Spherical collapse in νΛCDM

Marilena LoVerde
Phys. Rev. D 90, 083518 – Published 17 October 2014

Abstract

The abundance of massive dark matter halos hosting galaxy clusters provides an important test of the masses of relic neutrino species. The dominant effect of neutrino mass is to lower the typical amplitude of density perturbations that eventually form halos, but for neutrino masses 0.4eV the threshold for halo formation can be changed significantly as well. We study the spherical collapse model for halo formation in cosmologies with neutrino masses in the range mνi=0.051eV and find that halo formation is differently sensitive to Ων and mν. That is, different neutrino hierarchies with a common Ων are in principle distinguishable. The added sensitivity to mν is small but potentially important for scenarios with heavier sterile neutrinos. Massive neutrinos cause the evolution of density perturbations to be scale dependent at high redshift which complicates the usual mapping between the collapse threshold and halo abundance. We propose one way of handling this and compute the correction to the halo mass function within this framework. For mνi0.3eV, our prescription for the halo abundance is only 15% different than the standard calculation. However for larger neutrino masses the differences approach 50–100% which, if verified by simulations, could alter neutrino mass constraints from cluster abundance.

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  • Received 11 June 2014

DOI:https://doi.org/10.1103/PhysRevD.90.083518

© 2014 American Physical Society

Authors & Affiliations

Marilena LoVerde

  • Enrico Fermi Institute, Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, University of Chicago, Illinois 60637, USA

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Issue

Vol. 90, Iss. 8 — 15 October 2014

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