Slides from the talk - CP3-Origins

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Matter Power Spectrum & Bispectrum In Perturbation Theory ... P = P 0 + P loop G [P 0]+P loop NG [P 0,B 0 ] matter power spectrum Linear power spectrum Gravity-induced contributions (depending on P0 alone) Additional gravity-induced contributions present only for NG initial conditions (B0) B = B 0 + B tree G [P 0 ]+B loop G [P 0]+B loop NG [P 0,B 0 ] & bispectrum Primordial component
The matter bispectrum and PNG: large scales At large scales I can approximate the matter bispectrum with the tree-level expression on PT: B(k 1 ,k 2 ,k 3 ) B 0 + B tree G [P 0 ] Primordial component Gravity-induced component Bk,k,k 5000 2000 1000 500 200 Gravity Initial, f NL 100 Gravity Initial 0.01 0.02 0.05 0.1 k h Mpc 1 Equilateral configurations of the matter bispectrum B 0 (k, k, k) k→0 (k, k, k) ∼ B tree G f NL D(z)k 2 The primordial component has a different dependence on scale than the gravity-induced one! It is relevant at large scales and early times This is true for almost all models (local, equilateral, orthogonal ...)
Page 1 and 2: Testing the Initial Conditions of t
Page 3 and 4: Part 1 The “shapes” of Inflatio
Page 5 and 6: Non-Gaussian Initial Conditions Gau
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: Matter Power Spectrum In Perturbati
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

Slides from the talk - CP3-Origins

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