Yeinzon Rodriguez

Inflationary prediction for primordial non-gaussianity.

We extend the deltaN formalism so that it gives all of the stochastic properties of the primordial curvature perturbation zeta if the initial field perturbations are Gaussian. The calculation requires only the knowledge of some family of unperturbed universes. A formula is given for the normalization f(NL) of the bispectrum of zeta, which is the main signal of non-Gaussianity. Examples of the use of the formula are given, and its relation to cosmological perturbation theory is explained.

Statistical anisotropy of the curvature perturbation from vector field perturbations

The δN formula for the primordial curvature perturbation ζ is extended to include vector as well as scalar fields. Formulas for the tree-level contributions to the spectrum and bispectrum of ζ are given, exhibiting statistical anisotropy. The one-loop contribution to the spectrum of ζ is also worked out. We then consider the generation of vector field perturbations from the vacuum, including the longitudinal component that will be present if there is no gauge invariance. Finally, the δN formula is applied to the vector curvaton and vector inflation models with the tensor perturbation also evaluated in the latter case.

On the Issue of the ζ series convergence and loop corrections in the generation of observable primordial non-Gaussianity in slow-roll inflation. II. The trispectrum

We calculate the trispectrum

Leptogenesis and tensor polarisation from a gravitational Chern-Simons term

{T}_{\ensuremath{\zeta}}

Non-gaussianity from the trispectrum and vector field perturbations

of the primordial curvature perturbation

Non-gaussianity at tree- and one-loop levels from vector field perturbations

\ensuremath{\zeta}

THE SUYAMA–YAMAGUCHI CONSISTENCY RELATION IN THE PRESENCE OF VECTOR FIELDS

, generated during a slow-roll inflationary epoch by considering a two-field quadratic model of inflation with canonical kinetic terms. We consider loop contributions as well as tree-level terms, and show that it is possible to attain very high, including observable, values for the level of non-Gaussianity

Feynman-like Rules for Calculating n-Point Correlators of the Primordial Curvature Perturbation

{\ensuremath{\tau}}_{\mathrm{NL}}

LOW SCALE INFLATION AND THE IMMEDIATE HEAVY CURVATON DECAY

if

Scale and shape dependent non-Gaussianity in the presence of inflationary vector fields

{T}_{\ensuremath{\zeta}}