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Non-linear evolution of the cosmic neutrino background

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Non-linear evolution of the cosmic neutrino background

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dc.contributor.author	Villaescusa Navarro, Francisco Antonio
dc.contributor.author	Bird, S.
dc.contributor.author	Peña Garay, Carlos
dc.contributor.author	Viel, M.
dc.date.accessioned	2013-11-28T12:07:59Z
dc.date.available	2013-11-28T12:07:59Z
dc.date.issued	2013
dc.identifier.citation	Villaescusa-Navarro, F. Bird, S. Peña Garay, Carlos Viel, M. 2013 Non-linear evolution of the cosmic neutrino background Journal Of Cosmology And Astroparticle Physics 03 3 019
dc.identifier.uri	http://hdl.handle.net/10550/31481
dc.description.abstract	We investigate the non-linear evolution of the relic cosmic neutrino background by running large box-size, high resolution N-body simulations which incorporate cold dark matter (CDM) and neutrinos as independent particle species. Our set of simulations explore the properties of neutrinos in a reference Lambda CDM model with total neutrino masses between 0.05-0.60 eV in cold dark matter haloes of mass 10(11) ¿ 10(15) h(-1) M-circle dot, over a redshift range z = 0 ¿ 2. We compute the halo mass function and show that it is reasonably well fitted by the Sheth-Tormen formula, once the neutrino contribution to the total matter is removed. More importantly, we focus on the CDM and neutrino properties of the density and peculiar velocity fields in the cosmological volume, inside and in the outskirts of virialized haloes. The dynamical state of the neutrino particles depends strongly on their momentum: whereas neutrinos in the low velocity tail behave similarly to CDM particles, neutrinos in the high velocity tail are not affected by the clustering of the underlying CDM component. We find that the neutrino (linear) unperturbed momentum distribution is modified and mass and redshift dependent deviations from the expected Fermi-Dirac distribution are in place both in the cosmological volume and inside haloes. The neutrino density profiles around virialized haloes have been carefully investigated and a simple fitting formula is provided. The neutrino profile, unlike the cold dark matter one, is found to be cored with core size and central density that depend on the neutrino mass, redshift and mass of the halo, for halos of masses larger than similar to 10(13.5) h(-1) M-circle dot. For lower masses the neutrino profile is best fitted by a simple power-law relation in the range probed by the simulations. The results we obtain are numerically converged in terms of neutrino profiles at the 10% level for scales above similar to 200 h(-1) kpc at z = 0, and are stable with respect to box-size and starting redshift of the simulation. Our findings are particularly important in view of upcoming large-scale structure surveys, like Euclid, that are expected to probe the non-linear regime at the percent level with lensing and clustering observations.
dc.relation.ispartof	Journal Of Cosmology And Astroparticle Physics, 2013, vol. 03, num. 3, p. 019
dc.subject	Cosmologia
dc.subject	Astrofísica
dc.title	Non-linear evolution of the cosmic neutrino background
dc.type	journal article	es_ES
dc.date.updated	2013-11-28T12:07:59Z
dc.identifier.doi	10.1088/1475-7516/2013/03/019
dc.identifier.idgrec	092063
dc.rights.accessRights	open access	es_ES
dc.identifier.url	10.1088/1475-7516/2013/03/019