Constraints on neutrino physics from DESI DR2 BAO and DR1 full shape
The Dark Energy Spectroscopic Instrument (DESI) Collaboration has obtained robust measurements of baryon acoustic oscillations in the redshift range 0.1 < z < 4.2, based on the Lyman-a forest and galaxies from data release 2. We combine these measurements with cosmic microwave background (CMB)...
| Authors: | , , , , , , , , , |
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| Format: | article |
| Publication Date: | 2025 |
| Country: | España |
| Institution: | Universitat Politècnica de Catalunya (UPC) |
| Repository: | UPCommons. Portal del coneixement obert de la UPC |
| Language: | English |
| OAI Identifier: | oai:upcommons.upc.edu:2117/451071 |
| Online Access: | https://hdl.handle.net/2117/451071 https://dx.doi.org/10.1103/w9pk-xsk7 |
| Access Level: | Open access |
| Keyword: | Baryon acoustic oscillations Cosmic microwave background Dark energy Large scale structure of the Universe Neutrino mass Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| Summary: | The Dark Energy Spectroscopic Instrument (DESI) Collaboration has obtained robust measurements of baryon acoustic oscillations in the redshift range 0.1 < z < 4.2, based on the Lyman-a forest and galaxies from data release 2. We combine these measurements with cosmic microwave background (CMB) data from Planck and the Atacama Cosmology Telescope to place our tightest constraints yet on the sum of neutrino masses. Assuming the cosmological ¿CDM model and three degenerate neutrino states, we find P m¿ < 0.0642 eV (95%) with a marginalized error of sðP m¿Þ ¼ 0.020 eV. We also constrain the effective number of neutrino species, finding Neff ¼ 3.23þ0.35 -0.34 (95%), in line with the Standard Model prediction. When accounting for neutrino oscillation constraints, we find a preference for the normal mass ordering and an upper limit on the lightest neutrino mass of m l < 0.023 eV (95%). However, we determine using frequentist and Bayesian methods that our constraints are in tension with the lower limits derived from neutrino oscillations. Correcting for the physical boundary at zero mass, we report a 95% Feldman- Cousins upper limit of P m¿ < 0.053 eV, breaching the lower limit from neutrino oscillations. Considering a more general Bayesian analysis with an effective cosmological neutrino mass parameter, P m¿;eff , that allows for negative energy densities and removes unsatisfactory prior weight effects, we derive constraints that are in 3s tension with the same oscillation limit, while the error rises to sðP m¿;eff Þ ¼ 0.053 eV. In the absence of unknown systematics, this finding could be interpreted as a hint of new physics not necessarily related to neutrinos. The preference of DESI and CMB data for an evolving dark energy model offers one possible solution. In the w0waCDM model, we find P m¿ < 0.163 eV (95%), relaxing the neutrino tension. These constraints all rely on the effects of neutrinos on the cosmic expansion history. Using full-shape power spectrum measurements of data release 1 galaxies, we place complementary constraints that rely on neutrino free streaming. Our strongest such limit in ¿CDM, using selected CMB priors, is P m¿ < 0.193 eV (95%). |
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