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

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