2004/02/05 by Patrick Crotty, Julien Lesgourgues, S. Pastor +1 · 2 citations
Physics and Astronomy · #Anisotropy #Astrophysics #CMB cold spot #Cosmic microwave background #Cosmology and Gravitation Theories #Massless particle #Neutrino #Neutrino Physics Research #Particle physics #Particle physics theoretical and experimental studies #Physics #Planck #Quantum mechanics #Supernova #Upper and lower bounds #astro-ph #hep-ph
paper · pdf · doi:10.1103/physrevd.69.123007
published as Phys.Rev.D69:123007,2004 · 13 pages, 6 figures
arxiv created 2004/02/05 · openalex publication_date 2004/06/25 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We combine the most recent observations of large-scale structure (2dF and SDSS galaxy surveys) and cosmic microwave anisotropies (WMAP and ACBAR) to put constraints on flat cosmological models where the number of massive neutrinos and of massless relativistic relics are both left arbitrary. We discuss the impact of each data set and of various priors on our bounds. For the standard case of three thermalized neutrinos, we find \ensuremath∑m_\ensuremathν<1.0 (respectively, 0.6) eV (at 2\ensuremathσ), using only CMB and LSS data (respectively, including priors from supernova data and the HST Key Project), a bound that is quite insensitive to the splitting of the total mass between the three species. When the total number of neutrinos or relativistic relics, Neff, is left free, the upper bound on \ensuremath∑m_\ensuremathν (at 2\ensuremathσ, including all priors) ranges from 1.0 to 1.5 eV depending on the mass splitting. We provide an explanation of the parameter degeneracy that allows larger values of the masses when Neff increases. Finally, we show that the limit on the total neutrino mass is not significantly modified in the presence of primordial gravitational waves, because current data provide a clear distinction between the corresponding effects.