Fluctuations in strongly coupled cosmologies

In the early Universe, a dual component made of coupled CDM and a scalar field Phi, if their coupling beta > root 3/ 2, owns an attractor solution, making them a stationary fraction of cosmic energy during the radiation dominated era. Along the attractor, both such components expand proportional to a(-4) and have early density parameters Omega(d) = 1/(4 ss(2)) and Omega(c) = 2 Omega(d) (field and CDM, respectively). In a previous paper it was shown that, if a further component, expanding proportional to a(-3), breaks such stationary expansion at z similar to 3- 5 x 10(3), cosmic components gradually acquire densities consistent with observations. This paper, first of all, considers the case that this component is warm. However, its main topic is the analysis of fluctuation evolution: out of horizon modes are then determined; their entry into horizon is numerically evaluated as well as the dependence of Meszaros effect on the coupling beta; finally, we compute: (i) transfer function and linear spectral function; (ii) CMB C-l spectra. Both are close to standard ACDM models; in particular, the former one can be so down to a scale smaller than Milky Way, in spite of its main DM component being made of particles of mass < 1 keV. The previously coupled CDM component, whose present density parameter is O(infinity '(-).), exhibits wider fluctuations delta p/p, but approximately beta-independent delta p values. We discuss how lower scale features of these cosmologies might ease quite a few problems that ACDM does not easily solve.