List of Footnotes

1		Continuously updated information on Euclid is available on http://www.euclid-ec.org.
2		This subsection is based on [49 ].
3		Not to be confused with a different formalism of the same name by other authors [457 ].
4		In presence of massive neutrinos $fg$ depends also on the scale $k$ [501 ].
5		If we assume that neutrinos have a non-vanishing mass, then the transfer function is also redshift-dependent.
6		http://camb.info/
7		See [420 ]. $&tidle;ξ(σ,π )$ is the Fourier transform of $Ps(k) = (1 + βμ2)2Pr (k)$ [485 ].
8		For this reason, early dark-energy models can have a much stronger impact.
9		http://www.sdss3.org/surveys/boss.php
10		http://wigglez.swin.edu.au/site/index.html
11		http://www.darkenergysurvey.org
12		http://www.mpe.mpg.de/erosita/
13		http://www.wfxt.eu/home/Overview.html
14		It is anyway worth noticing the controversial results of DAMA/LIBRA, and more recently of CoGeNT.
15		In this case we have added the contribution from BOSS at redshifts $0.1 < z < zmin$ , where $zmin = 0.5$ is the minimum redshift of the Euclid spectroscopic survey.
16		$BMN$ is the antisymmetric partner of the metric, which in heterotic string theory gives rise to the model-independent axion. The indices $M, N$ run over the spacetime dimensions, $0,...,D − 1$ .
17		Very few $N$ -body simulations of the non-local models are currently available and none of them has very high spatial resolution.
18		Strictly speaking, isocurvature perturbations are defined by the condition that their total energy density in the total comoving gauge vanishes, i.e., $∑ αδρ(αcom.)= 0$ . Using the relativistic Poisson equation, one can verify that this implies that they do not contribute to the “curvature” potential.
19		In this case in the flat gauge one finds, for each species $α$ , $ζα = ζ$ , where $ζ$ is the Bardeen curvature perturbation conserved on super-Hubble scales.
20		Available from http://www.cosmology.org.za