• Journal of the Korea Academia-Industrial cooperation Society
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• v.15 no.4
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• pp.1844-1849
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• 2014

Existing measurement methods using microscopes or surface roughness measurement instruments for surface control in manufacturing die are low in their efficiency when they are applied in industrial fields due to structural problems. Therefore, it is very important to develop a measurement and analysis system which can enhance efficiency in the measurement of different-sized manufacturing dies and provide quality control regardless of location. This study aimed at the development of a portable surface measurement system to satisfy this need. This measurement system was designed and manufactured in such a way as to divide it into three parts: the Base, the Body, and the Optical system. As a result of testing the system, the surface roughness was measured with an accuracy between 94.9 and 99.9%, and the deviation in the measurement value of a circle was within $2{\mu}m$.

• Journal of The Korean Astronomical Society
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• v.53 no.4
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• pp.87-98
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• 2020

The Korea Astronomy and Space Science Institute (KASI) has been developing a next-generation coronagraph (NGC) in cooperation with NASA to measure the coronal electron density, temperature, and speed simultaneously, using four different optical filters around 400 nm. KASI organized an expedition to demonstrate the coronagraph measurement scheme and the instrumental technology during the 2017 total solar eclipse (TSE) across the USA. The observation site was in Jackson Hole, Wyoming, USA. We built an eclipse observation system, the Diagnostic Coronal Experiment (DICE), composed of two identical telescopes to improve the signal-to-noise ratio. The observation was conducted at four wavelengths and three linear polarization directions in the limited total eclipse time of about 140 seconds. We successfully obtained polarization data for the corona but we were not able to obtain information on the coronal electron temperature and speed due to the low signal-to-noise ratio of the optical system and strong emission from prominences located at the western limb. In this study, we report the development of DICE and the observation results from the eclipse expedition. TSE observation and analysis with our self-developed instrument showed that a coronagraph needs to be designed carefully to achieve its scientific purpose. We gained valuable experience for future follow-up NASA-KASI joint missions: the Balloon-borne Investigation of the Temperature and Speed of Electrons in the Corona (BITSE) and the COronal Diagnostic EXperiment (CODEX).

• Asian Journal of Atmospheric Environment
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• v.10 no.1
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• pp.13-21
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• 2016

The vertical distributions of aerosol extinction coefficient were estimated using the scaling height retrieved at Gwangju, Korea ($35.23^{\circ}N$, $126.84^{\circ}E$) during a spring season (March to May) of 2009. The aerosol scaling heights were calculated on a basis of the aerosol optical depth (AOD) and the surface visibilities. During the observation period, the scaling heights varied between 3.55 km and 0.39 km. The retrieved vertical profiles of extinction coefficient from these scaling heights were compared with extinction profile derived from the Light Detection and Ranging (LIDAR) observation. The retrieve vertical profiles of aerosol extinction coefficient were categorized into three classes according to the values of AODs and the surface visibilities: (Case I) the AODs and the surface visibilities are measured as both high, (Case II) the AODs and the surface visibilities are both lower, and (Others) the others. The averaged scaling heights for the three cases were $3.09{\pm}0.46km$, $0.82{\pm}0.27km$, and $1.46{\pm}0.57km$, respectively. For Case I, differences between the vertical profile retrieved from the scaling height and the LIDAR observation was highest. Because aerosols in Case I are considered as dust-dominant, uplifted dust above planetary boundary layer (PBL) was influenced this discrepancy. However, for the Case II and other cases, the modelled vertical aerosol extinction profiles from the scaling heights are in good agreement with the results from the LIDAR observation. Although limitation in the current modelling of vertical structure of aerosols exists for aerosol layers above PBL, the results are promising to assess aerosol profile without high-cost instruments.

• Journal of the Korean Society of Costume
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• v.38
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• pp.51-72
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• 1998

Futurists objected the existent style, that is the conventional fashion, and took part in these disciplines of fashion to make clothes the instruments being able to represent the individuality. Giacomo Balla and fortunato Depero, pain-ters who in 1915 were to work with Diaghilev's company, were the first to see clothing as a dynamic interfaced between th body and the atmosphere, between physical gestures and the urban context, which could be translated into encounters between forms and colours, volumes and architecture. For them, clothing began to exist as an object and an event, something to be removed from a mainly static conception and made mobile, active. The interaction between movement and clothing was based on the relativity of perception : the appearance and disappearance of the body produced points without dimension or duration which served, as Balla wrote in the Futurist Mnaifesto of Men's Clothing to“renew incessantly the enjoyment and impetuous movement of the body”. The historical achievement in the effort for the reformation of Futurist, Art to Wear. First, for Futurist, clothing is removed from a static conception and focused on dynamics. Second, Balla used asymmetry in men's clothing. Moreover he supposed dynamic men's clothes by using optical intersection. Third, the after image of Chronophotograph represented rapidity. This rhythmic expression is the fore-runner in Optical and Kinetic Art of Visual Art. Fourth, Futurist emphasized flexibility in fashion. They aimed to create‘Clothing Machines’whose parts would interact to aceelerate the real and virtual, inner and outer movement of the human being. Fifth, the variety and short life of cutting skills and colors are focused and‘Fast Substance’in fashion is admitted by Futurists. Futurist concern with clothing was not lim-ited its appearance in terms of cut and colour. What important was also the way it appeared and disappeared according to fashion. It was a“fast substance”, able to reflect rapid, sudden changes of social and aesthetic taste. To reach to the aim of internationalization, Gesamtkunstwerk in our Art to Wear, it is extremely meaningful to examine art fashion which is created under the conception of Gesamtkunstwerk production of avang garde artist in the early 20th century and look at formative conscious of truth, goodess and beauty synthetically which they faced on their works of art.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.39.2-39.2
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• 2010

In this paper, I present the domestic development of near infrared camera systems for the ground telescope and the space satellite. These systems are the first infrared instruments made for astronomical observation in Korea. KASINICS (KASI Near Infrared Camera System) was developed to be installed on the 1.8m telescope of the Bohyunsan Optical Astronomy Observatory (BOAO) in Korea. KASINICS is equipped with a $512{\times}512$ InSb array enable L band observations as well as J, H, and Ks bands. The field-of-view of the array is $3.3'{\times}3.3'$ with a resolution of 0.39"/pixel. It employs an Offner relay optical system providing a cold stop to eliminate thermal background emission from the telescope structures. From the test observation, limiting magnitudes are J=17.6, H=17.5, Ks=16.1 and L(narrow)=10.0 mag at a signal-to-noise ratio of 10 in an integration time of 100 s. MIRIS (Multi-purpose InfraRed Imaging System) is the main payload of the STSAT-3 in Korea. MIRIS Space Observation Camera (SOC) covers the observation wavelength from $0.9{\mu}m$ to $2.0{\mu}m$ with a wide field of view $3.67^{\circ}{\times}3.67^{\circ}$. The PICNIC HgCdTe detector in a cold box is cooled down below 100K by a micro Stirling cooler of which cooling capacity is 220mW at 77K. MIRIS SOC adopts passive cooling technique to chill the telescope below 200K by pointing to the deep space (3K). The cooling mechanism employs a radiator, a Winston cone baffle, a thermal shield, MLI of 30 layers, and GFRP pipe support in the system. Opto-mechanical analysis was made in order to estimate and compensate possible stresses from the thermal contraction of mounting parts at cryogenic temperatures. Finite Element Analysis (FEA) of mechanical structure was also conducted to ensure safety and stability in launching environments and in orbit. MIRIS SOC will mainly perform the Galactic plane survey with narrow band filters (Pa $\alpha$ and Pa $\alpha$ continuum) and CIB (Cosmic Infrared Background) observation with wide band filters (I and H) driven by a cryogenic stepping motor.

• Journal of KIISE:Computing Practices and Letters
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• v.8 no.6
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• pp.669-678
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• 2002

Currently, the domestic interests on the development of eyesight related measuring instruments are being increased. So we are developing such an electronic system of Refracto-keratometer, which contains a software and a hardware both. If this system could inform the examiner of the precise eyesight measuring result from the treatment of the image of optical system, then potentially the number of missed measuring results could be reduced. Our electronic system has been developed from the two areas divided into a software and a hardware. The software area was focused on the more exact eyesight measuring results, using morphological filtering methods and gray-leveled signal enhancing techniques. The hardware area is performing the same functions as the existing other systems. Besides, it provides the embedded software with free variables which could reduce the developing duration sharply as well as enlarge many kinds of application-extensions. Therefore, this electronic system has made effective eyesight measurement possible as the result of reducing the differences applied to sophisticated eyesight measurement.

• Asia-Pacific Journal of Business
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• v.8 no.2
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• pp.57-73
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• 2017

In this paper RCA and TSI has been analyzed based on Korean and Chinese lists of export (HS 6 units) and list of companies and products with competitive advantage has been deduced. The results of RCA and TSI analysis are as follows. From the list of 20 most exported items from Korea to China the RCA index for eleven of them (based on common items from 2011-2015) is bigger than 1, thus showing comparative advantage. As for the TSI index, all of the items has shown (+) value, and has been analyzed as specialization in export. In other words, companies in the fields of mineral fuel; mineral oil; organic chemicals; electrical equipment and parts; as well as optical, precision and medical instrument are industries with competitive advantage. From the list of 20 most exported items from China to Korea the RCA index for twelve of them (based on common items form 2011-2015) is bigger than 1, thus also showing comparative advantage, and the TSI index has also shown (+) value for all of the specified items, meaning specialization in export. Industries of mineral fuel; mineral oil; iron and steel, articles of iron and steel; machinery and mechanical parts, electrical equipment and parts; as well as optical, precision and medical instruments have shown competitive advantage.

• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.208.1-208.1
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• 2012

The Ultra Fast Flash Observatory (UFFO) pathfinder is a payload system on-board the Russian satellite Lomonosov, scheduled to be launched in 2013. The main purpose of the UFFO pathfinder is to observe the early photons from Gamma-Ray Bursts. It consists of two instruments. The first instrument is the UFFO Burst Alert X-ray Trigger telescope (UBAT) for the fast-trigger and detection of GRB location, and the second is the Slewing Mirror Telescope (SMT) for the observation of the UV/optical afterglow from the GRB located by the UBAT. It will provide the first-ever systematic study of UV/optical emission far earlier than 1 sec after trigger. We will present the design, fabrication and the preliminary performance of the UBAT.

• Korean Journal of Optics and Photonics
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• v.28 no.5
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• pp.187-193
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• 2017

The purpose of this study was to investigate some implications for optics education and improvement of the Examination for Appointing Secondary School Physics Teachers (EASSPT), by analyzing the problems in EASSPT. For these purpose, we analyzed 38 optics problems of the EASSPT from the 16 school years of 2002 to 2017. The results of the analysis are as follows: First, optics problems were presented in 10.8% of the physics subject area, which was least frequently. Second, many problems have addressed specific areas such as Snell's law, image of a single lens, or interference. Few problems were found in many other evaluation areas, including optical instruments and aberrations. Third, compared to other areas, optics problems were presented as relatively easy questions, and the problems were presented in more laboratory contexts than daily-life contexts. In addition, we have discussed implications for EASSPT and in-service physics-teacher training.

• The Bulletin of The Korean Astronomical Society
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• v.46 no.1
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• pp.45.2-46
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• 2021

The Hayabusa 2 mission target asteroid (162173) Ryugu is a near-Earth, carbonaceous (C-type) asteroid. Before the arrival, this asteroid is expected to be covered with mm- to cm- sized grains through the thermal infrared observations [1]. These grains are widely understood to be formed by past impacts with other celestial bodies and fractures induced by thermal fatigue [2]. However, the close-up images by the MASCOT lander showed lumpy boulders but no abundant fine grains [3]. Morota et al. suggested that there would be submillimeter particles on the top of these boulders but not resolved by Hayabusa 2's onboard instruments [4]. Hence, we conducted polarimetry of Ryugu to investigate microscopic grain sizes on its surface. Polarimetry is a powerful tool to estimate physical properties such as albedo and grain size. Especially, it is known that the maximum polarization degree (Pmax) and the geometric albedo (pV) show an empirical relationship depending on surface grain sizes [5]. We observed Ryugu from UT 2020 November 30 to December 10 at large phase angles (ranging from 78.5 to 89.7 degrees) to derive Pmax. We modified TRIPOL (Triple Range Imager and POLarimeter, [6]) to attach to the 1.8-m telescope at the Bohyunsan Optical Astronomy Observatory (BOAO). With this instrument, we observed the asteroid and determined linear polarization degrees at the Rc-band filter. We obtained sufficient data sets from 7 nights at this observatory to determine the Pmax value, and collaborated with other observatories in Japan (i.e., Hokkaido University, Higashi-Hiroshima, and Nishi-Harima) to acquire linear polarization degrees of the asteroid from total 24 nights observations with large phase angle coverage (From 28 to 104 degrees). The observational results have been published in Kuroda et al. (2021) [7]. We thus found the dominance of submillimeter particles on the surface of Ryugu from the comparison with other meteorite samples from the campaign observation. In this presentation, we report our activity to modify the TRIPOL for the 1.8-m telescope and the polarimetric performance. We also examine the rotational variability of the polarization degree using the TRIPOL data.