with the Cosmic Background Imager

Cited by 265 publications

References 23 publications

Observational Constraints with Recent Data on the DGP Modified Gravity

Observational Constraints with Recent Data on the DGP Modified Gravity

Cosmic Shear Statistics in the Suprime‐Cam 2.1 Square Degree Field: Constraints on Ω_mand σ₈

Constraints on isocurvature models from the WMAP first-year data

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The Anisotropy of the Microwave Background tol= 3500: Mosaic Observations with the Cosmic Background Imager

Cited by 265 publications

References 23 publications

Observational Constraints with Recent Data on the DGP Modified Gravity

Observational Constraints with Recent Data on the DGP Modified Gravity

Cosmic Shear Statistics in the Suprime‐Cam 2.1 Square Degree Field: Constraints on Ωmand σ8

Constraints on isocurvature models from the WMAP first-year data

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Product

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Cosmic Shear Statistics in the Suprime‐Cam 2.1 Square Degree Field: Constraints on Ω_mand σ₈