arXiv subjects

Jose Agustin Lozano Torres

Publications and source records attributed to Jose Agustin Lozano Torres.

5 recordsLinked to original sources

arXiv2026

The unified Bound Dark Energy--Bound Dark Matter model: theory and constraints from DESI DR2

The unified Bound Dark Energy--Bound Dark Matter (BDE-BDM) model derives both the dark energy and the whole of the dark matter from a single supersymmetric $SU(3)$ gauge group with $N_f=6$ flavors. Gauge-coupling unification predicts the scale at which it condenses, $\Lc=34^{+16}_{-11}$~eV, before any cosmological data are used, so the dark-energy sector adds no parameter to those of \LCDM\ and the dark-matter sector adds only one. Fitting DESI DR2 BAO, Planck CMB, Planck+ACT DR6 CMB lensing, and three supernova compilations (PantheonPlus, Union3.1, DES-Dovekie) gives, for Union3.1, $\Lc=43.67\pm0.13$~eV, inside the predicted range: a high-energy prediction met by a late-time measurement. The equation of state evolves to $w_0=-0.9262\pm0.0005$ and never crosses the phantom divide. Relative to \LCDM\ the model lowers the DESI BAO $χ^2$ by $2.95$--$3.67$ and the supernova $χ^2$ by $2.53$--$4.07$, recovering $57\%$--$71\%$ of the total reduction that \wowa\ obtains by fitting two dark-energy parameters to the same data, and reaching the lower BAO $χ^2$ of the two models for two of the three compilations. Its $Δ\mathrm{DIC}$ against \LCDM\ is strong for every compilation, $-8.28$ to $-7.47$, varying by $0.81$ where that of \wowa\ varies by $4.8$. Because the dark-energy sector adds no parameter to those of \LCDM, the likelihood gain survives the Occam penalty: $\ln B=+4.09$, $+4.12$, and $+4.83$ against \LCDM, where \wowa\ gives $-2.11$, $-0.26$, and $-0.56$. Among six models pairing a cosmological constant, the \wowa\ parametrization or bound dark energy with cold or bound dark matter, BDE-BDM has the largest Bayesian evidence.

astro-ph.CO↗

arXiv2026

Bound Dark Energy: Particle Physics model in alignment with recent DESI cosmological measurements

We present observational constraints on the Bound Dark Energy Cold Dark Matter (BDE-CDM) model using DESI DR2 baryon acoustic oscillation measurements combined with Planck CMB data and Type Ia supernovae compilations (PantheonPlus, Union3, DESY5). In BDE-CDM, dark energy originates from the lightest meson field within a supersymmetric SU(3) dark gauge group with $N_f = 6$ flavors, governed by an inverse power-law potential $V(ϕ) = Λ_{c}^{4+2/3} ϕ^{-2/3}$. Unlike $Λ$CDM and $w_0w_a$CDM, the dark energy sector contains no free parameters -- the condensation scale $Λ_c$ and transition epoch $a_c$ are determined by gauge coupling unification constraints. The equation of state evolves from relativistic behavior ($w = 1/3$) before condensation through a kinetic-dominated stiff phase ($w \simeq 1$), approaching $w_0 = -0.9298 \pm 0.0003$ at present, with $w > -1$ maintained throughout cosmic history, avoiding phantom-regime instabilities. We obtain $Λ_{c} = 43.93 \pm 0.13$~eV and $a_c = (2.489 \pm 0.007) \times 10^{-6}$, consistent with theoretical predictions. The $w_0$-$w_a$ confidence contours are approximately 10,000 times smaller than those of $w_0w_a$CDM while achieving comparable fits, and remain stable across different supernova datasets. Statistical analysis yields $Δ\mathrm{DIC} = -6.77$ and $Δ\mathrm{AIC} = -8.97$ relative to $Λ$CDM for BAO+DESY5, constituting strong evidence favoring BDE-CDM model. The model predicts distinctive signatures including 25\% enhancement in the matter power spectrum at $k \approx 4.3\,h\,\mathrm{Mpc}^{-1}$. These results establish BDE-CDM as a theoretically motivated framework that successfully addresses the DESI-observed preference for dynamical dark energy while connecting particle physics with cosmological observations.

astro-ph.CO↗

arXiv2025

Bound dark energy: Particle origin of dark energy with DESI BAO and DES supernova data

The recent findings from the Dark Energy Spectroscopic Instrument (DESI) indicate a preference for dynamical dark energy at a significance level above $2.5 σ$, with baryon acoustic oscillation (BAO) combined with cosmic microwave background (CMB) data and Type Ia supernovae (SNe) data, favoring a time dependent equation of state $w(z)$ rather than the cosmological constant ($w = -1$). We introduce the Bound Dark Energy (BDE) model, in which dark energy arises from the lightest meson field $ϕ$ in a dark SU(3) gauge group, developing dynamically through non perturbative interactions. Governed by an inverse power law potential $V(ϕ) = Λ_c^{4+2/3}ϕ^{-2/3}$, BDE features no dark energy free parameters: one less than $Λ$CDM ($Λ$) and three less than the $ w_{0}w_{a} $CDM ($ w_{0}, w_{a},Λ$) models. By integrating DESI BAO measurements, CMB data and Dark Energy Survey SN Ia distance data collected during the fifth year, BDE demonstrates a reduction of $42$ and $37$ percent in the reduced $χ^{2}_{BAO}$ as well as lower AIC and BIC values compared to the $w_{0}w_{a}$CDM and $Λ$CDM models, respectively, while maintaining a comparable fit for both type Ia supernovae and the cosmic microwave background data. Although the ($w_{0},w_{a}$) contour in BDE is 10,000 times smaller than that found in the $w_{0}w_{a}$CDM model, the BDE model suggests a dynamical dark energy scenario with precise values of $w_{0}=$-0.9301 $\pm$ 0.0004 and $w_{a}=$ -0.8085 $\pm$ 0.0053 while providing a consistency on the six Planck and derived parameters at the 1$σ$ level between BDE, $Λ$CDM and $w_{0}w_{a}$CDM models. The critical parameters condensation energy scale $Λ_{c} = 43.806 \pm 0.190$ eV and epoch $a_{c} = (2.497 \pm 0.011) \times 10^{-6}$ are consistent with predictions from high energy physics.

astro-ph.CO↗

arXiv2025

Bound Dark Energy: a particle's origin of dark energy

Dark energy, the enigmatic force driving the accelerated cosmic expansion of the universe, is conventionally described as a cosmological constant in the standard $Λ$CDM model. However, measurements from the Dark Energy Spectroscopic Instrument (DESI) reports a $> 2.5σ$ preference for dynamical dark energy, with baryon acoustic oscillation (BAO) data favoring a time varying equation of state $w(z)$ over the cosmological constant ($w=-1$). We present the Bound Dark Energy (BDE) model, where dark energy originates from the lightest meson field $ϕ$ in a dark SU(3) gauge sector, emerging dynamically via non perturbative interactions. Governed by an inverse-power-law potential $V(ϕ)=Λ_{c}^{4 + 2/3}ϕ^{-2/3}$, BDE has no free parameters, one less than $Λ$CDM and three less than $w_{0}w_{a}$CDM models. Combining the DESI BAO measurements, cosmic microwave background data, and Dark Energy Survey SN Ia distance measurements from the fifth year, BDE achieves a $42\%$ and $37\%$ reduction in the reduced $χ^{2}_{BAO}$ compared to $w_{0}w_{a}$CDM and $Λ$CDM, respectively, while having an equivalent fit for type Ia supernovae and the cosmic microwave background data. The model predicts a dark energy equation of state transitioning from radiation like $w=1/3$ at early times ($a < a_{c}$) to $ w_{0}=-0.9301 \pm 0.0004$ at present time. The ($w_{0},w_{a}$) contour is 10,000 times smaller in BDE than in $w_{0}w_{a}$CDM model, while having an equivalent cosmological fit. Key parameters the condensation energy scale $Λ_{c}=43.806 \pm 0.19$ eV and epoch $a_{c}=2.4972 \pm 0.011 \times 10^{-6}$ align with high-energy physics predictions. These results, consistent with current observational bounds, establish BDE as a predictive framework that unifies particle physics and cosmology, offering a first-principles resolution to dark energy dynamical nature.

astro-ph.CO↗

arXiv2022

Three-dimensional weak gravitational lensing of the 21-cm radiation background

We study weak gravitational lensing by the cosmic large-scale structure of the 21-cm radiation background in the 3d-weak lensing formalism. The interplay between source distance measured at finite resolution, visibility and lensing terms is analysed in detail and the resulting total covariance $C_{\ell}(k,k')$ is derived. The effect of lensing correlates different multipoles through convolution, breaking the statistical homogeneity of the 21-cm radiation background. This homogeneity breaking can be exploited to reconstruct the lensing field $\hatϕ_{\ell m}(κ)$ and noise lensing reconstruction $N_{\ell}^{\hatϕ}$ by means of quadratic estimators. The effects related to the actual measurement process (redshift precision and visibility terms) change drastically the values of the off-diagonal terms of the total covariance $C_{\ell}(k,k')$. It is expected that the detection of lensing effects on a 21-cm radiation background will require sensitive studies and high-resolution observations by future low-frequency radio arrays such as the SKA survey.

astro-ph.CO↗