Slides from the talk - CP3-Origins

More documents

Recommendations

Info

Primordial non-Gaussianity The Gaussianity of primordial fluctuations is one of the basic predictions of the simplest model of inflation confirmed (so far) at 0.1% level by CMB observations Therefore ... the possible detection of a large non-Gaussianity component in the intial conditions would, by itself, rule-out canonical, single-field, slow-roll inflation, providing a tool to discriminate between models of inflation
Non-Gaussian Initial Conditions Gaussian initial conditions: • their statistical properties are completely specified by the two-point correlation function or the power spectrum of the curvature perturbations: • All higher-order correlation functions are vanishing Bispectrum: Φ k1 Φ k2 = δ D ( k 1 + k 2 )P Φ (k 1 ) Φ k1 Φ k2 Φ k3 = δ D ( k 1 + k 2 + k 3 ) B Φ (k 1 ,k 2 ,k 3 )=0 Trispectrum: Φ k1 Φ k2 Φ k3 Φ k4 = δ D ( k 1 + ... + k 4 ) T Φ ( k 1 , k 2 , k 3 , k 4 )=0 Non-Gaussian initial conditions are characterized by an infinite set of functions: B Φ (k 1 ,k 2 ,k 3 ) = 0 T Φ ( k 1 , k 2 , k 3 , k 4 ) = 0 , etc ...
Page 1 and 2: Testing the Initial Conditions of t
Page 3: Part 1 The “shapes” of Inflatio
Page 7 and 8: The slang of non-Gaussianity Most i
Page 9 and 10: The CMB Bispectrum The Bispectrum o
Page 11 and 12: The CMB Bispectrum The Bispectrum o
Page 13 and 14: Non-Gaussianity in the Large-Scale
Page 15 and 16: Non-Gaussianity in the Large-Scale
Page 17 and 18: Non-Gaussianity from Gravitational
Page 19 and 20: Non-Gaussianity from Gravitational
Page 21 and 22: The Matter Bispectrum induced by Gr
Page 23 and 24: Non-Gaussianity from Galaxy Bias (m
Page 25 and 26: From the CMB to the Large-Scale Str
Page 27 and 28: Matter Power Spectrum In Perturbati
Page 29 and 30: Matter Power Spectrum In Perturbati
Page 31 and 32: The matter bispectrum and PNG: larg
Page 33 and 34: The matter bispectrum and PNG: larg
Page 35 and 36: The matter bispectrum and PNG: smal
Page 37 and 38: 0.8 0.6 0.01 0.1 1 10 k h Mpc 1 Th
Page 39 and 40: Galaxy bias and the galaxy power sp
Page 41 and 42: shear by → n- ad we 0). er- L) ng
Page 43 and 44: What about other models? approach [
Page 45 and 46: The interesting case of Quasi-Singl
Page 47 and 48: What about other models? approach [
Page 49 and 50: The Galaxy Bispectrum: NG and nonli
Page 51 and 52: The Galaxy Bispectrum: NG and nonli
Page 53 and 54: B B NG Sims Sims Theory Theory B
Page 55 and 56:
Halo Power Spectrum vs. Halo Bispec
Page 57:
Conclusions • The CMB is currentl
show all

Slides from the talk - CP3-Origins

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?