Revisiting holographic dark energy after DESI 2024
Abstract New insights from the Dark Energy Spectroscopic Instrument (DESI) 2024 baryon acoustic oscillations (BAO) data, in conjunction with cosmic microwave background (CMB) and Type Ia supernova (SN) data, suggest that dark energy may not be a cosmological constant. In this work, we investigate th...
Saved in:
| Main Authors: | , , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
SpringerOpen
2025-06-01
|
| Series: | European Physical Journal C: Particles and Fields |
| Online Access: | https://doi.org/10.1140/epjc/s10052-025-14279-7 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1849725180616638464 |
|---|---|
| author | Tian-Nuo Li Yun-He Li Guo-Hong Du Peng-Ju Wu Lu Feng Jing-Fei Zhang Xin Zhang |
| author_facet | Tian-Nuo Li Yun-He Li Guo-Hong Du Peng-Ju Wu Lu Feng Jing-Fei Zhang Xin Zhang |
| author_sort | Tian-Nuo Li |
| collection | DOAJ |
| description | Abstract New insights from the Dark Energy Spectroscopic Instrument (DESI) 2024 baryon acoustic oscillations (BAO) data, in conjunction with cosmic microwave background (CMB) and Type Ia supernova (SN) data, suggest that dark energy may not be a cosmological constant. In this work, we investigate the cosmological implications of holographic dark energy (HDE) and interacting holographic dark energy (IHDE) models, utilizing CMB, DESI BAO, and SN data. By considering the combined DESI BAO and SN data, we determine that in the IHDE model, the parameter $$c > 1$$ c > 1 and the dark-energy equation of state w does not cross $$-1$$ - 1 at the $$1\sigma $$ 1 σ confidence level, whereas in the HDE model, it marginally falls below this threshold. Upon incorporating CMB data, we observe that in the HDE model, the parameter $$c < 1$$ c < 1 and w crosses $$-1$$ - 1 at a level beyond $$10\sigma $$ 10 σ . Conversely, for the IHDE model, the likelihood of w crossing $$-1$$ - 1 is considerably diminished, implying that the introduction of interaction within the HDE model could potentially resolve or mitigate the cosmic big rip conundrum. Furthermore, our analysis reveals that the HDE and IHDE models are statistically as viable as the $$\Lambda $$ Λ CDM model when assessing Bayesian evidence with DESI BAO data combined with SN data. However, when CMB data are added, the HDE and IHDE models are significantly less favored than the $$\Lambda $$ Λ CDM model. Our findings advocate for further exploration of the HDE and IHDE models using forthcoming, more precise late-universe observations. |
| format | Article |
| id | doaj-art-17d7a9eb78e74f1a925d4e7491ffb3e2 |
| institution | DOAJ |
| issn | 1434-6052 |
| language | English |
| publishDate | 2025-06-01 |
| publisher | SpringerOpen |
| record_format | Article |
| series | European Physical Journal C: Particles and Fields |
| spelling | doaj-art-17d7a9eb78e74f1a925d4e7491ffb3e22025-08-20T03:10:32ZengSpringerOpenEuropean Physical Journal C: Particles and Fields1434-60522025-06-0185611310.1140/epjc/s10052-025-14279-7Revisiting holographic dark energy after DESI 2024Tian-Nuo Li0Yun-He Li1Guo-Hong Du2Peng-Ju Wu3Lu Feng4Jing-Fei Zhang5Xin Zhang6Liaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern UniversityLiaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern UniversityLiaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern UniversitySchool of Physics, Ningxia UniversityLiaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern UniversityLiaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern UniversityLiaoning Key Laboratory of Cosmology and Astrophysics, College of Sciences, Northeastern UniversityAbstract New insights from the Dark Energy Spectroscopic Instrument (DESI) 2024 baryon acoustic oscillations (BAO) data, in conjunction with cosmic microwave background (CMB) and Type Ia supernova (SN) data, suggest that dark energy may not be a cosmological constant. In this work, we investigate the cosmological implications of holographic dark energy (HDE) and interacting holographic dark energy (IHDE) models, utilizing CMB, DESI BAO, and SN data. By considering the combined DESI BAO and SN data, we determine that in the IHDE model, the parameter $$c > 1$$ c > 1 and the dark-energy equation of state w does not cross $$-1$$ - 1 at the $$1\sigma $$ 1 σ confidence level, whereas in the HDE model, it marginally falls below this threshold. Upon incorporating CMB data, we observe that in the HDE model, the parameter $$c < 1$$ c < 1 and w crosses $$-1$$ - 1 at a level beyond $$10\sigma $$ 10 σ . Conversely, for the IHDE model, the likelihood of w crossing $$-1$$ - 1 is considerably diminished, implying that the introduction of interaction within the HDE model could potentially resolve or mitigate the cosmic big rip conundrum. Furthermore, our analysis reveals that the HDE and IHDE models are statistically as viable as the $$\Lambda $$ Λ CDM model when assessing Bayesian evidence with DESI BAO data combined with SN data. However, when CMB data are added, the HDE and IHDE models are significantly less favored than the $$\Lambda $$ Λ CDM model. Our findings advocate for further exploration of the HDE and IHDE models using forthcoming, more precise late-universe observations.https://doi.org/10.1140/epjc/s10052-025-14279-7 |
| spellingShingle | Tian-Nuo Li Yun-He Li Guo-Hong Du Peng-Ju Wu Lu Feng Jing-Fei Zhang Xin Zhang Revisiting holographic dark energy after DESI 2024 European Physical Journal C: Particles and Fields |
| title | Revisiting holographic dark energy after DESI 2024 |
| title_full | Revisiting holographic dark energy after DESI 2024 |
| title_fullStr | Revisiting holographic dark energy after DESI 2024 |
| title_full_unstemmed | Revisiting holographic dark energy after DESI 2024 |
| title_short | Revisiting holographic dark energy after DESI 2024 |
| title_sort | revisiting holographic dark energy after desi 2024 |
| url | https://doi.org/10.1140/epjc/s10052-025-14279-7 |
| work_keys_str_mv | AT tiannuoli revisitingholographicdarkenergyafterdesi2024 AT yunheli revisitingholographicdarkenergyafterdesi2024 AT guohongdu revisitingholographicdarkenergyafterdesi2024 AT pengjuwu revisitingholographicdarkenergyafterdesi2024 AT lufeng revisitingholographicdarkenergyafterdesi2024 AT jingfeizhang revisitingholographicdarkenergyafterdesi2024 AT xinzhang revisitingholographicdarkenergyafterdesi2024 |