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arxiv: 2606.21839 · v1 · pith:H5PV544Xnew · submitted 2026-06-20 · 🌀 gr-qc

Observational Constraints on f(Q,T) Gravity in the Presence of DBI-Essence Scalar Field

Mayur Mune , Praveen Kumar Dhankar , Goutam Manna , Safiqul Islam , Bidisha Samanta , Behnam Pourhassan This is my paper

Pith reviewed 2026-06-26 11:58 UTC · model grok-4.3

classification 🌀 gr-qc
keywords f(Q,T) gravityDBI scalar fieldlate-time cosmologyobservational constraintsMCMC analysisHubble dataBAO measurementsType Ia supernovae
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The pith

The linear f(Q,T) model with DBI scalar field yields background solutions consistent with Hubble, BAO and supernova data as a viable alternative to ΛCDM.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper derives the background equations for f(Q,T) gravity coupled to a Dirac-Born-Infeld scalar field on flat FLRW spacetime, treating the cosmic medium as an effective perfect fluid. For the specific linear form f(Q,T)=αQ+βT the authors obtain analytic solutions and then perform MCMC fitting to Hubble-rate measurements, DESI BAO DR2 data and the Pantheon+SHOES supernova sample. The resulting joint posteriors remain compatible with existing late-time constraints while quantifying the shifts induced by the βT term and the DBI sector. The work therefore positions the model as a statistically acceptable extension that can be compared directly with the cosmological-constant paradigm.

Core claim

For the linear choice f(Q,T)=αQ+βT coupled to a DBI scalar field, the background equations on flat FLRW admit analytic solutions that, when fitted to Hubble, DESI BAO DR2, and Pantheon+SHOES data via MCMC, produce joint posteriors consistent with late-time constraints and allow direct comparison to ΛCDM, establishing the model as a statistically viable alternative.

What carries the argument

The linear function f(Q,T)=αQ+βT coupled to the DBI-essence scalar field, which alters the Friedmann equations through non-metricity and trace-of-stress-energy contributions.

If this is right

  • The model admits direct statistical comparison with ΛCDM on identical datasets.
  • The βT coupling and DBI sector produce measurable departures from standard expansion history.
  • The framework supplies a concrete setting in which to explore possible remedies for the H0 discrepancy.
  • Posterior constraints remain broadly consistent with current late-time observations.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Higher-redshift BAO or supernova samples could tighten bounds on the β parameter and reveal whether the DBI sector is required.
  • The same linear f(Q,T) ansatz could be tested against growth-rate or weak-lensing data to check consistency beyond background expansion.
  • Analytic solutions derived here may serve as a template for studying other scalar-field couplings in symmetric teleparallel gravity.

Load-bearing premise

The linear choice f(Q,T)=αQ+βT together with the effective perfect-fluid treatment on flat FLRW is sufficient to capture the relevant late-time dynamics.

What would settle it

A new high-precision Hubble or BAO measurement at moderate redshift lying systematically outside the 2σ range of the MCMC posterior predictions for the best-fit α, β and DBI parameters would falsify the viability statement.

Figures

Figures reproduced from arXiv: 2606.21839 by Behnam Pourhassan, Bidisha Samanta, Goutam Manna, Mayur Mune, Praveen Kumar Dhankar, Safiqul Islam.

Figure 1
Figure 1. Figure 1: Bayesian inference using a Gaussian approxi [PITH_FULL_IMAGE:figures/full_fig_p008_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Bayesian inference for all models with Gaus [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of Hubble cosmic chronometer data fits for all models. Table II lists the best-fit constraints on the Hub￾ble constant H0, the present-day matter density Ωm0 , and the sound-horizon scale rd for ΛCDM, wCDM, and our f(Q, T) + DBI model, using the combined Hubble, Pantheon+SH0ES, and DESIBAO datasets. For the standard scenarios, we obtain H0 ≃ 68.932 ± 1.867 km s−1 Mpc−1 , Ωm0 ≃ 0.303 ± 0.007, and… view at source ↗
Figure 5
Figure 5. Figure 5: Error-bar plot of the H(z) measurements compared with the best-fit f(Q, T) + DBI model, as well as the best-fit wCDM and ΛCDM models [PITH_FULL_IMAGE:figures/full_fig_p017_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Corner plot showing the 1D marginalized posteriors and 2D joint credible regions (68% and 95%) from the joint analysis of H(z) and Pantheon+SHOES supernovae [PITH_FULL_IMAGE:figures/full_fig_p018_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Distance modulus µ(z) from the Pan￾theon+SHOES sample compared with the best-fit f(Q, T) + DBI model and the corresponding ΛCDM prediction. Error bars indicate the observational un￾certainties [PITH_FULL_IMAGE:figures/full_fig_p018_7.png] view at source ↗
Figure 10
Figure 10. Figure 10: Marginalized 1σ and 2σ confidence contours for the model parameters obtained from the H(z)-only, Pantheon+SHOES-only, and joint H(z)+Pantheon+SHOES analyses. The combined dataset reduces parameter degeneracies and tightens the constraints on H0, Ωm0, β, and λ. • [PITH_FULL_IMAGE:figures/full_fig_p019_10.png] view at source ↗
read the original abstract

We investigate late-time cosmology in extended symmetric teleparallel gravity coupled to a Dirac-Born-Infeld (DBI) scalar field within $f(Q,T)$ gravity, where $Q$ is the non-metricity scalar and $T$ is the trace of the matter energy-momentum tensor. Working on a spatially flat Friedmann-Lema\^itre-Robertson-Walker background and treating the cosmic medium as an effective perfect fluid, we derive the background field equations for $f(Q,T)+\mathrm{DBI}$ gravity and obtain analytic solutions for the linear choice $f(Q,T)=\alpha Q+\beta T$. We then constrain the model parameters with a Markov Chain Monte Carlo analysis using Hubble-rate data, DESI BAO (DR2) measurements, and the Pantheon+SHOES Type~Ia supernova sample. The joint posteriors (Tables II and III) are broadly consistent with current late-time constraints and allow a direct comparison with $\Lambda$CDM, quantifying the departures driven by the $\beta T$ coupling and the DBI sector. Although the model does not reproduce every observational feature exactly, it provides a statistically viable alternative avenue to the standard paradigm and a useful framework for exploring potential remedies to existing tensions, including the $H_0$ discrepancy, without claiming a definitive resolution.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper derives background field equations for f(Q,T) gravity coupled to a DBI scalar field on flat FLRW, treating the medium as an effective perfect fluid. For the linear choice f(Q,T)=αQ+βT it obtains analytic solutions and performs MCMC constraints using Hubble-rate, DESI BAO (DR2), and Pantheon+SHOES data. The resulting joint posteriors (Tables II and III) are reported to be consistent with late-time observations and to position the model as a statistically viable alternative to ΛCDM, with quantified departures from the βT coupling and DBI sector.

Significance. If the background equations and perfect-fluid treatment are valid, the work supplies concrete observational bounds on α and β, enables direct comparison with ΛCDM, and offers a framework for exploring remedies to the H0 tension. The inclusion of recent DESI BAO data and the analytic solutions for the linear model are positive features that facilitate reproducibility of the fits.

major comments (2)
  1. [background field equations section] Background field equations section: the derivation adopts the effective perfect-fluid ansatz for the cosmic medium without demonstrating that the non-canonical DBI kinetic term remains compatible with this form once coupled to the βT piece of f(Q,T). If anisotropic stress or modified continuity equations arise, the Friedmann equations underlying the MCMC analysis would be incomplete, directly affecting the reliability of the posteriors in Tables II and III and the viability claim.
  2. [analytic solutions] Analytic solutions for linear f(Q,T)=αQ+βT: it is not shown whether these closed-form expressions satisfy the full set of modified continuity and acceleration equations that include the DBI contributions; an explicit substitution back into the field equations (or a numerical cross-check) is required to confirm internal consistency before the solutions can be used for parameter fitting.
minor comments (2)
  1. [Tables II and III] Tables II and III: reporting only marginalised posteriors without the corresponding minimum χ² values or Δχ² relative to ΛCDM makes it difficult to judge the absolute goodness-of-fit and the statistical weight of the claimed viability.
  2. Notation: the effective equation-of-state parameter for the combined f(Q,T)+DBI system is introduced without an explicit definition in terms of the DBI Lagrangian and the βT coupling; a short clarifying equation would improve readability.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments, which help improve the clarity of the manuscript. We address each major comment point by point below.

read point-by-point responses

  1. Referee: [background field equations section] Background field equations section: the derivation adopts the effective perfect-fluid ansatz for the cosmic medium without demonstrating that the non-canonical DBI kinetic term remains compatible with this form once coupled to the βT piece of f(Q,T). If anisotropic stress or modified continuity equations arise, the Friedmann equations underlying the MCMC analysis would be incomplete, directly affecting the reliability of the posteriors in Tables II and III and the viability claim.

    Authors: The effective perfect-fluid ansatz is preserved because the flat FLRW symmetries force the DBI stress-energy tensor to remain diagonal and isotropic, with no anisotropic stress generated by the non-canonical kinetic term. The βT coupling enters only through the trace T, which is a scalar, and is absorbed into the definitions of the effective energy density and pressure that appear in the modified Friedmann equations. The continuity equation is accordingly modified and is already incorporated when deriving the background equations used for the MCMC fits. We will add a short clarifying paragraph in the background-equations section to make this compatibility explicit. revision: yes

  2. Referee: [analytic solutions] Analytic solutions for linear f(Q,T)=αQ+βT: it is not shown whether these closed-form expressions satisfy the full set of modified continuity and acceleration equations that include the DBI contributions; an explicit substitution back into the field equations (or a numerical cross-check) is required to confirm internal consistency before the solutions can be used for parameter fitting.

    Authors: The closed-form solutions are obtained by direct integration of the complete set of background equations that already contain the DBI contributions to ρ and p. They therefore satisfy the full system by construction. To address the request for explicit verification, we will insert a brief appendix that substitutes the analytic expressions back into the modified continuity and acceleration equations and confirms that they hold identically; a short numerical consistency check for sample parameter values will also be included. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation and fitting are independent steps

full rationale

The paper first derives the background field equations from the f(Q,T)+DBI action on flat FLRW under the effective perfect-fluid assumption, obtains analytic solutions for the linear ansatz f(Q,T)=αQ+βT, and only then performs MCMC parameter estimation on Hubble+BAO+SNIa data. The consistency statement and quantified departures are outputs of that standard fit rather than a claimed first-principles prediction that reduces to the fitted inputs by construction. No self-definitional equations, load-bearing self-citations, or uniqueness theorems imported from the authors' prior work appear in the derivation chain. The central claim therefore remains self-contained against external data.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Abstract supplies only the linear ansatz and standard cosmological assumptions; full ledger cannot be completed without the manuscript.

free parameters (2)
  • α
    Coefficient multiplying the non-metricity scalar Q; fitted to data.
  • β
    Coefficient multiplying the trace T; fitted to data and drives the reported departures from ΛCDM.
axioms (2)
  • domain assumption Spatially flat FLRW metric
    Standard background assumption invoked for late-time cosmology.
  • domain assumption Cosmic medium treated as effective perfect fluid
    Used to close the background field equations.

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