• 한국해안해양공학회지
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• 제18권2호
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• pp.112-123
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• 2006

우리나라 연안 비조석 성분자료의 확률밀도함수 형태로 쌍봉형 정규분포 함수 형태를 제안하였다. 비조석 성분 자료는 국립해양조사원에서 제공하는 인천, 군산, 목포, 제주, 여수, 마산, 가덕도, 부산, 포항, 속초 검조소의 1시간 간격 조위자료에서 64개 분조성분을 이용하여 합성된 성분을 제외한 잔차성분이다. 제안된 분포함수와 비조석 성분자료 분포함수의 RMS 오차 및 결정계수(R2) 값을 비교·분석한 결과, 비조석 성분자료의 확률밀 도함수로 본 연구에서 제안한 쌍봉형 함수가 기존에 사용하던 정규분포형 함수보다 더 적합한 함수로 파악되었다. 본 연구에서 제안된 확률밀도함수의 매개변수는 Newton 방법을 수정한 Levenberg-Marquardt 방법으로 추정 하였으며, 비조석 성분 자료의 표준편차 및 왜곡도 계수는 목포, 제주, 속초 지점을 제외하고는 분석지점 검조소 자료의 비조화 상수와 밀접한 관계가 있는 것으로 파악되었다.

• 한국항공우주학회지
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• 제43권9호
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• pp.830-837
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• 2015

최근 지구를 공전하는 우주잔해물의 개수가 급격하게 증가함에 따라 인공위성과의 충돌 위험성이 높아져 우주잔해물은 우주개발 국가들에게 심각한 문제로 대두되고 있다. 현재 인공위성 충돌 위험성을 감시하고 회피기동 여부를 판단하기 위해서 레이더 및 전자광학 시스템이 사용되고 있다. 그러나 레이저추적 시스템과 같이 보다 정밀한 추적데이터와 연계하여 정밀한 예측 궤도력을 생성할 수 있다면 충돌회피기동 여부의 정확한 판단과 회피기동 계획 수행에 많은 도움을 줄 수 있다. 레이저추적 시스템은 가장 정밀한 거리측정 정보를 제공하기 때문에 기존 예측궤도력 정밀도를 향상시킬 수 있는 대안으로 인식되고 있다. 한국천문연구원은 반사경을 장착한 인공위성 레이저추적, 고출력 레이저를 이용한 우주잔해물 레이저추적 및 적응광학을 이용한 우주물체 영상취득이 가능한 우주물체 레이저추적 시스템을 개발하고 있다. 본 연구에서는 우주물체 레이저추적 시스템에 사용되는 고출력 레이저를 이용한 link budget, 배경잡음에 의한 오경보 및 신호검출 확률 분석을 통해 우주잔해물 레이저추적을 위한 성능분석을 수행하였다.

• 한국과학교육학회지
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• 제16권1호
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• pp.61-76
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• 1996

The purpose of this study was to apply the instructional strategies for conceptual change prescribed by Posner et al(1982) to the astronomic content domain taught in the elementary and middle school and to analyze the characteristics of students' knowledge revealed in the test before, during and after the instruction. Also, it was to investigate the intercorrelation of cognitive levels, spatial ability and science achievement. The major findings of this study are as follows: 1. Students had a great variety of misconceptions related to the motion of the moon before the instruction, that is, the phases, the names of phases and the cause of changing phases by the moon's orbit about the earth, the moon's appearance and location at the given time, the relative positions of earth, moon and sun during a lunar eclipse, the cause that a full moon is not at the line of node once a month. In the analysis of students' responses concerning the cause of changing phases of the moon and a lunar eclipse, the results indicate that the great majority of students had rote learning rather than meaningful learning in the middle school. 2. Students' reponses during the instruction concerning the changing phases of the moon and the predictive knowledge about the motions of the earth and the moon were analyzed. 1) According to the results of the test given before and after experiment, after discussion, achievement score of the whole of subjects and groups in both preformal and formal cognitive levels appeared to increase linearly. 2) There was no statistically significant differences of achievement scores before and after experiment, after discussion between preformal group and formal group in cognitive levels. 3. Distribution of achievement scores according to the whole of subjects and groups in preformal and formal cognitive levels shows that there was a statistically significant difference between pretest and posttest. 4. Types of conceptual changes concerning the cause of changing phases of the moon that occurred from pretest to posttest were classified as accommodation, incomplete accommodation, assimilation, no change and no model. Six of the seven students starting instruction with alternative frameworks didn't sustain those alternative models throughout instruction. Five of these six students accommodated completely and the last one partially. Seventy-nine percentage of students taking instruction with fragmental models assimilated correct propositions at the end of the instruction. These results suggest that conceptual change model prescribed by Posner et al(1982) has promised the meaningful learning to students taking with fragmental models, especially in cases where students with misconception enter instruction. 5. High correlation between achievement score of simple-recall items and that of written items in pretest and posttest indicates that the higher students got the score in simple-recall items the better they also performed in written items. However, there was no statistically significant differences among cognitive levels, spatial ability and science achievement in the whole of subjects and groups according to the cognitive levels.

• 천문학회지
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• 제36권4호
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• pp.271-282
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• 2003

We present results of a $H^{13}CN$ J=1-0 mapping survey of molecular clouds toward the Galactic Center (GC) region of $-1.6^{\circ}{\le}{\iota}{\le}2^{\circ}$ and $-0.23^{\circ}{\le}b{\le}0.30^{\circ}$ with 2' grid resolution. The $H^{13}CN$ emissions show similar distribution and velocity structures to those of the $H^{12}CN$ emissions, but are found to better trace the feature saturated with $H^{12}CN$ (1-0). The bright components among multi-components of $H^{12}CN$ line profiles usually appear in the $H^{13}CN$ line while most of the dynamically forbidden, weak $H^{12}CN$ components are seldom detected in the $H^{13}CN$ line. We also present results of other complementary observations in $^{12}CO$ (J=1-0) and $^{13}CO$ (J=1-0) lines to estimate physical quantities of the GC clouds, such as fractional abundance of HCN isotopes and mass of the GC cloud complexes. We confirm that the GC has very rich chemistry. The overall fractional abundance of $H^{12}CN$ and $H^{13}CN$ relative to $H_2$ in the GC region is found to be significantly higher than those of any other regions, such as star forming region and dark cloud. Especially cloud complexes nearer to the GC tend to have various higher abundance of HCN. Total mass of the HCN molecular clouds within $[{\iota}]{\le}6^{\circ}$ is estimated to be ${\~}2 {\times}10^7\;M_{\bigodot}$ using the abundances of HCN isotopes, which is fairly consistent with previous other estimates. Masses of four main complexes in the GC range from a few $10^5$ to ${\~}10^7\;M_{\bigodot}$ All the HCN spectra with multi-components for the four main cloud complexes were investigated to compare the line widths of the complexes. The largest mode (45 km $s^{-1}$) of the FWHM distributions among the complexes is in the Clump 2. The value of the mode tends to be smaller at the farther complexes from the GC.

• 천문학회지
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• 제37권4호
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• pp.199-203
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• 2004

The gas response to a proposed spiral stellar pattern for our Galaxy is presented here as calculated via 2D hydrodynamic calculations utilizing the ZEUS code in the disk plane. The locus is that found by Drimmel (2000) from emission profiles in the K band and at 240 ${\mu}m$. The self-consistency of the stellar spiral pattern was studied in previous work (see Martos et al. 2004). It is a sensitive function of the pattern rotation speed, $\Omega$p, among other parameters which include the mass in the spiral and its pitch angle. Here we further discuss the complex gaseous response found there for plausible values of $\Omega$p in our Galaxy, and argue that its value must be close to $20 km s^{-l}\;kpc^{-1}$ from the strong self-consistency criterion and other recent, independent studies which depend on such parameter. However, other values of $\Omega$p that have been used in the literature are explored to study the gas response to the stellar (K band) 2-armed pattern. For our best fit values, the gaseous response to the 2-armed pattern displayed in the K band is a four-armed pattern with complex features in the interarm regions. This response resembles the optical arms observed in the Milky Way and other galaxies with the smooth underlying two-armed pattern of the old stellar disk populations in our interpretation. The complex gaseous response appears to be related to resonances in stellar orbits. Among them, the 4:1 resonance is paramount for the axisymmetric Galactic model employed, and the set of parameters explored. In the regime seemingly proper to our Galaxy, the spiral forcing appears to be marginally strong in the sense that the 4:1 resonance terminates the stellar pattern, despite its relatively low amplitude. In current work underway, the response for low values of $\Omega$p tends to remove most of the rich structure found for the optimal self-consistent model and the gaseous pattern is ring-like. For higher values than the optimal, more features and a multi-arm structure appears.

• 천문학논총
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• 제24권1호
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• pp.53-64
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• 2009

MIRIS is the main payload of the STSAT-3 (Science and Technology Satellite 3) and the first infrared space telescope for astronomical observation 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 $3.67^{\circ}\times3.67^{\circ}$. 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 200 K by pointing to the deep space (3K). The cooling mechanism employs a radiator, a Winston cone baffle, a thermal shield, MLI (Multi Layer Insulation) of 30 layers, and GFRP (Glass Fiber Reinforced Plastic) pipe support in the system. Optomechanical 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 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.

• 천문학논총
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• 제27권5호
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• pp.419-429
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• 2012

In this paper, we propose a new re-quantization method after FFT processing to prevent the distortion of correlation result of VCS (VLBI Correlation Subsystem). The re-quantization is used to rearrange the data bit so as to reduce the data rate processed as 16-bit of FFT result of VCS. Having done this procedure, we found that the distorted spectrum of correlation result occurred in the delay tracking experiments by the re-quantization method introduced for initial design of VCS. In order to solve this, two kinds of re-quantization method, that is, the comparison and selection-type, are proposed. The first is to re-quantize the FFT result as a valid-bit by comparing with the input data after determining the adequate threshold. The second is manually to select the valid-bit of FFT result after finding the valid-field of data according to the bit-distribution of input data. We confirmed that the second is more effective compared with the first through the experimental result, and it will be implemented without so much modification of applied method in the condition of the limited resource of FPGA. The re-quantization is, however, carried out with 4-bit in the proposed second method for FFT result, and then the distortion of correlation result is also appeared. To fix this problem, the bit for re-quantization is extended to 8-bit. The proposed 8-bit selection-type is effectively verified so that the distortion of correlation result disappeared by applying to VCS in consequence of the simulation and correlation experiments.

• 천문학논총
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• 제27권5호
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• pp.399-409
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• 2012

NGC 6871을 중심으로 시계열 관측한 Cyg OB3 성협영역에서 모두 15개의 단주기 변광성을 찾았다. 이들은 모두 국부나선팔에 속한 ${\delta}$ Scuti 형 변광성으로 보인다. 그림 5의 영연령주계열 상에서 밝은쪽에 속한 V1-V4는 분광형이 모두 A, F 형으로서 Cyg OB3 성협보다 먼 거리에 있는 ${\beta}$ Cephei 형 변광성이라기 보다는 국부나선팔의 앞쪽에 놓인 ${\delta}$ Scuti 형 변광성이었다. 15개의 ${\delta}$ Scuti 형 변광성 중에는 2개(V1과 V3)는 GCVS에 ${\delta}$ Scuti 형 변광성으로 분류되어 이미 알려진 변광성이고, 나머지는 모두 새로 발견한 것이다. 새로 발견한 변광성 중에는 한 개의 이중모드 ${\delta}$ Scuti 형 변광성(V3)과 2개의 HADS 변광성(V13과 V14)이 포함되었다. 시계열 관측과는 별도로 표준화 관측을 수행하여 관측 영역의 색-등급도를 얻었는데 그림 6에서 Massey etal.(1995)의 결과와 잘 맞았다.

• 천문학회지
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• 제48권2호
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• pp.125-137
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• 2015

We report results of the performance evaluation of a new hardware correlator in Korea, the Daejeon correlator, developed by the Korea Astronomy and Space Science Institute (KASI) and the National Astronomical Observatory of Japan (NAOJ). We conduct Very Long Baseline Interferometry (VLBI) observations at 22 GHz with the Korean VLBI Network (KVN) in Korea and the VLBI Exploration of Radio Astrometry (VERA) in Japan, and correlated the aquired data with the Daejeon correlator. For evaluating the performance of the new hardware correlator, we compare the correlation outputs from the Daejeon correlator for KVN observations with those from a software correlator, the Distributed FX (DiFX). We investigate the correlated flux densities and brightness distributions of extragalactic compact radio sources. The comparison of the two correlator outputs shows that they are consistent with each other within < 8%, which is comparable with the amplitude calibration uncertainties of KVN observations at 22 GHz. We also find that the 8% difference in flux density is caused mainly by (a) the difference in the way of fringe phase tracking between the DiFX software correlator and the Daejeon hardware correlator, and (b) an unusual pattern (a double-layer pattern) of the amplitude correlation output from the Daejeon correlator. The visibility amplitude loss by the double-layer pattern is as small as 3%. We conclude that the new hardware correlator produces reasonable correlation outputs for continuum observations, which are consistent with the outputs from the DiFX software correlator.

• 천문학회보
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• 제36권2호
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• pp.77.2-77.2
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• 2011

We present our follow-up observation of the recently discovered supernova in M101. Being only 6.4 Mpc away from the Earth, the object is a Type-Ia supernova discovered this close in decades. We followed up this event with various observing facilities including on-campus telescopes at Seoul National University, the McDonald observatoy's 2.1m telescope, and UKIRT 4-m telescope. The light curves and the preliminary analysis of the multi-wavelength data will be presented, which cover the wavelengths from optical to NIR.