What can be learned about dark energy evolution?

DOI10.1051/0004-6361:20065067zbMATH Open1151.85337arXivastro-ph/0602491OpenAlexW2108326946WikidataQ68673862 ScholiaQ68673862MaRDI QIDQ3530162

Author name not available (Why is that?)

Publication date: 15 October 2008

Published in: Astronomy & Astrophysics (Search for Journal in Brave)

Abstract: We examine constraints obtained from SNIa surveys on a two parameter model of dark energy in which the equation of state $w(z)=P(z)/ho(z)$ undergoes a transition over a period significantly shorter than the Hubble time. We find that a transition between $wsim-0.2$ and $wsim-1$ (the first value being somewhat arbitrary) is allowed at redshifts as low as 0.1, despite the fact that data extend beyond $zsim1$. Surveys with the precision anticipated for space experiments should allow only slight improvement on this constraint, as a transition occurring at a redshift as low as $sim0.17$ could still remain undistinguishable from a standard cosmological constant. The addition of a prior on the matter density $Omeg{a}_{M}AT=0.3$ only modestly improves the constraints. Even deep space experiments would still fail to identify a rapid transition at a redshift above 0.5. These results illustrate that a Hubble diagram of distant SNIa alone will not reveal the actual nature of dark energy at a redshift above 0.2 and that only the local dynamics of the quintessence field can be infered from a SNIa Hubble diagram. Combinations, however, seem to be very efficient: we found that the combination of present day CMB data and SNIa already excludes a transition at redshifts below 0.8.

Full work available at URL: https://arxiv.org/abs/astro-ph/0602491

zbMATH Keywords

cosmology: cosmological parameterscosmology: observationscosmology: cosmic microwave background

Mathematics Subject Classification ID

Radiative transfer in astronomy and astrophysics (85A25) Astrophysical cosmology (85A40)

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