Constraints on the redshift dependence of the dark energy potential

Simón, Joan; Verde, Licia; Jiménez, Raúl

doi:10.1103/physrevd.71.123001

Cited by 1,168 publications

(1,434 citation statements)

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“…We re-analyzed our data estimating the Hubble parameter from the upper envelope of the D4000 n − z relation. This approach has been already applied in the literature [12,82], and probing only the oldest galaxy population at each redshift it should provide an estimate of H(z) as close as possible to the unbiased one. We have considered the following mass ranges: log(M/M ⊙ ) > 11.25 for SDSS MGS, 11.65 < log(M/M ⊙ ) < 11.9 for LRGs, and log(M/M ⊙ ) > 10.6 for z > 0.4; these mass ranges are defined so that there is no strong median mass evolution in each subsamples along the spanned redshift range.…”

Section: A1 Estimating the Effect Of The Progenitor-bias On H(z)mentioning

confidence: 99%

“…Compared to other approaches based on the global spectral or photometric analysis [11,12,[18][19][20][21], it has been found that one of the most direct and solid ways of doing this is to use the 4000Å break (hereafter D4000) in ETG spectra, thanks to its linear dependence on age for old stellar populations [7]. This break is a discontinuity of the spectral continuum around λ rest = 4000Å due to metal absorption lines whose amplitude correlates linearly with the age and metal abundance (metallicity, Z) of the stellar population (in some age and metallicity ranges), that is weakly dependent (for old passive stellar populations) on star formation history (SF H), and basically not affected by dust reddening [7,[22][23][24] (see also Sect.…”

Section: Contents 1 Introductionmentioning

confidence: 99%

“…The differential aging of cosmic chronometers has been used to measure the observed Hubble parameter [18,19], to set constraints on the nature of dark energy [18][19][20], and most recently to provide two new estimates of the Hubble parameter (even if with large errorbars) H(z ∼ 0.5) = 97 ± 62 km s −1 Mpc −1 and H(z ∼ 0.9) = 90 ± 40 km s −1 Mpc −1 [12], and to recover the local Hubble constant [7].…”

Section: Contents 1 Introductionmentioning

confidence: 99%

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Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Moresco

Cimatti

Jiménez

et al. 2012

J. Cosmol. Astropart. Phys.

730

365

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Abstract. We present new improved constraints on the Hubble parameter H(z) in the redshift range 0.15 < z < 1.1, obtained from the differential spectroscopic evolution of early-type galaxies as a function of redshift. We extract a large sample of early-type galaxies (∼ 11000) from several spectroscopic surveys, spanning almost 8 billion years of cosmic lookback time (0.15 < z < 1.42). We select the most massive, red elliptical galaxies, passively evolving and without signature of ongoing star formation. Those galaxies can be used as standard cosmic chronometers, as firstly proposed by Jimenez & Loeb (2002), whose differential age evolution as a function of cosmic time directly probesWe analyze the 4000Å break (D4000) as a function of redshift, use stellar population synthesis models to theoretically calibrate the dependence of the differential age evolution on the differential D4000, and estimate the Hubble parameter taking into account both statistical and systematical errors.We provide 8 new measurements of H(z) (see Tab. 4), and determine its change in H(z) to a precision of 5 − 12% mapping homogeneously the redshift range up to z ∼ 1.1; for the first time, we place a constraint on H(z) at z = 0 with a precision comparable with the one achieved for the Hubble constant (about 5-6% at z ∼ 0.2), and covered a redshift range (0.5 < z < 0.8) which is crucial to distinguish many different quintessence cosmologies.These measurements have been tested to best match a ΛCDM model, clearly providing a statistically robust indication that the Universe is undergoing an accelerated expansion. This method shows the potentiality to open a new avenue in constrain a variety of alternative cosmologies, especially when future surveys (e.g. Euclid) will open the possibility to extend it up to z ∼ 2.-1 -

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Section: A1 Estimating the Effect Of The Progenitor-bias On H(z)mentioning

confidence: 99%

Section: Contents 1 Introductionmentioning

confidence: 99%

Section: Contents 1 Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Moresco

Cimatti

Jiménez

et al. 2012

J. Cosmol. Astropart. Phys.

730

365

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“…We use the following datasets: a) observations of type Ia supernovae from the Joint Lightcurve Analysis (JLA) of the Sloan Digital Sky Survey (SDSS-II) and the Supernova Legacy Survey (SNLS) samples [12]; b) observations of baryon acoustic oscillations in the SDSS DR7 [13] and SDSS DR9 [14], in the WiggleZ Survey [15] and in the 6dF Galaxy Survey (6dFGRS) [16]; c) measurements of cosmic microwave background temperature anisotropy from 2015 Planck [17] and WMAP9-year [18]; d) observations of the Hubble rate H(z) from [19][20][21][22][23][24]. In the following subsections, the statistical analysis used to deal with those observables is briefly described.…”

Section: Observational Datamentioning

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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“…[15] it was used the recently published Hubble function H(z) data [Simon, Verde and Jimenez (SVJ)] [16], extracted from differential ages of passively evolving galaxies. This is interesting for, among other reasons, the function is not integrated over, in contrast to standard candle luminosity distances or standard ruler angular diameter distances.…”

Section: Observational Constraintsmentioning

confidence: 99%

Unified model of baryonic matter and dark components

Chimento

Forte

2008

Physics Letters B

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Editor: M. Cvetič We investigate an interacting two-fluid cosmological model and introduce a scalar field representation by means of a linear combination of the individual energy densities. Applying the integrability condition to the scalar field equation we show that this "exotic quintessence" is driven by an exponential potential and the two-fluid mixture can be considered as a model of three components. These components are associated with baryonic matter, dark matter and dark energy respectively. We use the Simon, Verde and Jimenez [J. Simon, L. Verde, R. Jimenez, Phys. Rev. D 71 (2005) 123001] determination of the redshift dependence of the Hubble parameter to constrain the current density parameters of this model. With the best fit density parameters we obtain the transition redshift between non-accelerated and accelerated regimes z acc = 0.66 and the time elapsed since the initial singularity t 0 = 19.8 Gyr. We study the perturbation evolution of this model and find that the energy density perturbation decreases with the cosmological time.

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Constraints on the redshift dependence of the dark energy potential

Cited by 1,168 publications

References 48 publications

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

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

Unified model of baryonic matter and dark components

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