Clustering of quintessence on horizon scales and its imprint on HI intensity mapping

Abstract

Quintessence can cluster only on horizon scales. What is the effect on the observed matter distribution? To answer this, we need a relativistic approach that goes beyond the standard Newtonian calculation and deals properly with large scales. Such an approach has recently been developed for the case when dark energy is vacuum energy, which does not cluster at all. We extend this relativistic analysis to deal with dynamical dark energy. Using three quintessence potentials as examples, we compute the angular power spectrum for the case of an HI intensity map survey. Compared to the concordance model with the same small-scale power at z=0, quintessence boosts the angular power by up to ~15% at high redshifts, while power in the two models converges at low redshifts. The difference is mainly due to the background evolution, driven mostly by the normalization of the power spectrum today. The dark energy perturbations make only a small contribution on the largest scales, and a negligible contribution on smaller scales. Ironically, the dark energy perturbations remove the false boost of large-scale power that arises if we impose the (unphysical) assumption that the dark energy is smooth.

8 pages, 4 figures. Typos in equations 27, 28 corrected; results unaffected

References in corpus (10)

• Dynamics of dark energy
• New Perspective on Galaxy Clustering as a Cosmological Probe: General Relativistic Effects
• Testing General Relativity with 21 cm intensity mapping
• Scalar Field Dark Energy Perturbations and their Scale Dependence
• Roles of dark energy perturbations in the dynamical dark energy models: Can we ignore them?
• Relativistic corrections and non-Gaussianity in radio continuum surveys
• Is the Dynamics of Tracking Dark Energy Detectable?
• Relativistic effects and primordial non-Gaussianity in the galaxy bias
• A comparison of perturbations in fluid and scalar field models of dark energy
• Confronting quintessence models with recent high-redshift supernovae data

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