In order to attract students to the radio universe, we have constructed a three-element radio interferometer in the National Youth Space Center, Goheung, Korea. It consists of three 1.8 m off-axis parabola antennas with driving systems, sideband separation receivers operating in 12 GHz, a narrow band digitizer, and correlation software. We have used as many commercial products as possible to reduce development costs. The maximum separation of 20 m gives an angular resolution of ∼4′, and the shortest baseline of 3.8 m prevents a serious missing flux. Fringes are detected for several radio sources, including the sun and Cas A. After a rough relative calibration, we have derived visibilities for the sun, whose amplitudes are decreasing for longer baselines. We have made a solar image using the visibility amplitudes and closure phases, referring to the 17 GHz image by Nobeyama Radioheliograph. Developing a flexible real-time correlator seems most crucial if this kind of the system is to be used for more rigorous scientific studies.

오늘날까지 적층 마이크로 외팔보의 고유진동수에 대하여 연구가 진행되었다. 마이크로 보는 실리콘 재질로 만들어 지지만, 그것의 상하 표면은 얇은 금 박막층(~30nm)이 증착되어 있다. 초음파 검사를 위해 초음파 테스트 플랫폼을 사용했으며, 시간영역 신호는 광학적으로 측정되었다. 고유진동수는 파형을 고속 Fourier 변환을 통해 정량화하였으며, 결과적으로 고전적인 보 이론과 일치하는 결과를 보여 주었다. 본 연구는 마이크로/나노스케일 재료와 마이크로 구조에 대한 동적평가기법 을 제공할 것으로 기대된다.

마이켈슨 간섭계를 이용하여 25 ℃에서 80 ℃까지 온도를 변화시키며 움직이는 간섭무늬의 개수 를 이용하여 투명매질들의 열광학계수를 측정하였다. 파장이 633 nm인 광원에 대해 BK7 광학유리, fused silica, fused quartz의 열광학계수는 각각 2.245×10-6 /K, 8.226×10-6 /K, 8.621×10-6 /K였고, 이는 문헌값과 비교하여 약 ± 2%의 범위 내에서 일치하였다. 붕규산 크라운 유리인 BK7과 SiO2 계열의 시료의 비교를 통해 온도 증가와 함께 유리의 광경로가 변하는 것은 열팽창계수보다는 굴절률변화의 영향을 더 많이 받 는다는 것을 확인할 수 있었다. 또한 동일한 SiO2 구성이라도 온도 증가에 따라 고온 열처리된 fused quart의 굴절률 변화가 fused silica보다 크다는 결과도 얻었다.

Phase transition in ferroelectric polymer is very interesting behavior and has been widely studiedfor real device applications, such as actuators and sensors. Through the phase transition, there is structuralchange resulting in the change of electrical and optical properties. In this study, we fabricated the Febry-Perotinterferometer with the thin film of ferroelectric P(VDF-TrFE) 50/50mol% copolymer, and thermo-opticalproperties were investigated. The effective thermo-optical coefficient of P(VDF-TrFE) was obtained as 2.3~3.8×10-4/K in the ferroelectric temperature region (45oC~65oC) and 6.0×10-4/K in the phase transition temperatureregion (65oC~85oC), which is a larger than optical silica-fiber and PMMA. The resonance transmission peakof P(VDF-TrFE) with the variation of temperature showed hysteretic variation and the phase transitiontemperature of the polymer in heating condition was higher than in the cooling condition. The elimination ofthe hysteretic phase transition of P(VDF-TrFE) is necessary for practical applications of optical devices.

As a continuation of a previous work by Park et al. (2006), we have developed a two-element radio interferometer that can measure both the phase and amplitude of a visibility function. Two small radio telescopes with diameters of 2.3 m are used as before, but this time an external reference oscillator is shared by the two telescopes so that the local oscillator frequencies are identical. We do not use a hardware correlator; instead we record signals from the two telescopes onto a PC and then perform software correlation. Complex visibilities are obtained toward the sun at λ=21cm for 24 baselines with the use of the earth rotation and positional changes of one element, where the maximum baseline length projected onto UV plane is ~90λ As expected, the visibility amplitude decreases with the baseline length, while the phase is almost constant. The image obtained by the Fourier transformation of the visibility function nicely delineates the sun, which is barely resolved due to the limited baseline length. The experiment demonstrates that this system can be used as a "toy" interferometer at least for the education of (under)graduate students.

Speckle Interferometer equipped with an ITT intensified CCD have been used on the NCUO ( National Central University Observatory, Taiwan) 24-inch telescope for studying the orbits of bright binary systems selected from the Yale's Bright Star Catalogue. The high resolution and high sensitivity ITT intensified solid state video camera ( F4577 ) has external gain and gate control functions which will simplify the design of the speckle camera and allow us to do precise speckle photometry. The goal of this project is trying to study the bright binary systems with separations between the average size of seeing disk and the diffraction limit of the 24-inch telescope. Recently some observing data have been reduced and compared with the other teams' results. We are now improving the data reduction technology and trying to use real time observing mode on the monthly routine observation.

The asymmetry of received intensity pattern within the bandwidth is derived from the analogy of the intensity distribution of two-slit interference. This suggests that the length of 1 2 λ delay line should be adjusted to the slightly upper frequency than the central frequency of the radio telescope with a wide bandwith. Some strange communication signals and man-made noises prevented us from obtaining the discernible information from the observed data for the sun. To overcome this difficulties, it is necessary to alter the operating frequency and site. It will be fo1lowed to measure the angular dimensions of the superposed radio sources by changing the distance between two antennas.

A Fabry-Perot interferometer (FPI) for mesospheric observations was installed at King Sejong Station (62.2°S, 58.9°W) in Antarctica in 2017. For the initial validation of the FPI measurements, we compare neutral wind data recorded with the FPI with those from a Meteor Radar (MR) located nearby. The overall characteristics of the FPI and MR winds of both OH 892.0 nm (87 km) and OI 557.7 nm (97 km) airglow layers are similar. The FPI winds of both layers generally match the MR winds well on the observed days, with a few exceptions. The correlation analysis of the FPI and MR wind data shows that the correlation coefficients for the zonal winds at 87 and 97 km are 0.28 and 0.54, respectively, and those for the meridional winds are 0.36 and 0.54, respectively. Based on the assumption that the distribution of the airglow emissions has a Gaussian function with respect to the altitude, we calculated the weighted mean winds from the MR wind profile and compared them with the FPI winds. By adjusting the peak height and full width at half maximum of the Gaussian function, we determined the change of the correlation between the two winds. The best correlation for the OH and OI airglow layers was obtained at a peak height of 88–89 km and 97–98 km, respectively.