The wide field (~20'×20') CCD photometry has been performed for more than 4,000 stars over a whole region of NGC 362 which is located inside the SMC halo. The Color-Magnitude diagram (CMD) and luminosit function (LF) for red giant branch (RGB) stars are presented, discussing a distinct bump along the RGB and some blue stars appearing in the blue horizontal branch (BHB) and above BHB. The anomalous globular cluster NGC 362 with highly populated red horizontal branch (RHB) stars is compared with the another anomalous globular cluster NGC 288 with highly populated BHB stars. A metal-rich, young blue component and metal-'poor, old red component of the SMC halo stars are examined.

The BV photographic photometry was made for 1714 stars (V < 19.5m) in NGC 6752, using 83 photoelectric stars and many secondary photographic standard stars over the area of 3.3' - 11.3' from the cluster center. Their data and finding chart are presented.

We present a near-infrared (K, J-K) color magnitude diagram(CMD) for the central region of a metal poor globular cluster NGC 6535. Our near-infrared data are combined with published optical BV data to construct (K, V-K) CMD. A new metallicity estimate is made by applying the relation between metallicity and MKo as proposed by Frogel, Cohen and Persson(1983). Our value is [Fe/H] = -1.66+-0.06, which is slightly higher than other results previously reported.

The first large-format CCD color-magnitude diagram (CMD) in the B and V passbands is presented for the Galactic globular cluster M53 (NGC 5024). We have discovered 117 new blue straggler (BS) candidates in the field of M53. The analysis of bright BS stars (V <19.0) clearly shows a bimodal radial distribution, with a high frequency in the inner and outer regions. The distribution is similar to that found in M3, a globular cluster with similar central density and concentration.

We have obtained the J K images of the central region of the globular cluster M3 (NGC5272), using the 256×256 InSb array. We present JK photometry of bright red giant branch stars in the central 2'.2×2'.2 region of M3. The infrared color-magnitude diagrams are presented. The comparison of the red giant branch of M3 with that of M13 confirms that both globular clusters have similar metal abundances.

In order to determine the metallicity of a globuar cluster, M3,by using the spectral indices, a kind of index grid has been establshed by stars in globular clusters, M3, M15, M71 and old open cluster, NGC 188. The indices were measured from the medium resolution spectra of about 2 Å. The summed indices were used to determine metallicity in order to increase signals. It is found that the core depth index is measured more accurately and leads result more accurate than the pseudo-equivalent width index. This method can be further improved by including many more calibration globular clusters of various metallicity to make finer grids. By this method, the metallicity of M3 is determined as [Fe/H] = -1.46±0.15.

More than 22,300 stars in NGC 6752 were measured over the region of 5' < r < 23' in B and V AAT plates. The most of these are main sequence(MS) stars and about 130 blue horizontal branch(BHB) stars were detected. The C-M diagram of all measured stars shows gaps appearing at V≈15.m2 and 16.m2 along the red giant branch(RGB) and their appearance shown by Lee & Cannon(1980) is found to be independent of measured region. The bimodal distribution of BHB stars is confirmed again and a wide gap shown by Lee & Cannon(1980) at V≈16m is clearly seen for stars in the outer part (8' < r < 13') in the cluster. It is noted, however, that this gap is occupied by about a dozen of BHB staIs located in the inner region (5' < r < 8'). The number ratio of bright BHB star (V < 15m) to faint BHB stars (V > 15m) decreases with increasing radial distance from the cluster center. Three faintest BHB stars were found, and two stars (V≈18.m5) of there are located in the inner region of r≈6' and the other faintest one (V≈19.m3) located in the outer part of r≈13'. Also a bluest star of (B - V) ≈ -0.5 at V≈17.m2 is found but it is located at the outer part of r≈13' in NE region. Therefore, the membership of the faintest BHB star and bluest star is suspected. The luminosity function(LF) and mass function(MF) for NGC 6752 were derived for MS stars. The LF for stars of Mv< 6m in the outer part of r > 8' shows a consistency with that derived by Penny & Dickens(1986).

The BVR CCD photometry was performed for the globular cluster M13 down to V=19m over the region from the center to the west 13 arcmin and the CMD of M13 is investigated. The major photometric error in the crowded field which is due to the variation in the sky background was corrected by the median filtering method and the direct sky method. Some characteristics of the CMD of M13 obtained in the present study are as follows: Firstly, the distribution of stars on the CMD is well consistent with the mean lines of Sandage(1970) along the red giant branch(RGB), horizontal branch(HB) and asymtotic giant branch(AGB). Secondly, some gaps exists along the RGB and blue horizontal branch(BHB). Thirdly, the UV-bright stars are more concentrated at the inner region of the cluster.

The BV-photographic photometry was made for 1714 stars (V<19.5) in NGC 6752. The C-M diagram of this cluster shows an unusually extended blue horizontal branch ( V = 13.5 ∼ 17.8 ) with a wide gap ( V = 16 ∼ 16.7 ) and the well defined giant branch with gaps at V=13.85 and 16.2. The turnoff point is defined at V = 17.25 ± 0.15 and (B-V) = 0.46 ± 0.02 . If we take V H B = 13.85 for NGC 6752, then Δ V = 2.80 , ( B − V ) 0 , g = 0.76 a n d Δ V T O = 3.40 and the chemical abundance is estimated to be [Fe/H]=-1.67 or Z = 4.3 × 10 − 4 a n d Y = 0.26 . Some other physical parameters of this cluster are derived and compared with those for the well observed clusters M 3, M 13, M 15 and M 92.