Constraining the Inflationary Equation of State
Abstract
We explore possible constraints on the inflationary equation state: p=w\rho. While w must be close to -1 for those modes that contribute to the observed power spectrum, for those modes currently out of experimental reach, the constraints on w are much weaker, with only w<-1/3 as an a priori requirement. We find, however, that limits on the reheat temperature and the inflationary energy scale constrain w further, though there is still ample parameter space for a vastly different (accelerating) equation of state between the end of quasi-de Sitter inflation and the beginning of the radiation-dominated era. In the event that such an epoch of acceleration could be observed, we review the consequences for the primordial power spectrum.
Keywords
Cite
@article{arxiv.1007.3511,
title = {Constraining the Inflationary Equation of State},
author = {Lotty Ackerman and Willy Fischler and Sandipan Kundu and Navin Sivanandam},
journal= {arXiv preprint arXiv:1007.3511},
year = {2015}
}
Comments
12 pages, 2 figure