We have conducted BVI photographic surface photometry of four spiral galaxies NGC1087, NGC2715, NGC2844 and NGC3593, by making use of the Kiso Schmidt plates. Detailed examination of the morphological properties of the galaxies using isophotal maps and luminosity profiles showed that all the program galaxies have some peculiarities in their luminosity distributions. NGC1087 and NGC2715 have extremely small nuclei with inner rings which contain several bright HII regions. NGC2844 has a very large bulge whose luminosity dominates over the disk luminosity in all the radii. The I-band luminosity profile of NGC3593 shows shallower gradient than B- and V-band profiles. We were able to successfully decompose the luminosity profile into a bulge following de Vaucouleurs γ 1 / 4 − l a w and an exponential disk only for NGC 3953. Other galaxies have more complicated luminosit profiles.

Three galaxies, NGC 0891(Sb),NGC 3359(SBc) and NGC 7640(SBc) have been taken to figure out the radio structural differences of spiral and barred spiral galaxies. Those galaxies have been observed in 21 cm neutral hydrogen emission line with 300 feet N.R.A.O, radio telescone(Rots, 1979). As Rots' observational line profiles have low angular resoulution, we could not distinguish the radix structural differences of those galaxies: Instead, the neutral hydrogen gases of each galaxy have been shown to tie widely distributed and the HI extents are much larger than the photographically shown ones. Furthermore, as peak column density regions coincide with the central regions of the galaxies, the large extensive radio structures may reveal the neutral gas distributions of the halo parts. The neutral hydrogen mass of each galaxy has been derived from the column density distributions. The line profiles of each galaxy help to obtain the velocity curves, from which the total kinematic mass can be calculated.

PDS was used to get the structure of two barred spiral galaxies NGC 1313 and NGC 1365. The result shows that NGC 1365 has both a deep spheroidal component and an exponential disk, but NGC 1313 has only an prominent exponential component. The luminosity profiles indicate that KGC 1313 is in type I and NGC 1365 belongs to type II. The length scales ( α − 1 ) were derived from the exponential luminosity distributions as 1.64 kpc for NGC 1313 and 2.49kpc for KGC 1365.