  We present a new method which constructs an HI super-profile of a galaxy
which is based on profile decomposition analysis. The decomposed velocity
profiles of an HI data cube with an optimal number of Gaussian components are
co-added after being aligned in velocity with respect to their centroid
velocities. This is compared to the previous approach where no prior profile
decomposition is made for the velocity profiles being stacked. The S/N improved
super-profile is useful for deriving the galaxy's global HI properties like
velocity dispersion and mass from observations which do not provide sufficient
surface brightness sensitivity for the galaxy. As a practical test, we apply
our new method to 64 high-resolution HI data cubes of nearby galaxies in the
local Universe which are taken from THINGS and LITTLE THINGS. In addition, we
also construct two additional HI super-profiles of the sample galaxies using
symmetric and all velocity profiles of the cubes whose centroid velocities are
determined from Hermite $h_3$ polynomial fitting, respectively. We find that
the HI super-profiles constructed using the new method have narrower cores and
broader wings in shape than the other two super-profiles. This is mainly due to
the effect of either asymmetric velocity profiles' central velocity bias or the
removal of asymmetric velocity profiles in the previous methods on the
resulting HI super-profiles. We discuss how the shapes
($\sigma_{\rm{n}}/\sigma_{\rm{b}}$, $A_{\rm{n}}/A_{\rm{b}}$, and
$A_{\rm{n}}/A_{\rm{tot}}$) of the new HI super-profiles which are measured from
a double Gaussian fit are correlated with star formation rates of the sample
galaxies and are compared with those of the other two super-profiles.
