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Limits on decaying dark energy density models from the CMB temperature-redshift relation

Jetzer, Philippe ; Puy, Denis ; Signore, Monique ; Tortora, Crescenzo

In: General Relativity and Gravitation, 2011, vol. 43, no. 4, p. 1083-1093

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    Titre
    • Limits on decaying dark energy density models from the CMB temperature-redshift relation
    Auteur
    • Jetzer, Philippe. Institut für Theoretische Physik, Universität Zürich, Winterthurerstrasse 190, 8057, Zürich, Switzerland
    • Puy, Denis. Groupe de Recherche d'Astronomie et d'Astrophysique du Languedoc, Université des Sciences Montpellier II, GRAAL CC72, 34095, Montpellier cedex 09, France
    • Signore, Monique. Observatoire de Paris, LERMA, 61 av. de l'Observatoire, 75014, Paris, France
    • Tortora, Crescenzo. Institut für Theoretische Physik, Universität Zürich, Winterthurerstrasse 190, 8057, Zürich, Switzerland
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • General Relativity and Gravitation, 2011, vol. 43, no. 4, p. 1083-1093. Springer US; http://www.springer-ny.com
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:310509
    Summary
    The nature of the dark energy is still a mystery and several models have been proposed to explain it. Here we consider a phenomenological model for dark energy decay into photons and particles as proposed by Lima (Phys Rev D 54:2571, 1996). He studied the thermodynamic aspects of decaying dark energy models in particular in the case of a continuous photon creation and/or disruption. Following his approach, we derive a temperature redshift relation for the cosmic microwave background (CMB) which depends on the effective equation of state w eff and on the "adiabatic index” γ. Comparing our relation with the data on the CMB temperature as a function of the redshift obtained from Sunyaev-Zel'dovich observations and at higher redshift from quasar absorption line spectra, we find w eff=−0.97 ± 0.03, adopting for the adiabatic index γ=4/3, in good agreement with current estimates and still compatible with w eff=−1, implying that the dark energy content being constant in time