On counterterms in cosmological perturbation theory
  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
one-loop contribution to a correlator determines the number of counter terms
(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 counter terms 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 counter
terms shall be needed to renormalize the theory than are actually required. We
also comment on how the field strength of curvature perturbation, $\zeta$,
could get renormalized.
