1 | Continuously updated information on Euclid is available on ![]() |
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2 | This subsection is based on [49![]() |
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3 | Not to be confused with a different formalism of the same name by other authors [457![]() |
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4 | In presence of massive neutrinos ![]() ![]() |
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5 | If we assume that neutrinos have a non-vanishing mass, then the transfer function is also redshift-dependent. | |
6 | ![]() |
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7 | See [420]. ![]() ![]() ![]() |
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8 | For this reason, early dark-energy models can have a much stronger impact. | |
9 | ![]() |
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10 | ![]() |
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11 | ![]() |
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12 | ![]() |
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13 | ![]() |
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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 ![]() ![]() |
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16 | ![]() ![]() ![]() |
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17 | Very few ![]() |
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18 | Strictly speaking, isocurvature perturbations are defined by the condition that their total energy density in the total
comoving gauge vanishes, i.e., ![]() |
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19 | In this case in the flat gauge one finds, for each species ![]() ![]() ![]() |
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20 | Available from ![]() |
http://www.livingreviews.org/lrr-2013-6 |
Living Rev. Relativity 16, (2013), 6
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