The notorious lamiine species Asian Longhorn Beetle, Anoplophora glabripennis, is one of the major invasive pests of street trees, which is an endemic species of Korea and China. By far, the distributional range of Korean A. glabripennis population is restricted to only central to northeastern forest region of South Korea. In this study, we found unreported A. glabripennis populations in 4 different port cities and adjacent cities. These new populations are found in very much urbanic regions; Incheon, western part of Seoul, Busan and Ulsan. These populations can be distinctly differentiated with previously reported populations by massive damage on trees, unusual usage of host plant and spotted elytral pattern. To test their identity, we analyse the genetic patterns of the A. glabripennis populations sampled across South Korea based on three mitochondrial genes, Cytochrome Oxidase I – leucin tRNA – Cytochrome Oxidase II (COI-tRNALeu- COII). Additionally, we used available sequences of COI - tRNALeu - COII of 104 Chinese and 15 Korean individuals from NCBI. Here we show that Korean population is distinctly divided into two major clades, namely native populations and non-native ones, with 0.7% ~ 1.2% of genetic divergence. Hence, the non-native ones can be divided into two subgroups, which we call Incheon-Seoul complex and Busan-Ulsan complex. We observed that these newly found groups, Incheon-Seoul complex and Busan-Ulsan complex share perfectly identical COI haplotype within each group. This study strongly suggests that newly found populations are introduced respectively and these populations might be derived from very small number of introduced founders.

매스틱(Mastic) 아스팔트 포장은 독일에서 최초 개발된 Guss 아스팔트 포장으로 국내에는 강상판 데크 (steel deck) 교량의 아스팔트 포장시 중간층(intermediate course)용으로 도입되었다. 하지만 강상판 교 면포장용으로 사용되던 매스틱 아스팔트 포장이 근래에는 노후 콘크리트 포장을 절삭하고 덧씌우는 일반 구간 아스팔트 포장의 중간층용으로도 사용되고 있다. 매스틱 포장의 특징은 방수가 잘되고 진동이 심한 강상판 데크의 진동흡수에 적합토록 유연성이 큰 것이다. 하지만 이를 콘크리트 포장위의 덧씌우기 (overlay)에 사용 시 주목적인 방수 외에 반사균열(reflection cracking) 문제에 대한 저항성 여부는 구명 된 바가 없다. 따라서 본 연구의 목적은 매스틱 아스팔트를 중간층으로 사용 시 반사균열 저항성이 어느 정도인지를 실내시험을 통하여 파악하는 것이다. 이를 위하여 10mm 콘크리트 조인트 위에 2개 층의 아 스팔트 층을 상하(중간층과 표층)로 70mm 포설하는 구조를 모사한 시험체(test body)를 만들고 Mode II (전단 모드) 반사균열 시험을 실내에서 수행하였다(그림 1). 비교 대상은 일반 밀입도 아스팔트 (dense-graded asphalt: DGA) 콘크리트 상하층, SMA 아스팔트 콘크리트 상하층, 매스틱 중간층과 DGA 및 SMA를 표층으로 하는 층상구조로 하였다. 또한 관행적으로 사용해 온 DGA 아스팔트 콘크리트 단층과 SMA 및 매스틱 단층도 참고적으로 비교하였다. 시험 결과 매스틱을 중간층으로 한 시험체의 반사 균열 저항성이 그 외의 덧씌우기 층상구조보다 반사균열 저항성이 우수한 것으로 확인되어, 매스틱 층은 방수기능 외에도 응력흡수 층으로 좋은 역할을 하는 것으로 판명되었다.

We present population synthesis models for the calcium II triplet (CaT), currently the most popular metallicity indicator, based on high-resolution empirical spectral energy distributions (SEDs). Our new CaT models, based on empirical SEDs, show a linear correlation below [Fe/H] ~ -0.5, but the linear relation breaks down in the metal-rich regime by converging to the same equivalent width. This relation shows good agreement with the observed CaT of globular clusters (GCs) in NGC 1407 and the Milky Way. However, a model based on theoretical SEDs does not show this feature of the CaT and fails to reproduce observed GCs in the metal-rich regime. This linear relation may cause inaccurate metallicity determination for metal-rich stellar populations. We have also conrmed that the effect of horizontal- branch stars on the CaT is almost negligible in models based on both empirical and theoretical SEDs. Our new empirical model may explain the difference between the color distributions and CaT distributions of GCs in various early-type galaxies. Based on our model, we claim that the CaT is not a good metallicity indicator for simple stellar populations in the metal-rich regime.

This paper presents on the structural behavior of the the methyl methacrylate monomer (MMA) double wide flanged the glass fiber-reinforced polymer(GFRP) pipe composite structures for the manhole raise. The evaluation of structural performance on this composite structure was conducted by the axial load, fatigue load, and ultimate load test. The assessment indicates that the MMA double wide flanged GFRP pipe composite structures was confirmed safety, durability and reliability in result as expected. It was found that this composite structure was able to short working times to around 30-50% and construction costs to around 10-23% with compare other construction methods. Also, environmental pollution and civil complaints will be prevented because there will be no longer any noises, vibrations, dust, or construction wastes.

Astronomical observation is the beginning of scientific attitudes in the history of mankind. According to Indian tradition, there existed 18 early astronomical texts (siddhantas) composed by Surya, Pitamaha and many others. Varahamihira compiled five astronomical texts in a book named panchasiddhantika, which is now the link between early and later siddhantas. Indian scholars had no practice of writing their own names in their works, so, it is very dicult to identify them. Aryabhata is the rst name noticed, in the book Aryabhatiya. After this point most astronomers and astro-writers wrote their names in their works. In this paper I have tried to analyze the works of astronomers like Aryabhata, Varahamihira, Brah- magupta, Bhaskara I, Vateswara, Sripati and Bhaskaracharya in a modern context and to obtain an account of Indian astronomical knowledge. Aryabhata is the first Indian astronomer who stated that the rising and setting of the Sun, the Moon and other heavenly bodies was due to the relative motion of the Earth caused by the rotation of the Earth about its own axis. He also estabished the `yuga' theory (one Mahayuga = 432000 years). Varahamihira com- piled panchasiddhantika and wrote Brihatsamhita. Brahmagupta is the most distinguished astronomer known to us. His two major works are i) Brahmasphutasiddhanta and ii) Khandkhadaka. Bhaskara I was the follower of Aryabhata. His three known works are Mahabhaskariya, Laghubhaskariya and Aryab- hatiyabhasya. Vateswara follows Aryapaksha and Saurapaksha. His master work is Vateswarasiddhanta. Sripati, in his siddhantasekhara, gives the rules for determining the Moon's second inequality. Bhaskara II wrote the most comprehensive astronomical work in Indian astronomy. The result of these works is the account of the Indian astronomical heritage. These works are written in the Sanskrit language. A very few of these manuscripts have been translated in English but many are yet to be done. So, it is necessary to translate these astronomical texts into English with proper commentary for modern scholars. This paper will be helpful in this work.

KaVA (KVN and VERA Array) is a new combined VLBI array composed of KVN (Korean VLBI Network) and VERA (VLBI Exploration of Radio Astrometry). Here, we report the following two issues. (1) We review the initial results of imaging observations of M87 at 23 GHz following Niinuma et al. (2014). The KaVA images reveal extended out ows including complex substructures such as knots and limb-brightening, in agreement with previous VLBI observations. KaVA achieves a high dynamic range of ~1000, more than three times better than that achieved by VERA alone. (2) Based on subsequent observations and discussions led by the KaVA AGN SubWorking Group, we set monitoring observations of Sgr A* and M87 as our Key Science Project (hereafter KSP) because of the closeness and largeness of their central super-massive black holes. The main science goals of the KSP are (i) testing the magnetically- driven-jet paradigm by mapping velocity fields of the M87 jet, and (ii) obtaining tight constraints on physical properties of the radio emitting region in Sgr A*. Towards KSP, we show the first preliminary images of M87 at 23 GHz and Sgr A* at 43 GHz with the bandwidth of 256 MHz.

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 presents a study of interactions between galaxies in the low-redshift group known as the NGC 4065 group. Imaging data were taken using the 2.4 meter telescope at the Thai National Observatory (TNO) for B, V and Rc broadband filters and [S ii] and Red-continuum narrowband filters. There are 21 galaxies in our sample. The results show that most early type galaxies (ETGs) with equivalent width EW(Hα) < 10 Å are gas-deficient galaxies, while late type galaxies (LTGs) show more EW(Hα) and are bluer than the ETGs. This means that star formation activity in the LTGs could be triggered by tidal interactions between galaxy members due to dense environmental effects in the compact group.

SnS-TiO2 nanocomposites are synthesized using simple, cheap, and less toxic SnCl2 as the tin (II) precursor. The prepared nanoparticles are characterized using powder X-ray diffraction (XRD), transmission electron microscopy (TEM), and UV-Vis diffuse reflectance spectra (DRS). The XRD and TEM results indicate that the prepared product has SnS nanoparticles and a grain diameter of 30 nm. The DRS demonstrate that SnS-TiO2 possesses the absorption profile across the entire visible light region. The generation of reactive oxygen species is detected through the oxidation reaction from 1,5-diphenyl carbazide (DPCI) to 1,5-diphenyl carbazone (DPCO). It is found that the photocurrent density and photocatalytic effect increase with the modified SnS. Excellent catalytic degradation of Texbrite BA-L (TBA) solution is observed using the SnS-TiO2 composites under visible light irradiation. It is proposed that both the strong visible light absorption and the multiple exciton excitations contribute to the high visible light photocatalytic activity.

In this paper we introduce the Plasma Physics of Active Galactic Nuclei project, which is an ongoing experiment with Korean VLBI Network (KVN) and KVN and VERA Array (KaVA) to study multi- frequency polarimetric properties on parsec scales of active galaxies. The goal of the project is to improve our understanding of fundamental jet physics, especially evolution of the relativistic out ow coupled with the large-scale magnetic field. We selected six radio-loud AGN as our targets. So far we (i) detected resolved emissions regions at 86 and 129 GHz on VLBI scales, (ii) constructed 2D spectral index maps of the out ows, and (iii) found polarizations at 22 and 43 GHz for a few targets. Here we present spectral index distributions of 3C 120 between 22 and 43 GHz and a linear polarization map of BL Lac at 43 GHz obtained with KVN.

1913년부터 2013년까지 한국에서 육성된 콩 172품종의 생 육 및 수량구성형질의 변이를 평가하고 주성분 분석과 군집 분석을 통하여 품종군을 분류하여 콩 육종의 기초자료로 이용 코자 수행하였다. 생육 및 수량구성형질의 변이계수는 각 형 질에 따라 차이가 있었으며, 엽장폭비, 경장, 분지수, 100립중 및 주당종실중은 높았고, 엽면적, 주경절수, 주당협수 및 주당 립수는 중간정도이었으며, 생육시기에 관련된 개화일수, 성숙 일수 및 생육일수는 낮았다. 콩 품종들의 생육 및 수량구성형 질에 대한 주성분 분석을 한 결과, 주성분의 기여율은 제 1주 성분은 34.02%, 제 2주성분은 18.44%, 제 3주성분은 10.67%, 제 4주성분은 9.96%로, 상위 4주성분까지의 고유값이 1이상 이며, 누적기여율이 73.09%로 제 4주성분까지만 가지고도 한 국 콩 품종의 군집분류가 가능하였다. Average linkage cluster 에 의하여 분류된 군집분류에서 평균 거리를 1.1로 하였을 때 5개 군집으로 분류되었고, I군집은 전체 품종의 69.7%가 속해 있는 가장 큰 군집이었고, 다음으로 II군집이 19.8%가 속하는 큰 군집이었고, 그 다음으로 IV군집이 8.7%가 속하였으며, III 군집과 V군집은 1 ~ 2품종이 속하는 소군집이었다. 각 군집의 품종을 육성년대(1980년 이전, 1980년대, 1990년대, 2000년 이후) 및 용도별(장류 및 두부용, 나물용, 밥밑용, 풋콩 및 올 콩용)로 분류하면 품종의 분포가 차이가 있었다. 육성년대별로 는 1980년 이전과 1980년대에 육성된 품종은 I과 II군집에, 1990년대와 2000년 이후에 육성된 품종은 모든 군집에 넓게 분포하였다. 용도별로는 I군집에는 장류 및 두부용 품종이, II 군집에는 나물용 품종이, IV군집에는 풋콩 및 올콩용 품종이 가장 많이 속하였으며, III과 V군집에 속하는 품종은 나물용 품종이었다.

섬진강의 본류와 지류를 대상으로 2010년 5월부터 2013년 9월까지 어류상을 연구한 결과, 총 13목 41과 81속 107종 37,751개체가 확인되었다. 출현어류 중에서 1차 담수어류는 57종 (53.3%), 2차 담수어류는 10종 (9.3%), 해산어류는 40종 (37.4%)으로 확인되었다. 전체 우점종은 피라미 Zacco platypus (28.7%), 아우점종은 참갈겨니 Z. koreanus (15.0%)로 나타났다. 한국 고유종은 전체 21종 (31.3%)이 출현하였으며 보성강 수계에서 19종으로 다양하게 확인되었다. 환경부지정 멸종위기 야생동물 I급인 임실납자루 Acheilognathus somjinensis, II급인 다묵장어 Lampetra reissneri와 모래주사 Microphysogobio koreensis 등 3종이었다. 외래종은 모두 3종으로 떡붕어 Carassius cuvieri, 블루길 Lepomis macrochirus 및 베스 Micropterus salmoides였다. 얼록동사리 Odontobutis interrupta는 섬진강 수계에 이입되어 서식하는 것으로 추정되었다.

This study examined whether learning context and language aptitude affected the use of pronunciation learning strategies and pronunciation proficiency. One hundred thirty-eight Chinese learners (88 KFL Ss & 50 KSL Ss) learners were investigated for the correlation between learning context(KSL, KFL), language aptitude (high/low), pronunciation learning strategy and pronunciation proficiency. Participants' sound discrimination ability was measured by PLAB and then they were divided into high group (upper 30%) and low group (lower 30%) by scores. SPLS and personal information survey were also conducted. The results showed that (i) a significant difference was found in pronunciation proficiency pursuant to learning context and language aptitude, (ii) use of pronunciation learning strategy differed significantly pursuant to learning context and language aptitude, and (ⅲ) use of pronunciation learning strategy could predict pronunciation proficiency. The findings suggest that effective pronunciation learning strategy should be investigated and taught in L2 Korean classroom.

One of the long-standing problems in modern astronomy is the curious division of globular clusters (GCs) into two groups, according to the mean period (hPabi) of type ab RR Lyrae variables. In light of the recent discovery of multiple populations in GCs, we suggest a new model explaining the origin of the Sandage period-shift and the difference in mean period of type ab RR Lyrae variables between the two Oosterhoff groups. In our models, the instability strip in the metal-poor group II clusters, such as M15, is populated by second generation stars (G2) with enhanced helium and CNO abundances, while the RR Lyraes in the relatively metal-rich group I clusters like M3 are mostly produced by first generation stars (G1) without these enhancements. This population shift within the instability strip with metallicity can create the observed period-shift between the two groups, since both helium and CNO abundances play a role in increasing the period of RR Lyrae variables. The presence of more metal-rich clusters having Oosterhoff-intermediate characteristics, such as NGC 1851, as well as of most metal-rich clusters having RR Lyraes with the longest periods (group III) can also be reproduced, as more helium-rich third and later generations of stars (G3) penetrate into the instability strip with further increase in metallicity. Therefore, although there are systems where the suggested population shift cannot be a viable explanation, for the most general cases, our models predict that RR Lyraes are produced mostly by G1, G2, and G3, respectively, for the Oosterhoff groups I, II, and III.

Recent narrow-band Ca photometry discovered two distinct red giant branch (RGB) populations in some massive globular clusters (GCs) including M22, NGC 1851, and NGC 288. In order to investigate the dierences in light/heavy elements abundances between the two subpopulations, we have performed low-resolution spectroscopy for stars on the two RGBs in these GCs. We find a significant difference (more than 4) in calcium abundance from the spectroscopic HK0 index for both M22 and NGC 1851. We also find a more than 8 difference in CN band strength between the Ca-strong and Ca-weak subpopulations. For NGC 288, however, we detect the presence of a large difference only in the CN strength. The calcium abundances of the two subpopulations in this GC are identical within errors. We also find interesting differences in CN-CH relations among these GCs. While CN and CH indices are correlated in M22, they show an anti-correlation in NGC 288. However, NGC 1851 shows no dierence in CH between two groups of stars having different CN strengths. The CN bimodality in these GCs could be explained by pollution from intermediate-mass asymptotic giant branch stars and/or fast-rotating massive stars. For the presence or absence of calcium bimodality and the differences in CN-CH relations, we suggest these would be best explained by how strongly type II supernovae enrichment has contributed to the chemical evolutions of these GCs.

Low resolution spectra of Nova Delphini 2013 (V339 Del) in the optical range have been obtained at Bosscha Observatory, Indonesia during its maximum light (V = 4.3). Spectra were observed from August 16 to 27, 2013. The GAO-ITB RTS 20.3 cm telescope, and SBIG DSS-7 spectrograph and SBIG ST-7 XE as the detector have been employed throughout the observations. The spectra show P-Cygni profiles in Balmer, NaI`D' and Fe II lines, from which we determined shell expansion velocities of 1421.6639.18 km/s, 1227.5421.57 km/s and 1402.86 km/s, respectively. Our spectroscopic observations followed the spectral evolution of V339 Del from the pre-maximum phase to early Orion phase. The characteristics of the nova Delphini 2013 resembles those of Fe II-type novae.

식품안전보건지표는 그 활용성이 높아 국외에서는 종합적인 환경보건지표 내 세부영역에서 개발되어 활용되고 있으나, 국내의 경우 환경보건지표와 독자적으로 개발되어 도입단계에 있다. 본 연구에서는 기 개발된 식품안전 보건지표를 활용할 수 있는 방안을 사례연구의 형태로 제시하였다. 본 연구에서 선정하여 제시한 활용방안으로는 지수화를 통한 통합식품안전보건지수 산출, 통합식품안전 보건지수와 이를 구성하는 식품안전보건지표간의 상관성평가, 통합식품안전보건지수와 사회경제적 지위와의 상관성평가가 있다. 지역 내에서 식품안전보건상태의 변화를 나타내는 통합식품안전보건지수I과 해당 년도의 지역별 식품안전보건수준을 나타내는 통합식품안전보건지수II가 산출되었다. 통합식품안전보건지수I은 Campylobacter jejuni, Bacillus cereus, 살모넬라, 원인미상으로 인한 식품매개질환 발생건수, 식품매개 법정감염병 발생률 중 장출혈성 대장균 발생률와 통계적으로 유의한 상관관계가 있었다. 통합식품안전보건지수II는 외국인 비율과 여성 비율이 증가할수록 통계적으로 유의하게 감소하였고, 인구밀도가 증가할 수록 통계적으로 유의하게 증가하였다. 제시된 활용방안을 통해 전반적인 국내 식품안전보건상태와 지역별연도별 식품안전보건상태의 변화원인을 파악할 수 있으며, 식품안전과 관련이 있을 것으로 예상되는 기타 요인과의 연관성을 분석하여 추가적인 추론을 할 수 있다. 이 외에도 식품안전보건지표는 다양한 방면으로 활용이 가능하고, 정책적 기준 설정 및 방향성 제시의 근거자료로도 활용할 수 있으므로 향후 더욱 활발한 연구와 지속적인 관심이 필요하다.

We have carried out integral field unit (IFU) spectroscopy of Hα, [N ii] and [Oiii] emission lines for a sample of Galactic planetary nebulae (PNe) with Wolf-Rayet (WR) stars and weak emission-line stars (wels). Comparing their spatially-resolved kinematic observations with morpho-kinematic models allowed us to disentangle their three-dimensional gaseous structures. Our results indicate that these PNe have axisymmetric morphologies, either bipolar or elliptical. In many cases the associated kinematic maps for the PNe around hot central stars also reveal the presence of so-called fast low-ionization emission regions.

In order to understand the relationship between the distribution of epilithic diatoms and the habitual environments, land-use, water qualities, and epilithic diatoms were studied at 141 sampling sites in the midwestern stream of Korean peninsula (Geum river, Mangyeong river, Dongjin river, and Sapgyo river). The total 183 diatom taxa was appeared in the study, while the dominant species were found to be Nitzschia palea (10.9%) and Achnanthes convergens (8.4%). Based on the abundance of epilithic diatoms, a cluster analysis results indicate that the sampling sites divided the sampling sites into 4 groups (G) at the 25% level. In term of geographic and aquatic environments, G-I and -II accounted for the upper and mid streams of the Geum river, and had large forest areas and good in water quality. G-III accounted for farmland and urban, and high concentration nutrient levels (TN and TP) and electric conductivity. G-IV accounted for mostly farmland, and high levels in turbidity, BOD, nutrient and electric conductivity. CCA results showed that the saproxenous taxa Meridion circulare was the indicator species of G-I, which strongly influenced by altitude and forests. In G-II, the indifferent taxa Navicula cryptocephala was influenced by Chl-a, AFDM, and DO. In G-III and -IV, the indifferent taxa Fragilaria elliptica and saprophilous taxa Aulacoseira ambigua were influenced by electric conductivity, turbidity, and nutrient counts. Meanwhile, random forest results showed that the predicting factor of indicator species appearance in G-I, -II, and -III was found to be electric conductivity whereas in G-IV it was found to be turbidity. Collectively, the distribution of diatoms in the midwestern of Korean peninsula was found to depend more on the land-use and its subsequent water qualities than the inherent characteristics of the aquatic environment.

Young Galactic supernova remnants (SNRs) are where we can observe closely supernova (SN) ejecta and their interaction with the circumstellar/interstellar medium. They also provide an opportunity to explore the explosion and the final stage of the evolution of massive stars. Near-infrared (NIR) emission lines in SNRs mostly originate from shocked dense material. In shocked SN ejecta, forbidden lines from heavy ions are prominent, while in shocked circumstellar/interstellar medium, [Fe II] and H2 lines are prominent. [Fe II] lines are strong in both media, and therefore [Fe II] line images provide a good starting point for the NIR study of SNRs. There are about twenty SNRs detected in [Fe II] lines, some of which have been studied in NIR spectroscopy. We will review the NIR [Fe II] observations of SNRs and introduce our recent NIR spectroscopic study of the young core-collapse SNR Cas A where we detected strong [P II] lines.