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Investigating the CMB Hemispherical Power Asymmetry

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A.I. Malz

on 18 February 2014

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Transcript of Investigating the CMB Hemispherical Power Asymmetry

Investigating the CMB Hemispherical Power Asymmetry
18 February 2014 A.I. Malz
Quantum vacuum fluctuations seeded curvature perturbations amplified by inflation.
Acoustic oscillations in the matter-photon fluid enhanced perturbations after inflation.
Sunyaev-Zeldovich Effect
Foreground sources are anisotropic.
Angular Power Spectrum
Local motion induces a dipole via the Doppler Effect.
Sachs-Wolfe Effect
Gravitational Lensing
< 1%
spatial gradient
constrained by octupole
What do we assume?
Single inflaton field
Homogeneous
Isotropic
Gaussian
What do we assume?
Two inflaton fields
decouple background from perturbations
Homogeneous
Isotropic
Gaussian
spatial gradient
only in perturbing field
constrained by
quadrupole and octupole
sum of Gaussian fields is highly non-Gaussian
What do we assume?
Single inflaton field
Homogeneous
Isotropic
Non-Gaussian
decouples background from asymmetry
violates scale-invariance
What do we assume?
Single inflaton field
Homogeneous
Isotropic
Gaussian
Spatially modulated parameters
Changing any parameter
affecting total density
will conflict with observations.
leads to insufficient
A
leads to temperature dipole
gravitational wave
amplitude
leads to insufficient
A
scalar spectral index
reionization optical depth
requires 10-fold asymmetry
plausible
What next?
Single inflaton field
Homogeneous
Isotropic
Non-gaussian
Spatially modulated parameters
Small vs. large volume statistics
Change of basis
Questions?
Full transcript