The abnormal meat could caused by abscess, fibrosis and granuloma in the region of the neck by the adverse effect of foot-and-mouth disease (FMD) vaccination practice for Korean swine. After FMD vaccination was implemented in 2010, the number of incidences of abnormal meat has been increasing. In this study, it was evaluated whether needless intradermal injection (NII) of FMD vaccine reduces abnormal meat at the injection site in comparison to conventional intramuscular injection (IM). In addition, the onset of humoral immunity was analyzed in order to see if NII of this vaccine is able to mount comparable antibody response with IM. This study was carried out in four Korean pig farms. The O-type FMD vaccine was implemented via NII at three farms and the control group was vaccinated via IM. Antibody titers were compared from the serum samples taken from 10 random pigs at age of 8, 12, 16 and 22~24 weeks of age. The O+A type FMD vaccine was also compared with the same protocol. When test animals were slaughtered, incidence, type and size of abnormal meat were recorded. The results of this study showed that the antibody titers between intradermal and intramuscular group were similar but a significant difference in the incidence of abnormal meat formation was observed between two groups (p < 0.05). In summary, needless intradermal injection of FMD vaccination was proven to be effective for the onset of humoral immunity and reducing abnormal meat formation.

We present results of a H13CN J=1-0 mapping survey of molecular clouds toward the Galactic Center (GC) region of -1.6° ≤ l ≤ 2° and -0.23° ≤ b ≤ 0.30° with 2' grid resolution. The H13CN emissions show similar distribution and velocity structures to those of the H12CN emissions, but are found to better trace the feature saturated with H12CN (1-0). The bright components among multi-components of H12CN line profiles usually appear in the H13CN line while most of the dynamically forbidden, weak H12CN components are seldom detected in the H13CN line. We also present results of other complementary observations in 12CO (J=1-0) and 13CO (J=1-0) lines to estimate physical quantities of the GC clouds, such as fractional abundance of HCN isotopes and mass of the GC cloud complexes. We confirm that the GC has very rich chemistry. The overall fractional abundance of H12CN and H13CN relative to H2 in the GC region is found to be significantly higher than those of any other regions, such as star forming region and dark cloud. Especially cloud complexes nearer to the GC tend to have various higher abundance of HCN. Total mass of the HCN molecular clouds within |l|≤ 6° is estimated to be ~2 ×10 7 M⊙ using the abundances of HCN isotopes, which is fairly consistent with previous other estimates. Masses of four main complexes in the GC range from a few 10 5 to ~ 10 7 M⊙ All the HCN spectra with multi-components for the four main cloud complexes were investigated to compare the line widths of the complexes. The largest mode (45 km s-1) of the FWHM distributions among the complexes is in the Clump 2. The value of the mode tends to be smaller at the farther complexes from the GC.

The structure and environments of the molecular clouds near the SNR HB3(G132.7±1.3) HB3(G132.7±1.3) are studied. The molecular complex which is located at the southern rim of HB3 was proposed by former investigators as the one interacting with HB3. This complex region of 2∘×2∘atl=133∘ 2∘×2∘atl=133∘ has been observed at 12CO,13CO,J=1−0ata1′ 12CO,13CO,J=1−0ata1′ , resolution with the 14-m radio telescope at Taeduk Radio Astronomy Observatory. We have reached to the following four conclusions. The possibility that these molecular complex and HB3 are interacting with each other cannot be supported with any of our data. The morphologies of the two show no similarities. Neither particular features for the interaction are found in the CO lines. The hypothetical 'Molecular wall' which was expected to exist on the northwestern rim of HB3 as a cause for the noncircular morphology of HB3 is turned out to be nonexistent in CO. The molecular complex which resembles a 'bar' at a low resolution is now resolved into a U-shaped shell. It seems that the U-shape is consist of two independent components. No peculiarities, such as unseen masses or bright stars capable of forming HlI regions, are found within the U-shape region. The total mass included in the complex is estimated to be Mtotal=2.9\~8.4×105M⨀ Mtotal=2.9\~8.4×105M⨀ , which is in good agreement with previous observations within errors. Considering about 12 clumps distinguishable within the complex, the total mass implies that masses of each of clumps are on the order of 104M⨀ 104M⨀ , which makes these good objects for further studies in relation to star-formation. Especially the clumps associated with W3 are worthy for more high resolution observations for better understanding of astrophysical phenomenon ongoing in them.

The initial mass functions (IMF) of 15 selected open clusters are investigated by making use of C-M diagrams and theoretical evolutionary tracks. Among 15 clusters 13 have peaks in their IMFs and it is thought to be not due to incomplete photometry but to intrinsic property. The mass where IMF peaks is about 2 M ⊙ and it is similar to that of the second peak in the IMF of nearby field stars. The mean slope of the IMF in the high mass part is 1.9 ± 0.6 with some variations among clusters. But there seems to be no correlation between the slope and physical parameters such as ages, diameters, and metal abundances.