  We have imaged a sample of 17 inclined spiral galaxies with measured
H$\alpha$ rotation curves in the K-band, in order to determine the morphology
of the old stellar population which dominates the mass in the disc. The K-band
images of the galaxies have been used to determine the radial extent of
Grand-Design spiral structure and compare this with the turnover radius in
their rotation curves, where the rotation curve transforms from solid-body
rotation to differential rotation. Thus, if the arms do not extend past this
radius, the winding problem is solved. We find in all 17 cases, the arms extend
past this radius, with the radius of grand-design spiral structure being a
factor of 1.3-9.6 times larger than the rotation curve turnover radius. Of
these galaxies, 4 have nearby neighbours and central bars and a further 7 have
a central bar. These bars or near neighbours may be the cause of the driving of
the spiral potential in the discs of these galaxies. Of the remaining 6
galaxies, 5 show some evidence for a bar or oval distortion in their K-band
images. The remaining galaxy (UGC 14) shows no evidence for a central bar and
has no nearby neighbours.
  Finally we also find that the spiral structure of these galaxies in the
near-infrared is extremely regular, although some range in the regularity of
spiral structure is found. To quantify this range in spiral structure, we
introduce the dust-penetrated arm class, which is analogous to the
dust-penetrated classification scheme of Block & Puerari (1999) and based on
the optical arm class of Elmegreen & Elmegreen (1982).
