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The CMB spectrum also gives us the density of ordinary atomic matter built of baryons, which are bound states of quarks. From the CMB we can deduce that only about twenty percent of the total matter density is baryonic. , 2008). The fact that baryonic energy density is only a fraction of the total matter density excludes the simplest possibility that dark matter is composed of regular atomic matter. But then what is dark matter made of? To address this question we have to ask: What do we know about the properties of dark matter so far?

83), (84) and (88) yield 2 · 11 19 f 1 ( Rmax − R) < 2 · 7 f2 72 ± (102) It follows from eq. (101) that (+) f2 <0 and (−) f2 >0 (103) Then the stability condition (82) is obeyed for any value of R. As regards the (−)-case, there are two possibilities depending upon the sign of f 1 . Should f 1 be positive, all the remaining stability conditions are automatically satisfied, ie. in the case of both (−) f2 (−) > 0 and f 1 > 0. F() Supergravity and Early Universe: the Meeting Point F (R) Supergravity and Early Universe: the Meeting Point of Cosmology and High-Energy Physicsof Cosmology and High-Energy Physics 21 19 (−) Should f 1 be negative, f 1 < 0, we find that the remaining stability conditions (100) and (102) are the same, as they should, while they are both given by 192 f 12 3 · 5 f 12 f = − − 32 0 ≡ Rins max f2 23 · 11 f 22 23 · 11 f 22 R < Rmax − (104) As regards the (+)-case, eq.

166), the F (R)-supergravity Z -potential (173) implies the superpotential √ 2 2 ξ 3/2 3 Φ (174) WKS (Φ ) = 3 f 1/2 3 It coincides with the superpotential (169) of the WZ-model, provided that we identify the couplings as 32ξ 3 (175) f3 = 2 λ We conclude that the original nonminimally coupled matter-supergravity theory (156) in the slow-roll approximation with the superpotential (169) is classically equivalent to the F (R)-supergravity theory with the F-function given by eq. (171) when the couplings are related by eq.

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