Constraint on neutrino masses from SDSS-III/BOSS Lyα forest and other cosmological probes

By N. Palanque-Delabrouille, C. Yéche, Julien Lesgourgues, G. Rossi, A. Borde, M. Viel, E. Aubourg, David Kirkby, J. Legoff, J. Rich and 4 more. 2014

134 citations recorded by the source corpus.

We present constraints on the parameters of the ΛCDM cosmological model in the presence of massive neutrinos, using the one-dimensional Lyα forest power spectrum obtained with the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey (SDSS) by Palanque-Delabrouille et al. [1], complemented by additional cosmological probes. The interpretation of the measured Lyα spectrum is done using a second-order Taylor expansion of the simulated power spectrum. BOSS Lyα data alone provide better bounds than previous Lyα results, but are still poorly constraining, especially for the sum of neutrino masses ∑ mν, for which we obtain an upper bound of 1.1 eV (95% CL), including systematics for both data and simulations. Lyα constraints on ΛCDM parameters and neutrino masses are compatible with CMB bounds from the {\rm Planck} collaboration [2]. Interestingly, the combination of Lyα with CMB data reduces the uncertainties significantly, due to very different directions of degeneracy in parameter space, leading to the strongest cosmological bound to date on the total neutrino mass, ∑ mν < 0.15 eV at 95% CL (with a best-fit in zero). Adding recent BAO results further tightens this constraint to ∑ mν < 0.14 eV at 95% CL. This bound is nearly independent of the statistical approach used, and of the different combinations of CMB and BAO data sets considered in this paper in addition to Lyα. Given the measured values of the two squared mass differences Δ m2, this result tends to favor the normal hierarchy scenario against the inverted hierarchy scenario for the masses of the active neutrino species.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1833afbd49e0dda2cd9b91a82670f8c9f919ed74

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Citations in the corpus

Neutrinoless Double Beta Decay: 2015 Review (2016, methodology): “Quite recently, a very stringent limit, Σ < 146meV (2σ CL), was set by PalanqueDelabrouille and collaborators [136].”
The one-dimensional power spectrum from the SDSS DR14 Lyα forests (2018, methodology): “Using the model of [16, 17] where the power spectrum is described by four cosmological parameters, five parameters for a simplified model of the IGM thermal history, two for the mean transmitted flux, and nuisance parameters for astrophysical”
Neutrino masses and cosmology with Lyman-alpha forest power spectrum (2015, methodology): “This paper refers extensively to the earlier paper [2] that reported the first constraints on cosmological parameters and total neutrino mass using Lyα data from the SDSS-III/BOSS survey.”
Neutrino masses and mixings: Status of known and unknown 3ν parameters (2016, unknown): “[61–67] and references therein.”
KiDS-450: The tomographic weak lensing power spectrum and constraints on cosmological parameters (2017, methodology): “Combining the Planck CMB results with measurements of the Ly α power spectrum and BAO measurements yields the very stringent upper limit of mν < 0.14 eV at 95 per cent confidence (Palanque-Delabrouille et al. 2015).”
Multimodal Data Fusion: An Overview of Methods, Challenges, and Prospects (2015, background): “surveys, galaxy clustering [54], [55], and stacked gravitational lensing, also serve as important cosmological probes [51], [52].”
THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: OVERVIEW AND EARLY DATA (2015, methodology): “When combining the BOSS measurement with CMB and BAO measurements, the sum of the neutrino masses is constrained with a 95% upper limit ∑ mν < 0.15 eV (Palanque-Delabrouille et al. 2015b), improved to ∑ mν < 0.12 eV (Palanque-Delabrouille et al. 2015a).”
Lyman-alpha forests cool warm dark matter (2015, methodology): “Using a splicing technique described in [29] and first applied in [13, 30], we infer the flux power spectrum of an equivalent (L = 100 h−1 Mpc, N = 3072) simulation from a combination of three lesser ones: a scaled-down (25, 768) to provide high resolution on small scales, a large-box low-resolution”