Counterterms in cosmological perturbation theory
Abstract
Cosmological perturbation theory is the theory of fluctuations (scalar as well as tensor) around the inflationary cosmological background solution. It is important to understand the details of the process of renormalization in this theory. In more familiar applications of quantum field theory, the dependence on the external momenta of the dimensionally regulated expression of the oneloop contribution to a correlator determines the number of counterterms (and their forms) required to renormalize it. In this work, it is pointed out that in cosmological perturbation theory, though this still happens, it happens in a completely different way such that in the late time limit, the information about the number and forms of counterterms required gets erased. This is to be compared with what happens in spontaneous symmetry breaking where the use of fluctuation fields around a chosen vacuum seems to suggest that more counterterms are needed to renormalize the theory than are actually required. We also comment on how the field strength of curvature perturbation, ζ, could get renormalized.
 Publication:

Physical Review D
 Pub Date:
 January 2014
 DOI:
 10.1103/PhysRevD.89.023504
 arXiv:
 arXiv:1307.4735
 Bibcode:
 2014PhRvD..89b3504G
 Keywords:

 98.80.k;
 Cosmology;
 Astrophysics  Cosmology and Extragalactic Astrophysics;
 High Energy Physics  Theory
 EPrint:
 8 pages