Neutrino Mass Priors for Cosmology from Random Matrices

Abstract

Cosmological measurements of structure are placing increasingly strong constraints on the sum of the neutrino masses, $Σm_ν$, through Bayesian inference. Because these constraints depend on the choice for the prior probability $π(Σm_ν)$, we argue that this prior should be motivated by fundamental physical principles rather than the ad hoc choices that are common in the literature. The first step in this direction is to specify the prior directly at the level of the neutrino mass matrix $M_ν$, since this is the parameter appearing in the Lagrangian of the particle physics theory. Thus by specifying a probability distribution over $M_ν$, and by including the known squared mass splittings, we predict a theoretical probability distribution over $Σm_ν$ that we interpret as a Bayesian prior probability $π(Σm_ν)$. We find that $π(Σm_ν)$ peaks close to the smallest $Σm_ν$ allowed by the measured mass splittings, roughly $0.06 \, {\rm eV}$ ($0.1 \, {\rm eV}$) for normal (inverted) ordering, due to the phenomenon of eigenvalue repulsion in random matrices. We consider three models for neutrino mass generation: Dirac, Majorana, and Majorana via the seesaw mechanism; differences in the predicted priors $π(Σm_ν)$ allow for the possibility of having indications about the physical origin of neutrino masses once sufficient experimental sensitivity is achieved. We present fitting functions for $π(Σm_ν)$, which provide a simple means for applying these priors to cosmological constraints on the neutrino masses or marginalizing over their impact on other cosmological parameters.

16+2 pages, two column, 8 figures, 2 tables; v2 -- references added, matches PRD