Scalar Field Dark Energy Perturbations and their Scale Dependence

Abstract

We estimate the amplitude of perturbation in dark energy at different length scales for a quintessence model with an exponential potential. It is shown that on length scales much smaller than hubble radius, perturbation in dark energy is negligible in comparison to that in in dark matter. However, on scales comparable to the hubble radius (${\lambda }_p>1000\mathrm{Mpc}$) the perturbation in dark energy in general cannot be neglected. As compared to the $\Lambda$CDM model, large scale matter power spectrum is suppressed in a generic quintessence dark energy model. We show that on scales ${\lambda }_p<1000\mathrm{Mpc}$, this suppression is primarily due to different background evolution compared to $\Lambda$CDM model. However, on much larger scales perturbation in dark energy can effect matter power spectrum significantly. Hence this analysis can act as a discriminator between $\Lambda$CDM model and other generic dark energy models with $w_{de}\ne -1$.

12 pages, 13 figures, added new section, accepted for publication in Phys. Rev. D

References in corpus (12)

• WMAP constraints on low redshift evolution of dark energy
• Dark Energy and Gravity
• Interacting holographic generalized Chaplygin gas model
• Interacting Holographic Phantom
• Dynamical Dark Energy or Simply Cosmic Curvature?
• Holographic tachyon model of dark energy
• Structure formation in the presence of dark energy perturbations
• Interacting Energy Components and Observational $H(z)$ Data
• The Evolution of Universe with th B-I Type Phantom Scalar Field
• Direct evidence of acceleration from distance modulus redshift graph
• A mathematical analysis of the evolution of perturbations in a modified Chaplygin gas model
• Constraining the dark energy and smoothness-parameter with supernovae

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• Perturbed dark energy: classical scalar field versus tachyon