We present a study of the old open cluster Trumpler 5 (Tr 5), based on the CDS archival data. From the color-magnitude diagrams of Tr 5, we have found the positions of main-sequence turn-off (MSTO) and red giant clump (RGC) stars. Using the mean magnitude of the RGC stars, we have estimated the reddening toward Tr 5, E(B - V) = 0.60 ± 0.10. Using the stars common in two data sets and the theoretical isochrones of Padova group, we have estimated the distance modulus Vo - Mv = 12.64 ± 0.20 (d = 3.4 ± 0.3 kpc), the metallicity [Fe/H) = -0.30 ± 0.10, and the age of 2.4 ± 0.2 Gyr (log t = 9.38). These metallicity and distance values are consistent with the relation between the metallicity and the Galactocentric distance of other old open clusters, for which we obtain the slope of Δ[Fe/H]/ Rgc = -0.064 ± 0.010 dex kpc-1.

We have conducted VI CCD photometry of the open cluster NGC 6819 in order to understand the effects of dynamical evolution in old open clusters. Our photometry covers 18'× 18' on the sky, centered on the cluster, which seems to cover the whole cluster field. Our photometry reaches down to V ≈ 20.5, which allows us to analyze the luminosity function and spatial distribution of stars brighter than Mv ≈ 8.5. There is a clear evidence for mass segregation in NGC 6819, i.e., the giants and upper main-sequence stars are concentrated in the inner regions, whereas the lower main-sequence stars distribute almost uniformly throughout the cluster. The luminosity function of the main-sequence stars of NGC 6819 is almost flat. The flat luminosity function indicates that a large number of low mass stars has escaped from the cluster unless its initial mass function is much different from the Salpeter type (Φ(m)∝ m-(1+x),x = 1.35).

We have conducted UBVI CCD photometry of an intermediate-age open cluster NGC 559 to investigate the effect of dynamical evolution on the stellar distributions in NGC 559. Our photometry allows better estimates of distance and age of the cluster owing to much deeper photometry (V ≤ 21) than previous ones. It is found that the luminosity function and mass function as well as the spatial stellar distributions are affected by the dynamical evolution. Mass segregation leads to the central concentration of the high mass stars, which results in the flattened mass function inside the half mass radius.

UBV RI and Hα photometry has been performed for the open cluster NGC 6531. A total of 56 bright main sequence (MS) members were selected from their positions in photometric diagrams. We also classified 7 pre-main sequence (PMS) stars and 6 PMS candidates with Hα emission from Hα photometry. We determined a reddening of < E(B - V) >= 0.29 ± 0.03 and a distance modulus of Vo - Mv = 10.5 for the cluster. From the comparison of our photometric results to theoretical evolution models, we derived a MS turnoff age of 7.5 Myr and a PMS age spread of ~4 Myr. The IMF slope Γ, calculated in the mass range of 0.45 ≤ log m ≤ 1.35 is a steep value of Γ = -1.8 ±0.6.

UBVI CCD photometry of open cluster NGC 2324 is presented. C-M diagrams of this cluster show well-defined main sequence with a red giant clump centered at B - V =1.05, V =13.45. We derived the major cluster characteristics; E(B - V)=0.17±0.12 from color-color diagram and mean color of red giant clump stars, (m - M)o=13.1±0.1 from zero age main sequence fitting, and [Fe/H]~-0.32 from comparison the theoretical model developed by Bertelli et al. (1994) to the observed C-M diagrams. We estimate the age of NGC 2324 to be log t~8.8 by applying isochrone fitting and morphological age index method.

We present the results of near-IR band (JHK) photometric study for the old open cluster To 2. Combined with existing optical data, our IR photometry is used to derive the reddening E(B- V)=0.24±0.12 and the distance (m-M)o=14.6±0.42. Comparison with theoretical isochrones suggests the age and metallicity of To 2 are log t~9.3 and [Fe/H]~-0.3, respectively.

We present BVRI CCD photometry and near-infrared K photometry of the intermediate-aged open cluster NGC 7790. The reddening, E(B - V) = 0.54 ± 0.05 and the distance modulus, (m - M)o = 12.45 ± 0.10 for the cluster were determined by zero-age-main-sequence fitting and theoretical isochrone fitting using not only (V, B - V), (V, V - 1), (V, V - R) but also (V, V - K) color-magnitude diagrams. The reddening corresponded approximately to the average value derived from previous studies, while the distance modulus was found to be almost midway between the CCD photometric results of Romeo et al. (1989) and those of Mateo & Madore (1988). We have used four colors to distinguish members from field stars. The expected colors were calculated using the derived distance modulus, and were then were compared with the observed colors (B - V), (V - 1), (V - R), and (V - K). Thus, a color excess E(B - V) for each star was determined which could give the minimum difference between the calculated and observed colors. Single and binary members of the cluster were determined on the basis of the E(B - V) distribution of stars.

We present a new UBVI CCD photometry of the intermediate-age open cluster NGC 2420. Our photometry covers a field of 7′9×7.′7 7′9×7.′7 of the sky centered on the cluster. We determined the reddening and distance to the cluster by the main sequence fitting as E(B−V)=0.05±0.02 E(B−V)=0.05±0.02 and (m−M)o=11.9±0.1 (m−M)o=11.9±0.1 , along with the age of \~2 \~2 Gyr by fitting the Padova isochrones to the observed color-magnitude diagrams of the cluster. The fraction of binaries is found to be 44±5% 44±5% and they are likely to locate in the central region of the cluster. The spatial distributions of the binaries and the variation of the cluster luminosity functions along the radius suggest mass segregations due to the dynamical evolution of the cluster.

We present UBV CCD photometry of Be 2, previously unstudied open cluster. Our photometry covers a field of 3'.2×3'.8 of the sky centered on the cluster, which is slightly smaller than the cluster diameter estimated to be about 260". We have determined the reddening, distance, age and metallicity of the cluster by fitting the Pad ova isochrones to the observed stellar distributions in color-magnitude diagram as well as main sequence fitting: E(B-V)=0.8±0.05, (m-M)o=13.6±0.1, log(t) =8.9±0.1, and Z=0.008. The present photometry shows that Be 2 is a distant open cluster of intermediate age. that it is a distant intermediate-age open duster.

We have estimated a metal abundance of [Fe/H]= -0.48 ± 0.14 dex, a reddening of E(B- V)= 0.30 mag, an age of 2.0 ± 0.4 Gyr, and a distance of 7.9 ± 0.8 kpc for Tombaugh 2 using the Washington filter system.

We have estimated a metal abundance of [Fe/H]= -0.04 ± 0.05 dex, a reddening of E(B- V)= 0.28 mag, an age of 1.1 ± 0.1 Gyr, and a distance of 2.5 ± 0.2 kpc for NGC 1245 using the Washington filter system.

Galactic open clusters NGC 1907 and NGC 1912 are known as a binary cluster candidate by Subramaniam et al.(1995). With the SNUO 0.6m telescope, UBV CCD photometric observations were performed for 62 stars in NGC 1907 within the area of 8′×8′ 8′×8′ and 203 stars in NGC 1912 within the area of 15′×15′ 15′×15′ area. We obtained C-M and C-C diagrams. Their mean reddenings are E(B-V) = 0.50±0.03 0.50±0.03 for NGC 1907 and 0.27±0.03 0.27±0.03 for NGC 1912. The distance moduli are estimated as 10.9±0.15 10.9±0.15 and 10.4±0.10 10.4±0.10 for NGC 1907 and NGC 1912, respectively. The ages for these clusters are 400±50Myr 400±50Myr for NGC 1907 and 150±30Myr 150±30Myr for NGC 1912. The distance difference of the two clusters is 300pc and the age difference is 150Myr. These results imply that the two clusters are not physically connected.