Position space CMB anomalies from multi-stream inflation. Yi Wang, IPMU, May 2013

Transcription

1 Position space CMB anomalies from multi-stream inflation Yi Wang, IPMU, May 2013

2 Outline: Cosmology after Planck - standard model, extensions and anomalies Multi-stream inflation - the model - hemispherical power asymmetry - the cold spot - low suppression, multipole alignment - constraining multi-field inflation

3 Cosmology after Planck

4 Planck: Collecting data since 2009 Data release: 21 Mar, 2013

5 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization history: τ =

6 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 h was (Ω +ΩΛ for = 1)WMAP+SPT+ACT+SNLS3 b+ωc71.2 As a result, t₀ is now 13.8 Gyr (13.7 before). Initial perturbations: Aζ = , ns = 0.96 Reionization history: τ =

7 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization history: τ =

8 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 ΩΛbwas for WMAP+SPT+ACT+SNLS3 (Ω +Ωc+Ω Λ = 1) Initial perturbations: Aζ = , ns = 0.96 Reionization history: τ =

9 The 6-parameter standard model works well: Background: H = , ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization history: τ =

10 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Almost unchanged. Initial perturbations: But h decreased thus Ωb and Ωc are now 10% greater Aζ = , ns = 0.96 Reionization history: τ =

11 The 6-parameter standard model works well: Background: H = , ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization history: τ =

12 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = 0.96 Reionization τ = WMAP+SPT+ACT+SNLS A was 2.407history: 10-9 for ζ

13 The 6-parameter standard model works well: Background: H = , ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization history: τ =

14 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization τ = n was 0.967history: for WMAP+SPT+ACT+SNLS3 s ns<1: previously 5σ (WMAP9+BAO), now at 5.4σ.

15 The 6-parameter standard model works well: Background: H = , ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization history: τ =

16 The 6-parameter standard model works well: Background: h = 67.11, ΩΛ = 0.68, Ωbh² = 0.022, Ωch² = 0.12 (Ωb+Ωc+ΩΛ = 1) Initial perturbations: Aζ = , ns = Reionization history: τ = τ was for WMAP+SPT+ACT+SNLS3 But error bar is 0.03ish, Planck + WP central value agrees with WMAP

17 One parameter extensions: (95% CL) Spatial curvature: < Ωk < Neutrino Σmν < 0.230eV, 2.79 < neff < 3.84 Tensor to scalar ration: r < 0.111, Running of spetial index: < αs < EoS of dark energy: < w < Non-Gaussianities: local: -8.9 < fnl < 14.3, equil: -192 < fnl < 108, ortho: -103 < fnl < 53

18 One parameter extensions: (95% CL) Spatial curvature: < Ωk < Neutrino Σmν < 0.230eV, 2.79 < neff < 3.84 Tensor to scalar ration: r < 0.111, Running of spetial index: < αs < Currently polarization yet used. EoS ofplanck dark energy: <not w< c.f. r<0.13 (95% CL) for (low WMAP9 + SPT + ACT + BAO + H0 Non-Gaussianities: agree with WMAP) local: -8.9 < fnl < 14.3, equil: -192 < fnl < 108, ortho: -103 < fnl < 53

19

20 Green: WMAP9 + SPT + ACT Red: WMAP9 + SPT + ACT + BAO + H0

21 One parameter extensions: (95% CL) Spatial curvature: < Ωk < Neutrino Σmν < 0.230eV, 2.79 < neff < 3.84 Tensor to scalar ration: r < 0.111, Running of spectral index: < αs < EoS of dark energy: < w < Non-Gaussianities: local: -8.9 < fnl < 14.3, equil: -192 < fnl < 108, ortho: -103 < fnl < 53

22 WMAP9: One parameter extensions: (95% CL) local: -3 < fnl < 77, Spatial curvature: < Ωk < equil: -221 < fnl < 323, ortho: -445 < fnl < -45 Neutrino Σmν < 0.230eV, 2.79 < neff < 3.84 Interestingly, Planck agrees with WMAP at low Tensor to scalar ration: r < 0.111, Running of spetial index: < αs < EoS of dark energy: < w < Non-Gaussianities: local: -8.9 < fnl < 14.3, equil: -192 < fnl < 108, ortho: -103 < fnl < 53

23 Planck 2013 on Quasi-single field non-g (C. Chen & YW, 2009) c.f. Planck-Suppressed Operators, Assassi, Baumann, Green, McAllister, 2013

24 Anomalies overview L. Page

25

26 Anomalies overview Hemispherical asym (Eriksen, et. al. 2003) Dipolar asymmetry (Gordon et. al. 2005) Cold spot (Vielva et. al. 2003) Mode alignment (Tegmark et. al. 2003) Power suppression at low multipoles (WMAP, Planck) Parity asymmetry, phase correlations,...

27 Anomalies asymmetry Hemispherical asymmetry Asymmetry between two hemispheres Dipolar asymmetry Asymmetry characterized by a dipole A(n) = (1 + w n) A0 They are related but different effects See, e. g. WMAP 7

28 From Planck website (anomalous regions enhanced, caption was wrong)

29 Hemispherical: directions (Planck 2013) High directions Small directions

30 Hemispherical: amplitude difference (Planck 2013)

31 Anomalies asymmetry Hemispherical asymmetry v.s. Dipolar asymmetry For small, say < 100: both ~ 10% modulation For large, say > 100: Only hemispherical asym (and direction then points to dipole direction) There is a tension at > 100.

32 Anomalies cold spot About 5 degree² with 70µK colder than average More than 4σ unlikely from statistics

33 Anomalies cold spot Different masks and CL (Planck 2013):

34 Anomalies cold spot

35 Alignment (axis of evil) (Planck 2013) 9, 98%; or 13, 96.7% Quadrupole (WMAP 7 was 3 ) Octopole +: Quadrupole direction *: Octopole direction

36 Low suppression (Planck 2013) A power deficit of 5%~10% at 40, 2.5σ ~ 3σ multipole moment

37 Multi-stream inflation

38 Multi-stream inflation M. Li and YW, S. Li, Y. Liu, Y. Piao, ; YW, N. Afshordi, A. Slosar, YW, F. Duplessis, YW, R. Brandenberger, YW,

39

40 Examples include:

41 Distance of rolling EoM

42

43 Asymmetries

44 Cold spot: a) Sachs-Wolfe b) ISW, etc.

45 Constraint on multi-field potential

46 Constraint on multi-field potential

47 Temporary domain wall

48

49 Wang, Cho, Wu 2010, Wang, Wu, Hsu, 2011

50 Wang, Cho, Wu 2010, Wang, Wu, Hsu, 2011

51 In the locally de Sitter frame:

52 Observations are made in the domain wall rest frame

53 Domain wall induced power asymmetry

54 Probability of multipole directions

55 Probability of (3D) alignment

56 Future directions: In-in formalism for non-unique classical traj. Full grav. pert. with domain wall Beyond planar domain wall Time dependence of the domain wall tension Project the 3D alignment prob. to 2D Fitting multi-stream inflation with data Multiple dimensional random potential

57 Thank you!