Version 1
: Received: 7 May 2019 / Approved: 8 May 2019 / Online: 8 May 2019 (11:36:01 CEST)
Version 2
: Received: 17 June 2020 / Approved: 18 June 2020 / Online: 18 June 2020 (09:25:41 CEST)
How to cite:
Capistrano, A.; Seidel, P.T.Z.; Duarte, H.R. Subhorizon Linear Nash Perturbations with Joint Analysis of Cosmic Growth and Expansion with Constrains on H(z) and the Deceleration Parameter q(z). Preprints2019, 2019050096
Capistrano, A.; Seidel, P.T.Z.; Duarte, H.R. Subhorizon Linear Nash Perturbations with Joint Analysis of Cosmic Growth and Expansion with Constrains on H(z) and the Deceleration Parameter q(z). Preprints 2019, 2019050096
Capistrano, A.; Seidel, P.T.Z.; Duarte, H.R. Subhorizon Linear Nash Perturbations with Joint Analysis of Cosmic Growth and Expansion with Constrains on H(z) and the Deceleration Parameter q(z). Preprints2019, 2019050096
APA Style
Capistrano, A., Seidel, P.T.Z., & Duarte, H.R. (2020). Subhorizon Linear Nash Perturbations with Joint Analysis of Cosmic Growth and Expansion with Constrains on H(z) and the Deceleration Parameter q(z). Preprints. https://doi.org/
Chicago/Turabian Style
Capistrano, A., Paola T. Z. Seidel and Hemerson R. Duarte. 2020 "Subhorizon Linear Nash Perturbations with Joint Analysis of Cosmic Growth and Expansion with Constrains on H(z) and the Deceleration Parameter q(z)" Preprints. https://doi.org/
Abstract
The Hubble parameter H(z), as a function of redshift, is modified by the presence of a new term originated from the extrinsic curvature in an embedded space-time. Assuming an asymptotic expansion factor $a\sim 0$ or, equivalently $z\rightarrow \infty$, it is obtained a nearly resemblance of the present model ($\beta$-model) with quintessence $w$CDM model with $H(z)\sim H_{wCDM}(z)$ at background level. In conjunction with $\Lambda$CDM, we test the models using a pack of recent datasets like that of the ``Gold 2018'' growth data, the best-fit Planck2018/$\Lambda$CDM parameters on the Cosmic Microwave Background (CMB), the Baryon Acoustic Oscillations (BAO) measurements, the Pantheon Supernovae type Ia and the Hubble parameter data with redshift ranging from $0.01 < z < 2.3$. Performing the Akaike Information Criterion (AIC) to ascertain the statistical viability of the model from Jeffreys' scale, we apply a joint likelihood analysis to the data with the Markov Chain Monte Carlo (MCMC) method. We find that the present model is in very good agreement with observations with a close statistical equivalence with the $\Lambda$CDM and $w$CDM cosmologies at 1-$\sigma$ level. We also show that a mild alleviation of the $\sigma$ tension between the growth amplitude factor and the matter content $(\sigma_8$-$\Omega_m)$ of the observations from CMB and Large Scale Structure (LSS) probes. A comparison of the aforementioned full pack of data in MCMC chains is made with the resulting MCMC from Pantheon SNIa+$H(z)$ in order to analyse the sensitivity of the models and how they respond to a cosmography analysis on the evolution of $H(z)$ and the deceleration parameter $q(z)$. In this sense, we find that only the $\beta$-model can be unaffected to the variations of the previous datasets due to its several minima in the likelihood (degeneracies) of the related parameters with an overall percentage relative difference only up to 4$\%$.
Keywords
modified Friedman equations; modified gravity; dark energy
Subject
Physical Sciences, Astronomy and Astrophysics
Copyright:
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Commenter: Abraao Capistrano
Commenter's Conflict of Interests: Author