Late time transitions in the quintessence field and the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline" id="d1e6133" altimg="si2.svg"><mml:msub><mml:mrow><mml:mi mathvariant="bold-italic">H</mml:mi></mml:mrow><mml:mrow><mml:mi mathvariant="bold">0</mml:mi></mml:mrow></mml:msub></mml:math> tension

Valentino, Eleonora Di; Ferreira, Ricardo Z.; Visinelli, Luca; Danielsson, Ulf H.

doi:10.1016/j.dark.2019.100385

Cited by 72 publications

(25 citation statements)

References 76 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…33 Due to this early dark energy-like behaviour, pseudo-scalars are often invoked when building models of quintessence [174][175][176] and inflation [177,178]. 34 The code is available as a Mathematica package at the GIT repository https://github.com/lucavisinelli.…”

Section: Vacuum Realignment Mechanismmentioning

confidence: 99%

“…In models where a direct coupling between axion and top quarks exists, the efficiency of the thermal production is enhanced by up to three orders of magnitude [316]. More generally, a direct coupling of the axion to quarks and leptons leads to significant enhancements in ∆N eff [313,318], which might even alleviate the tension between the local direct measurement of H 0 and the model-dependent value of H 0 inferred from the CMBR [176,312], which is currently existing between CMBR [238] and Supernovae measurements [319][320][321]. A prediction for ∆N eff is also useful to set a target for future CMB-S4 surveys [288].…”

Section: Qcd Axions As Dark Radiationmentioning

confidence: 99%

See 1 more Smart Citation

The landscape of QCD axion models

et al. 2020

Self Cite

View full text Add to dashboard Cite

show abstract

Section: Vacuum Realignment Mechanismmentioning

confidence: 99%

Section: Qcd Axions As Dark Radiationmentioning

confidence: 99%

The landscape of QCD axion models

et al. 2020

Self Cite

View full text Add to dashboard Cite

show abstract

“…There are many attempts to alleviate the issue in the literature (see for an incomplete list of works Refs. [ 36 , 37 , 38 , 39 , 40 , 41 , 42 , 43 , 44 , 45 , 46 , 47 , 48 , 49 , 50 , 51 , 52 , 53 , 54 , 55 , 56 , 57 , 58 , 59 , 60 , 61 , 62 , 63 , 64 , 65 , 66 , 67 , 68 , 69 , 70 , 71 , 72 , 73 , 74 , 75 , 76 , 77 , 78 ] and the recent overview in [ 79 , 80 ]). It has been recently discussed [ 81 , 82 ] that a transition in absolute magnitude

for SnIa can also explain the apparent tension between the local and CMB measurements of the Hubble parameter

.…”

Section: Introductionmentioning

confidence: 99%

Dark Energy with Phantom Crossing and the H0 Tension

Valentino

Mukherjee

Sen

2021

Entropy

Self Cite

113

View full text Add to dashboard Cite

We investigate the possibility of phantom crossing in the dark energy sector and the solution for the Hubble tension between early and late universe observations. We use robust combinations of different cosmological observations, namely the Cosmic Microwave Background (CMB), local measurement of Hubble constant (H0), Baryon Acoustic Oscillation (BAO) and SnIa for this purpose. For a combination of CMB+BAO data that is related to early universe physics, phantom crossing in the dark energy sector was confirmed at a 95% confidence level and we obtained the constraint H0=71.0−3.8+2.9 km/s/Mpc at a 68% confidence level, which is in perfect agreement with the local measurement by Riess et al. We show that constraints from different combinations of data are consistent with each other and all of them are consistent with phantom crossing in the dark energy sector. For the combination of all data considered, we obtained the constraint H0=70.25±0.78 km/s/Mpc at a 68% confidence level and the phantom crossing happening at the scale factor am=0.851−0.031+0.048 at a 68% confidence level.

show abstract

“…For example, the value of the Hubble constant H 0 predicted by the cosmic microwave background (CMB) Planck data [2,5] within the framework of the standard CDM model is in serious disagreement with the direct local distance ladder measurements [23][24][25][26]. This tension becomes even more compelling as it worsens (relieves only partially) when the is replaced by the simplest minimally coupled single-field quintessence (phantom or quintom models), see [27][28][29][30] and [31] for further references. Surprisingly, it has been reported that the H 0 tension -as well as a number of other persistent low-redshift tensions -may be alleviated by a dynamical dark energy (DE) whose density can assume negative values or vanish at high redshifts [31][32][33][34][35][36][37][38][39][40][41][42][43][44].…”

Section: Introductionmentioning

confidence: 99%

Rastall gravity extension of the standard $$\Lambda $$CDM model: theoretical features and observational constraints

et al. 2020

View full text Add to dashboard Cite

We present a detailed investigation of the Rastall gravity extension of the standard $$\Lambda $$ Λ CDM model. We review the model for two simultaneous modifications of different nature in the Friedmann equation due to the Rastall gravity: the new contributions of the material (actual) sources (considered as effective source) and the altered evolution of the material sources. We discuss the role/behavior of these modifications with regard to some low redshift tensions, including the so-called $$H_0$$ H 0 tension, prevailing within the standard $$\Lambda $$ Λ CDM. We constrain the model at the level of linear perturbations, and obtain the first constraints through a robust and accurate analysis using the latest full Planck cosmic microwave background (CMB) data, with and without including baryon acoustic oscillations (BAO) data. We find that the Rastall parameter $$\epsilon $$ ϵ (null for general relativity) is consistent with zero at 68% CL (with a tendency towards positive values, $$-0.0001< \epsilon < 0.0007$$ - 0.0001 < ϵ < 0.0007 (CMB+BAO) at 68% CL), which in turn implies no significant statistical evidence for deviation from general relativity, and also a precision of $$\mathcal {O}(10^{-4})$$ O ( 10 - 4 ) for the coefficient $$-1/2$$ - 1 / 2 of the term $$g_{\mu \nu }R$$ g μ ν R in the Einstein field equations of general relativity (guaranteeing the local energy-momentum conservation). We explore the consequences led by the Rastall gravity on the cosmological parameters in the light of the observational analyses. It turns out that the effective source, with a present-day density parameter $$\Omega _\mathrm{X0}=-0.0010\pm 0.0013$$ Ω X 0 = - 0.0010 ± 0.0013 (CMB+BAO, 68% CL), dynamically screens the usual vacuum energy at high redshifts, but this mechanism barely works due to the opposition by the altered evolution of cold dark matter. Consequently, two simultaneous modifications of different nature in the Friedmann equation by the Rastall gravity act against each other, and do not help to considerably relax the low redshift tensions, including the so-called $$H_0$$ H 0 tension. Our results may offer a guide for the research community that studies the Rastall gravity in various aspects of gravitation and cosmology.

show abstract

Late time transitions in the quintessence field and the H0 tension

Cited by 72 publications

References 76 publications

The landscape of QCD axion models

The landscape of QCD axion models

Dark Energy with Phantom Crossing and the H0 Tension

Rastall gravity extension of the standard $$\Lambda $$CDM model: theoretical features and observational constraints

Contact Info

Product

Resources

About