Although disinfection in drinking water treatment plants provides a safer water supply by inactivating pathogenic microorganisms, harmful disinfection by-products may be formed. In this study, the disinfectant, chlorine, was produced on-site from the electrolysis of salt (NaCl), and the by-products of the disinfection process, bromate and chlorate, were analyzed. The provisional guideline levels for bromate and chlorate in drinking water are 10 μg/L and 700 μg/L, in Korea, respectively. Bromide salt was detected at concentrations ranging from 6.0 ~ 622 mg/kg. Bromate and chlorate were detected at concentrations ranging from non-detect (ND) ~ 45.3mg/L and 40.5 ~ 1,202 mg/L, respectively. When comparing the bromide concentration in the salt to the bromate concentration in the chlorine produced by salt electrolysis, the correlation of bromide to bromate concentration was 0.870 (active chlorine concentration from on-site production: 0.6–0.8%, n=40). The correlation of bromate concentration in the chlorine produced to that in the treated water was 0.866.

MgB2 bulk superconductors are synthesized by the solid state reaction of (MgB4+xMg) precursors withexcessive Mg compositions (x=1.0, 1.4, 2.0 and 2.4). The MgB4 precursors are synthesized using (Mg+B) powders. Thesecondary phases (MgB4 and MgO) present in the synthesized MgB4 are removed by HNO3 leaching. It is found thatthe formation reaction of MgB2 is accelerated when Mg excessive compositions are used. The magnetization curves ofMg1+xB2 samples show that the transition from the normal state to the superconducting state of the Mg excessive sam-ples with x=0.5 and x=0.7 are sharper than that of MgB2. The highest Jc-B curve at 5 K and 20 K is achieved forx=0.5. Further addition of Mg decreases the Jc owing to the formation of more pores in the MgB2 matrix and smallervolume fraction of MgB2.

One of the endoparasitoid wasp, Cotesia plutellae (Braconidae), parasitizes young larvae of the diamondback moth, Plutella xylostella. For the successful parasitization, C. plutellae required suppression of immune response in P. xylostella. Maternal (polydnavirus, venom proteins and ovary proteins) and embryonic (teratocytes) factors have been involved in immune-suppression. In this study, we performed transcriptome analysis of venom of C. plutellae and identify neprilysin-1 (Cp-NEP1) as a potential immunosuppressive protein. Cp-NEP1 encoded 451 amino acids and largely belongs to the hymeopteran neprilysin family via phylogenetic analysis. It is of interest that Cp-NEP1 has no conserved motifs such as zinc-binding domain (HExxH), substate binding domain (NAYY/F) and protein folding and maturation domain (CxxW) generally identified in other neprilysin family. In order to examine the biochemical function of Cp-NEP1, the recombinant Cp-NEP1 tagged with N-terminally 6X His was constructed and expressed in Escherichia coli. Expression of Cp-NEP1 was confirmed with SDS-PAGE and peptide sequencing. Recombinant Cp-NEP1 significantly suppressed nodule formation when the co-injection with E. coli. These results suggest that Cp-NEP1 contributes to suppression of immune response in P. xylostella and that the conserved motifs reported from other neprilysin do not involve immunosupperssion.

Star formation activities dominate the evolution of galaxies. Elliptical galaxies are believed to be old galaxies in the Hubble sequence, and elliptical galaxies at different evolution epochs might have different star formation activities and/or morphologies. We investigate the connection between star formation rates and the morphology of elliptical galaxies. With the Sloan Digital Sky Survey (SDSS) and the Galaxy Zoo, we select a sample of elliptical galaxies by morphology and consider their infrared emission as an index of star formation rate to study the relation between the star formation rates and their morphological properties, such as ellipticities. In addition, we select some nearby spiral galaxies with very low MIR emission to probe the mechanisms of these red spiral galaxies. We display our preliminary results and discuss their implication on the evolution of galaxies in this poster.

This work aims to study the evolution of galaxies, located in the dense environment of the NGC 4095 compact group, which have recession velocities 6,000 < v (km s-1) < 8,000. Imaging observations for BV Rc broad-band, and [S ii] and red-continuum narrow-band were carried out with the 2.4 m Thai National Telescope (TNT) at Doi Inthanon, Chiang Mai, Thailand. The sample contains 13 galaxies, consisting of 8 spirals, 4 ellipticals and 1 irregular morphological type. Late type galaxies tend to be bluer than early type galaxies. The results show that most of the late type galaxies have ongoing star formation activity, which could be triggered by galaxy-galaxy or tidal interactions, and that young massive stars in these galaxies cause their colors to be bluer than the early type galaxies.

We use multi-wavelength observations of galaxy groups to probe the formation models for galaxy for- mation in cosmological simulations, statistically. The observations include Chandra and XMM-Newton X-ray observations, optical photometry and radio observations at 1.4 GHz and 610 MHz. Using a large sample of galaxy groups observed by the XMM-Newton X-ray telescope as part of the XMM-Large Scale Survey, we carried out a statistical study of the redshift evolution of the luminosity gap for a well de- fined mass-selected group sample and show the relative success of some of the semi-analytic models in reproducing the observed properties of galaxy groups up to redshift z ~ 1.2. The observed trend argues in favour of a stronger evolution of the feedback from active galactic nuclei at z < 1 compared to the models. The slope of the relation between the magnitude of the brightest cluster galaxy and the value of the luminosity gap does not evolve with redshift and is well reproduced by the models. We find that the radio power of giant elliptic galaxies residing in galaxy groups with a large luminosity gap are lower compared to giant ellipticals of the same stellar masses but in typical galaxy groups.

We present an analysis of the relation between star-formation (SF) and accretion luminosities of local type-2 active galactic nuclei (AGNs) at 0:01 ≤ z < 0:22. We match type-2 AGNs found in the Sloan Digital Sky Survey to current far-infrared (FIR) survey catalogues based on AKARI and Herschel. Estimating AGN luminosities from [O iii]5007 and [O i]6300 emission lines, we find a positive linear trend between FIR and AGN luminosities over a wide dynamical range. This result appears to be inconsistent with recent reports that low-luminosity AGNs show no correlation between FIR and X-ray luminosities; this contradiction is likely due to Malmquist and sample selection biases. Moreover, we also nd that pure- AGN candidates, for which the FIR radiation is thought to be AGN-dominated, show significant low-SF activities. These AGNs hosted by low-SF galaxies are rare in our sample. However, it is possible that the low fraction of low-SF AGN is caused by observational limitations, as recent FIR surveys are not suffcient to examine the population of high-luminosity AGNs hosted by low-SF galaxies.

NGC147 and NGC185, paired satellites of the Andromeda galaxy, possess the same order of mass and analogous structures, but they show dierent star formation and different amounts of interstellar gas and dust. Therefore, we present the first reconstruction of the star formation history of NGC147 and NGC185. Asymptotic Giant Branch stars are highly evolved stars that are brightest in K-band. This maximum K-band magnitude is related to the birth mass of stars. As a result, we have found a 9.9 Gyrold single star formation epoch for NGC185 followed by relatively continuous star formation. NGC147, however, has passed through two star formation episodes; one is as old as ~6 Gyr and the other is as recent as 850 Myr. Asymptotic Giant Branch stars are also important dust factories; by fitting Spectral Energy Distributions to observed near and mid infrared data for each star, we were able to measure the dust production rates of individual stars; on order of 10-5M⊙yr-1. Hence, we estimate the total mass entering the interstellar medium to be 1.06 X 10-4M⊙ yr-1 and 2.89 X 10-4M⊙ yr-1 for NGC147 and NGC185.

The Galactic center uniquely provides opportunities to resolve how star clusters form in neutral gas overdensities engulfed in a large-scale accretion flow. We have performed sensitive Green Bank 100m Telescope (GBT), Karl G. Jansky Very Large Array (JVLA), and Submillimeter Array (SMA) mapping observations of molecular gas and thermal dust emission surrounding the Galaxy's supermassive black hole (SMBH) Sgr A*. We resolved several molecular gas streams orbiting the center on ≳10 pc scales. Some of these gas streams appear connected to the well-known 2-4 pc scale molecular circumnuclear disk (CND). The CND may be the tidally trapped inner part of the large-scale accretion flow, which incorporates in ow via exterior gas filaments/arms, and ultimately feeds gas toward Sgr A*. Our high resolution GBT+JVLA NH3 images and SMA+JCMT 0.86 mm dust continuum image consistently reveal abundant dense molecular clumps in this region. These gas clumps are characterized by ≳100 times higher virial masses than the derived molecular gas masses based on 0.86 mm dust continuum emission. In addition, Class I CH3OH masers and some H2O masers are observed to be well associated with the dense clumps. We propose that the resolved gas clumps may be pressurized gas reservoirs for feeding the formation of 1-10 solar-mass stars. These sources may be the most promising candidates for ALMA to probe the process of high-mass star-formation in the Galactic center.

How high-mass stars form is currently unclear. Calculations suggest that the radiation pressure of a forming star can halt spherical infall, preventing further growth when it reaches 10 M⊙. Two major theoretical models on the further growth of stellar mass have been proposed. One model suggests the merging of less massive stellar objects, and the other is through accretion, but with the help of a disk. In ow motions are key evidence for how forming stars gain further mass to build up massive stars. Recent developments in technology have boosted the search for in ow motion. A number of high-mass collapse candidates were obtained with single dish observations, and mostly showed blue proles. Infalling signatures seem to be more common in regions which have developed radiation pressure than in younger cores, which is the opposite of the theoretical prediction and is also very different from observations of low mass star formation. Interferometer studies so far confirm this tendency with more obvious blue profiles or inverse P Cygni profiles. Results seem to favor the accretion model. However, the evolution of the infall motion in massive star forming cores needs to be further explored. Direct evidence for monolithic or competitive collapse processes is still lacking. ALMA will enable us to probe more detail of the gravitional processes.

We present observational results characterizing molecular out ows from very low-mass objects in ρ Ophiuchi and Taurus. Our results provide us with important implications that clarify the formation process of very low-mass objects.

This study aimed to investigate the effect of various emulsifiers on the formation of nanoemulsions and their stability properties. MCT (medium chain triglyceride) nanoemulsions were prepared (10 wt% oil, 10 wt% emulsifiers, 20 mM bis-tris, pH 7) with emulsifier such as Tween 20 (Polyoxyethylene(20) sorbitan monolaurate), Almax 3800 (Sorbitan monooleate), soy lecithin, and SSL (sodium stearoyl lactylate) and changes in fat globule size with respect to storage period and stability properties by Turbiscan were investigated. In case of control nanoemulsion with 10 wt% Tween 20, the initial fat globule size was 89.0 nm and 113.4 nm after 28 day of storage and this large increase (ca. 24 nm) was thought to be caused by Ostwald ripening. When Tween 20 was partially replaced with Almax 3800, lecithin and SSL in nanoemulsions, their physicochemical properties (i.e., fat globule size and stability) were changed accordingly. In general, the intial fat globule size was decreased with increasing the concentration of the emulsifiers and the stability against Ostwald ripening increased. The most stable nanoemulsions against Ostwald ripening could be prepared with emulsifiers of Tween 20 and Almax 3800 or lecithin in the ratio of 6:4 (wt%), which was verified with Ostwald ripening rate (ω). In addition, the emulsion stability by Turbiscan was observed to be consistent with results of changes in fat globule size with storage period.

The study was conducted to investigate the effects of post-incubation period and temperature treatment conditionsduring incubation on the uniform primordia formation and cultural characteristics of oyster mushroom (Pleurotus ostreatus). Threekinds post-incubation period; 25, 30, 35 days and control were applied for 30 days while two kinds incubation roomtemperature 23oC and 26oC and control were used 20oC. The substrate temperature during pre-incubation was of ‘Suhan No. 1’and ‘Gonji No. 7’. Oyster mushroom varieties tended to increase between 24oC to 26oC at 11 to 15 days after inoculation andthen they were maintained in treatment temperature during post -incubation period. The CO2 occurrence was at the highest at6,500ppm for ‘Suhan No. 1’ and 5,800ppm for ‘Gonji No. 7’ at the time of the highest temperature increase. The ratio of un-uniformal primordia formation and the ratio of non-commercial fruit body were reduced by 40%, 10.5%, respectively comparedto control for ‘Suhan No. 1’ when in the post-incubation temperature was 26oC, and incubated for 10days and 15daystreatment. Also, ‘Gonji No. 7’ was reduced by 19%, 9.5%, respectively when in the post-incubation temperature was 26oC, andincubated for 10 days treatment. Therefore, the higher post-incubation temperature of room and longer post-incubation periodresulted in the higher percentage of primordia formation of two cultivars.

CESL은 EU 역내 계약법을 개정하지 않고 개별회원국이 채택하는 경 우 특별법의 지위를 점할 수 있도록 성안되었다. 이에 CESL은 국제상사 계약에 있어 계약당사자의 합의에 따라 자발적으로 적용된다. CESL상 계약당사자의 의무 및 불이행에 관한 규정체계는 구체적이고도 광범위하 다. 주요 내용은 의사표시하자, 계약의 현저한 불균형 내지 불공정성, 표 준약관 삽입과 관련한 법적 유효성, 소유권 또는 담보권의 이전에 대한 법률효과, 계약의 유효성, 서비스 계약 및 디지털 콘텐츠와 관련한 계약 등이다. 이 경우 CESL은 서식의 교전에 관한 규정을 보유하여 보다 포 괄적이고 응집된 규칙을 보유하고 있는 특징이 있다. CESL은 독립적으로 그리고 당해 목적과 일반원칙에 따라 해석되어져 야 하고, 나아가 CESL의 범위 내에 있지만 명시적으로 규정하고 있지 않는 사안에 대하여도 그 처지는 마찬가지다. CESL의 적용에 대하여는 해석, 합리성, 불요식, 개별적으로 협상되지 않는 계약내용, 계약의 해제, 혼합목적의 계약, 통지, 기간의 계산, 일방적인 진술 또는 행동 등이다. CESL은 계약체결 전 일방이 계약내용에 기한 정보를 제공하지 않을 경우 신의 및 공정거래 위반에 해당되는 것으로 취급하고 있다. 나아가 원거리 계약의 경우 전자적 방법의 계약체결을 용인하고 있고 계약체결 전 또는 체결 시 정보를 제공하는 일방은 계약내용의 구속력 확보를 위 해 그리고 특정장소에서 당해 의무를 준수하기 위한 정보가 정확히 전달 되었음을 확인할 수 있도록 합리적 주의의무를 부과하고 있다. 만약 당 해 의무위반에 기하여 부정하거나 잘못된 정보가 제공된 경우 타방은 특 단의 구제권을 행사할 수 있다. CESL은 당사자의 합의, 합의에 기한 법적 구속력, 충분한 계약의 내 용과 확실성 등을 계약체결의 요건으로 두고 있다. 또한 의사표시의 하 자에 기하여 착오ㆍ사기ㆍ강박ㆍ부당한 착취에 대해 계약을 취소할 수 있는 권리를 보장하고 있으며, 취소통지, 취소효과, 추인, 손해배상금, 구 제수단의 배제 또는 제안과 구제수단의 선택 등을 이에 추보하고 있다. 나아가 계약내용의 해석기준으로서 계약내용 해석의 원칙, 계약내용 및 그 효력, 불공정한 계약내용 등으로 구분하여 다루고 있는 특징이 있다.