Smoothing the $H_0$ tension with a dynamical dark energy model
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arXiv
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| Format: | Preprint |
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2023
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| author | Dahmani, Safae Bouali, Amine Bojaddaini, Imad El Errahmani, Ahmed Ouali, Taoufik |
| author_facet | Dahmani, Safae Bouali, Amine Bojaddaini, Imad El Errahmani, Ahmed Ouali, Taoufik |
| contents | The discrepancy between Planck data and direct measurements of the current expansion rate $H_0$ and the matter fluctuation amplitude $S_8$ has become one of the most intriguing puzzles in cosmology nowadays. The $H_0$ tension has reached $4.2σ$ in the context of standard cosmology i.e $Λ$CDM. Therefore, explanations to this issue are mandatory to unveil its secrets. Despite its success, $Λ$CDM is unable to give a satisfying explanation to the tension problem. Unless some systematic errors might be hidden in the observable measurements, physics beyond the standard model of cosmology must be advocated. In this perspective, we study a phantom dynamical dark energy model as an alternative to $Λ$CDM in order to explain the aforementioned issues. This phantom model is characterised by one extra parameter, $Ω_{pdde}$, compared to $Λ$CDM. We obtain a strong positive correlation between $H_0$ and $Ω_{pdde}$, for all data combinations. Using Planck measurements together with BAO and Pantheon, we find that the $H_0$ and the $S_8$ tensions are $3σ$ and $2.6σ$, respectively. By introducing a prior on the absolute magnitude, $M_B$, of the SN Ia, the $H_0$ tension decreases to $2.27σ$ with $H_0 = 69.76_{-0.82}^{+0.75}$ km s$^{-1}$ Mpc$^{-1}$ and the $S_8$ tension reaches the value $2.37σ$ with $S_8 =0.8269_{-0.012}^{+0.011}$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2301_04200 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Smoothing the $H_0$ tension with a dynamical dark energy model Dahmani, Safae Bouali, Amine Bojaddaini, Imad El Errahmani, Ahmed Ouali, Taoufik Cosmology and Nongalactic Astrophysics The discrepancy between Planck data and direct measurements of the current expansion rate $H_0$ and the matter fluctuation amplitude $S_8$ has become one of the most intriguing puzzles in cosmology nowadays. The $H_0$ tension has reached $4.2σ$ in the context of standard cosmology i.e $Λ$CDM. Therefore, explanations to this issue are mandatory to unveil its secrets. Despite its success, $Λ$CDM is unable to give a satisfying explanation to the tension problem. Unless some systematic errors might be hidden in the observable measurements, physics beyond the standard model of cosmology must be advocated. In this perspective, we study a phantom dynamical dark energy model as an alternative to $Λ$CDM in order to explain the aforementioned issues. This phantom model is characterised by one extra parameter, $Ω_{pdde}$, compared to $Λ$CDM. We obtain a strong positive correlation between $H_0$ and $Ω_{pdde}$, for all data combinations. Using Planck measurements together with BAO and Pantheon, we find that the $H_0$ and the $S_8$ tensions are $3σ$ and $2.6σ$, respectively. By introducing a prior on the absolute magnitude, $M_B$, of the SN Ia, the $H_0$ tension decreases to $2.27σ$ with $H_0 = 69.76_{-0.82}^{+0.75}$ km s$^{-1}$ Mpc$^{-1}$ and the $S_8$ tension reaches the value $2.37σ$ with $S_8 =0.8269_{-0.012}^{+0.011}$. |
| title | Smoothing the $H_0$ tension with a dynamical dark energy model |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2301.04200 |