There is increasing evidence for the presence of multiple red giant branches (RGBs) in the color-magnitude diagrams of massive globular clusters (GCs). In order to investigate the origin of this split on the RGB, we have performed new narrow-band Ca photometry and low-resolution spectroscopy for M22, NGC 1851, and NGC 288. We find significant differences (more than 4σ) in calcium abundance from the spectroscopic HK ′ index for M22 and NGC 1851. We also find more than 8σ differences in CN band strength between the Ca-strong and Ca-weak subpopulations for these GCs. For NGC 288, however, a large difference is detected only in the CN strength. The calcium abundances of RGB stars in this GC are identical to within the errors. This is consistent with the conclusion from our new Ca photometry, where the RGB splits are confirmed in M22 and NGC 1851, but not in NGC 288. We also find interesting differences in CN-CH correlations among these GCs. While CN and CH are anti-correlated in NGC 288, they show positive correlation in M22. NGC 1851, however, shows no difference in CH between the two groups of stars with different CN strengths. We suggest that all of these systematic differences would be best explained by how strongly type II supernovae enrichment has contributed to the chemical evolution of these GCs.

A new isoprenylated flavonoid, 2S-5,7,2',4'-tetrahydroxy-3',5'-di-(γ,γ-dimethylallyl)flavanone, sanggenol Q (1), along with seven known isoprenylated flavonoids, sanggenol A (2), sanggenol L (3), kuwanon T (4), cyclomorusin (5), sanggenon F (6), sanggenol O (7), and sanggenon N (8), three known Diels-Alder type adducts, sanggenon G (9), mulberrofuran G (10), and mulberrofuran C (11), and a known benzofuran, moracin E (12), were isolated from the root bark of Morus alba using silica gel, ODS, and Sephadex LH-20 column chromatography. Chemical structures were determined based on spectroscopic data analyses including NMR, MS, CD, and IR. For the first time, compounds 1 and 7 were isolated from the root bark of M. alba. All compounds were evaluated for hepatoprotective activity on t-BHP-induced oxidative stress in HepG2 cells and neuroprotective activity on glutamate-induced cell death in HT22 cells. Compounds 1, 4, 8, 10, and 11 showed protective effects on t-BHP-induced oxidative stress with EC50 values of 6.94 ± 0.38, 30.32 ± 6.82, 23.45 ± 4.72, 15.31 ± 2.21, and 0.41 ± 0.48 μM, respectively, and compounds 1, 2, 10, 11, and 12 showed protective effects on glutamate-induced cell death with EC50 values of 5.54 ± 0.86, 34.03 ± 7.71, 19.71 ± 0.71, 16.50 ± 7.82, and 1.02 ± 0.13 μM, respectively.

Most globular clusters (GCs) are now known to host multiple stellar populations with different light element abundances. Here we use narrow-band photometry and low-resolution spectroscopy for NGC 362 and NGC 6723 to investigate their chemical properties and radial distributions of subpopulations. We confirm that NGC 362 and NGC 6723 are among the GCs with multiple populations showing bimodal CN distribution and CN-CH anti-correlation without a significant spread in calcium abundance. These two GCs show more centrally concentrated CN-weak earlier generation stars compared to the later generation CN-strong stars. These trends are reversed with respect to those found in previous studies for many other GCs. Our findings, therefore, seem contradictory to the current scenario for the formation of multiple stellar populations, but mass segregation acting on the two subpopulations might be a possible solution to explain this reversed radial trend.

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In our recent investigation (Lim et al. 2015), we have shown that narrow-band photometry can be combined with low-resolution spectroscopy to effectively search for globular clusters (GCs) with supernovae (SNe) enrichments. Here we apply this technique to the metal-poor bulge GC NGC 6273, and find that the red giant branch stars in this GC are clearly divided into two distinct subpopulations having different calcium abundances. The Ca rich subpopulation in this GC is also enhanced in CN and CH, showing a positive correlation between them. This trend is identical to the result we found in M22, suggesting that this might be a ubiquitous nature of GCs more strongly affected by SNe in their chemical evolution. Our results suggest that NGC 6273 was massive enough to retain SNe ejecta which would place this cluster in the growing group of GCs with Galactic building block characteristics, such as ω Centauri and Terzan 5.