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Peer-reviewedCC BY 4.0The European Physical Journal C

Testing the direction of dark sector interaction using late-time datasets

  • Anil Kandel1
  • Phongpichit Channuie2
  • Ertan Güdekli3
  • Farruh Atamurotov4,5,6
6 affiliations
  1. 1Tribhuvan University
  2. 2Walailak University
  3. 3Istanbul University
  4. 4National University of Uzbekistan
  5. 5University of Tashkent for Applied Sciences
  6. 6Andijan State University
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Abstract

We constrain the phenomenological interacting dark energy ( ξ ξ IDE) model, in which the relative evolution of dark matter and dark energy is characterized by the scaling relation ρ X/ρ m ∝ aξ ρ X / ρ m ∝ a ξ , using baryon acoustic oscillation measurements from DESI Data Releases 1 and 2, combined with cosmic chronometers, compressed CMB likelihoods, and the Pantheon + + , DES-Dovekie, and Union3 Type Ia supernova samples. Parameter constraints are obtained using the cosmological inference code . Relative to Λ Λ CDM, the ξ ξ IDE model mildly favors higher values of the Hubble constant, reducing but not resolving the H0 H 0 tension. The parameter ξ ξ remains close to its Λ Λ CDM limit, while most dataset combinations favor wX>−1 w X > - 1 , indicating a mild preference for quintessence-like dark energy. The interaction combination ξ +3wX ξ + 3 w X is negative for all dataset combinations, corresponding to energy transfer from dark energy to dark matter. The strongest deviation from the non-interacting limit is obtained for CMB + DESI DR2 + CC + Union3, with ξ +3wX=−0.035± 0.023 ξ + 3 w X = - 0.035 ± 0.023 , corresponding to only 1.52σ 1.52 σ . Although the Nσ N σ statistic shows a weak preference for the interacting scenario, Bayesian evidence consistently favors Λ Λ CDM. Overall, observations provide no compelling evidence for a nonzero dark-sector interaction, despite a consistent mild preference for energy transfer from dark energy to dark matter.

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Cite

BibTeXRIS
BibTeX
@article{kandel2026testing,
  title = {{Testing the direction of dark sector interaction using late-time datasets}},
  author = {Anil Kandel and Phongpichit Channuie and Ertan Güdekli and Farruh Atamurotov},
  journal = {The European Physical Journal C},
  year = {2026},
  month = oct,
  doi = {10.1140/epjc/s10052-026-16492-4},
  url = {https://link.springer.com/article/10.1140/epjc/s10052-026-16492-4},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Testing the direction of dark sector interaction using late-time datasets
AU  - Anil Kandel
AU  - Phongpichit Channuie
AU  - Ertan Güdekli
AU  - Farruh Atamurotov
PY  - 2026
DA  - 2026/10/23
JO  - The European Physical Journal C
DO  - 10.1140/epjc/s10052-026-16492-4
UR  - https://link.springer.com/article/10.1140/epjc/s10052-026-16492-4
AB  - We constrain the phenomenological interacting dark energy ( ξ ξ IDE) model, in which the relative evolution of dark matter and dark energy is characterized by the scaling relation ρ _X/ρ _m ∝ a^ξ  ρ X / ρ m ∝ a ξ , using baryon acoustic oscillation measurements from DESI Data Releases 1 and 2, combined with cosmic chronometers, compressed CMB likelihoods, and the Pantheon ^+ + , DES-Dovekie, and Union3 Type Ia supernova samples. Parameter constraints are obtained using the cosmological inference code . Relative to Λ Λ CDM, the ξ ξ IDE model mildly favors higher values of the Hubble constant, reducing but not resolving the H_0 H 0 tension. The parameter ξ ξ remains close to its Λ Λ CDM limit, while most dataset combinations favor w_X>−1 w X > - 1 , indicating a mild preference for quintessence-like dark energy. The interaction combination ξ +3w_X ξ + 3 w X is negative for all dataset combinations, corresponding to energy transfer from dark energy to dark matter. The strongest deviation from the non-interacting limit is obtained for CMB + DESI DR2 + CC + Union3, with ξ +3w_X=−0.035± 0.023 ξ + 3 w X = - 0.035 ± 0.023 , corresponding to only 1.52σ 1.52 σ . Although the Nσ N σ statistic shows a weak preference for the interacting scenario, Bayesian evidence consistently favors Λ Λ CDM. Overall, observations provide no compelling evidence for a nonzero dark-sector interaction, despite a consistent mild preference for energy transfer from dark energy to dark matter.
SN  - 1434-6044
SN  - 1434-6052
ER  -