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Similar

Alkistis Pourtsidou and Thomas Tram, “Reconciling CMB and structure growth measurements with dark energy interactions,” Phys. Rev. D 94
Original
2016
Cited alongside, same era.
Rafael C. Nunes, Supriya Pan, and Emmanuel N. Saridakis, “New constraints on interacting dark energy from cosmic chronometers,” Phys. Rev. D 94
Original
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Cited alongside, same era.
Michael Kopp, Constantinos Skordis, and Dan B. Thomas, “Extensive investigation of the generalized dark matter model,” Phys. Rev. D 94
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Then

Jian-Ping Hu and Fa-Yin Wang, “Hubble Tension: The Evidence of New Physics,” Universe 9
Original
2023
Later among the works it cites.
Licia Verde, Nils Schöneberg, and Héctor Gil-Marín, “A tale of many H 0 H_{0} ,” (2023), arXiv:2311.13305 [astro-ph.CO]
Original
2023
Later among the works it cites.
T. M. C. Abbott et al. (Kilo-Degree Survey, DES), “DES Y3 + KiDS-1000: Consistent cosmology combining cosmic shear surveys,” Open J. Astrophys. 6
Original
2023
Later among the works it cites.
Roohi Dalal et al. , “Hyper Suprime-Cam Year 3 results: Cosmology from cosmic shear power spectra,” Phys. Rev. D 108
Original
2023
Later among the works it cites.
Andrej Dvornik et al. , “KiDS-1000: Combined halo-model cosmology constraints from galaxy abundance, galaxy clustering and galaxy-galaxy lensing,” Astron. Astrophys. 675

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2025

A low-redshift preference for an interacting dark energy model

Zhai, Yuejia, de Cesare, Marco, van de Bruck, Carsten et al.

Understand

We explore an interacting dark sector model in trace-free Einstein gravity where dark energy has a constant equation of state, $w=-1$, and the energy-momentum transfer potential is proportional to the cold dark matter density.

Compared to the standard $\Lambda$CDM model, this scenario introduces a single additional dimensionless parameter, $\epsilon$, which determines the amplitude of the transfer potential.
Using a combination of \textit{Planck} 2018 Cosmic Microwave Background (CMB), DESI 2024 Baryon Acoustic Oscillation (BAO), and Pantheon+ Type Ia supernovae (SNIa) data, we derive stringent constraints on the interaction, finding $\epsilon$ to be of the order of $\sim \mathcal{O}(10^{-4})$.
While CMB and SNIa data alone do not favor the presence of such an interaction, the inclusion of DESI data introduces a mild $1\sigma$ preference for an energy-momentum transfer from dark matter to dark energy.