A Model-independent Determination of the Hubble Constant from Lensed Quasars and Supernovae Using Gaussian Process Regression

Liao, Kai; Shafieloo, Arman; Keeley, Ryan E.; Linder, Eric V.

doi:10.3847/2041-8213/ab5308

“…Local measurements other than the R19 one exist, but most of them appear to consistently point towards values of H 0 significantly higher than the CMB one (see e.g. [27][28][29][30][31][32][33][34][35][36][37][38][39][40][41]). 3 Other scenarios worth mentioning include the possibility that properly accounting for cosmic variance (due to the fact that a limited sample of the Hubble flow is observed) enlarges the DM and DE beyond the purely gravitational ones are not forbidden by any fundamental symmetry in nature [118][119][120][121][122][123] and could help addressing the so called coincidence or why now?…”

Section: Introductionmentioning

confidence: 99%

Nonminimal dark sector physics and cosmological tensions

Valentino

¹

,

Melchiorri

²

,

Mena

³

et al. 2020

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We explore whether non-standard dark sector physics might be required to solve the existing cosmological tensions. The properties we consider in combination are: (a) an interaction between the dark matter and dark energy components, and (b) a dark energy equation of state w different from that of the canonical cosmological constant w = −1. In principle, these two parameters are independent. In practice, to avoid early-time, superhorizon instabilities, their allowed parameter spaces are correlated. Moreover, a clear degeneracy exists between these two parameters in the case of Cosmic Microwave Background (CMB) data. We analyze three classes of extended interacting dark energy models in light of the 2019 Planck CMB results and Cepheid-calibrated local distance ladder H0 measurements of Riess et al. (R19), as well as recent Baryon Acoustic Oscillation (BAO) and Type Ia Supernovae (SNeIa) distance data. We find that in quintessence coupled dark energy models, where w > −1, the evidence for a non-zero coupling between the two dark sectors can surpass the 5σ significance. Moreover, for both Planck+BAO or Planck+SNeIa, we found a preference for w > −1 at about three standard deviations. Quintessence models are, therefore, in excellent agreement with current data when an interaction is considered. On the other hand, in phantom coupled dark energy models, there is no such preference for a non-zero dark sector coupling. All the models we consider significantly raise the value of the Hubble constant easing the H0 tension. In the interacting scenario, the disagreement between Planck+BAO and R19 is considerably reduced from 4.3σ in the case of ΛCDM to about 2.5σ. The addition of low-redshift BAO and SNeIa measurements leaves, therefore, some residual tension with R19 but at a level that could be justified by a statistical fluctuation. We conclude that non-minimal dark energy cosmologies, such as coupled quintessence or phantom models, may soften the existing cosmological tensions. * eleonora.divalentino@manchester.ac.uk † alessandro.melchiorri@roma1.infn.it ‡ omena@ific.uv.es § sunny.vagnozzi@ast.cam.ac.uk 1 In Ref. [15,16] the reader can find complete reviews comparing the CMB and local determinations of H 0 .

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“…It is important to note that such systems have recently become a powerful astrophysical tool. For instance, the Hubble constant has been estimated by time-delay measurements [48][49][50][51][52][53], the CDDR was tested by using these systems in the Refs. [28,34,54,55].…”

Section: Strong Gravitational Lensing Systemsmentioning

confidence: 99%

Strong lensing systems and galaxy cluster observations as probe to the cosmic distance duality relation

Holanda

¹

,

Lima

²

,

Rana

³

et al. 2022

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In this paper, we use large scale structure observations to test the redshift dependence of cosmic distance duality relation (CDDR), $$D_\mathrm{L}(1+z)^{-2}/D_\mathrm{A}=\eta (z)$$ D L ( 1 + z ) - 2 / D A = η ( z ) , with $$D_\mathrm{L}$$ D L and $$D_\mathrm{A}$$ D A , being the luminosity and angular diameter distances, respectively. In order to perform the test, the following data set are considered: strong lensing systems and galaxy cluster measurements (gas mass fractions). No specific cosmological model is adopted, only a flat universe is assumed. By considering two $$\eta (z)$$ η ( z ) parametrizations, It is observed that the CDDR remain redshift independent within $$1.5\sigma $$ 1.5 σ which is in full agreement with other recent tests involving cosmological data. It is worth to comment that our results are independent of the baryon budget of galaxy clusters.

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“…Therefore, in this paper, we will calibrate the distances of SGL via a cosmological model-independent method, Gaussian Process (GP), which could make us reconstruct a smooth distance-redshift curve from SN Ia observation without assuming any parametrization forms. This reconstruction method has been widely used in cosmology (Wang et al 2020;Qi et al 2019;Seikel et al 2012a,b;Wang et al 2021a;Liao et al 2019).…”

Section: Gaussian Processmentioning

confidence: 99%

Galaxy-Scale Test of General Relativity with Strong Gravitational Lensing

Liu,

Li,

Qi

et al. 2021

Preprint

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Although general relativity (GR) has been precisely tested at the solar system scale, precise tests at a galactic or cosmological scale are still relatively insufficient. Here, in order to test GR at the galactic scale, we use the newly compiled galaxy-scale strong gravitational lensing (SGL) sample to constrain the parameter γ PPN in the parametrized post-Newtonian (PPN) formalism. We employ the Pantheon sample of type Ia supernovae observation to calibrate the distances in the SGL systems using the Gaussian Process method, which avoids the logical problem caused by assuming a cosmological model within GR to determine the distances in the SGL sample. Furthermore, we consider three typical lens models in this work to investigate the influences of the lens mass distributions on the fitting results. We find that the choice of the lens models has a significant impact on the constraints on the PPN parameter γ PPN . We use the Bayesian information criterion as an evaluation tool to make a comparison for the fitting results of the three lens models, and we find that the most reliable lens model gives the result of γ PPN = 1.065 +0.064 −0.074 , which is in good agreement with the prediction of γ PPN = 1 by GR. As far as we know, our 6.4% constraint result is the best result so far among the recent works using the SGL method.

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A Model-independent Determination of the Hubble Constant from Lensed Quasars and Supernovae Using Gaussian Process Regression

Cited by 116 publications

References 56 publications

Nonminimal dark sector physics and cosmological tensions

Nonminimal dark sector physics and cosmological tensions

Strong lensing systems and galaxy cluster observations as probe to the cosmic distance duality relation

Galaxy-Scale Test of General Relativity with Strong Gravitational Lensing

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