Large‐scale cosmic microwave background anisotropies and dark energy

By Jochen Weller, A. Lewis. 2003

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In this note we investigate the effects of perturbations in a dark energy component with a constant equation of state on large scale cosmic microwave background anisotropies. The inclusion of perturbations increases the large scale power. We investigate more speculative dark energy models with w < 1 and find the opposite behaviour. Overall the inclusion of perturbations in the dark energy component increases the degeneracies. We generalise the parameterization of the dark energy fluctuations to allow for an arbitrary constant sound speeds and show how constraints from cosmic microwave background experiments change if this is included. Combining cosmic microwave background with large scale structure, Hubble parameter and Supernovae observations we obtain w = 1.02 ± 0.16 (1σ) as a constraint on the equation of state, which is almost independent of the sound speed chosen. With the presented analysis we find no significant constraint on the constant speed of sound of the dark energy component.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0a3ee735a0e0ea094cf75dc153fd355e29db23eb

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Citations in the corpus

Observational probes of cosmic acceleration (2012, background): “…models that have a sound speed (c2s = δp/δρ) much smaller than c allow fluctuations to grow on sub-horizon scales (e.g., Hu 1998; Erickson et al. 2002; Weller and Lewis 2003; DeDeo et al. 2003; Bean and Doré 2004). de Putter et al. (2010) provide a clear discussion of the background physics and…”
The effective theory of quintessence: the w < 1 side unveiled (2008, background): “The effect of a clustering quintessence can be measured with the cosmic microwave background [22, 23, 24, 25], galaxy redshift surveys [26], large neutral hydrogen surveys [27], or by cross-correlating the integrated Sachs-Wolfe effect in the cosmic microwave background with large scale structures [”
A kinematical approach to dark energy studies (2006, background): “Current data allow models with w < −1 (Weller & Lewis 2003; Riess et al. 2004; Allen et al. 2004; Astier et al. 2005; Spergel et al. 2006; Cabre et al. 2006) and models in which w(z) crosses the boundary w = −1 c© 2005 RAS, MNRAS 000, 1–12 (Jassal et al. 2005; Corasaniti et al. 2004; Seljak et al.…”
Weighing the giants – IV. Cosmology and neutrino mass (2014, methodology): “…(Section 4.4), as in our previous analyses, we obtain the contribution of the ISW effect to the anisotropy power spectrum of the CMB temperature fluctuations through an integral over time of the variation of the gravitational potential with respect to conformal time, φ̇ (Weller & Lewis 2003).”
WMAP constraints on low redshift evolution of dark energy (2004, background): “Perturbations in dark energy also lead to observable signatures, though these can easily be confused with other physical effects (Caldwell, Dave & Steinhardt 1998; Weller & Lewis 2003; Bean & Doré 2004).”
Using the Full Power of the Cosmic Microwave Background to Probe Axion Dark Matter (2017, background): “(18) Equivalent expressions for scalar-field variables are given in Weller & Lewis (2003); Bean & Doré (2004).”