Accelerating Universes With Scaling Dark Matter

Chevallier, M.; Polarski, David

doi:10.1142/s0218271801000822

Cited by 2,121 publications

(2,236 citation statements)

References 11 publications

Supporting

Mentioning

2,160

Contrasting

Unclassified

Order By: Relevance

“…We use a CDM cosmology with a varying dark energy equation of state, where the free parameters are M , B , σ 8 , w 0 , w a , h, n s (respectively the dimensionless matter density; dimensionless baryon density; the amplitude of matter fluctuations on 8 h −1 Mpc scales -a normalization of the power spectrum of matter perturbation; the dark energy equation of state parametrized by w(z) = w 0 + w a z/(1 + z) (Chevallier & Polarski 2001); the Hubble parameter h = H 0 /100 km s −1 Mpc −1 ; and the scalar spectral index of initial matter perturbations). For each parameter, we use the Planck maximum likelihood values (Planck Collaboration XVI 2014) about which we take derivatives of the power spectra for the Fisher matrix and bias vector.…”

Section: Prediction Methodsmentioning

confidence: 99%

On scale-dependent cosmic shear systematic effects

Kitching

Taylor

Cropper

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

In this paper we investigate the impact that realistic scale-dependence systematic effects may have on cosmic shear tomography. We model spatially varying residual ellipticity and size variations in weak lensing measurements and propagate these through to predicted changes in the uncertainty and bias of cosmological parameters. We show that the survey strategy -whether it is regular or randomised -is an important factor in determining the impact of a systematic effect: a purely randomised survey strategy produces the smallest biases, at the expense of larger parameter uncertainties, and a very regularised survey strategy produces large biases, but unaffected uncertainties. However, by removing, or modelling, the affected scales (ℓ-modes) in the regular cases the biases are reduced to negligible levels. We find that the integral of the systematic power spectrum is not a good metric for dark energy performance, and we advocate that systematic effects should be modelled accurately in real space, where they enter the measurement process, and their effect subsequently propagated into power spectrum contributions.

show abstract

Section: Prediction Methodsmentioning

confidence: 99%

On scale-dependent cosmic shear systematic effects

Kitching

Taylor

Cropper

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…A more useful two-parameter model (Chevallier and Polarski, 2001;Linder, 2003a) is w(a) = w 0 + w a (1 − a),…”

Section: Model Parameterizationsmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

View full text Add to dashboard Cite

The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

show abstract

“…The second one is the Chevalier-Polarski-Linder (CPL) parametric model [3], one of most studied in the literature.…”

Section: Dark Energy Modelsmentioning

confidence: 99%

“…Since the DM and DE origins remain unknown, a coupling in the dark sector can not be discarded and it constitutes another appealing hypothesis to alleviate the cosmological constant problem. In this paper, we will use the nonextensive Tsallis' statistics in order to investigate the Barboza-Alcaniz [2] and Chevalier-Polarski-Linder [3] time-dependent parametric models of DE and the WangMeng [4] and Dalal [5] vacuum decay models.…”

Section: Introductionmentioning

confidence: 99%

Dark energy models through nonextensive Tsallis’ statistics

Barboza

Nunes

Abreu

et al. 2015

Physica A: Statistical Mechanics and its Applications

105

View full text Add to dashboard Cite

The accelerated expansion of the Universe is one of the greatest challenges of modern physics. One candidate to explain this phenomenon is a new field called dark energy. In this work we have used the Tsallis nonextensive statistical formulation of the Friedmann equation to explore the BarbozaAlcaniz and Chevalier-Polarski-Linder parametric dark energy models and the Wang-Meng and Dalal vacuum decay models. After that, we have discussed the observational tests and the constraints concerning the Tsallis nonextensive parameter.PACS numbers: 98.80. Es, 98.80.Jk

show abstract

Accelerating Universes With Scaling Dark Matter

Cited by 2,121 publications

References 11 publications

On scale-dependent cosmic shear systematic effects

On scale-dependent cosmic shear systematic effects

Observational probes of cosmic acceleration

Dark energy models through nonextensive Tsallis’ statistics

Contact Info

Product

Resources

About