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18 May 2018: You paint this onto glass, let it dry for 24 hours and bake it in the oven at 160C.

8 Oct 2018: In cgs units:. H0 = 3.24 1018h s1 (1.11). Clearly, the time for a galaxy at a distance d, moving at velocity v, to moveapart by a further distance d

10 Oct 2018: ρ 1a4. (2.23). 7. and. a(t) =. (t. t0. )1/2; ρ(t) =. ρ0a4. =ρ0t. 20. t2(2.24). This is the second classic cosmological solution.

11 Oct 2018: 2.12), the Friedmann equation (3.21) takes theform:. ȧ20 =8π. 3Ga20ρ0 kc2 = H20a200 kc2 (3.24).

18 Oct 2018: 2.21 and 2.24). Thus,we do have a horizon. We also recall (from eq. ... 2.24). With this func-tional form, we find that in the radiation dominated era, the horizon scalewas.

23 Oct 2018: 9. 14. 16. 18. 20. 22. 24. 0.0 0.2 0.4 0.6 0.8 1.01.0. ... ρk = 3. 8πG. k. a2(6.24). which varies as ρk a2, so that for curvature w = 1/3.

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: We also saw in Lecture 2 (eq. 2.24) that in the radiation-dominated era thescale factor of the Universe evolves as a(t) = (t/t0). ... 7. 8. g. 2aT 4 for fermions,. (7.24). in equilibrium when kT mc2.

6 Nov 2018: a1/2da. (9.24). Performing the simple integration and now changing to redshift, we have:.

6 Nov 2018: IRJνIRJν. = 2y (10.23). and. y =. kT. mec2σT ne dl (10.24). ... Note that the so-called. Compton y parameter in eq. 10.24 increases with T, since the temperaturedetermines the average energy transfer per scattering event.