Primordial non-Gaussianity in the cosmological perturbations - CBPF

Literature
During the preparation of this set of notes, we have been found useful consulting the following
reviews and textbooks:
N. Bartolo, E. Komatsu, S. Matarrese and A. Riotto, “Non-Gaussianity from inflation: Theory and
observations,” Phys. Rept. 402, 103 (2004). [astro-ph/0406398];
X. Chen, “Primordial Non-Gaussianities from Inflation Models,” Adv. Astron. 2010, 638979 (2010)
[arXiv:1002.1416 [astro-ph.CO]];
V. Desjacques and U. Seljak, “Primordial non-Gaussianity in the large scale structure of the Uni-
verse,” Adv. Astron. 2010 (2010) 908640 [arXiv:1006.4763 [astro-ph.CO]];
S. Dodelson, “Modern Cosmology”, Academic Press, 2003;
J.A. Peacock, “Cosmological Physics”, Cambridge University Press, 1999.
Units
We will adopt natural, or high energy physics, units. There is only one fundamental dimension,
energy, after setting = c = kb = 1,
[Energy] = [Mass] = [Temperature] = [Length] −1 = [Time] −1 .
The most common conversion factors and quantities we will make use of are
1 GeV −1 = 1.97 × 10 −14 cm=6.59 × 10 −25 sec,
1 Mpc= 3.08×10 34 cm=1.56×10 33 GeV −1 ,
MPl = 1.22 × 10 19 GeV,
H0= 100 h Km sec −1 Mpc −1 =2.1 h × 10 −42 GeV −1 ,
ρc = 1.87h 2 · 10 −29 g cm −3 = 1.05h 2 · 10 4 eV cm −3 = 8.1h 2 × 10 −47 GeV 4 ,
T0 = 2.75 K=2.3×10 −13 GeV,
Teq = 5.5(Ω0h 2 ) eV,
Tls = 0.26 (T0/2.75 K) eV.
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