A low-redshift preference for an interacting dark energy model
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| Format: | Preprint |
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2025
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| _version_ | 1866916657879842816 |
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| author | Zhai, Yuejia de Cesare, Marco van de Bruck, Carsten Di Valentino, Eleonora Wilson-Ewing, Edward |
| author_facet | Zhai, Yuejia de Cesare, Marco van de Bruck, Carsten Di Valentino, Eleonora Wilson-Ewing, Edward |
| contents | 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 $Λ$CDM model, this scenario introduces a single additional dimensionless parameter, $ε$, 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 $ε$ 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 $1σ$ preference for an energy-momentum transfer from dark matter to dark energy. This preference is primarily driven by low-redshift DESI BAO measurements, which favor a slightly lower total matter density $Ω_m$ compared to CMB constraints. Although the interaction remains weak and does not significantly alleviate the $H_0$ and $S_8$ tensions, our results highlight the potential role of dark sector interactions in late-time cosmology. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2503_15659 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A low-redshift preference for an interacting dark energy model Zhai, Yuejia de Cesare, Marco van de Bruck, Carsten Di Valentino, Eleonora Wilson-Ewing, Edward Cosmology and Nongalactic Astrophysics General Relativity and Quantum Cosmology High Energy Physics - Phenomenology 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 $Λ$CDM model, this scenario introduces a single additional dimensionless parameter, $ε$, 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 $ε$ 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 $1σ$ preference for an energy-momentum transfer from dark matter to dark energy. This preference is primarily driven by low-redshift DESI BAO measurements, which favor a slightly lower total matter density $Ω_m$ compared to CMB constraints. Although the interaction remains weak and does not significantly alleviate the $H_0$ and $S_8$ tensions, our results highlight the potential role of dark sector interactions in late-time cosmology. |
| title | A low-redshift preference for an interacting dark energy model |
| topic | Cosmology and Nongalactic Astrophysics General Relativity and Quantum Cosmology High Energy Physics - Phenomenology |
| url | https://arxiv.org/abs/2503.15659 |