Weighing neutrinos using high redshift galaxy luminosity functions

TL;DR

This paper demonstrates that high redshift galaxy luminosity functions can be used to place stringent constraints on the total mass of neutrinos, providing a complementary astronomical method to existing limits.

Contribution

It introduces a novel approach using galaxy luminosity functions and semi-analytic models to constrain neutrino masses, improving existing bounds significantly.

Findings

Neutrino mass sum constrained to < 0.52 eV using LF and WMAP7 data.

Adding Hubble constant prior tightens the neutrino mass limit to < 0.29 eV.

Method offers a complementary and potentially more precise way to measure neutrino masses.

Abstract

Laboratory experiments measuring neutrino oscillations, indicate small mass differences between different mass eigenstates of neutrinos. The absolute mass scale is however not determined, with at present the strongest upper limits coming from astronomical observations rather than terrestrial experiments. The presence of massive neutrinos suppresses the growth of perturbations below a characteristic mass scale, thereby leading to a decreased abundance of collapsed dark matter halos. Here we show that this effect can significantly alter the predicted luminosity function (LF) of high redshift galaxies. In particular we demonstrate that a stringent constraint on the neutrino mass can be obtained using the well measured galaxy LF and our semi-analytic structure formation models. Combining the constraints from the Wilkinson Microwave Anisotropy Probe 7 year (WMAP7) data with the LF data at z = 4, we get a limit on the sum of the masses of 3 degenerate neutrinos \Sigma m_\nu < 0.52 eV at the 95 % CL. The additional constraints using the prior on Hubble constant strengthens this limit to \Sigma m_\nu < 0.29 eV at the 95 % CL. This neutrino mass limit is a factor of order 4 improvement compared to the constraint based on the WMAP7 data alone, and as stringent as known limits based on other astronomical observations. As different astronomical measurements may suffer from different set of biases, the method presented here provides a complementary probe of \Sigma m_\nu . We suggest that repeating this exercise on well measured luminosity functions over different redshift ranges can provide independent and tighter constraints on \Sigma m_\nu .