Cosmological tests of parametrization q = α − β H in f(Q) FLRW cosmology

Bouali, Amine; Shukla, B. K.; Chaudhary, Himanshu; Tiwari, R. K.; Samar, Mahvish; Mustafa, G.

doi:10.1142/s0219887823501529

Cited by 18 publications

(7 citation statements)

References 75 publications

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“…[58][59][60][61] Building on these EoS parameterizations, researchers have also thoroughly examined the deceleration parameter in their studies. [62][63][64][65][66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81] Recently, in ref. [75] explored a new parameter parametrization of the deceleration parameter and estimated the best-fit values for the free parameters using the chi-square and a Markov Chain Monte Carlo (MCMC) technique.…”

Section: Introductionmentioning

confidence: 99%

Exploring Late‐Time Cosmic Acceleration with Eos Parameterizations in Horava‐Lifshitz Gravity via Baryon Acoustic Oscillations

Khurana,

Chaudhary,

Debnath

et al. 2024

Fortschritte der Physik

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In this study, the framework of Horava‐Lifshitz gravity to model the Universe's dark matter and dark energy (DE) components is adopted. Specifically, two recent parametrizations for DE models: the CBDRM‐type and CADMM‐type parameterizations is considered. In the analysis, the Hubble parameter is explicitly expressed, denoted as , for these two distinct dark energy models. By doing so, investigate and quantify the accelerated cosmic expansion rate characterizing the late‐time Universe is aimed. This study uses a wide range of datasets. This dataset consists of recent measurements of baryon acoustic oscillations (BAOs) collected over a period of 22 years with the Cosmic Chronometers (CC) dataset, Type Ia supernovae (SNIa) dataset, the Hubble diagram of gamma‐ray bursts (GRBs), quasars (Q), and the latest measurement of the Hubble constant (R22). Consequently, a crucial aspect of this study by plotting the vs. H0 plane is presented. In the context of the ΛCDM model, after incorporating all the datasets, including the R22 prior, the following results: H0 = 71.674089 ± 0.734089 and is obtained. For the CBDRM model, H0 = 72.355058 ± 1.004604 and is found. In the case of the CADMM model, the analysis yields H0 = 72.347804 ± 0.923328 and . Cosmographic analyses for both of the proposed parameterizations in comparison to the ΛCDM paradigm are conducted. Additionally, Diagnostic tests to investigate the evolution of both models is applied. Finally, the Information Criteria test demonstrates that the ΛCDM model emerges as the preferred choice among the models is considered.

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Section: Introductionmentioning

confidence: 99%

Exploring Late‐Time Cosmic Acceleration with Eos Parameterizations in Horava‐Lifshitz Gravity via Baryon Acoustic Oscillations

Khurana,

Chaudhary,

Debnath

et al. 2024

Fortschritte der Physik

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“…In the study of the generalized holographic dark energy model, some well-known parametrization type models have been considered [22,23]. Till now, some authors have assumed some possible forms of parametrization of deceleration parameter [24][25][26][27][28][29][30][31][32][33][34][35]. The main advantage behind introducing a parameterization of the deceleration parameter is to provide a framework that is independent of specific gravitational theories.…”

Section: Introductionmentioning

confidence: 99%

Constraints on the parameterized deceleration parameter in FRW universe

Chaudhary¹,

Bouali²,

Debnath³

et al. 2023

Phys. Scr.

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Confirmation of accelerated expansion of the universe probed the concept of dark energy theory, and since then, numerous models have been introduced to explain its origin and nature. The present work is based on reconstructing dark energy by parametrization of the deceleration parameter in the FRW universe filled with radiation, dark matter and dark energy. We have chosen some well-motivated parametrized models 1-3 in an attempt to investigate the energy density in terms of deceleration parameters by estimating the cosmological parameters with the help of different observational datasets. Also, we have introduced a new model 4 for the parametrization of the deceleration parameter. Then we analyzed the cosmography parameters using the best-fit values of the parameters. Using the information criteria, we have examined the viability of the models.

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“…[19,20] A large body of literature is available on the possible parametrization of DP. [21][22][23][24][25][26][27][28][29][30] Consequently, the results may be independent of any particular gravitational theory which is one of the prominent advantages of parameterizing the DP. An analogous parameterized DP has also been introduced for the well-established models in place of parameterized DE equation of state.…”

Section: Introductionmentioning

confidence: 99%

Observational Constraining Study of New Deceleration Parameters in FRW Universe

Bouali

Chaudhary

Mumtaz

et al. 2023

Fortschritte der Physik

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In the current paper, a dark energy (DE) model reconstructed from the well‐motivated deceleration parameter (DP) is analyzed. A flat FRW Universe filled with radiation, dark matter (DM), and dark energy fluids is considered. The free parameters are constrained using measurements from Supernovae, Hubble, Gamma Ray Bursts, Quasars, and Baryon acoustic Oscillations. The model under study is found to be very supported by observation with respect to ΛCDM since . Besides, a cosmographic analysis is performed showing that the reconstructed model behaves similarly as ΛCDM does. Finally, a diagnostic analysis is performed reporting that the studied model behaves quintessence type at a late time.

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Cosmological tests of parametrization q = α − β H in f(Q) FLRW cosmology

Cited by 18 publications

References 75 publications

Exploring Late‐Time Cosmic Acceleration with Eos Parameterizations in Horava‐Lifshitz Gravity via Baryon Acoustic Oscillations

Exploring Late‐Time Cosmic Acceleration with Eos Parameterizations in Horava‐Lifshitz Gravity via Baryon Acoustic Oscillations

Constraints on the parameterized deceleration parameter in FRW universe

Observational Constraining Study of New Deceleration Parameters in FRW Universe

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