Open AccessConstraints on perfect fluid and scalar field dark energy models from future redshift surveys
Author(s) -
Amendola L.,
Quercellini C.,
Giallongo E.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.08558.x
Subject(s) - physics , dark energy , redshift , astrophysics , baryon acoustic oscillations , cosmic microwave background , dark matter , matter power spectrum , photometric redshift , scalar field , supernova , cosmology , galaxy , mathematical physics , quantum mechanics , anisotropy
We discuss the constraints that future photometric and spectroscopic redshift surveys can put on dark energy through the baryon oscillations of the power spectrum. We model the dark energy either with a perfect fluid or a scalar field and take into account the information contained in the linear growth function. We show that the growth function helps to break the degeneracy in the dark energy parameters and reduce the errors on w 0 , w 1 roughly by 30 per cent, making more appealing multicolour surveys based on photometric redshifts. We find that a 200‐deg 2 spectroscopic survey reaching z ≈ 3 can constrain w 0 , w 1 to within Δ w 0 = 0.21, Δ w 1 = 0.26 , to Δ w 0 = 0.39, Δ w 1 = 0.54 using photometric redshifts with an absolute uncertainty of 0.02, and to Δ w 0 = 0.43, Δ w 1 = 0.66 with an uncertainty of 0.04. In the scalar field case, we show that the slope n of the inverse power‐law potential for dark energy can be constrained to Δ n = 0.26 (spectroscopic redshifts) or Δ n = 0.40 (photometric redshifts), i.e. better than with future ground‐based supernovae surveys or cosmic microwave background data.