Slides from the talk - CP3-Origins

More documents

Recommendations

Info

The CMB Bispectrum The Bispectrum of the CMB is the most direct probe of the initial bispectrum B l1 l 2 l 3 ∼ B Φ (k 1 ,k 2 ,k 3 )∆ l1 (k 1 )∆ l2 (k 2 )∆ l3 (k 3 )j l1 (k 1 r)j l2 (k 2 r)j l3 (k 3 r) CMB angular bispectrum curvature bispectrum transfer functions • The CMB provides a snapshot of density perturbations at early times • Power spectrum measurements (Clʼs) are matched by linear predictions (so far) • The CMB bispectrum is an optimal estimator for the fNL parameter No evidence (yet)! (despite 2-sigma “hints” in previous data releases ...) WMAP 7 years: Local -10 < fNL < 74 Equilateral -214 < fNL < 266 Orthogonal -410 < fNL < 6 @ 95% CL Komatsu et al. (2011) The CMB bispectrum is equally sensitive to any model of non-Gaussianity
The CMB Bispectrum The Bispectrum of the CMB is the most direct probe of the initial bispectrum B l1 l 2 l 3 ∼ B Φ (k 1 ,k 2 ,k 3 )∆ l1 (k 1 )∆ l2 (k 2 )∆ l3 (k 3 )j l1 (k 1 r)j l2 (k 2 r)j l3 (k 3 r) CMB angular bispectrum curvature bispectrum transfer functions • The CMB provides a snapshot of density perturbations at early times • Power spectrum measurements (Clʼs) are matched by linear predictions (so far) • The CMB bispectrum is an optimal estimator for the fNL parameter No evidence (yet)! (despite 2-sigma “hints” in previous data releases ...) Planck will improve WMAP results by a factor of ~ 4 ΔfNL local ΔfNL equilateral WMAP 21 140 Planck ~ 5 ~ 30 The CMB bispectrum is equally sensitive to any model of non-Gaussianity
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: 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

Slides from the talk - CP3-Origins

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

Delete template?

Save as template?