Baryon bias and structure formation in an accelerating universe

By Luca Amendola, D. Tocchini-Valentini. 2001

181 citations recorded by the source corpus.

In most models of dark energy the structure formation stops after the accelerated expansion begins. In contrast, we show that the coupling of dark energy to dark matter may induce the growth of perturbations even in the accelerated regime. In particular, we show that this occurs in the models proposed to solve the cosmic coincidence problem, in which the ratio of dark energy to dark matter is constant. Depending on the parameters, the growth may be much faster than in a standard matter-dominated era. Moreover, if the dark energy couples only to dark matter and not to baryons, as requested by the constraints imposed by local gravity measurements, the baryon fluctuations develop a constant, scale-independent, large-scale bias which is in principle directly observable. We find that a lower limit to the baryon bias $bg0.5$ requires the total effective parameter of state ${w}_{e}=1+p/\ensuremath{\rho}$ to be larger than $0.6$ while a limit $bg0.73$ would rule out the model.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/eb79dec2f8818b6183ad44f9b669d52db4aa8afd

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Citations in the corpus

The Cosmological Constant and Dark Energy (2002, background): “An example is discussed by Amendola and Tocchini-Valentini (2002).”
Observational constraints on an interacting dark energy model (2009, background): “…a non-gravitational ‘drag’ on dark matter, and thus can introduce new features to structure formation, including possibly a new large-scale bias (Amendola & Tocchini-Valentini 2002) and a violation by dark matter of the weak equivalence principle on cosmological scales (Bertolami et al. 2007;…”
Cluster number counts dependence on dark energy inhomogeneities and coupling to dark matter (2005, background): “A non-minimal coupling of the quintessence field to dark matter is therefore worth investigating (Amendola 2000; Mainini & Bonometo 2004; Amendola & Tocchini-Valentini 2002a; Farrar & Peebles 2004; Amendola & Tocchini-Valentini 2002b; Wetterich 1995; Tocchini-Valentini & Amendola 2002).”
Structure formation in inhomogeneous dark energy models (2004, background): “3 C O U P L E D QU I N T E S S E N C E Let us now look at the case when the scalar field has a coupling with all or part of the dark matter (see for e.g. Amendola 2004; Tocchini-Valentini & Amendola 2002; Amendola & Tocchini-Valentini 2002).”
The growth of structure in interacting dark energy models (2009, background): “And interacting dark energy, by exerting a non-gravitational ‘drag’ on dark matter, introduces new features to structure formation, including possibly a new bias [4] and a violation by dark matter of the weak equivalence principle [5, 6].”
Interacting Dark Matter and Dark Energy (2003, methodology): “…b ð Þ @ @t ¼ 4 G bð1þ Þ : ð19Þ This differs from the usual expression by the factor 1þ , which takes into account the fifth force, and the part ̇b=ð b Þ, from the evolving DM particle mass (as has been discussed by Amendola & Tocchini-Valentini 2002; Matarrese, Pietroni, & Schimd 2003; and others).”