A 2 per cent distance to<i>z</i>= 0.35 by reconstructing baryon acoustic oscillations – III. Cosmological measurements and interpretation

Mehta, Kushal; Cuesta, Antonio J.; Xu, Xiaoying; Eisenstein, Daniel J.; Padmanabhan, Nikhil

doi:10.1111/j.1365-2966.2012.21112.x

Cited by 57 publications

(52 citation statements)

References 90 publications

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“…This correction is sufficiently accurate over the range of ω m and ω b allowed by the CMB in the base ΛCDM cosmology (see e.g. Mehta et al 2012) and also for the extended ΛCDM models discussed in Sect. 6.…”

Section: Baryon Acoustic Oscillationsmentioning

confidence: 83%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

4,999

163

2,253

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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: Baryon Acoustic Oscillationsmentioning

confidence: 83%

Planck2013 results. XVI. Cosmological parameters

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

4,999

163

2,253

View full text Add to dashboard Cite

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“…We show in Figure 11 a comparison of the cosmological constraints of the two lenses, BAOs (e.g., Percival et al 2010;Blake et al 2011;Mehta et al 2012), and supernovae (SN; e.g., Hicken et al 2009;Suzuki et al 2012), when each is combined with WMAP7 in the owCDM cosmology. The figures are qualitative since the samples for WMAP7 chain in the owCDM cosmology are sparse and we have smoothed the contours after importance sampling.…”

Section: Comparison Of Lenses and Other Cosmographic Probesmentioning

confidence: 99%

“…In Figure 12, we compare the precisions on Ω k and w in owCDM from the following cosmological probes in combination with WMAP: BAO from the Sloan Digital Sky Survey (SDSS; Percival et al 2010), our two time-delay lenses, SN from the Union 2.1 sample (Suzuki et al 2012), the Cepheids distance ladder (Riess et al 2011), 19 and reconstructed BAO using the SDSS galaxies (Mehta et al 2012). We note that the precisions on the Cepheids and the time-delay lenses are only approximates since the samples of WMAP7 are sparse in owCDM due 19 To derive the constraints on Ω k and w from the combination of Cepheids and WMAP7, we sample the WMAP7 chain by a Gaussian likelihood centered on H 0 = 73.…”

Section: Comparison Of Lenses and Other Cosmographic Probesmentioning

confidence: 99%

Two Accurate Time-Delay Distances From Strong Lensing: Implications for Cosmology

Suyu

Auger

Hilbert

et al. 2013

ApJ

372

553

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Strong gravitational lenses with measured time delays between the multiple images and models of the lens mass distribution allow a one-step determination of the time-delay distance, and thus a measure of cosmological parameters. We present a blind analysis of the gravitational lens RXJ1131−1231 incorporating (1) the newly measured time delays from COSMOGRAIL, the COSmological MOnitoring of GRAvItational Lenses, (2) archival Hubble Space Telescope imaging of the lens system, (3) a new velocity-dispersion measurement of the lens galaxy of 323 ± 20 km s −1 based on Keck spectroscopy, and (4) a characterization of the line-of-sight structures via observations of the lens' environment and ray tracing through the Millennium Simulation. Our blind analysis is designed to prevent experimenter bias. The joint analysis of the data sets allows a time-delay distance measurement to 6% precision that takes into account all known systematic uncertainties. Time-delay lenses constrain especially tightly the Hubble constant H 0 (5.7% and 4.0% respectively in wCDM and open ΛCDM) and curvature of the universe. The overall information content is similar to that of Baryon Acoustic Oscillation experiments. Thus, they complement well other cosmological probes, and provide an independent check of unknown systematics. Our measurement of the Hubble constant is completely independent of those based on the local distance ladder method, providing an important consistency check of the standard cosmological model and of general relativity.

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“…These measurements are therefore analysed separately, for details see Anderson et al (2014). A number of these BAO measurement have been calculated using the approximate fitting formula for rs(z d ) from Eisenstein & Hu (1998); hence throughout, where appropriate, the BAO measurements derived using this approximation are scaled to be consistent with the result from camb (cf., Mehta et al 2012).…”

Section: Baosmentioning

confidence: 99%

Searching for modified gravity: scale and redshift dependent constraints from galaxy peculiar velocities

Johnson

Blake

Dossett

et al. 2016

Mon. Not. R. Astron. Soc.

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We present measurements of both scale-and time-dependent deviations from the standard gravitational field equations. These late-time modifications are introduced separately for relativistic and non-relativistic particles, by way of the parameters G matter (k, z) and G light (k, z) using two bins in both scale and time, with transition wavenumber 0.01 Mpc −1 and redshift 1. We emphasize the use of two dynamical probes to constrain this set of parameters, galaxy power spectrum multipoles and the direct peculiar velocity power spectrum, which probe fluctuations on different scales. The multipole measurements are derived from the WiggleZ and BOSS Data Release 11 CMASS galaxy redshift surveys and the velocity power spectrum is measured from the velocity sub-sample of the 6-degree Field Galaxy Survey. We combine with additional cosmological probes including baryon acoustic oscillations, Type Ia SNe, the cosmic microwave background (CMB), lensing of the CMB, and the temperaturegalaxy cross-correlation. Using a Markov Chain Monte Carlo likelihood analysis, we find the inferred best-fit parameter values of G matter (k, z) and G light (k, z) to be consistent with the standard model at the 95% confidence level. Furthermore, accounting for the Alcock-Paczynski effect, we perform joint fits for the expansion history and growth index gamma; we measure γ = 0.665 ± 0.0669 (68% C.L) for a fixed expansion history, and γ = 0.73 +0.08 −0.10 (68% C.L) when the expansion history is allowed to deviate from ΛCDM. With a fixed expansion history the inferred value is consistent with GR at the 95% C.L; alternatively, a 2σ tension is observed when the expansion history is not fixed, this tension is worsened by the combination of growth and SNe data.

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A 2 per cent distance toz= 0.35 by reconstructing baryon acoustic oscillations – III. Cosmological measurements and interpretation

Cited by 57 publications

References 90 publications

Planck2013 results. XVI. Cosmological parameters

Planck2013 results. XVI. Cosmological parameters

Two Accurate Time-Delay Distances From Strong Lensing: Implications for Cosmology

Searching for modified gravity: scale and redshift dependent constraints from galaxy peculiar velocities

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