• Corrosion Science and Technology
• /
• 제4권6호
• /
• pp.217-221
• /
• 2005

In the present investigation, holographic interferometry was utilized for the first time to monitor in situ the thickness of the oxide film of aluminium samples during anodization processes in boric acid solutions. The anodization process (oxidation) of the aluminium samples was carried out by the technique of the electrochemical impedance spectroscopy(EIS), in different concentrations of boric acid (0.5-5.0% $H_3BO_3$) at room temperature. In the mean time, the real-time holographic interferometry was used to measure the thickness of anodized (oxide) film of the aluminium samples in solutions. Consequently, holographic interferometry is found very useful for surface finish industries especially for monitoring the early stage of anodization processes of metals, in which the thickness of the anodized film of the aluminium samples can be determined without any physical contact. In addition, measurements of electrochemical values such as the alternating current (A.C) impedance(Z), the double layer capacitance($C_{dl}$), and the polarization resistance(Rp) of anodized films of aluminium samples in boric acid solutions were made by the electrochemical impedance spectroscopy(EIS). Attempts to measure electrochemical values of Z, Cdl, and Rp were not possible by holographic interferometry in boric acid especially in low concentrations of the acid. This is because of the high rate of evolutions of interferometric fringes during the anodization process of the aluminium samples in boric acid, which made measurements of Z, Cdl, and Rp are difficult.

• 천문학회지
• /
• 제40권4호
• /
• pp.131-132
• /
• 2007

The research of OH maser emission sources with high angular resolution is complicated by the effects of interstellar scattering: more over, most of the OH maser sources are located in the galactic plane where the scattering is largest. However, the data available from pulsar studies on the spatial distribution of the amount of scattering indicate that there is a strong non-uniformity in the distribution of the amount of scattering material. There are directions in the galactic plane where the scattering is an order of magnitude higher than the average, as well as directions where the scattering is much lower. The latter provide an opportunity to investigate OH masers with the full angular resolution offered by very long baseline interferometry instruments, like the VLBA, and measure their true angular size, shape and brightness temperature. We have observed approximately 100 OH maser sources, distributed all over the northern hemisphere, with the VLBA in order to study the scattering properties of the interstellar medium.

• 천문학논총
• /
• 제30권2호
• /
• pp.115-118
• /
• 2015

We made phase-referencing Very Long Baseline Interferometry (VLBI) observations of Galactic 22 GHz $H_2O$ maser sources with VLBI Exploration of Radio Astrometry (VERA). We measured the parallax distances of G48.61+0.02, G48.99-0.30, G49.19-0.34, ON1, IRAS 20056+3350, IRAS 20143+3634, ON2N, and IRAS 20126+4104, which are located near the tangent point and the Solar circle. The angular velocity of the Galactic rotation at the LSR (i.e. the ratio of the Galactic constants) is derived using the measured parallax distances and proper motions of these sources. The derived value of ${\Omega}_0=28.8{\pm}1.7km\;s^{-1}kpc^{-1}$ is consistent with recent values obtained using VLBI astrometry but 10% larger than the International Astronomical Union (IAU) recommended value of $25.9km\;s^{-1}kpc^{-1}=(220km\;s^{-1})$ / (8.5 kpc).

• 천문학논총
• /
• 제30권2호
• /
• pp.633-636
• /
• 2015

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 outflows 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 $A^{\ast}$ 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 $A^{\ast}$. Towards KSP, we show the first preliminary images of M87 at 23 GHz and Sgr $A^{\ast}$ at 43 GHz with the bandwidth of 256 MHz.

• 천문학논총
• /
• 제30권2호
• /
• pp.629-631
• /
• 2015

In this proceedings, preliminary results of the KVN Source-Frequency Phase-Referencing (SFPR) observation of 3C 66A and 3C 66B are presented. The motivation of this work is to measure the core-shift of these 2 sources and study the temporal evolution of the jet opacity. Two more sources were observed as secondary reference calibrators and each source was observed at 22, 43, and 86 GHz simultaneously. Our preliminary results show that after using the observations at the lower frequency to calibrate those at the higher frequency of the same source, the residual visibility phases for each source at the higher frequencies became more aligned, and the coherence time became much longer; also, the residual phases for different sources, within 10 degrees angular separations, follow similar trends. After reference to the nearby calibrator, the SFPRed maps were obtained as well as the astrometric measurements, i.e. the combined coreshift. The measurements were found to be affected by structural blending effects because of the large beamsize of KVN, but this can be corrected with higher resolution maps (e.g. KAVA maps).

• 천문학논총
• /
• 제30권2호
• /
• pp.453-455
• /
• 2015

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 outflow 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 outflows, 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.

• 천문학회지
• /
• 제52권5호
• /
• pp.207-216
• /
• 2019

In this paper we introduce a software package, the Very long baseline interferometry Network SIMulator (VNSIM), which provides an integrated platform assisting radio astronomers to design Very Long Baseline Interferometry (VLBI) experiments and evaluate the network performance, with a user-friendly interface. Though VNSIM is primarily motivated by the East Asia VLBI Network, it can also be used for other VLBI networks and generic interferometers. The software package not only integrates the functionality of plotting (u, v) coverage, scheduling the observation, and displaying the dirty and CLEAN images, but also adds new features including sensitivity calculations for a given VLBI network. VNSIM provides flexible interactions on both command line and graphical user interface and offers friendly support for log reports and database management. Multi-processing acceleration is also supported, enabling users to handle large survey data. To facilitate future developments and updates, all simulation functions are encapsulated in separate Python modules, allowing independent invoking and testing. In order to verify the performance of VNSIM, we performed simulations and compared the results with other simulation tools, showing good agreement.

• 대한공간정보학회지
• /
• 제6권2호
• /
• pp.21-34
• /
• 1998

SAR 센서는 자체의 에너지원으로 영상을 취득하는 능동센서이며, 대기 중 투과효과가 매우 높으므로 기존의 광학센서로는 해결하지 못하였던 지역이나 상황의 분석에 그 가치가 매우 높다. 본 논문에서는 SAR 센서에 의해 취득된 영상들을 이용하여 수치표고모형을 추출하는 기법들의 이론적인 연구와 실제적인 적용을 통하여 그 문제점과 활용 가능성을 평가하여 보았다. 비교평가에 사용한 자료는 수치지도의 등고선 자료를 이용하였으며, 추출된 수치표고모형과 평균제곱근오차를 계산함으로서 추출 정확도를 평가하였다 수치표고모형 추출에 이용된 기법은 기존의 광학 영상에 적용되어왔던 입체모델 형성을 통한 지형표고를 추출하는 기법과 레이다 간섭 효과를 통한 지형표고 추출 기법이었다. 본 논문의 결과를 토대로, 현재 한국내의 지형여건을 고려한다면 입체시 기법에 의한 DEM 추출이 가장 적절할 것이며 레이다 간섭을 이용한 DEM 추출은 시기적인 문제와 산림의 산란효과에 의한 비상관 문제가 해결되어야만 할 것으로 생각된다.

• 대한원격탐사학회지
• /
• 제28권1호
• /
• pp.121-128
• /
• 2012

조간대 지역의 고해상 지형도는 해수 운동에 의한 퇴적 및 침식량의 변화와 같이 과학적인 연구의 기초자료로 쓰일 뿐만 아니라 연안 습지의 실제적인 관리 및 환경변화 모니터링의 도구로서도 그 활용의 가치가 높다. 그러나 조간대는 하상 퇴적물의 유입과 조석현상에 의해 빠르게 변화하고 있어 원격탐사와 같이 단기간에 넓은 지역을 조사할 수 있는 기술의 적용이 필요하다. 레이더 간섭기술은 가장 보편적이면서 성공적인 고해상 지형도 작성 기술로 알려져 있으나, 조간대에서는 지표노출시간의 제약 및 빠른 상태변화로 인해 일반적인 repeat-pass 간섭기술로는 충분한 긴밀도를 얻기 힘들다. 이 연구에서는 재방문주기가 짧은 Cosmo-SkyMed 1일 간격 관측자료와 ERS2-ENVISAT 30분 간격 관측자료를 이용하여 레이더 간섭기술을 이용한 조간대 지형도 작성을 실험하였다. 두 자료 모두 긴 수직기선으로 인한 높은 고도민감도와 짧은 관측주기로 인한 높은 긴밀도로 간섭위상을 구할 수 있었으나, Cosmo-SkyMed 관측자료에서는 대기에 의한 위상지연 효과와 조석에 의한 조간대 표층의 함수율 변화로 인하여 조간대와 같이 평평한 지역의 지형정보를 추출하는데에 어려움이 발생한다. 반면에 ERS2-ENVISAT 관측자료는 이종센서간의 관측중심주파수 차이를 상쇄하기 위해 설정된 긴 수직기선 덕분에 매우 높은 고도민감도를 가지며, 30분이라는 짧은 관측주기는 간섭쌍을 이루는 두 영상에 포함된 대기지연효과를 대부분 상쇄시키므로 조간대의 지형도 작성에 이상적인 자료로 판단된다.

• 천문학회지
• /
• 제47권6호
• /
• pp.235-253
• /
• 2014

Intensity interferometry, based on the Hanbury Brown-Twiss effect, is a simple and inexpensive method for optical interferometry at microarcsecond angular resolutions; its use in astronomy was abandoned in the 1970s because of low sensitivity. Motivated by recent technical developments, we argue that the sensitivity of large modern intensity interferometers can be improved by factors up to approximately 25 000, corresponding to 11 photometric magnitudes, compared to the pioneering Narrabri Stellar Interferometer. This is made possible by (i) using avalanche photodiodes (APD) as light detectors, (ii) distributing the light received from the source over multiple independent spectral channels, and (iii) use of arrays composed of multiple large light collectors. Our approach permits the construction of large (with baselines ranging from few kilometers to intercontinental distances) optical interferometers at the cost of (very) long-baseline radio interferometers. Realistic intensity interferometer designs are able to achieve limiting R-band magnitudes as good as $m_R{\approx}14$, sufficient for spatially resolved observations of main-sequence O-type stars in the Magellanic Clouds. Multi-channel intensity interferometers can address a wide variety of science cases: (i) linear radii, effective temperatures, and luminosities of stars, via direct measurements of stellar angular sizes; (ii) mass-radius relationships of compact stellar remnants, via direct measurements of the angular sizes of white dwarfs; (iii) stellar rotation, via observations of rotation flattening and surface gravity darkening; (iv) stellar convection and the interaction of stellar photospheres and magnetic fields, via observations of dark and bright starspots; (v) the structure and evolution of multiple stars, via mapping of the companion stars and of accretion flows in interacting binaries; (vi) direct measurements of interstellar distances, derived from angular diameters of stars or via the interferometric Baade-Wesselink method; (vii) the physics of gas accretion onto supermassive black holes, via resolved observations of the central engines of luminous active galactic nuclei; and (viii) calibration of amplitude interferometers by providing a sample of calibrator stars.