Academic Development of International Commerce and its Policy Contribution

국제통상 전공은 국제대학원의 설립과 함께 도입된 신설 학제이나 지난 20년간 괄목할 만한 성장을 하였고 현재 사회과학 분야에서 독자적인 학문 분야로 성장하고 있다. 정책 및 실무적 활용성이 높은 분야에 대한 이론 연구가 융합된 다학제적 특성을 가지는 국제통상 전공의 발전에는 우루과이 라운드 협상과정을 거치는 시기 양성된 실무적 식견과 경험이 겸비된 경제학자들이 지대한 역할을 하였다. 국제통상 전공의 핵심 공통학사과정을 수립하고, 심도있는 다학제적 연구교류의 장을 발전시키고, 전공자들에 대한 사회적 수요 및 국제무대 진출 기회를 확대함으로써 향후 전공의보다 본격적인 성장을 이루어야 할 것이다.International Commerce as an academic major was introduced primarily when the Graduate School of International Studies was first established twenty years ago and has evolved as an independent subject area of social science at least in Korea. For this remarkable development, uniquely nurtured experts with both academic understanding and practical experiences in trade policy areas—especially honed through the Uruguay Round negotiation—have played significant roles in promoting interdisciplinary curriculum contents with high policy applicability. Future tasks for further development of International Commerce include deliberating on its core curriculum, building a more comprehensive academic forum to incorporate interdisciplinary scholars, and fostering career development opportunities both abroad and at home.본 논문의 집필에 도움을 준 연구재단 SSK사업(NRF 2014S1A3A2043505) 및 서울대 아시아연구소(SNUAC-2016-008)의 연구지원에 감사한다

The eighth data release of the sloan digital sky survey: First data from SDSS-III

The Sloan Digital Sky Survey (SDSS) started a new phase in 2008 August, with new instrumentation and new surveys focused on Galactic structure and chemical evolution, measurements of the baryon oscillation feature in the clustering of galaxies and the quasar Lyα forest, and a radial velocity search for planets around 8000 stars. This paper describes the first data release of SDSS-III (and the eighth counting from the beginning of the SDSS). The release includes five-band imaging of roughly 5200 deg2 in the southern Galactic cap, bringing the total footprint of the SDSS imaging to 14,555 deg2, or over a third of the Celestial Sphere. All the imaging data have been reprocessed with an improved sky-subtraction algorithm and a final, self-consistent photometric recalibration and flat-field determination. This release also includes all data from the second phase of the Sloan Extension for Galactic Understanding and Exploration (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars at both high and low Galactic latitudes. All the more than half a million stellar spectra obtained with the SDSS spectrograph have been reprocessed through an improved stellar parameter pipeline, which has better determination of metallicity for high-metallicity stars. © 2011. The American Astronomical Society. All rights reserved

Comparison of the Asteroseismic Mass Scale of Red Clump Giants with Photometric Mass Estimates

Asteroseismology can provide joint constraints on masses and radii of individual stars. While this approach has been extensively tested for red giant branch (RGB) stars, it has been more difficult to test for helium core-burning red clump (RC) giants because of the lack of fundamental calibrators. To provide independent mass estimates, we utilize a number of widely used horizontal-branch models in the literature and derive photometric masses from a comparison with griBVI(C)JHK(s) photometry. Our selected models disagree with each other on the predicted mass-luminosity-temperature relation. We adopt first-order corrections on colors and magnitudes to minimize the dispersion between different models by forcing models to match the observed location in the solar-metallicity cluster M67. Even for these calibrated models, however, the internal consistency between models deteriorates at higher metallicities, and photometric masses become smaller than asteroseismic masses, as seen from metal-rich field RC stars with Gaia parallaxes. Similarly, the average photometric mass for metal-rich NGC. 6791 stars ranges from 0.7 to 1.1 M-circle dot, depending on the specific set of models employed. An ensemble average of the photometric masses (0.88 +/- 0.16 M-circle dot) in NGC 6791 is marginally consistent with the asteroseismic mass (1.16 +/- 0.04 M-circle dot). There is a clear tension between the masses that one would predict from photometry for metal-rich field RC stars, asteroseismic masses, and those that would be expected from the ages of stars in the Galactic disk populations and canonical RGB mass loss. We conclude that standard RC models need to be reexamined in light of these powerful new data sets

THE FRACTIONS OF INNER- AND OUTER-HALO STARS IN THE LOCAL VOLUME

We obtain a new determination of the metallicity distribution function (MDF) of stars within similar to 5-10 kpc of the Sun, based on recently improved co-adds of ugriz photometry for Stripe. 82 from the Sloan Digital Sky Survey. Our new estimate uses the methodology developed previously by An et al. to study in situ halo stars, but is based on a factor of two larger sample than available before, with much-improved photometric errors and zero-points. The newly obtained MDF can be divided into multiple populations of halo stars, with peak metallicities at [Fe/H] approximate to 1.4 and 1.9, which we associate with the inner-halo and outer-halo populations of the Milky Way, respectively. We find that the kinematics of these stars (based on proper-motion measurements at high Galactic latitude) supports the proposed dichotomy of the halo, as stars with retrograde motions in the rest frame of the Galaxy are generally more metal-poor than stars with prograde motions, consistent with previous claims. In addition, we generate mock catalogs of stars from a simulated Milk Way halo system, and demonstrate for the first time that the chemically and kinematically distinct properties of the inner-and outer-halo populations are qualitatively in agreement with our observations. The decomposition of the observed MDF and our comparison with the mock catalog results suggest that the outer-halo population contributes on the order of similar to 35%-55% of halo stars in the local volume

Massive young stellar objects in the Galactic center. I. Spectroscopic identification from Spitzer infrared spectrograph observations

We present results from our spectroscopic study, using the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope, designed to identify massive young stellar objects (YSOs) in the Galactic center (GC). Our sample of 107 YSO candidates was selected based on Infrared Array Camera (IRAC) colors from the high spatial resolution, high sensitivity Spitzer/IRAC images in the Central Molecular Zone, which spans the central ∼300pc region of the Milky Way. We obtained IRS spectra over 5-35 μm using both high- and low-resolution IRS modules. We spectroscopically identify massive YSOs by the presence of a 15.4 μm shoulder on the absorption profile of 15 μm CO 2 ice, suggestive of CO 2 ice mixed with CH 3OH ice on grains. This 15.4 μm shoulder is clearly observed in 16 sources and possibly observed in an additional 19 sources. We show that nine massive YSOs also reveal molecular gas-phase absorption from CO 2, C 2H 2, and/or HCN, which traces warm and dense gas in YSOs. Our results provide the first spectroscopic census of the massive YSO population in the GC. We fit YSO models to the observed spectral energy distributions and find YSO masses of 8-23 M ⊙, which generally agree with the masses derived from observed radio continuum emission. We find that about 50% of photometrically identified YSOs are confirmed with our spectroscopic study. This implies a preliminary star formation rate of ∼0.07 M ⊙ yr -1 at the GC. © 2011. The American Astronomical Society. All rights reserved

The Photometric Metallicity and Carbon Distributions of the Milky Way's Halo and Solar Neighborhood from S-PLUS Observations of SDSS Stripe 82

We report photometric estimates of effective temperature, T (eff), metallicity, [Fe/H], carbonicity, [C/Fe], and absolute carbon abundances, A(C), for over 700,000 stars from the Southern Photometric Local Universe Survey (S-PLUS) Data Release 2, covering a substantial fraction of the equatorial Sloan Digital Sky Survey Stripe 82. We present an analysis for two stellar populations: (1) halo main-sequence turnoff stars and (2) K-dwarf stars of mass 0.58 < M/M (circle dot) < 0.75 in the Solar Neighborhood. Application of the Stellar Photometric Index Network Explorer (SPHINX) to the mixed-bandwidth (narrow- plus wide-band) filter photometry from S-PLUS produces robust estimates of the metallicities and carbon abundances in stellar atmospheres over a wide range of temperatures, 4250 < T (eff)(K) < 7000. The use of multiple narrow-band S-PLUS filters enables SPHINX to achieve substantially lower levels of "catastrophic failures" (i.e., large offsets in metallicity estimates relative to spectroscopic determinations) than previous efforts using a single metallicity-sensitive narrow-band filter. We constrain the exponential slope of the Milky Way's K-dwarf halo metallicity distribution function (MDF), lambda (10,[Fe/H]) = 0.85 +/- 0.21, over the metallicity range -2.5 < [Fe/H] < -1.0; the MDF of our local-volume K-dwarf sample is well-represented by a gamma distribution with parameters alpha = 2.8 and beta = 4.2. S-PLUS photometry obtains absolute carbon abundances with a precision of similar to 0.35 dex for stars with T (eff) < 6500 K. We identify 364 candidate carbon-enhanced metal-poor stars, obtain assignments of these stars into the Yoon-Beers morphological groups in the A(C)-[Fe/H] space, and we derive the CEMP frequencies

Erratum: The eighth data release of the sloan digital sky survey: First data from SDSS-III (The Astrophysical Journal Supplement Series (2011) 193 (29))

[No abstract available

A Study on Internal Trade between South/North Korea in the WTO System and Gaesung Industrial Complex

남북한 간 교역은 수많은 정치외교적인 난제에도 불구하고 한반도의 미래를 위해 필수적으로 확대해가야 할 부분이며, 실제로 우리 정부는 개성공단 등을 통해 지속적으로 경제협력 관계를 심화해왔다. 그러나 세계무역기구체제(WTO)를 통해 국제통상규범이 강화되면서 남북한 간의 교역이 우리 경제의 내부 문제로만 간주될 수 없는 상황이며, 한국뿐만 아니라 남북한의 대외교역에 중요한 쟁점들을 제기하고 있다. 그러한 남북한 교역을 WTO체제에서 제도적으로 보호하기 위해서 우선적으로 추진되어야 하는 사안은 남북한 FTA다. 남북한 FTA는 장기적으로 남북한 교류를 활성화하는 제도적 틀을 구축하는 기능도 있으나, 단기적으로는 점진적으로 확대되는 남북한 교역을 WTO협정상 비차별원칙 의무로부터 보호하고 북한의 경제체제 정비를 위한 중요한 계기가 될 것으로 판단된다. 또한 최근 FTA를 통해 구축해 둔 개성공단의 원산지특례조항도 개선의 여지가 있는데, 개성공단 투입재 비율을 제고하거나 생산 주체, 또는 공정의 중요도 등으로 역외가공 원산지를 인정하는 방식, 그리고 품목 군을 제한하는 경우에도 개성공단의 생산구조를 반영하여 필요한 경우 양허품목을 재조정하는 방식이 검토될 수 있다. In spite of numerous political and diplomatic dilemma, internal trade between South and North Korea must be continued and expanded. The Government of Korea, in fact, has enhanced the economic cooperation with the North through Gaesung Industrial Complex. Under the regulations of the WTO system, however, the issues in internal trade could no longer be a sole problem of the two Koreas, but often cause controversies, particularly related to non-discriminatory treatment measure. In order to justify the internal trade and the special treatments between the two under the WTO regime, the FTA between the two Koreas could be a key step to push forward. The FTA between the South and North, in long-term, could vitalize the mutual exchanges, yet in short-term, could also motivate the changes in North Korean economic system and make the existing privilege legitimate. On the same token, the special provisions regarding the rules of origin of the products manufactured in Gaesung Industrial Complex in the recent FTAs of South Korea still need some revisions and improvements. It is significant to further negotiate to raise the rate of non-originating content, or recognize the origin based upon the identity of the principal manufacturer or the importance of processing. When the Agreement restricts the types of items, it is required to readjust and expand the types, reflecting the latest structure of production in Gaesung Industrial Complex

Formation and evolution of the disk system of the milky way: [α/Fe] ratios and kinematics of the segue G-dwarf sample

We employ measurements of the [α/Fe] ratio derived from low-resolution (R 2000) spectra of 17,277 G-type dwarfs from the SEGUE survey to separate them into likely thin- and thick-disk subsamples. Both subsamples exhibit strong gradients of orbital rotational velocity with metallicity, of opposite signs, -20 to -30kms-1dex-1 for the thin-disk and +40 to +50kms-1dex-1 for the thick-disk population. The rotational velocity is uncorrelated with Galactocentric distance for the thin-disk subsample and exhibits a small trend for the thick-disk subsample. The rotational velocity decreases with distance from the plane for both disk components, with similar slopes (-9.0 1.0kms-1kpc-1). Thick-disk stars exhibit a strong trend of orbital eccentricity with metallicity (about -0.2 dex-1), while the eccentricity does not change with metallicity for the thin-disk subsample. The eccentricity is almost independent of Galactocentric radius for the thin-disk population, while a marginal gradient of the eccentricity with radius exists for the thick-disk population. Both subsamples possess similar positive gradients of eccentricity with distance from the Galactic plane. The shapes of the eccentricity distributions for the thin- and thick-disk populations are independent of distance from the plane, and include no significant numbers of stars with eccentricity above 0.6. Among several contemporary models of disk evolution that we consider, radial migration appears to have played an important role in the evolution of the thin-disk population, but possibly less so for the thick disk, relative to the gas-rich merger or disk heating scenarios. We emphasize that more physically realistic models and simulations need to be constructed in order to carry out the detailed quantitative comparisons that our new data enable. © 2011. The American Astronomical Society. All rights reserved

Signatures of minor mergers in the Milky Way disc - I. The SEGUE stellar sample

It is now known that minor mergers are capable of creating structure in the phase-space distribution of their host galaxy's disc. In order to search for such imprints in the Milky Way, we analyse the Sloan Extension for Galactic Understanding and Exploration (SEGUE) F/G dwarf and the Schuster et al. stellar samples. We find similar features in these two completely independent stellar samples, consistent with the predictions of a Milky Way minor-merger event. We next apply the same analyses to high-resolution, idealized N-body simulations of the interaction between the Sagittarius dwarf galaxy and the Milky Way. The energy distributions of stellar particle samples in small spatial regions in the host disc reveal strong variations of structure with position. We find good matches to the observations for models with a mass of Sagittarius' dark matter halo progenitor 10 11M ⊙. Thus, we show that this kind of analysis could be used to provide unprecedentedly tight constraints on Sagittarius' orbital parameters, as well as place a lower limit on its mass. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS