How the dark energy can reconcile Planck with local determination of the Hubble constant

Huang, Qing-Guo; Wang, Ke

doi:10.1140/epjc/s10052-016-4352-x

Cited by 96 publications

(60 citation statements)

References 29 publications

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“…It is important to stress that w is strongly correlated with H 0 ; see the triangular plots in Appendix B. More precisely, the high value of H R18 0 pushes w towards (somehow troubling) phantom values; in other words, the wCDM model can alleviate the tension between global and local determination of the Hubble constant [1, 11,16].…”

Section: B Wcdm Parametrizationmentioning

confidence: 99%

Impact of the cosmic variance on H0 on cosmological analyses

Camarena

Marra

2018

Phys. Rev. D

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The current 3.8σ tension between local [1] and global [2] measurements of H0 cannot be fully explained by the concordance ΛCDM model. It could be produced by unknown systematics or by physics beyond the standard model. In particular, non-standard dark energy models were shown to be able to alleviate this tension. On the other hand, it is well known that linear perturbation theory predicts a cosmic variance on the Hubble parameter H0, which leads to systematic errors on its local determination. Here, we study how including in the likelihood the cosmic variance on H0 affects statistical inference. In particular we consider the γCDM, wCDM and γwCDM parametric extensions of the standard model, which we constrain with the latest CMB, BAO, SNe Ia, RSD and H0 data. We learn two important lessons. First, the systematic error from cosmic variance is -independently of the model -approximately σcv ≈ 0.88 km s −1 Mpc −1 (1.2% H loc 0 ) when considering the redshift range 0.0233 ≤ z ≤ 0.15, which is relative to the main analysis of [1], and σcv ≈ 1.5 km s −1 Mpc −1 (2.1% H loc 0 ) when considering the wider redshift range 0.01 ≤ z ≤ 0.15. Although σcv affects the total error budget on local H0, it does not significantly alleviate the tension which remains at ≈ 3σ. Second, cosmic variance, besides shifting the constraints, can change the results of model selection: much of the statistical advantage of non-standard models is to alleviate the now-reduced tension. We conclude that, when constraining non-standard models it is important to include the cosmic variance on H0 if one wants to use the local determination of the Hubble constant by Riess et al. [1]. Doing the contrary could potentially bias the conclusions.

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Section: B Wcdm Parametrizationmentioning

confidence: 99%

Impact of the cosmic variance on H0 on cosmological analyses

Camarena

Marra

2018

Phys. Rev. D

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“…This could bring the Planck constraint into better agreement with higher values of the Hubble constant. By varying both parameters simultaneously, it has been shown that there is no privilege for dark radiation if allowance is made for dynamical dark energy Di Valentino et al (2016bValentino et al ( , 2017b; Huang & Wang (2016); Zhao et al (2017). Phantom energy can be shown to also ameliorate the age conflict Cepa (2004).…”

Section: Introductionmentioning

confidence: 99%

H ₀ Tension and the Phantom Regime: A Case Study in Terms of an Infrared f(T) Gravity

El-Zant

Hanafy

Elgammal

2019

ApJ

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We propose an f (T ) teleparallel gravity theory including a torsional infrared (IR) correction. We show that the governing Friedmann's equations of a spatially flat universe include a phantom-like effective dark energy term sourced by the torsion IR correction. As has been suggested, this phantom phase does indeed act as to reconcile the tension between local and global measurements of the current Hubble value H 0 . The resulting cosmological model predicts an electron scattering optical depth τ e ≈ 0.058 at reionization redshift z re ∼ 8.1, in agreement with observations. The predictions are however in contradiction with baryon acoustic oscillations (BAO) measurements, particularly the distance indicators. We argue that this is the case with any model with a phantom dark energy model that has effects significant enough at redshifts z 2 as to be currently observable. The reason being that such a scenario introduces systematic differences in terms of distance estimates in relation to the standard model; e.g., if the angular diameter distance to the recombination era is to be kept constant while H 0 is increased in the context of a phantom scenario, the distances there are systematically overestimated to all objects at redshifts smaller than recombination. But no such discrepancies exist between ΛCDM predictions and current data for z 2.

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“…To avoid the extra effect of the tension on cosmological models, we consider the additional parameter N eff in the cosmological model because the addition of the parameter N eff is considered to be a good scheme to relieve the tension between the direct H 0 measurement and the Planck observation [23,24,[46][47][48][49][50]. In fact, in the literature it is shown that the tension could also be relieved to some extent by considering a dynamical dark energy [51][52][53][54][55] or light sterile neutrinos [47,48,[56][57][58][59][60][61][62][63].…”

Section: Introductionmentioning

confidence: 99%

Constraints on brane inflation after Planck 2015: Impacts of the latest local measurement of the Hubble constant

Guo

Zhang

et al. 2018

Sci. China Phys. Mech. Astron.

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We investigate the observational constraints on three typical brane inflation models by considering the latest local measurement of the Hubble constant in the global fit. We also employ other observational data, including the Planck 2015 CMB data, the BICEP2/Keck Array B-mode data, and the baryon acoustic oscillations data, in our analysis. Previous studies have shown that the addition of the latest local H0 measurement favors a larger spectral index, and can exert a significant influence on the model selection of inflation. In this work, we investigate its impacts on the status of brane inflation models. We find that, when the direct H0 measurement is considered, the prototype model of brane inflation is still in good agreement with the current observational data within the 2σ level range. For the KKLMMT model, the consideration of the H0 measurement allows the range of the parameter β to be amplified to O(10 −2 ), which slightly alleviates the fine-tuning problem.For the IR DBI model, the addition of the H0 measurement does not provide a better fit. These results show that the consideration of the new H0 prior can exert a considerable influence on the brane inflation models. At last, we show that, when β 1.1, the equilateral non-Gaussianity in the IR DBI inflation model is compatible with the current CMB data at the 1σ level.

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How the dark energy can reconcile Planck with local determination of the Hubble constant

Abstract: We try to reconcile the tension between the local 2.4 % determination of Hubble constant and its global determination by Planck CMB data and BAO data through modeling the dark energy variously. We find that the chi-

Cited by 96 publications

References 29 publications

Impact of the cosmic variance on H0 on cosmological analyses

Impact of the cosmic variance on H0 on cosmological analyses

H ₀ Tension and the Phantom Regime: A Case Study in Terms of an Infrared f(T) Gravity

Constraints on brane inflation after Planck 2015: Impacts of the latest local measurement of the Hubble constant

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How the dark energy can reconcile Planck with local determination of the Hubble constant

Abstract: We try to reconcile the tension between the local 2.4 % determination of Hubble constant and its global determination by Planck CMB data and BAO data through modeling the dark energy variously. We find that the chi-

Cited by 96 publications

References 29 publications

Impact of the cosmic variance on H0 on cosmological analyses

Impact of the cosmic variance on H0 on cosmological analyses

H 0 Tension and the Phantom Regime: A Case Study in Terms of an Infrared f(T) Gravity

Constraints on brane inflation after Planck 2015: Impacts of the latest local measurement of the Hubble constant

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H ₀ Tension and the Phantom Regime: A Case Study in Terms of an Infrared f(T) Gravity