  In the near-infrared, the morphology of older star-dominated disks indicates
a simple classification scheme (1) H$m$ where $m$ is the dominant harmonic, (2)
a pitch angle (derived from the Fourier spectra) associated with the rate of
shear A/$\omega$ in the stellar disk and (3) a `bar strength' parameter,
robustly derived from the gravitational potential or torque of the bar. A
spiral galaxy may present two radically different morphologies in the optical
and near-infrared regime; there is no correlation between our quantitative dust
penetrated tuning fork and that of Hubble. Applications of our $z\sim$0 Fourier
template to the HDF are discussed using $L$ and $M$ band simulations from an
8-m NGST; the rest-wavelength IR morphology of high-$z$ galaxies should
probably be a key factor in deciding the final choice of instruments for the
NGST.
