• Journal of The Korean Astronomical Society
• /
• v.12 no.1
• /
• pp.11-15
• /
• 1979

Four stars in the central region of 47 Tuc were observed spectroscopically using IPCS. The observed result showed that two asymptotic giant branch stars have the excess of nitrogen compared with the red giant branch stars, which indicates that the radial colour gradient in a globular clursters, at least for 47 Tuc, comes from the abundance gradient among the giant stars.

• Journal of The Korean Astronomical Society
• /
• v.34 no.3
• /
• pp.137-141
• /
• 2001

We derive a new relationship between the giant branch slope as measured in the color-magnitude diagram (K, J - K) and [Fe/H] metallicity for old open clusters. Previously such relationships have been derived for globular clusters, while similar tendency has been expected for open clusters. New derived correlation, [Fe/H]=-17.2($\pm$0.23)GB slope - 1.95($\pm$0.02), is based on a collection of data for 10 old open clusters. Most clusters behave as expected from the theoretical predictions.

• Journal of Astronomy and Space Sciences
• /
• v.17 no.1
• /
• pp.1-10
• /
• 2000

To derive the metallicities of M3 and M5, we used the shape of red giant branch, horizontal branch magnitude, and red giant branch bump on the (V-I)-V color magnitude diagrams. [Fe/H] values ranging -1.46 ∼ -1.69 for M3, and -1.00 ∼ -1.49 for M5 are estimated. These values are in good agreements with the previously determined ones. This result leads the morphologies of red giant and horizontal branches on the (V-I)-V color magnitude diagrams can be good indirect metallicity indicators of galactic globular clusters.

• Journal of The Korean Astronomical Society
• /
• v.38 no.2
• /
• pp.23-31
• /
• 2005

CN and CH band strengths for fourteen bright giants in the globular cluster M71 have been measured from archival spectra obtained with the Multiple Mirror Telescope. Adding the collected. data from the literature we confirm a bimodality of CN distribution on the red giant branch and the honzontal branch, and CN-CH anti-correlations on the lower giant branch and horizontal branch. However a CN-CH anti-correlation on the upper red giant branch is not quite clear as those of other branches. The small number If statistics could not be excluded as a possible cause. To confirm this, a greater number of sample stars are needed. We also confirm that the ratio of CN-strong to CN-weak stars is quite different from that in 47 Tuc, although the anti-correlation between CN and CH bands, the bimodality of the CN distribution, and the spatial distribution of CN stars in M71 are found to be similar to those III 47 Tuc.

• Journal of Astronomy and Space Sciences
• /
• v.27 no.4
• /
• pp.279-288
• /
• 2010

To study properties of the pulsation in the infrared emission for long period variables, we have collected and analyzed the infrared observational data at M band for 12 OH/IR stars. We present the light curves using the data that cover about 30 years including recent observations of ISO and Spitzer. We use Marquardt-Levenberg algorithm to determine the pulsation periods and amplitudes and compare them with previous results of infrared and radio investigations. Generally, the newly determined pulsation parameters show much less errors because of the larger database. We find that the relationship between the pulsation period and amplitudes at M band is fairly well fitted with a simple linear equation in a wide period range. For OH 42.3-0.1, we find some evidences that the object could be a post-asymptotic giant branch star.

• Journal of Astronomy and Space Sciences
• /
• v.17 no.2
• /
• pp.133-140
• /
• 2000

From the VI images of M13, obtained by using 2K CCD camera and the BOAO 1.8m telescope, we derive the(V - I) - V CMD of M13. From the shapes of red giant branch, the magnitude of horizontal branch, and the giant branch bump on the constructed CMD, we determined the metallicity of the globular cluster to be 1.74${\lesssim}$[Fe/H]${\lesssim}$-1.41. The good agreement between our determination of [Fe/H] and those determined by using other methods implies that the morphology of red giant and horizontal branches on (V - I) - V CMD's can be good indirect metallicity indicators of Galactic globular clusters.

• Asian Pacific Journal of Cancer Prevention
• /
• v.17 no.2
• /
• pp.673-676
• /
• 2016

Background: In the maxillofacial region, giant cell granulomas occur in 2 clinical forms, central and peripheral. Despite histopathological similarity between these 2 forms totally different clinical behaviors have been reported. The present study was undertaken to compare mast cell and vascular concentrations in these pathologic lesions. Materials and Methods: In this cross-sectional descriptive study, 20 pathological samples of central giant cell granuloma (CGCG) and 20 samples of peripheral giant cell granuloma (PGCG) were selected and examined through toluidine blue staining for mast cell assessment and immunohistochemical staining by VEGEF antibody for comparing the number of mast cells. T-test, chi-squared test and backward multivariate linear regression were used for statistical analysis using SPSS 20. Statistical significance was set at P<0.05. Results: This study showed significantly greater VEGF expression and mast cell concentrations in CGCG compared to PGCG cases. Also there was a significant correlation between VEGF expression and the concentration of mast cells. No relation was found between age, sex and site of the lesion and concentration of mast cells or VEGF expression. Conclusions: It is feasible that higher concentrations of mast cells in CGCG versus PGCG samples might lead to more aggressive clinical behavior via vascular proliferation and angiogenesis. However, other biologic mechanisms should be considered in this situation.

• Bulletin of the Korean Space Science Society
• /
• 2009.10a
• /
• pp.35.3-36
• /
• 2009

To investigate properties of the stellar contents of the resolved asymptotic giant branch stars in the nearby dwarf galaxies, we obtained wide-field JHKs images of the dwarf irregular galaxies NGC 6822, IC 1613 and the dwarf elliptical galaxy NGC 205, using the WIRCam near-infrared imager of the CFHT. The obtained (J-Ks, Ks) and (H-Ks, Ks) color-magnitude diagrams for the resolved stars in the galaxies contain populations of foreground stars, super giant stars, red giant stars and the asymptotic giant branch (AGB) stars. Using corollary photometric data in the visible bands, AGB stars were selected in the color-magnitude diagrams with a wide wavelength baseline in color indices. In color-color diagrams of the resolved AGB stars, we identified C stars from M giant stars for each galaxies, i.e., 726 C stars in NGC 6822, 126 C stars in IC 1613 and 593 C stars in NGC 205. The number ratios of C stars to M-giants were estimated to be $0.59\pm0.03$ in NGC 6822, $0.30\pm0.03$ in IC 1613 and $0.14\pm0.01$ in NGC 205. From analyses of the correlations of the spatial distribution of the C/M ratios with the HI properties and dynamical structures of the target galaxies, we discuss environmental effects of the star formation in the galaxies. We also discuss the epochs of the AGB star formation in the galaxies by comparing theoretical isochrones with the color distributions and luminosity functions of the AGB stars.

• The Bulletin of The Korean Astronomical Society
• /
• v.42 no.2
• /
• pp.51.2-51.2
• /
• 2017

As a result of our decade-long effort, we developed a new approach wherein small-aperture telescope powered by ingeniously designed narrow-band filter systems can have the capability to measure not only the heavy but also the lighter elemental abundances of the red-giant branch (RGB) and asymptotic-giant branch (AGB) stars in the globular clusters. Our novel approach can complement the intrinsic weakness of the results from the prestigious instruments, such as HST and the VLT. In our talk, we will present the multiple stellar populations of the RGB and the AGB stars in M5, as a pilot work.

• Journal of The Korean Astronomical Society
• /
• v.29 no.2
• /
• pp.171-179
• /
• 1996

We have obtained the J K images of the central region of the globular cluster M3 (NGC5272), using the $256\pm256$ InSb array. We present JK photometry of bright red giant branch stars in the central $2'.2\pm2'.2$ 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.