Neutrino masses and the dark energy equation of state - relaxing the cosmological neutrino mass bound

TL;DR

When the dark energy equation of state parameter is taken as a free (but constant) parameter, the neutrino mass bound is sigma m(v) < or = 1.48 eV (95% C.L.) in the standard model where thedark energy is in the form of a cosmological constant.

Abstract

Cosmology at present provides the nominally strongest constraint on the masses of standard model neutrinos. However, this constraint extremely dependent on the nature of the dark energy component of the Universe. When the dark energy equation of state parameter is taken as a free (but constant) parameter, the neutrino mass bound is sum m_nu < 1.48 eV (95% C.L.), compared with sum m_nu < 0.65 eV (95% C.L.) in the standard model where the dark energy is in the form of a cosmological constant. This has important consequences for future experiments aimed at the direct measurement of neutrino masses. We also discuss prospects for future cosmological measurements of neutrino masses.

Figures (3)

• Figure 1: $\Delta \chi^2$ as a function of neutrino mass for various different data sets and parameter assumptions. The dashed line is for a fixed $w=-1$, using WMAP, SDSS, HST, and SNI-a data. The full line is for a free $w$ with the same data. The horizontal lines show $\Delta \chi^2 = 1$ and 4, corresponding to 68% and 95% C.L. respectively.
• Figure 2: 68% and 95% allowed contours as a function of neutrino mass and dark energy equation of state using WMAP, SDSS, HST, and SNI-a data.
• Figure 3: The value of $\Omega_m$ for the best fit models, as a function of $\sum m_\nu$. The curve labels are the same as in Fig. 1. The horizontal (red) lines are the 2$\sigma$ bounds from the present Riess et al. supernova data SNIA for the case of $w=-1$.