Interacting dark energy constraints from Fermi GRBs and Pantheon+ SNe Ia with full GRB covariance
Abstract
The standard ΛCDM model faces long-standing theoretical and observational problems, such as the Hubble tension, which motivate extensions beyond ΛCDM, including interacting dark energy (IDE). Type Ia supernovae (SNe Ia) are precise probes of the late-time expansion history, while gamma-ray bursts (GRBs) can extend the Hubble diagram to higher redshifts. However, GRB cosmology depends on careful calibration and uncertainty modeling. Using an Amati relation calibrated with the corresponding low-redshift GRBs, we construct distance moduli for the high-redshift subsets of the 15-year \textit{Fermi}/GBM GOLD and FULL samples and combine them with Pantheon+ SNe Ia to compare flat ΛCDM, wCDM, IDE-ρde, and IDE-ρc models. The covariance of the calibrated Amati intercept and slope is propagated into a full, non-diagonal GRB distance-modulus covariance, and an effective residual scatter, σres,μ, is fitted jointly with the cosmological parameters. The GOLD and FULL samples yield very similar constraints on the main cosmological parameters. With either the full or diagonal GRB covariance, the IDE models do not improve likelihood sufficiently to compensate for their additional parameters, and the BIC favors ΛCDM. A SNe-only comparison shows that the additional constraining power of the GRBs is generally modest. Current GRB and Pantheon+ distance measurements provide no significant evidence for either of the two IDE interactions considered here.
Versions
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BibTeX
@misc{meng2026interacting,
title = {{Interacting dark energy constraints from Fermi GRBs and Pantheon+ SNe Ia with full GRB covariance}},
author = {Jianfeng Meng and Xiaofeng Yang and Yunliang Ren and Yangjun Shi and Bohao Wang and Jingze Li and Xiongwei Liu},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2606.00549},
eprint = {2606.00549},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2606.00549},
}
RIS
TY - UNPB
TI - Interacting dark energy constraints from Fermi GRBs and Pantheon+ SNe Ia with full GRB covariance
AU - Jianfeng Meng
AU - Xiaofeng Yang
AU - Yunliang Ren
AU - Yangjun Shi
AU - Bohao Wang
AU - Jingze Li
AU - Xiongwei Liu
PY - 2026
DA - 2026/10/03
PB - arXiv
DO - 10.48550/arxiv.2606.00549
UR - https://arxiv.org/abs/2606.00549
AB - The standard ΛCDM model faces long-standing theoretical and observational problems, such as the Hubble tension, which motivate extensions beyond ΛCDM, including interacting dark energy (IDE). Type Ia supernovae (SNe Ia) are precise probes of the late-time expansion history, while gamma-ray bursts (GRBs) can extend the Hubble diagram to higher redshifts. However, GRB cosmology depends on careful calibration and uncertainty modeling. Using an Amati relation calibrated with the corresponding low-redshift GRBs, we construct distance moduli for the high-redshift subsets of the 15-year \textit{Fermi}/GBM GOLD and FULL samples and combine them with Pantheon+ SNe Ia to compare flat ΛCDM, wCDM, IDE-ρ_de, and IDE-ρ_c models. The covariance of the calibrated Amati intercept and slope is propagated into a full, non-diagonal GRB distance-modulus covariance, and an effective residual scatter, σ_res,μ, is fitted jointly with the cosmological parameters. The GOLD and FULL samples yield very similar constraints on the main cosmological parameters. With either the full or diagonal GRB covariance, the IDE models do not improve likelihood sufficiently to compensate for their additional parameters, and the BIC favors ΛCDM. A SNe-only comparison shows that the additional constraining power of the GRBs is generally modest. Current GRB and Pantheon+ distance measurements provide no significant evidence for either of the two IDE interactions considered here.
ER -