Testing power-law cosmology with galaxy clusters

Zhu, Zong-Hong; Hu, Ming-Guang; Alcaniz, J. S.; Liu, Y.-X.

doi:10.1051/0004-6361:20077797

Cited by 47 publications

(33 citation statements)

References 67 publications

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“…Most recent PLANCK evaluate of the Hubble constant gives a value of H 0 = 67.3 ± 1.2 km/s/Mpc [26]. Along with the above mentioned evaluates of H 0 , several other authors, [7], [9][10][11][12][13] obtained the constraints on cosmological parameters including H 0 , q and β for open, closed and flat power law cosmology. Numerical results for flat power-law cosmology have been described in Table 2.…”

Section: Introductionmentioning

confidence: 99%

“…In such a model, the cosmological evolution is explained by the geometrical scale factor a(t) ∝ t β with β as a positive constant. The power law evolution with β ≥ 1 has been discussed at length in a series of articles in distinct contexts [2][3][4][5][6][7][8][9][10]; phantom power-law cosmology is discussed in reference [14]. The motivation for such a scenario comes from a number of considerations.…”

Section: Introductionmentioning

confidence: 99%

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Constraints on cosmological parameters in power-law cosmology

Rani

Altaibayeva

Shahalam

et al. 2015

J. Cosmol. Astropart. Phys.

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Abstract. In this paper, we examine observational constraints on the power law cosmology; essentially dependent on two parameters H 0 (Hubble constant) and q (deceleration parameter). We investigate the constraints on these parameters using the latest 28 points of H(z) data and 580 points of Union2.1 compilation data and, compare the results with the results of ΛCDM. We also forecast constraints using a simulated data set for the future JDEM, supernovae survey. Our studies give better insight into power law cosmology than the earlier done analysis by Kumar [arXiv:1109.6924] indicating it tuning well with Union2.1 compilation data but not with H(z) data. However, the constraints obtained on < H 0 > and < q > i.e. H 0 average and q average using the simulated data set for the future JDEM, supernovae survey are found to be inconsistent with the values obtained from the H(z) and Union2.1 compilation data. We also perform the statefinder analysis and find that the power-law cosmological models approach the standard ΛCDM model as q → −1. Finally, we observe that although the power law cosmology explains several prominent features of evolution of the Universe, it fails in details.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Constraints on cosmological parameters in power-law cosmology

Rani

Altaibayeva

Shahalam

et al. 2015

J. Cosmol. Astropart. Phys.

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“…In Melia (2015) several claims against R h = ct were refuted, and a list of works favouring R h = ct over ΛCDM was compiled in Melia (2017). Power-law cosmologies with n ≥ 1 have been explored against data in several works such as Gehlaut et al (2003), Dev et al (2008), Sethi et al (2005), Zhu et al (2008), Shafer (2015), Rani et al (2015), Dolgov et al (2014), finding n ∼ 1.5 consistently. In a more recent work (Shafer 2015), power-law and R h = ct models were tested with SN Ia and BAO datasets and were found to be highly disfavoured against ΛCDM.…”

Section: Introductionmentioning

confidence: 99%

Strong evidence for an accelerating Universe

Haridasu

Luković

D’Agostino

et al. 2017

A&A

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A recent analysis of supernova Ia (SN Ia) data claims a "marginal" (∼3σ) evidence for a cosmic acceleration. This result has been complemented with a non-accelerating R h = ct cosmology, which was presented as a valid alternative to the ΛCDM model. In this paper we use the same analysis to show that non-marginal evidence for acceleration is truly found. We compare the standard Friedmann models to the R h = ct cosmology by complementing SN Ia data with baryon acoustic oscillations, gamma ray bursts, and observational Hubble datasets. We also study the power-law model, which is a functional generalisation of R h = ct. We find that the evidence for late-time acceleration cannot be refuted at a 4.56σ confidence level from SN Ia data alone, and at an even stronger confidence level (5.38σ) from our joint analysis. In addition, the non-accelerating R h = ct model fails to statistically compare with the ΛCDM, having a ∆(AIC) ∼ 30.

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“…The Hubble parameter and its time derivative are H =ȧ/a = α/t, andḢ = −α/t 2 . The value of α can be evaluated with data from gravitational lensing statistics [113], compact radio source [114], X-ray gas mass fraction measurements of galaxy cluster [115]. Values of α from various observational data are listed in [110].…”

Section: Resultsmentioning

confidence: 99%

Non-minimal derivative coupling gravity in cosmology

Gumjudpai

Rangdee

2015

Gen Relativ Gravit

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We give a brief review of the non-minimal derivative coupling (NMDC) scalar field theory in which there is non-minimal coupling between the scalar field derivative term and the Einstein tensor. We assume that the expansion is of power-law type or super-acceleration type for small redshift. The Lagrangian includes the NMDC term, a free kinetic term, a cosmological constant term and a barotropic matter term. For a value of the coupling constant that is compatible with inflation, we use the combined WMAP9 (WMAP9+eCMB+BAO+ H0) dataset, the PLANCK+WP dataset, and the PLANCK T T, T E, EE+lowP+Lensing+ext datasets to find the value of the cosmological constant in the model. Modeling the expansion with power-law gives a negative cosmological constants while the phantom power-law (super-acceleration) expansion gives positive cosmological constant with large error bar. The value obtained is of the same order as in the ΛCDM model, since at late times the NMDC effect is tiny due to small curvature.

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Testing power-law cosmology with galaxy clusters

Cited by 47 publications

References 67 publications

Constraints on cosmological parameters in power-law cosmology

Constraints on cosmological parameters in power-law cosmology

Strong evidence for an accelerating Universe

Non-minimal derivative coupling gravity in cosmology

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