  The observable universe is fundamentally inhomogeneous and anisotropic.
Quantum description of the generation of these inhomogeneities and anisotropies
is ill-understood and unsatisfactory. After providing a brief account of the
standard approach of the generation of the classical density perturbations
starting from the quantum fluctuations of inflaton field, I critically review
various assumptions which are crucial for the success of this description, and
point out various shortcomings around it. I also discuss the basic ideas and
recent works by using an alternative path to overcome those shortcomings which
is motivated by the so-called Collapse Model interpretation of quantum
mechanics. Inspired by these works, I argue the necessity of constructing a
class of manifestly inhomogeneous and anisotropic quantum states after
inflation and discuss my recent works which provide one such prescription of
building such a state, called the $T-$vacuum, defined in the radiation
dominated stage of the early universe.
