Constraints on Quintom Dark Energy Model with Matter Interaction
Abstract
The quintom model consisting of quintessence and phantom scalar fields with linear coupling to matter is explored and constrained by updated DESI and supernovae type Ia~(SNIa) observational data. The matter interaction is assumed only between phantom and matter and the quintessence self potential is in an exponential form. The quintom evolution shows a class of solutions with phantom crossing scenario consistent with the current DESI data. From low redshift observations, we place constraints on the model with BAO data from DESI and distance measurements from SNIa Pantheon+ samples and SH0Es. For high-redshift constraints, we use CMB priors from Planck and found that the quintom model gives the best-fit Hubble parameter H0=65.780 (68.736)~km s−1 Mpc−1 for DESI+CMB+SNIa~(+SH0ES) respectively. The marginalized statistical constrained values are H0=66.21± 0.84 (68.49+0.46−0.40)~km s−1 Mpc−1 for DESI+CMB+SNIa~(+SH0ES) respectively. Using the BBN prior for high-redshift constraints, the corresponding best-fit values for DESI+BBN+SNIa~(+SH0ES) constraints are H0=63.999 (71.962)~km s−1 Mpc−1 and the marginalized statistical values for DESI+BBN+SNIa~(+SH0ES) constraints are H0=61.6+6.6−3.0 (71.86± 0.88)~km s−1 Mpc−1 respectively. Generally, adding SH0ES significantly raises the best-fit and marginalized value of H0 for all datasets. In comparison to ΛCDM, the interacting quintom model gives lower values of σ8=0.74−0.79 for combination of datasets with CMB prior. Lastly, the fifth-force constraint from local scale solar system Cassini probe is estimated, we find the constraint on the phantom-matter coupling |δ|<3.3× 10−3.
Related
- A Natural Dark Matter-Dark Energy Interaction from Axion-Monopole Dynamics
- Constraints on interacting dark energy with a constant equation of state in light of DESI DR2: The role of the interaction term
- Higgsino dark matter compatible with the LUX-ZEPLIN high-energy nuclear-recoil event and IceCube constraints
- JWST lensed quasar dark matter survey. IV. Stringent warm dark matter constraints from the joint reconstruction of extended lensed arcs and quasar flux ratios
- Direct detection constraints on EFT operators for inelastic dark matter
BibTeX
@misc{kaeonikhom2026constraints,
title = {{Constraints on Quintom Dark Energy Model with Matter Interaction}},
author = {Chakkrit Kaeonikhom and Theppawan Rukpakawong and Piyabut Burikham},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.08523},
eprint = {2611.08523},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.08523},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Constraints on Quintom Dark Energy Model with Matter Interaction
AU - Chakkrit Kaeonikhom
AU - Theppawan Rukpakawong
AU - Piyabut Burikham
PY - 2026
DA - 2026/11/01
PB - arXiv
DO - 10.48550/arxiv.2611.08523
UR - https://arxiv.org/abs/2611.08523
AB - The quintom model consisting of quintessence and phantom scalar fields with linear coupling to matter is explored and constrained by updated DESI and supernovae type Ia~(SNIa) observational data. The matter interaction is assumed only between phantom and matter and the quintessence self potential is in an exponential form. The quintom evolution shows a class of solutions with phantom crossing scenario consistent with the current DESI data. From low redshift observations, we place constraints on the model with BAO data from DESI and distance measurements from SNIa Pantheon+ samples and SH0Es. For high-redshift constraints, we use CMB priors from Planck and found that the quintom model gives the best-fit Hubble parameter H_0=65.780 (68.736)~km s^−1 Mpc^−1 for DESI+CMB+SNIa~(+SH0ES) respectively. The marginalized statistical constrained values are H_0=66.21± 0.84 (68.49^+0.46_−0.40)~km s^−1 Mpc^−1 for DESI+CMB+SNIa~(+SH0ES) respectively. Using the BBN prior for high-redshift constraints, the corresponding best-fit values for DESI+BBN+SNIa~(+SH0ES) constraints are H_0=63.999 (71.962)~km s^−1 Mpc^−1 and the marginalized statistical values for DESI+BBN+SNIa~(+SH0ES) constraints are H_0=61.6^+6.6_−3.0 (71.86± 0.88)~km s^−1 Mpc^−1 respectively. Generally, adding SH0ES significantly raises the best-fit and marginalized value of H_0 for all datasets. In comparison to ΛCDM, the interacting quintom model gives lower values of σ_8=0.74−0.79 for combination of datasets with CMB prior. Lastly, the fifth-force constraint from local scale solar system Cassini probe is estimated, we find the constraint on the phantom-matter coupling |δ|<3.3× 10^−3.
ER -