• Journal of the Optical Society of Korea
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• 제18권3호
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• pp.230-235
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• 2014

Two-step quadrature phase-shifting digital holography based on the calculated intensity of a reference wave is proposed. In the Mach-Zehnder interferometer (MZI) architecture, the method only records two quadrature-phase holograms, without reference-wave intensity or object-wave intensity measurement, to perform object recoding and reconstruction. When the reference-wave intensity is calculated from the 2D correlation coefficient (CC) method that we presented, the clear reconstruction image can be obtained by some specific algorithm. Its feasibility and validity were verified by a series of experiments with 2D objects and 3D objects. The presented method will be widely used in real-time or dynamic digital holography applications.

• 한국지구물리탐사학회:학술대회논문집
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• 한국지구물리탐사학회 2004년도 대한지구물리학회.한국지구물리탐사학회 공동학술대회 초록집
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• pp.3-17
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• 2004

Space-borne Earth observation technique is one of the most cost effective and rapidly advancing Earth science research tools today and the potential field and micro-wave radar applications have been leading the discipline. The traditional optical imaging systems including the well known Landsat, NOAA - AVHRR, SPOT, and IKONOS have steadily improved spatial imaging resolution but increasing cloud covers have the major deterrent. The new Earth observation satellites ENVISAT (launched on March 1 2002, specifically for Earth environment observation), ALOS (planned for launching in 2004 - 2005 period and ALOS stands for Advanced Land Observation Satellite), and RADARSAT-II (planned for launching in 2005) all have synthetic aperture radar (SAR) onboard, which all have partial or fully polarimetric imaging capabilities. These new types of polarimetric imaging radars with repeat orbit interferometric capabilities are opening up completely new possibilities in Earth system science research, in addition to the radar altimeter and scatterometer. The main advantage of a SAR system is the all weather imaging capability without Sun light and the newly developed interferometric capabilities, utilizing the phase information in SAR data further extends the observation capabilities of directional surface covers and neotectonic surface displacements. In addition, if one can utilize the newly available multiple frequency polarimetric information, the new generation of space-borne SAR systems is the future research tool for Earth observation and global environmental change monitoring. The potential field strength decreases as a function of the inverse square of the distance between the source and the observation point and geophysicists have traditionally been reluctant to make the potential field observation from any space-borne platforms. However, there have recently been a number of potential field missions such as ASTRID-2, Orsted, CHAMP, GRACE, GOCE. Of course these satellite sensors are most effective for low spatial resolution applications. For similar objects, AMPERE and NPOESS are being planned by the United States and France. The Earth science disciplines which utilize space-borne platforms most are the astronomy and atmospheric science. However in this talk we will focus our discussion on the solid Earth and physical oceanographic applications. The geodynamic applications actively being investigated from various space-borne platforms geological mapping, earthquake and volcano .elated tectonic deformation, generation of p.ecise digital elevation model (DEM), development of multi-temporal differential cross-track SAR interferometry, sea surface wind measurement, tidal flat geomorphology, sea surface wave dynamics, internal waves and high latitude cryogenics including sea ice problems.

• Journal of Astronomy and Space Sciences
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• 제22권1호
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• pp.1-12
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• 2005

한국우주전파관측망(Korean VLBI Network: KVN)은 우리나라 최초의 초장기선 전파간섭계로 새로운 천문우주 연구 분야 및 측지, 지구물리 등의 연구를 위하여 3기의 21m 최첨단 밀리미터파 전파 안테나를 이용하여 우주를 바라보는 새로운 영역을 개척할 예정이다. 전파간섭계의 성능은 안테나 배열 및 관측 대상 천체의 적위, 그리고 천체와 크기 및 형태에 따른 의존성이 매우 크다. 본 연구는 현재 설정되어있는 KVN관측소 및 시스템 자료를 근거로 단일 점광원, 다중 점광원, 원형광원 2개, Cygnus A의 5개 모델 영상에 대하여 가상관측을 수행하였다. 적위에 따른 KVN의 UV 궤적 분포로부터 가장 이상적이라고 여겨지는 적위 60도인 천체에 대하여 22GHz의 관측 파장으로 12시간 동안 가상관측을 수행하여 얻어진 UV데이터를 가지고 간섭계 표준 영상처리를 하였다. 그 결과 22GHz에서 예상되는 KVN의 빔 크기에 의해 분해가 되지 않는 모델들의 RMS 대비 최대밝기 강도(Jy/Beam)가 대략 점광원의 징우 l0000:1, 지름 6mas(milli arcsecond) 원형 광원의 경우 5000:1 정도로 매우 높은 반면, 빔 크기보다 큰 모델에서는 115:1 및 34:1정도로 현저하게 감소하였으며 영상의 복원 정도도 이와 같은 결과를 보였다. 이것은 KVN이 상대적으로 적은 기선의 개수로 인하여 UV평면을 충분히 채우지 못하며, 동시에 짧은 기선이 부족하여 넓은 분포를 가지는 천체들에 대한 영상화능력이 떨어지기 때문이다. 그러나 각 모델과 CLEAN 영상과의 픽셀 좌표비교에서는 12mas 원형광원을 제외하고는 정확하게 일치함을 보였다. 그러므로 KVN의 주요한 관측 대상은 콤팩트한 천체들이 적당할 것이며, 이러한 천체들에 대하여 KVN은 위치측정에 우수한 성능을 보였다.

• 대한원격탐사학회:학술대회논문집
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• 대한원격탐사학회 2002년도 Proceedings of International Symposium on Remote Sensing
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• pp.429-434
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• 2002

The Synthetic Aperture Radar (SAR) data are considered to contain the greatest amount of information among various microwave techniques developed for measuring ocean variables from aircraft or satellites. They have the potential of measuring wavelength, wave direction and wave height of the ocean waves. But, it is difficult to retrieve significant ocean wave heights and surface current from conventional SAR data, since the imaging mechanism of ocean waves by a SAR is determined by the three basic modulation processes arise through the tilt modulation, hydrodynamic modulation and velocity bunching which are poorly known functions. Along-Track Interferometric (ATI) SAR systems can directly detect the Doppler shift associated with each pixel of a SAR image and have been used to estimate wave fields and surface currents. However, the Doppler shift is not simply proportional to the component of the mean surface current. It includes also contributions associated with the phase velocity of the Brags waves and orbital motions of all ocean waves that are longer than Brags waves. In this paper, we have developed a new method for extracting the surface current vector using multiple-frequency (L- & C-band) ATI SAR data, and have generated surface wave height information.

• Journal of the Optical Society of Korea
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• 제20권6호
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• pp.784-793
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• 2016

We present a single shot low coherence white light Hilbert phase microscopy (WL-HPM) for quantitative phase imaging of Si optoelectronic devices, i.e., Si integrated circuits (Si-ICs) and Si solar cells. White light interferograms were recorded by a color CCD camera and the interferogram is decomposed into the three colors red, green and blue. Spatial carrier frequency of the WL interferogram was increased sufficiently by means of introducing a tilt in the interferometer. Hilbert transform fringe analysis was used to reconstruct the phase map for red, green and blue colors from the single interferogram. 3D step height map of Si-ICs and Si solar cells was reconstructed at multiple wavelengths from a single interferogram. Experimental results were compared with Atomic Force Microscopy and they were found to be close to each other. The present technique is non-contact, full-field and fast for the determination of surface roughness variation and morphological features of the objects at multiple wavelengths.

• 천문학회보
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• 제44권1호
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• pp.59.1-59.1
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• 2019

Immediate vicinity of a supermassive black hole (SMBH) is an important place to test general relativity in strong gravity regime. Also, this is a place where mass accretion and jet formation actively occurs at the centers of active galaxies. Theoretical studies predict presence of bright ring-like emission encircling an accreting SMBH with a diameter of about 5 Schwarzschild radii, and a flux depression at the center (i.e., BH shadow). Direct imaging of the BH shadow is accordingly of great importance in modern astrophysics. However, the angular sizes of the horizon-scale structures are desperately small (e.g., ~40-50 microarcseconds (uas) diameter for the nearest best candidates). This poses serious challenges to observe them directly. Event Horizon Telescope (EHT) is a global network of sensitive radio telescopes operating at 230 GHz (1.3 mm), providing ultra-high angular resolution of 20 uas by cutting-edge very long baseline interferometry techniques. With this resolution, EHT aims to directly image the nearest SMBHs; M87 and the galactic center Sgr $A{\ast}$ (~40-50 uas diameters). In Spring 2017, the EHT collaboration conducted a global campaign of EHT and multiwavelength observations of M87 and Sgr $A{\ast}$, with addition of the phased ALMA to the 1.3mm VLBI array. In this talk, I review results from past mm-VLBI and EHT observations, provide updates on the results from the 2017 campaign, and future perspectives.

• 대한원격탐사학회지
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• 제23권6호
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• pp.559-566
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• 2007

레이더 위성간섭기법은 지형의 고도 및 변위를 정밀하게 측정하는데 널리 사용되고 있는 기술이다. 이 중 L 밴드의 경우, C또는 X 밴드의 영상보다 시간간격의 영향이 적기 때문에 긴 기선거리를 가진 간섭쌍도 DEM생성을 위한 충분한 긴밀도를 유지하게 된다. 따라서 L 밴드를 사용할 경우, DEM 정밀도에 영향을 주는 고도 민감도가 높아지게 되므로 연안 지역과 같은 평탄한 지형의 DEM 제작에 매우 효과적이다. 국내 서해안의 경우, 얕은 수심과 큰 조차로 인해 넓은 갯벌이 존재하며 국토 확장의 목적으로 시작된 대규모의 간척 사업에 행해졌다. 따라서 연안지역의 지속적인 관리와 보전을 위하여 정밀한 DEM이 필요하다. 본 연구의 목적은 L밴드 ALOS PALSAR 자료의 위상간섭기법을 통한 서해안 연안지역의 지형고도 정보 획득 및 연안지역 DEM 생성의 가능성을 살펴보는 것이다. 한반도 서해안 시화, 화옹간척지 및 강화 남부 갯벌에서 46일의 기간간격을 지닌 2007/05/22 과 2007/08/22의 간섭쌍과 2007/08/22 과 2007/10/22의 간섭쌍을 이용하여 DEM을 제작하였다. 각 각의 고도민감도는 2007/05/22 과 2007/08/22 간섭쌍의 경우 73m 이며, 2007/08/22 과 2007/10/22 간섭쌍은 185m의 값을 갖는다. 그러나, 2007/05/22 과 2007/08/22간섭쌍의 경우 두 자료간의 긴밀도 값이 낮으며(강화도 남쪽 갯벌: 0.5-0.6, 화옹, 시화 간척지: 0.6-0.7), 연구 지역의 조위차로 인하여 전체적인 강화도 남쪽 갯벌의 고도가 측정되지 않았다. 반면, 2007/08/22 과 2007/10/22 간섭쌍의 경우 2007/05/22 과 9007/08/22 간섭쌍에 비하여 높은 긴밀도값 (강화도 남쪽 갯벌 및 화옹, 시화 간척:0.9-1)을 가지며, 전체적인 강화도 남쪽 갯벌의 고도 또한 측정 할 수 있었다. 그러나 간섭쌍간의 짧은 기선거리로 인한 낮은 고도민감도로 인하여 정밀한 DEM을 획득하지 못하였다. 따라서, 향후 획득한 ALOS PALSAR 자료간의 시간간격 및 기선거리가 충분히 유지된다면 획득 간섭쌍간의 높은 긴밀도와 고도 민감도를 가진 자료를 통하여 한반도 서해안지역의 정밀한 DEM 제작이 가능할 것으로 보인다.

• 한국광학회지
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• 제15권1호
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• pp.39-45
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• 2004

CCD의 입력면에서의 물체광과 참조광의 간섭을 수치적 방법으로 생성한 광 강도 분포 홀로그램을 대상으로 퓨리어 변환방법을 이용한 0차 회절광의 제거를 전산 모사 방법으로 구현하였고, 0차 회절광 성분이 제거된 광 강도 분포와 위상을 갖는 홀로그램을 생성하였다. 그리고 그 결과를 수치적 재생 방법을 사용하여 0차 회절광 성분의 제거를 확인하였다. 그리고 퓨리어 변환 방법에 의한 0차 회절광 성분이 제거된 위상홀로그램의 생성이 가능하다. 0차 회절광을 제거하기 위한 제거 함수를 도입하였고 제거 영역에 따른 0차 회절광의 제거와 재생되는 실상의 정보 손실 정도를 비교하였고, 기존의 방법에 비하여 효과적임을 증명하였다.

• 천문학회지
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• 제48권5호
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• pp.237-255
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• 2015

The Interferometric Monitoring of Gamma–ray Bright Active galactic nuclei (iMOGABA) program provides not only simultaneous multifrequency observations of bright gamma–ray detected active galactic nuclei (AGN), but also covers the highest Very Large Baseline Interferometry (VLBI) frequencies ever being systematically monitored, up to 129 GHz. However, observation and imaging of weak sources at the highest observed frequencies is very challenging. In the second paper in this series, we evaluate the viability of the frequency phase transfer technique to iMOGABA in order to obtain larger coherence time at the higher frequencies of this program (86 and 129 GHz) and image additional sources that were not detected using standard techniques. We find that this method is applicable to the iMOGABA program even under non–optimal weather conditions.

• 천문학회보
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• 제42권1호
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• pp.46.2-46.2
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• 2017

Atmospheric propagation effects at millimeter wavelengths can significantly alter the phases of radio signals and reduce the coherence time, putting tight constraints on high frequency Very Long Baseline Interferometry (VLBI) observations. In previous works it has been shown that non-dispersive (e.g. tropospheric) effects can be calibrated with the frequency phase transfer (FPT) technique. The coherence time can thus be significantly extended. Ionospheric effects, which can still be significant, remain however uncalibrated after FPT, as well as the instrumental effects. In this work, we implement a further phase transfer between two FPT residuals (i.e. so-called FPT2) to calibrate the ionospheric effects based on their frequency dependence. We show that after FPT2, the coherence time at 3 mm can be further extended beyond 8 hours, and the residual phase errors can be sufficiently canceled by applying the calibration of another source, which can have a large angular separation from the target (> $20{\circ}$). Calibrations for all-sky distributed sources with a few calibrators are also possible after FPT2. One of the strengths and uniqueness of this calibration strategy is the suitability for high frequency all-sky survey observations including very weak sources. We discuss the introduction of a pulse calibration system in the future to calibrate the remaining instrumental effects and allowing the possibility of imaging the source structure at high frequencies with FPT2, where all phases are fully calibrated without involving any sources other than the target itself.