Larger value for 
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 by an evolving gravitational constant

Braglia, Matteo; Ballardini, M.; Emond, William T.; Finelli⋆, F.; Gümrükçüoğlu, A. Emir; Koyama, K.; Paoletti, D.

doi:10.1103/physrevd.102.023529

Cited by 111 publications

(93 citation statements)

References 69 publications

(131 reference statements)

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“…And Ref. [52] also finds a larger value for H 0 by an evolving gravitational constant. Here, we simply set G as a free parameter in the base CDM model to enlarge the value of H 0 .…”

Section: Introductionmentioning

confidence: 91%

Constraints on Newton’s constant from cosmological observations

Wang

Chen

2020

Eur. Phys. J. C

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Newton's constant has observational effects on both the CMB power spectra and the light curves of SNIa. We use Planck data, BAO data and the SNIa measurement to constrain the varying Newton's constant G during the CMB epoch and the redshift ranges of PANTHEON samples, and find no evidence indicating that G is varying with redshift. By extending the CDM model with one free parameter G, we get G = (6.65635 +0.18766 −0.18560 ) × 10 −11 m 3 kg −1 s −2 and H 0 = 67.62 +1.24 −1.25 km s −1 Mpc −1 at 68% CL from Planck+BAO+uncalibrated PANTHEON. The results show the value of G is consistent with CODATA 2018, but the H 0 tension can't be solved in this way.

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“…And Ref. [52] also finds a larger value for H 0 by an evolving gravitational constant. Here, we simply set G as a free parameter in the base CDM model to enlarge the value of H 0 .…”

Section: Introductionmentioning

confidence: 91%

Constraints on Newton’s constant from cosmological observations

Wang

Chen

2020

Eur. Phys. J. C

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“…The former ones, however, seem to be preferred over since reduce the value of the comoving size of the sound horizon at baryon drag r s , without spoiling the fit to CMB and BAO data [30][31][32]. Two well studied frameworks to modify the early time dynamics of the Universe and inject the required energy into the cosmic fluid to lower r s with respect to the ΛCDM one are modified gravity (MG) [33][34][35][36][37][38][39][40][41][42][43][44][45] and early dark energy (EDE) models [46][47][48][49][50][51][52][53][54][55][56][57][58][59][60][61][62][63]. 1 In this paper, we extend the model with a scalar field on-minimally coupled to the Ricci scalar of the form FðσÞ ¼ M 2 pl þ ξσ 2 in presence of a cosmological constant Λ [41,42], by providing it with a small effective mass.…”

Section: Introductionmentioning

confidence: 99%

Early modified gravity in light of the H0 tension and LSS data

et al. 2021

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We present a model of early modified gravity (EMG) consisting in a scalar field σ with a nonminimal coupling to the Ricci curvature of the type M 2 pl þ ξσ 2 plus a cosmological constant and a small effective mass and demonstrate its ability to alleviate the H 0 tension while providing a good fit to cosmic microwave background (CMB) anisotropies and baryon acoustic oscillations (BAO) data. In this model the scalar field, frozen deep in the radiation era, grows around the redshift of matter-radiation equality because of the coupling to nonrelativistic matter. The small effective mass, which we consider here as induced by a quartic potential, then damps the scalar field into coherent oscillations around its minimum at σ ¼ 0, leading to a weaker gravitational strength at early times and naturally recovering the consistency with laboratory and Solar System tests of gravity. We analyze the capability of EMG with positive ξ to fit current cosmological observations and compare our results to the case without an effective mass and to the popular early dark energy models with ξ ¼ 0. We show that EMG with a quartic coupling of the order of λ ∼ OðeV 4 =M 4 pl Þ can substantially alleviate the H 0 tension also when the full shape of the matter power spectrum is included in the fit in addition to CMB and Supernovae (SN) data.

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“…The addition of light relics is a typical example of physics that helps ease the tension by changing the early-time dynamics of the Universe [16][17][18][19][20]. Modified gravity models also lead to interesting solutions to the H 0 tension [21][22][23][24][25][26][27][28][29].…”

Section: Introductionmentioning

confidence: 99%

Unified framework for early dark energy from α -attractors

et al. 2020

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One of the most appealing approaches to ease the Hubble tension is the inclusion of an early dark energy (EDE) component that adds energy to the Universe in a narrow redshift window around the time of recombination and dilutes faster than radiation afterwards. In this paper, we analyze EDE in the framework of α-attractor models. As is well known, the success in alleviating the Hubble tension crucially depends on the shape of the energy injection. We show how different types of energy injections can be obtained, thanks to the freedom in choosing the functional form of the potential inspired by α-attractor models. To confirm our intuition, we perform a Markov-chain Monte Carlo analysis for three representative cases and find indeed that H 0 is significantly larger than in ΛCDM, like in other EDE models. Unlike axion-driven EDE models with a super-Planckian decay constant, the curvature of the potential in the EDE models required by the data is natural in the context of recent theoretical developments in α-attractors.

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Larger value for H0 by an evolving gravitational constant

Cited by 111 publications

References 69 publications

Constraints on Newton’s constant from cosmological observations

Constraints on Newton’s constant from cosmological observations

Early modified gravity in light of the H0 tension and LSS data

Unified framework for early dark energy from α -attractors

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