Models of inflation are instructive playgrounds for supersymmetry breaking in Supergravity and String Theory. In particular, combinations of branes and orientifolds that are not mutually BPS can lead to emphbrane supersymmetry breaking, a phenomenon where non--linear realizations are accompanied, in tachyon--free vacua, by the emergence of steep exponential potentials. When combined with milder terms, these exponentials can lead to slow--roll after a fast ascent and a turning point. This leaves behind distinctive patterns of scalar perturbations, where pre--inflationary peaks can lie well apart from an almost scale invariant profile. I review recent attempts to connect these power spectra to the low--$ell$ CMB, and a corresponding one--parameter extension of $Lambda$CDM with a low--frequency cut $Delta$. A detailed likelihood analysis led to $Delta = (0.351 pm 0.114) imes 10^-3 , mboxMpc^-1$, at $99.4%$ confidence level, in an extended Galactic mask with $f_sky=39%$, to be compared with a nearby value at $88.5%$ in the standard Planck 2015 mask with $f_sky=94%$. In these scenarios one would be confronted, in the CMB, with relics of an epoch of deceleration that preceded the onset of slow--roll.

Low-ℓ CMB from string-scale SUSY breaking?

SAGNOTTI, AUGUSTO
2017

Abstract

Models of inflation are instructive playgrounds for supersymmetry breaking in Supergravity and String Theory. In particular, combinations of branes and orientifolds that are not mutually BPS can lead to emphbrane supersymmetry breaking, a phenomenon where non--linear realizations are accompanied, in tachyon--free vacua, by the emergence of steep exponential potentials. When combined with milder terms, these exponentials can lead to slow--roll after a fast ascent and a turning point. This leaves behind distinctive patterns of scalar perturbations, where pre--inflationary peaks can lie well apart from an almost scale invariant profile. I review recent attempts to connect these power spectra to the low--$ell$ CMB, and a corresponding one--parameter extension of $Lambda$CDM with a low--frequency cut $Delta$. A detailed likelihood analysis led to $Delta = (0.351 pm 0.114) imes 10^-3 , mboxMpc^-1$, at $99.4%$ confidence level, in an extended Galactic mask with $f_sky=39%$, to be compared with a nearby value at $88.5%$ in the standard Planck 2015 mask with $f_sky=94%$. In these scenarios one would be confronted, in the CMB, with relics of an epoch of deceleration that preceded the onset of slow--roll.
Settore FIS/02 - Fisica Teorica, Modelli e Metodi Matematici
astro-ph.CO; astro-ph.CO; General Relativity and Quantum Cosmology; High Energy Physics - Phenomenology; High Energy Physics - Theory
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11384/65892
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