Constraints on the Dark Side of the Universe and Observational Hubble Parameter Data

Zhang, Tong-Jie; Ma, Cong; Lan, Tian

doi:10.1155/2010/184284

Cited by 70 publications

(57 citation statements)

References 142 publications

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“…In the future, with the developments in the observational technique of LRGs, the H(z) measurements can provide useful complements to other cosmic observations [459,460].…”

Section: Hubble Parameter Measurementsmentioning

confidence: 99%

Dark Energy

Li¹,

Li²,

Wang³

et al. 2011

Commun. Theor. Phys.

753

560

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“…In the future, with the developments in the observational technique of LRGs, the H(z) measurements can provide useful complements to other cosmic observations [459,460].…”

Section: Hubble Parameter Measurementsmentioning

confidence: 99%

Dark Energy

Li¹,

Li²,

Wang³

et al. 2011

Commun. Theor. Phys.

753

560

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show abstract

“…The two main methods to measure the Hubble parameter as a function of redshift, H(z), are the differential age method and the radial BAO size method. For review, including a discussion on systematic uncertainties and possible source of errors, see [36]. The differential age method has been proposed in [37].…”

Section: H(z)mentioning

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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“…The metric for a space-time with homogeneous and isotropic sections is the maximally-symmetric Robertson-Walker (RW) metric [9], which can be written in the form…”

Section: Hubble Parameter In Perturbed Universementioning

confidence: 99%

“…Recently, the Hubble parameter has been widely used to constrain the cosmological parameters, such as dark energy, dark matter, and dark age [9,10].…”

Section: Introductionmentioning

confidence: 99%

Fluctuation of the Hubble parameter

Li¹,

Qin²,

Zhang³

et al. 2015

Phys. Rev. D

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We study the Hubble parameter $H(z)$ in perturbed Friedmann universe and obtain an expression of the perturbed Hubble parameter $H(z,\textbf{n})$. We derive the Hubble parameter power spectrum by using the initial spectrum during inflation and the Bardeen transfer function. We obtain a semi-analytical expression in the case of cold dark matter (CDM) universe. Similar with luminosity distance, the Hubble parameter spectrum is suggested to be an useful observational tool to determine some cosmological parameters. In addition, we show that the Hubble parameter power spectrum could be used to check whether the expansion is accelerated by the second order small scale fluctuation.Comment: 13 pages, 9 figures, accepted for publication PR

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Constraints on the Dark Side of the Universe and Observational Hubble Parameter Data

Cited by 70 publications

References 142 publications

Dark Energy

Dark Energy

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

Fluctuation of the Hubble parameter

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