Juan Carlos Bueno Sánchez Universidad del Valle (Santiago de Cali), Universidad Antonio Nariño...

Juan Carlos Bueno Sánchez

Universidad del Valle (Santiago de Cali), Universidad Antonio Nariño (Bogotá),

Universidad Industrial de Santander (Bucaramanga)

CMB anisotropy constraint

Liberating vector fields from their

Based on:

JCBS, Phys. Lett. B 739 (2014) 269-278

JCBS, arxiv 1509.XXXX (On a local approach to CMB anomalies)

Warsaw, 9 Sept. 15

How much you need to twist the inflationary paradigm to obtain CMB anomalies?(i.e. breaking homogeneity & isotropy of the CMB)

The question

Apart from the inflaton, other scalar field(s) contributes to the perturbation spectrum imprinted on the CMB

The ingredient

(Isocurvature perturbation)

A framework to understand CMB anomalies

Inhomogeneous distribution of the iso-field at the end of inflation

Breaking of statistical homogeneity of the CMB

The outcome

Avenue towards CMB anomalies

A framework to understand CMB anomalies

How much you need to twist the inflationary paradigm to obtain CMB anomalies?(i.e. breaking homogeneity & isotropy of the CMB)

The question

Apart from the inflaton, other scalar field(s) contributes to the perturbation spectrum imprinted on the CMB

The ingredient

(Isocurvature perturbation)

An initially excited isocurvature field does not fully decay due

The set-up

Inflaton responsible for most of the CMB perturbations (homogeneous & isotropic)

to its interactions during inflation

Fluctuations + dynamics

Fluctuations + dynamics

Light fields can be caught ‘’in the middle’’ by the end of inflation

Snapshot at the end of inflation

The link to CMB anomalies

Field interactions become important before the end of inflation

Field decay

Field oblivious to interactions

Slow-roll phase

LSS

Interacting spectator s during inflation

The setting

Initial condition

s retains a large EV where it is oblivious of interactions

if interactions become important at x

if s evoles as a free field

Emergence of a patchy structure(JCBS ’14)

Dynamical regimes(JCBS & Enqvist ’13)

c integrated out s as a free field(slow-roll phase)

c production(Kofman et al. ‘04)

Trapping mechanism for s(decay phase)

Cold Spot accounted for through localized inhomogeneous reheating

(Separation between the slow-roll and decay phases is too crude)

A necessary (more) realistic probability density

Nc = O(10)

Nc = O(102)

Free field dynamics: Interacting field dynamics:

Numerical solution for the interacting dynamics

Nend = 45




Nend = 50




Nend = 51




Nend = 52




Nend = 53




Nend = 54




Nend = 55




Nend = 56




Can a Local direction-dependent contribution to the CMB be generated?

Vector fields strongly constrained in the CMB

g* 0.02Kim & Komatsu, 2013

Local breaking of statistical isotropy

LSS

Planck, 2015


Slow-roll phase

Slow-roll phase

Slow-roll phase

Scale invariance for a = -4

Decay phase

Decay phase

Decay phase

End of scaling

A simple example: vector curvaton with varying kinetic functionDimopoulos et al. ‘10

A motivated choice:

Evolution of the vector field

Energy densityModulated kinetic function


Center of the s distribution

Left end of s distribution

Right end of s distribution

Dimopoulos et al. ’09, ‘10Vector curvaton contribution to the CMB

Probability density for the curvature perturbation

Probability density for rA,end

Probability density for (z or (z x)/ zsr)

Interacting dynamics of s

Kinetic function f(s)

Initial Probability density for s(Gaussian, fixed by fluctuations)


A cartoon

Correlated spatial variation of r

Full sky maps required with enough sensitivity (CORE,CMB-

Pol,LiteBIRD)

Correlated parity violating signal

Non-vanishing EB

correlations


The contribution of these fields to the curvature perturbation (given the

appropriate tuning) provides a mechanism to break statistical homogeneity

and isotropy of the CMB

(Local versions of inhomogeneous reheating , vector curvaton , …)

Wishful thinking: The production of localized perturbations may

provide a framework to understand some of the CMB anomalies (if they

turn out to exist)

Conclusions

Vector fields source GW: Looking for correlated spatial variations of r might

reveal the presence of a vector field hidden in the CMB

Vector fields might be allowed to contribute substantially to z as long as

they do it in a relatively small patch of the CMB

The CMB Vector Spot

Juan Carlos Bueno Sánchez Universidad del Valle (Santiago de Cali), Universidad Antonio Nariño...

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