arXiv:0907.1838 [hep-ph]arXiv:0909.0475 [astro-ph.CO]

With Konstantinos Dimopoulos and Mindaugas Karčiauskas.

Jacques M. WagstaffJacques M. Wagstaff

VECTOR CURVATON MODEL VECTOR CURVATON MODEL

and its distinct and its distinct

A CompellingA Compelling

Observational Signatures Observational Signatures

Introduction/MotivationsIntroduction/MotivationsIN

FLA

TIO

NIN

FLA

TIO

N Solves horizon and flatness problems of standard Hot Big Bang cosmology

Mechanism to generate the primordial curvature perturbation which seeds all structure in the universe

Observations:Particle production Inflation produces such perturbations by amplifying by amplifying quantum fluctuations of suitable fields.

Particle production in Scalar fields seem to agree well with observations.

Particle production in Scalar fields seem to agree well with observations.

Predominantly Gaussian

AdiabaticHawking radiation in de Sitter space.

l=5 multipole in preferred frame l=5 multipole in galactic coordinates

Why are Vector Fields Interesting?Why are Vector Fields Interesting?

Scalar fields cannot give rise to a preferred direction!

Land & Magueijo (2005)

Longo (2007)

‘Axis of evil’

Alignment of galaxy spins.

K. Dimopoulos (2006)Vector Curvaton mechanism.

•VECTOR BOSONS ARE FOUND IN NATURE.•VECTOR BOSONS ARE FOUND IN NATURE.

Non-Gaussianity:

Statistical Anisotropy:

•ANOMALIES IN THE CMB.•ANOMALIES IN THE CMB.

Vector Curvaton with Varying Kinetic FunctionVector Curvaton with Varying Kinetic Function

Modulated kinetic function and mass.

The Spectrum:

Physical vector field: with mass:

Vector Curvaton with Varying Kinetic FunctionVector Curvaton with Varying Kinetic Function

Modulated kinetic function and mass.

For scale invariant transverse components: For scale invariant longitudinal component:

Physical vector field: with mass:

Vector Curvaton with Varying Kinetic FunctionVector Curvaton with Varying Kinetic Function

Modulated kinetic function and mass.

For scale invariant transverse components: For scale invariant longitudinal component:

Physical vector field: with mass:

DYNAMICAL ATTRACTORDYNAMICAL ATTRACTOR

Statistical Anisotropy in the SpectrumStatistical Anisotropy in the Spectrum

Isotropic

Observations require:(Groeneboom et al. 2009)

(Pullen et al. 2007)

Ho

rizo

n e

xit

Inflation

Infl

atio

n e

nd

sSecond oscillating regime:

Power law regime:

Case 1: The AttractorCase 1: The Attractor

Infl

atio

n e

nd

s

Mode functions

Infl

atio

n e

nd

s

Highly anisotropic spectrum:

Anisotropic BispectrumAnisotropic Bispectrum

The highly anisotropic and subdominant limit:The highly anisotropic and subdominant limit:

Non-Gaussianity is correlated to statistical anisotropy in the Spectrum.

Non-Gaussianity is itself anisotropic.

The almost isotropic and dominant limit:The almost isotropic and dominant limit:

SMOKING GUN FOR A VECTOR FIELD CONTRIBUTION TO THE CURVATURE PERTURBATION OF THE UNIVERSE!SMOKING GUN FOR A VECTOR FIELD CONTRIBUTION TO THE CURVATURE PERTURBATION OF THE UNIVERSE!

CONCLUSIONSCONCLUSIONS

arXiv:0907.1838 [hep-ph], arXiv:0909.0475 [astro-ph.CO]Konstantinos Dimopoulos, Mindaugas Karčiauskas, and Jacques M. Wagstaff.

Non-Gaussianity is correlated to statistical anisotropy in the Spectrum.

The Spectrum and Bispectrum are generally anisotropic.

Non-Gaussianity is predominantly anisotropic.

Non-Gaussianity is the same for the different configurations.Magnitude and direction of anisotropy is identical in the Spectrum and Bispectrum.

Falsifiable case if Non-Gaussianity is observed to be Isotropic.

Falsifiable case if anisotropy is different in Spectrum and Bispectrum.

LIGHT FIELDLIGHT FIELD

HEAVY FIELDHEAVY FIELD

Do not need scalar fields to generate the curvature perturbation.

•Flat spectrum as an attractor solution.•Flat spectrum as an attractor solution.

Ho

rizo

n e

xit

Inflation

Infl

atio

n e

nd

s

Case 1:Case 1:

Highly anisotropic spectrum:

Mode functions