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 depends also on the scale [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]. is the Fourier transform of [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 , where is the minimum redshift of the Euclid spectroscopic survey. | |

16 | is the antisymmetric partner of the metric, which in heterotic string theory gives rise to the model-independent axion. The indices run over the spacetime dimensions, . | |

17 | Very few -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., . 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 , , where is the Bardeen curvature perturbation conserved on super-Hubble scales. | |

20 | Available from http://www.cosmology.org.za |

Living Rev. Relativity 16, (2013), 6
http://www.livingreviews.org/lrr-2013-6 |
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