  Primordial non-Gaussianity arising from inflationary models is a unique probe
of non-trivial dynamics of the inflaton field and its interactions with other
fields. Often when examining and constraining the scalar non-Gaussianity
arising from inflation, certain templates are adopted for the scalar
non-Gaussianity parameter $f_{_{\rm NL}}$, in classifying their behaviors in
terms of wavenumbers. The current constraints from cosmic microwave background
(CMB) on such templates of $f_{_{\rm NL}}$ are weak and provide rather large
bounds on their amplitudes. In this work, we explore a different method of
constraining $f_{_{\rm NL}}$ through their effect on the scalar power. We
compute the correction to the scalar power due to $f_{_{\rm NL}}$ while
accounting for its generic scale dependence. We then compute the angular power
spectrum of CMB arising from such non-Gaussian corrections to explore possible
imprints. We initially illustrate this method using the conventional templates
of $f_{_{\rm NL}}$ such as local, equilateral and orthogonal types, with and
without the running of the parameter. We further employ this method to an
oscillatory form of $f_{_{\rm NL}}$ and lastly on a realistic model of
inflation proposed by Starobinsky. Though this method does not improve much on
the constraints on the first three templates of $f_{_{\rm NL}}$, it provides
interesting insights on models that do not conform to these templates. We infer
that the non-Gaussian correction to the spectrum can be sensitive to model
parameters that are degenerate at the level of the original power spectrum.
Hence, this method of computing indirect imprints of $f_{_{\rm NL}}$ on angular
power spectrum of CMB provides a new avenue to explore primordial scalar
non-Gaussianity and possibly constrain them effectively.
