By J M Overduin, P S Wesson
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Additional resources for Dark Sky Dark Matter
E. a negative curvature) enhances them. Open models, in other words, expand more quickly at any given redshift z (and therefore last longer) than closed ones. This curvature term, however, goes only as (1 + z)2 , which means that its importance drops off relative to the matter and radiation terms at early times, and relative to the vacuum term at late ones. 40), in which not only the ﬁrst (radiation) term on the right-hand side was neglected, but the third (vacuum) and fourth (curvature) terms as well.
J. 459 415  Alexander D R et al 1997 Astron. Astrophys. 1 The spectral background The previous chapter has convinced us that the bolometric intensity (or luminosity per unit area at all wavelengths) of the light reaching us is low mostly because the galaxies have not had enough time to ﬁll up the Universe with light. Cosmic expansion does reduce this further, but only by a factor of about one-half. However, galaxies do not emit their light equally in all parts of the spectrum, and it could be that expansion plays a relatively larger role at some wavelengths than others.
40) When r,0 = 0, this is sometimes referred to as the Friedmann equation after the Russian mathematician who obtained the ﬁrst cosmological solutions of Einstein’s equations under the assumption of zero pressure. 40) as the Friedmann– Lemaˆıtre equation. The form of this equation already reveals a great deal about the contents and evolution of the Universe. For example, the term m,0 (1 + z)3 shows that matter acts to increase the expansion rate H (z) as one goes to higher z—that is, to slow down the expansion rate with time.
Dark Sky Dark Matter by J M Overduin, P S Wesson