arXiv subjects

Muhammad Yarahmadi

Publications and source records attributed to Muhammad Yarahmadi.

14 recordsLinked to original sources

arXiv2026

Late-Time Alleviation of the Hubble Tension in CPL Cosmology with Massive Neutrinos via Bayesian Physics-Informed Neural Networks

We present a comprehensive Bayesian analysis of the Hubble constant within the framework of Physics-Informed Neural Networks (PINNs), focusing on the standard $\Lambda$CDM model and its dynamical dark energy extensions described by the Chevallier-Polarski-Linder (CPL) parametrization, both with and without massive neutrinos. By embedding the cosmological background equations directly into a Bayesian PINN architecture, we reconstruct the Hubble expansion history $H(z)$ in a data-driven yet physically consistent manner, while rigorously propagating epistemic uncertainties. Our analysis combines late-time observational probes, including Cosmic Chronometers, Baryon Acoustic Oscillations (BAO DESI DR2), and the Pantheon supernova sample, and quantifies the resulting tension in the inferred Hubble constant with respect to Planck 2018 Cosmic Microwave Background constraints and the SH0ES (R22) local distance ladder measurement. Within $\Lambda$CDM, we find that data combinations involving BAO tend to favor lower values of $H_0$, alleviating the tension with Planck at the expense of increased disagreement with SH0ES. Allowing for a time-evolving dark energy equation of state in the CPL framework systematically shifts the posterior of $H_0$ toward higher values, leading to a notable reduction of the SH0ES tension, particularly for combinations including supernova data. The most flexible scenario, CPL with a free total neutrino mass $\Sigma m_\nu$, yields a balanced reconciliation between early- and late-Universe determinations of $H_0$, with tension levels typically reduced to the $\sim1$-$2\sigma$ range relative to both Planck and SH0ES. Our results highlight the nontrivial interplay between dark energy dynamics and neutrino mass in addressing the Hubble tension and demonstrate the efficacy of Bayesian PINNs as a robust and versatile tool for precision cosmology beyond the standard paradigm.

astro-ph.CO↗

arXiv2025

Towards a Machine Learning Solution for Hubble Tension: Physics-Informed Neural Network (PINN) Analysis of Tsallis Holographic Dark Energy in Presence of Neutrinos

We present a Physics-Informed Neural Network (PINN) framework for reconstructing the redshift-dependent Hubble parameter $H(z)$ within the Tsallis Holographic Dark Energy (THDE) model extended by massive neutrinos. In this approach, the modified Friedmann equation is incorporated into the neural network loss function, enabling training on Cosmic Chronometers data up to $z \leq 2$. The framework allows for the simultaneous estimation of the Hubble constant $H_0$, the neutrino density parameter $\Omega_\nu$, and the Tsallis non-extensivity index $\delta$. Uncertainty quantification is performed through dropout simulations, resulting in statistically consistent $1\sigma$ confidence bands. Our results show that the THDE+$\nu$ model, reconstructed via PINN, alleviates the statistical Hubble tension from the canonical $\sim 5\sigma$ level down to a range of $0.5\sigma \leq T \leq 2.2\sigma$, depending on the redshift sampling. Additionally, we constrain the total neutrino mass to $\Sigma m_\nu < 0.11\,\text{eV}$. A detailed comparison with the traditional Markov Chain Monte Carlo (MCMC) analysis demonstrates the consistency of both methods, while highlighting the competitiveness of the PINN-based THDE framework as a robust, data-driven approach for non-parametric cosmological inference within generalized thermodynamics.

astro-ph.CO↗

arXiv2025

Coupled non-canonical scalar field to neutrinos could alleviate the Hubble tension and cross the phantom barrier

This study presents an analysis of cosmological parameters, focusing on resolving the Hubble tension and constraining neutrino masses within a coupled quintom model. By utilizing datasets from the Cosmic Microwave Background (CMB), Pantheon + Analysis, Cosmic Chronometers (CC), Baryon Acoustic Oscillations (BAO), and CMB Lensing, we explore the interplay between cosmological parameters and observational constraints. The model effectively reduces the Hubble tension, achieving a consistency in $H_0$ measurements of $1.37\sigma$ and $1.24\sigma$ for the CMB + ALL dataset For Planck 2018 and R22 respectively. Additionally, the study refines constraints on the total mass of neutrinos ($\Sigma_{m_{\nu}}$), with a finding of $0.115\,\text{eV}$ for the CMB + ALL dataset. The analysis examines the effective equation of state parameter ($w_{\text{eff}}$), indicating a transition towards a universe dominated by exotic energy forms. The combined datasets refine $w_{\text{eff}}$ to $-1.02\pm0.018$, underscoring the importance of multi-dataset integration in understanding dark energy dynamics. Furthermore, the interaction constant $\beta$ between the quintom scalar field and neutrinos is constrained to $0.65 \pm 0.12$ for the CMB + ALL dataset. The potential parameters $\lambda_{\sigma} = -2.09 \pm 0.082$ and $\lambda_{\phi} = 2.43 \pm 0.12$ are also determined, providing insights into the quintom model's implications for cosmological dynamics. This study offers compelling evidence for the coupled quintom model's capability to resolve the Hubble tension and refine constraints on neutrino properties, enhancing our understanding of the universe's evolution.

astro-ph.CO↗

arXiv2025

A Bayesian PINN Framework for Barrow-Tsallis Holographic Dark Energy with Neutrinos: Toward a Resolution of the Hubble Tension

We investigate the Barrow-Tsallis Holographic Dark Energy (BTHDE) model using both traditional Markov Chain Monte Carlo (MCMC) methods and a Bayesian Physics-Informed Neural Network (PINN) framework, employing a range of cosmological observations. Our analysis incorporates data from Cosmic Microwave Background (CMB), Baryon Acoustic Oscillations (BAO), CMB lensing, Cosmic Chronometers (CC), and the Pantheon+ Type Ia supernova compilation. We focus on constraining the Hubble constant $ H_0 $, the nonextensive entropy index $ q $, the Barrow exponent $ \Delta $, and the Granda-Oliveros parameters $ \alpha $ and $ \beta $, along with the total neutrino mass $ \Sigma m_\nu $. The Bayesian PINN approach yields more precise constraints than MCMC, particularly for $ \beta $, and tighter upper bounds on $ \Sigma m_\nu $. The inferred values of $ H_0 $ from both methods lie between those from Planck 2018 and SH$_0$ES (R22), alleviating the Hubble tension to within $ 1.3\sigma $-$2.1\sigma $ depending on the dataset combination. Notably, the Bayesian PINN achieves consistent results across CC and Pantheon+ datasets, while maintaining physical consistency via embedded differential constraints. The combination of CMB and late-time probes leads to the most stringent constraints, with $ \Sigma m_\nu < 0.114 $ eV and $ H_0 = 70.6 \pm 1.35 $ km/s/Mpc. These findings suggest that the BTHDE model provides a viable framework for addressing cosmological tensions and probing modified entropy scenarios, while highlighting the complementary strengths of machine learning and traditional Bayesian inference in cosmological modeling.

astro-ph.CO↗

arXiv2025

Exploring Hubble Tension Alleviation through Neutrino-Coupled Perturbed $f(R)$ Gravity

This work examines the Hubble constant ($H_0$) tension within the frameworks of perturbed $f(R)$ gravity and perturbed $f(R)$ gravity coupled with neutrinos, using lastest observational data. The datasets incorporate the Cosmic Microwave Background (CMB), Baryon Acoustic Oscillations (BAO), Cosmic Chronometers (CC), lensing, and Pantheon supernovae. We compare the ability of these models to bridge the discrepancy between Planck 2018 ($H_0 = 67.4 \pm 0.5 \ \text{km/s/Mpc}$) and the local R22 measurement ($H_0 = 73.5 \pm 1.04 \ \text{km/s/Mpc}$). In perturbed $f(R)$ gravity, the derived $H_0$ values align closely with Planck, leaving a substantial tension with R22. The inclusion of neutrino interactions introduces additional parameters that shift $H_0$ toward higher values, reducing the tension with local measurements. Notably, the coupled model achieves a smaller residual tension compared to the standalone perturbed $f(R)$ model, indicating that neutrino physics plays a significant role in modifying the late-time expansion dynamics. While both models provide insights into addressing the Hubble tension, the coupled $f(R)$ gravity with neutrinos offers a more consistent alignment across the datasets.

gr-qc↗

arXiv2025

Cosmic Bulk Flow Analysis in Modified Gravity Theories: $f(R)$ and Perturbed $f(R)$ Models with Neutrino Coupling

In this study, we explore the characteristics of bulk flow across various redshift ranges within the frameworks of $f(R)$ gravity, perturbed $f(R)$ gravity, and perturbed $f(R)$ gravity coupled with neutrinos. Our investigation reveals profound insights into large-scale cosmic flows and their interactions with major cosmic structures, such as the Sloan Great Wall (SGW) and the King Ghidorah Supercluster (KGSc). We find that incorporating neutrinos into the perturbed $f(R)$ gravity model results in a substantial increase in bulk flow velocities across all redshifts, with notable enhancements in the higher redshift ranges, where velocities can exceed $3000 \, \mathrm{km/s}$ in the $0.8 < z < 1.4$ range. Moreover, the direction of the bulk flow in this model closely aligns with the dark energy dipole, especially at redshifts $z > 0.4$, showing near-perfect congruence with cosmic superclusters. This suggests a significant interaction between neutrinos and cosmic structures, influencing cosmic acceleration. At lower redshifts, such as $0.1 < z < 0.2$, the bulk flow aligns with the SGW, while in the $0.4 < z < 0.6$ range, it aligns with the KGSc. In the low redshift range $0.001 < z < 0.016$, although velocities are lower, neutrinos still subtly increase the bulk flow velocity and maintain alignment with nearby cosmic structures, like the Local Supercluster. Our results underscore the critical role of neutrinos in shaping cosmic flows and offer new insights into the interplay between dark energy, neutrinos, and modified gravity models.

astro-ph.CO↗

arXiv2025

Using the Kaniadakis horizon entropy in the presence of neutrinos to alleviate the Hubble and $ S_{8} $ Tensions

The $H_{0}$ tension stands as a prominent challenge in cosmology, serving as a primary driver for exploring alternative models of dark energy. Another tension arises from measurements of the $ S_{8} $ parameter, which is characterize the amplitude of matter fluctuations in the universe. In this study, we address the alleviation of both the Hubble tension and $ S_{8} $ tension by incorporating Kaniadakis horizon entropy. We investigate two scenarios to explore the impact of this entropy on cosmological parameters. In the first scenario, utilizing modified Friedmann equations through Kaniadakis entropy, we estimate the values of $H_{0}$ and $ S_{8} $. In the subsequent scenario, we introduce the neutrino term and assess its effect on mitigating the Hubble and $ S_{8} $ tensions. Our findings reveal that when considering the first scenario, the results closely align with Planck's 2018 outcomes for Hubble and $ S_{8} $ tensions. Moreover, with the inclusion of neutrinos, these tensions are alleviated to approximately 2$\sigma$, and the $ S_{8} $ value is in full agreement with the results from the KiDS and DES survey. Furthermore, we impose a constraint on the parameter $K$ in each scenario. Our analysis yields $K = 0.12\pm 0.41$ for Kaniadakis entropy without neutrinos and $K = 0.39\pm 0.4$ for the combined dataset considering Kaniadakis entropy in the presence of neutrinos. We demonstrate that the value of K may be affected by neutrino mass, which can cause energy transfer between different parts of the universe and alter the Hubble parameter value.

astro-ph.CO↗

arXiv2025

Barrow Interacting holographic dark energy cosmology with Hubble horizon as IR cutoff: A model can Alleviating the Hubble and $S_{8}$ Tension

In this study, we perform a comprehensive analysis of the Hubble constant ($H_0$) and matter clustering ($S_8$) tensions within the framework of non-interacting and interacting Barrow Holographic Dark Energy (BHDE) models. Utilizing a combination of observational datasets, including the Cosmic Microwave Background (CMB), Baryon Acoustic Oscillations (BAO), cosmic chronometers (CC), Pantheon, and lensing data, we assess the degree of tension relative to the Planck 2018 results and recent measurements such as the Riess et al. 2022 (R22) value for $H_0 = 73.04 \pm 1.04 \ \text{km s}^{-1} \text{Mpc}^{-1}$ in 68\% C.L and KiDS-1000 and DES-Y3 for $S_8$. Our findings show that both BHDE models mitigate the $H_0$ and $S_8$ tensions compared to the standard $\Lambda$ Cold Dark Matter ($\Lambda$CDM) model. The non-interacting BHDE model achieves a moderate reduction in the $H_0$ tension, while the interacting BHDE model offers a better fit for both parameters, suggesting it is more effective in addressing the tensions. Additionally, the quantum-gravitational deformation parameter $\Delta$, constrained using the CMB+All dataset, indicates significant quantum effects in both models. The interacting scenario provides tighter constraints on $\Delta$ and total neutrino mass $\sum m_{\nu}$, offering a more precise representation of these effects. This study highlights the potential of BHDE models as viable alternatives to the $\Lambda$CDM framework for resolving cosmological tensions.

astro-ph.CO↗

arXiv2025

Comparative Analysis of Perturbed $f(R)$ Gravity and Perturbed Rastall Gravity Models in Describing Cosmic Evolution from Early to Late Universe Relative to the $\Lambda$CDM Model

This study conducts a meticulous examination of the cosmological implications inherent in Rastall gravity and $f(R)$ gravity models, assessing their efficacy across distinct cosmic epochs, from early universe structure formation to late-time acceleration. In the initial stages, both models exhibit commendable compatibility with observed features of structure formation, aligning with the established $\Lambda$CDM model. The derived Jeans' wavenumbers for each model support their viability. However, as the cosmic timeline progresses into the late universe, a discernible disparity surfaces. Utilizing the Markov Chain Monte Carlo method, we reconstruct the deceleration parameter $(q)$ and identify Deceleration - Acceleration redshift transition values. For $f(R)$ gravity, our results align closely with previous studies, emphasizing its superior ability to elucidate the recent cosmic acceleration. In contrast, Rastall gravity exhibits distinct redshift transition values. Our rigorous analysis underscores the prowess of $f(R)$ gravity in capturing the observed cosmic acceleration, positioning it as a compelling alternative to the conventional $\Lambda$CDM model. The discernible shifts observed in the peaks of the CMB power spectrum and evolution of deceleration parameter (q) for both $f(R)$ gravity and Rastall gravity models in the Early and Late universe, in relation to the $\Lambda $CDM model, provide compelling evidence supporting the proposition that these alternative gravity models can account for the anisotropy of the universe without invoking the need for dark energy.

gr-qc↗

arXiv2024

Perturbed $f(R)$ gravity coupled with neutrinos: exploring cosmological implications

We conduct a thorough examination of cosmological parameters within the context of $f(R)$ gravity coupled with neutrinos, leveraging a diverse array of observational datasets, including Cosmic Microwave Background (CMB), Cosmic Chronometers (CC), Baryon Acoustic Oscillations (BAO), and Pantheon supernova data. Our analysis unveils compelling constraints on pivotal parameters such as the sum of neutrino masses ($\sum m_{\nu}$), the interaction strength parameter ($\Gamma$), sound speed ($c_s$), Jean's wavenumbers ($k_J$), redshift of non-relativistic matter ($z_{\rm nr}$), and the redshift of the Deceleration-Acceleration phase transition ($z_{\rm DA}$). The incorporation of neutrinos within the $f(R)$ gravity framework emerges as a key factor significantly influencing cosmic evolution, intricately shaping the formation of large-scale structures and the dynamics of cosmic expansion. Additionally, a detailed analysis of bulk flow direction and amplitude across various redshifts provides valuable insights into the nature of large-scale structures. A notable aspect of our model is the nuanced integration of $f(R)$ gravity theory with neutrinos, representing a distinctive approach to unraveling cosmological phenomena. This framework, unlike previous models, explicitly considers the impact of neutrinos on gravitational interactions, the formation of large-scale structures, and the overarching dynamics of cosmic expansion within the $f(R)$ gravity paradigm. Furthermore, our study addresses the Hubble tension problem by comparing $H_0$ measurements within our model, offering a potential avenue for reconciling discrepancies. Our findings not only align with existing research but also contribute novel perspectives to our understanding of dark energy, gravitational interactions, and the intricate challenges posed by the Hubble tension.

astro-ph.CO↗

arXiv2024

Neutrino Interactions with perturbed Rastall Gravity: A Novel Approach to Reducing the Hubble Tension

We investigate the cosmological implications of coupling neutrinos to perturbed Rastall gravity, focusing on its impact on the Hubble constant ($H_0$) and the associated tension between early- and late-universe measurements with MCMC and PINN method. Utilizing observational data from the Cosmic Microwave Background (CMB), Cosmic Chronometers (CC), Baryon Acoustic Oscillations (BAO), and the Pantheon+ Type Ia supernovae, CMB Lensing, we perform a detailed statistical analysis. Our findings demonstrate that the Rastall model provides an improved fit to the data compared to the standard $\Lambda$CDM model, as indicated by lower Akaike Information Criterion (AIC) values in both early and late-universe regimes. The model introduces a deviation parameter $\alpha$, which remains consistent with existing literature and differs across epochs, supporting a dynamic gravitational framework. Combining all datasets, the Rastall model yields $H_0 = 70.23 \pm 2.01$ km,s$^{-1}$,Mpc$^{-1}$, significantly reducing the tension with Planck ($1.34\sigma$) and SH0ES ($1.16\sigma$) compared to the $\sim 4\sigma$ discrepancy in $\Lambda$CDM. Additional dataset combinations confirm this alleviation, with Planck tensions consistently below $1.6\sigma$. Overall, our results highlight Rastall gravity with neutrino coupling as a promising alternative to $\Lambda$CDM, capable of addressing current cosmological tensions while aligning with observational data, it can be concluded that the Hubble tension may be resolved.

gr-qc↗

arXiv2023

Anisotropic Signatures: Neutrinos -- Dark Energy Interaction and Its Effect on the Transition from Radiation to Matter, and Dark Energy Dominated Phases

This paper explains the significance of neutrino mass in the cosmic progression from the radiation-dominated phase to matter and subsequently to the dark energy-dominated era. We have put a constraint on the total mass of neutrinos by coupling them with quintessence. For the combination of full data(Pantheon+CMB+BAO+CC), we find $ \sum m_{\nu}<0.101$eV \ \ (95$\% $CL.) and for the relativistic to non-relativistic phase transition redshif ${z_{\rm nr}} = 180$ which is in the matter-dominated era. Our findings confirm that when neutrinos become non-relativistic, the universe transitions from a radiation-dominated era to a matter-dominated era. Coupled neutrinos with quintessence (CQ) have also a significant impact on transitions from a matter-dominated era to a dark energy era. We have shown this effect by investigating the impact of neutrino mass on the bulk flow direction and amplitude of bulk velocity. Moreover, we have discussed the impact of this coupling on the CMB power spectrum to show the anisotropy in the universe. Finally, we have established a link between the quintessence field coupled with neutrinos and the bulk flow, which allowed us to demonstrate that the mass of neutrinos could be the cause of anisotropy in the universe.

gr-qc↗

arXiv2023

Revisiting the history of the evolution of the universe from radiation dominated to dark energy dominated

Most of our knowledge of the universe has been obtained from the anisotropy spectrum of the cosmic microwave background and observations of large-scale structures. During the history of the Universe, neutrinos from the early Universe evolve from a relativistic phase at very early times to a massive-particle behavior at later times. The mass of neutrinos affects the history of the expansion of the universe and the growth of the disturbances of the various components of the cosmic microwave background, therefore the anisotropy spectrum of the cosmic radiation and the observations of the large-scale structures. In this article, by using the coupling of neutrinos with dark energy, we investigate the cosmic evolution from the era of matter dominated to the era of dark energy dominated and show that neutrinos can play an important role in the evolution from radiation dominated to matter dominated and the evolution from Matter dominated to dark energy dominated. Also, we investigate the effect of non-relativistic neutrino on bulk flow and show that the direction of bulk flow has a little difference in scales smaller than 0.1, and the more we consider the scales higher than the local universe, the more difference is observed in the direction of bulk flow.

gr-qc↗

arXiv2022

The interaction of neutrinos with Phantom, Quintessence, and Quintum scalar fields and its effect on the formation of structures in the early Universe

Despite the fact that the mass of the neutrinos is so small, they are produced in such vast numbers in the early Universe that their mass induces subtle effects on cosmological observables, primarily the growth of structure and the expansion history in the Universe. We consider the models where neutrino interacts with dark energy scalar field models; phantom, quintessence, and quintom. Also, we obtained the $z_{\rm nr}$ (the redshift at which a mass of neutrino $m_{\nu}$ will become non-relativistic) and surveyed the effect of non-relativistic neutrinos on the structure formation. The data used in this paper are Pantheon + Analysis catalog, CMB, and BAO data. We obtained coupling constant $\beta$ for neutrino and three scalar fields and found that larger $\beta$ values will generally lead to larger neutrino mass in the Universe. For combination data, we found that the total mass of neutrino $\sum m_{\nu}< 0.1197$eV $(95\% $ Confidence Level (C.L.) for quintom model and $\sum m_{\nu}< 0.121 $eV $(95\% $ Confidence Level (C.L.) for phantom model and $\sum m_{\nu}< 0.122$eV $(95\% $ Confidence Level (C.L.) for quintessence model. These results are in broad agreement with the results of Planck 2018 where the total neutrino mass is $\sum m_{\nu}<0.12$eV ($95\%$ C.L., TT, TE, EE+lowE+lensing+BAO). Using the neutrino mass obtained from different models, we calculated $z_{\rm nr}$ and co-moving wave number $k_{\rm nr}$ and showed that neutrinos played a role on the structure formation in the early Universe.

gr-qc↗