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23 Oct 2018: SN Cosmology Project. 14. 16. 18. 20. 22. 24. 0.0 0.2 0.4 0.6 0.8 1.01.0.

25 Oct 2018: u =g. (2πh̄)3. 0. f(E)E(p) 4πp2 dp (7.20). The distribution function in energy terms, f(E), is given generally by:. ... 3; dp =. kT. cdy. so that eq. 7.20 can be re-written as:.

30 Oct 2018: n. p= exp. [mc. 2. kTd. ]= exp. [1.3. 0.8. ]= 0.20 = 1 : 5 (8.6). ... 0.43. 20. Figure 8.4: The abundances of light elements relative to H predicted by BBN calculationsare shown as functions of η nb/nγ (bottom x-axis) and b,0h2

30 Oct 2018: 0.43. 20. Cyburt+ 2015. L Kewley. Aver+ 2015. BBN theory confronts observations 2015.

6 Nov 2018: c dt. a(t). (9.20). We want shor at redshift z. Using ȧ = da/dt, dt = da/ȧ = da/aH, wehave:.

6 Nov 2018: δT. T. )SW. =1. 3. δΦ. c2. (10.20). There are two competing effects here. ... 10.20. Note that there is no scale dependence of the temperature fluctuations ineq.

6 Nov 2018: Kunz. 20,70,3, H. Kurki-Suonio. 30,52, G. Lagache. 5,70, A. Lähteenmäki. 2,52, J.-M.

8 Nov 2018: In the last 20 years, the near-exponential increase incomputational power (in both hardware and software) has made it possibleto carry out increasingly sophisticated simulations of large volumes of theUniverse to

13 Nov 2018: 20. 8πGmH(12.16). (Y is the baryonic mass fraction in He: Yp = 0.24) and. ... bHubble H(z) L/2 km s1 (12.20). where H(z) is the Hubble parameter which, as we know (Lecture 5) isgiven by:.

14 Nov 2018: By z = 0, the intensity of the UV background has decreased by a factorof 20.