We use WMAP5 and other cosmological data to constrain model parameters in quintessence cosmologies, focusing also on their shift when we allow for non-vanishing neutrino masses. The Ratra-Peebles (RP) and SUGRA potentials are used here, as examples of slowly or fastly varying state parameter w(a). Both potentials depend on an energy scale Λ. Here we confirm the results of previous analysis with WMAP3 data on the upper limits on Λ, which turn out to be rather small (down to ∼ 10 -9 in RP cosmologies and ∼ 10 -5 for SUGRA). Our constraints on Λ are not heavily affected by the inclusion of neutrino mass as a free parameter. On the contrary, when the neutrino mass degree of freedom is opened, significant shifts in the best-fit values of other parameters occur. © 2009 IOP Publishing Ltd.
LA VACCA, G., Kristiansen, J. (2009). Dynamical dark energy model parameters with or without massive neutrinos. JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, 2009(7), 036-036 [10.1088/1475-7516/2009/07/036].
Dynamical dark energy model parameters with or without massive neutrinos
LA VACCA, GIUSEPPE;
2009
Abstract
We use WMAP5 and other cosmological data to constrain model parameters in quintessence cosmologies, focusing also on their shift when we allow for non-vanishing neutrino masses. The Ratra-Peebles (RP) and SUGRA potentials are used here, as examples of slowly or fastly varying state parameter w(a). Both potentials depend on an energy scale Λ. Here we confirm the results of previous analysis with WMAP3 data on the upper limits on Λ, which turn out to be rather small (down to ∼ 10 -9 in RP cosmologies and ∼ 10 -5 for SUGRA). Our constraints on Λ are not heavily affected by the inclusion of neutrino mass as a free parameter. On the contrary, when the neutrino mass degree of freedom is opened, significant shifts in the best-fit values of other parameters occur. © 2009 IOP Publishing Ltd.
I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
