Slides from the talk - CP3-Origins

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The Galaxy Bispectrum: NG and nonlinear bias The galaxy bispectrum at large scales B g (k 1 ,k 2 ,k 3 )=b 3 1 B(k 1 ,k 2 ,k 3 )+b 2 1 b 2 P (k 1 ) P (k 2 )+2perm. + ...
The Galaxy Bispectrum: NG and nonlinear bias The galaxy bispectrum at large scales B g (k 1 ,k 2 ,k 3 )=b 3 1 B(k 1 ,k 2 ,k 3 )+b 2 1 b 2 P (k 1 ) P (k 2 )+2perm. + ... B = B 0 + B tree G Primordial component (large scales) [P 0 ]+B loop G [P 0]+B loop NG [P 0,B 0 ]
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 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: What about other models? approach [
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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