• Title/Summary/Keyword: observation noise

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Optical Orbit Determination of a Geosynchronous Earth Orbit Satellite Effected by Baseline Distances between Various Ground-based Tracking Stations I: COMS simulation case

  • Son, Ju Young;Jo, Jung Hyun;Choi, Jin
    • Journal of Astronomy and Space Sciences
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    • v.32 no.3
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    • pp.221-228
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    • 2015
  • To protect and manage the Korean space assets including satellites, it is important to have precise positions and orbit information of each space objects. While Korea currently lacks optical observatories dedicated to satellite tracking, the Korea Astronomy and Space Science Institute (KASI) is planning to establish an optical observatory for the active generation of space information. However, due to geopolitical reasons, it is difficult to acquire an adequately sufficient number of optical satellite observatories in Korea. Against this backdrop, this study examined the possible locations for such observatories, and performed simulations to determine the differences in precision of optical orbit estimation results in relation to the relative baseline distance between observatories. To simulate more realistic conditions of optical observation, white noise was introduced to generate observation data, which was then used to investigate the effects of baseline distance between optical observatories and the simulated white noise. We generated the optical observations with white noise to simulate the actual observation, estimated the orbits with several combinations of observation data from the observatories of various baseline differences, and compared the estimated orbits to check the improvement of precision. As a result, the effect of the baseline distance in combined optical GEO satellite observation is obvious but small compared to the observation resolution limit of optical GEO observation.

The generalized methodology of signal detection in noise

  • Tuzlukov, Vyacheslav-P.
    • 제어로봇시스템학회:학술대회논문집
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    • 1992.10b
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    • pp.255-260
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    • 1992
  • It is reported on the methodology of signal detection in noise which is based on a comparison of statistical parameters of observation sample from region of frequency-time noise space where a signal may be present and observation sample from region of this noise space and it is known a priori about the latter that the signal is absent in this region.

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A Study On Identification Of A Linear Discrete System When The Statistical Characteristics Of Observation Noise Are Unknown (측정잡음의 통계적 성질이 미지인 경우의 선형 이산치형계통의 동정에 관한 연구)

  • 하주식;박장춘
    • 전기의세계
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    • v.22 no.4
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    • pp.17-24
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    • 1973
  • In the view point of practical engineering the identification problem may be considered as a problem to determine the optimal model in the sense of minimizing a given criterion function using the input-output records of the plant. In the system identification the statistical approach has been known to be very effective when the topological structure of the system and the statistical characteristics of the observation noises are known a priori. But in the practical situation there are many cases when the inforhation about the observation noises or the system noises are not available a priori. Here, the authors propose a new identification method which can be used effectively even in the cases when the variances of observation noises are unknown a priori. In the method, the identification of unknown parameters of a linear diserete system is achieved by minimizing the improved quadratic criterion function which is composed of the term of square equation errors and the term to eliminate the affection of observation noises. The method also gives the estimate of noise variance. Numerical computations for several examples show that the proposed procedure gives satisfactory results even when the short time observation data are provided.

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Missing Data Correction and Noise Level Estimation of Observation Matrix (관측행렬의 손실 데이터 보정과 잡음 레벨 추정 방법)

  • Koh, Sung-shik
    • Journal of the Institute of Electronics and Information Engineers
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    • v.53 no.3
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    • pp.99-106
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    • 2016
  • In this paper, we will discuss about correction method of missing data on noisy observation matrix and uncertainty analysis for the potential noise. In situations without missing data in an observation matrix, this solution is known to be accurately induced by SVD (Singular Value Decomposition). However, usually the several entries of observation matrix have not been observed and other entries have been perturbed by the influence of noise. In this case, it is difficult to find the solution as well as cause the 3D reconstruction error. Therefore, in order to minimize the 3D reconstruction error, above all things, it is necessary to correct reliably the missing data under noise distribution and to give a quantitative evaluation for the corrected results. This paper focuses on a method for correcting missing data using geometrical properties between 2D projected object and 3D reconstructed shape and for estimating a noise level of the observation matrix using ranks of SVD in order to quantitatively evaluate the performance of the correction algorithm.

On a Detection Scheme for Weak Deterministic Signals in Non-Additive Noise (비가산성 잡음에서의 약한 화정적 신호의 검파방식에 관하여)

  • Song, Iick-Ho
    • Journal of the Korean Institute of Telematics and Electronics
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    • v.25 no.9
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    • pp.1019-1026
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    • 1988
  • A parametric detection scheme for determenistic signals is obtained in a generalized observation model which contains non-additive noise. The model employed in this paper includes several special cases such as those describing purely-additive noise, multiplicative noise, and signal dependent noise and allows the consideration of deterministic and random signals. Locally optimum detectors for known deterministic signals in the model are derived and analyzed for performance. It is shown that the locally optimum detectors are interesting generalizations of those for the purely-additive noise model. Performance of the locally optimum detectors designed for the generalized observation model is compared to that of other common detectors.

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A Comparative Study of Wind Speed Spectrum based on the In-Situ Observation at the SeoHae Bridge Site (서해대교 현장계측에 기반한 풍속스펙트럼 모형의 비교인구)

  • Kim, Saang-Bum;Lee, Sung-Jin;Ahn, Sang-Sub
    • Proceedings of the Korean Society for Noise and Vibration Engineering Conference
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    • 2006.11a
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    • pp.417-421
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    • 2006
  • A comparative study of wind speed spectrum based on the in-situ observation at the SeoHae bridge site is conducted. Wind speed and directions of the SeoHae bridge site is measured and analyzed. Mean wind speed and turbulence intensity are estimated. The power spectral density function of the fluctuating component of the wind velocity is estimated. Several wind spectrum models of gust wind turbulence are compared and discussed based on the estimated wind spectrum.

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Development of Mini-Weather Buoy (연근해용 소형기상관측부이의 개발)

  • Lee, Dong-Kyu;Oh, Jai-Ho;Suh, Young-Sang
    • The Sea:JOURNAL OF THE KOREAN SOCIETY OF OCEANOGRAPHY
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    • v.4 no.2
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    • pp.155-159
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    • 1999
  • The mini-weather buoy using newly developed Weather Observation Through Ambient Noise (WOTAN) technology is developed. The buoy uses the cellular phone system for communication between the mini-weather buoy and the receiving station. The developed mini-weather buoy was deployed near Kijang and the comparison with land observation station was good: the rms error for wind speed estimation from underwater ambient noise was about 1 m/s. The only shortcoming of developed mini-weather buoy is that the buoy must be within the range of the cellular phone system, but it can be easily solved when satellite phone system is available.

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DEVELOPMENT OF THE 5GHZ CONTINUUM RECEIVER SYSTEM (5GHZ대 연속 전파 수신 시스템의 개발)

  • Byeon, Do-Yeong;Choi, Han-Gyu;Lee, Jeong-Won;Gu, Bon-Cheol
    • Publications of The Korean Astronomical Society
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    • v.11 no.1
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    • pp.109-123
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    • 1996
  • We have developed a 5GHz continuum receiver system. The receiver is a direct type receiver. In order to reduce the noise due to the fluctuation of the gain in the amplifiers, the system employs the Dicke switching method. We made the 5GHz low-noise amplifier and the bandpass filter. The low-noise amplifier gives ${\sim}35dB$ gain and has ${\sim}210K$ noise temperature. The bandpass filter has a passband between 4.3 and 5.4GHz. We also made switch driver, video amplifiers, phase detector, and integrator. Using a 1.8 meter offset parabolic antenna, we measured the efficiency of the system. Since the antenna does not have a driver to track objects, observations were performed with the antenna fixed. The measured noise temperature of the system is ${\sim}650K$. From the observation of the blank sky, noise level was measured. It was found that the systematic noise(${\sim}0.5K$: peak to peak value) is much larger than the thermal noise. The systematic noise is possibly related to the stability of the DC power supplied to the receiver system. Besides the noise of the system, it was found that the airplanes are the very serious noise sources. We measured the radio flux of the Sun using the developed system. The observed radio flux of the Sun is ${\sim}10^6Jy$, which is close to the known value of the quiet Sun. The test observation of the Sun shows that the angular beam size of the antenna is ${\sim}2.2^{\circ}$.

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UNDERWATER DISTRIBUTION OF VESSEL NOISE (선박소음의 수중분포에 관한 연구)

  • PARK Jung Hee
    • Korean Journal of Fisheries and Aquatic Sciences
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    • v.10 no.4
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    • pp.227-235
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    • 1977
  • The noise pressure scattered underwater on account of the engine revolution of a pole and liner, Kwan-Ak-San(G. T. 234.96), was measured at the locations of Lat. $34^{\circ}47'N$, Long. $128^{\circ}53'E$ on the 16th of August 1976 and Lat. $34^{\circ}27'N$, Long. $128^{\circ}23'E$ on the 28th of July, 1977. The noise pressure passed through each observation point (Nos. 1 to 5), which was established at every 10m distance at circumference of outside hull was recorded when the vessel was cruising and drifted. In case of drifting, the revolution of engine was fixed at 600 r. p. m. and the noise was recorded at every 10 m distance apart from observation point No. 3 in both horizontal and vertical directions with $90^{\circ}$ toward the stern-bow line. In case of cruising, the engine was kept in a full speed at 700 r.p.m. and the sounds passed through underwater in 1 m depth were also recorded while the vessel moved back and forth. The noise pressure was analyzed with sound level meter (Bruel & Kjar 2205, measuring range 37-140 dB) at the anechoic chamber in the Institute of Marine Science, National Fisheries University of Busan. The frequency and sound waves of the noise were analyzed in the Laboratory of Navigation Instrument. From the results, the noise pressure was closely related to the engine revolution shelving that the noise pressure marked 100 dB when .400 r. p. m. and increase of 100 r. p. m. resulted in 1 dB increase in noise pressure and the maximum appeared at 600 r. p. m. (Fig.5). When the engine revolution was fixed at 700 r. p. m., the noise pressures passed through each observation point (Nos. 1 to 5) placed at circumference of out side hull were 75,78,76,74 and 68 dB, the highest at No.2, in case of keeping under way while 75,76,77,70 and 67 dB, the highest at No.3 in case of drifting respectively (Fig.5). When the vessel plyed 1,400 m distance at 700 r.p.m., the noise pressure were 67 dB at the point 0 m, 64 dB at 600m and 56 dB at 1,400m on forward while 72 at 0 m, 66 at 600 m and 57 dB at 1,400 m on backward respectively indicating the Doppler effects 5 dB at 0 m and 3 dB at 200 m(Fig.6). The noise pressures passed through the points apart 1,10,20,30,40 and 50 m depth underwater from the observation point No.7 (horizontal distance 20 m from the point No.3) were 68,75,62,59,55 and 51 dB respectively as the vessel was being drifted maintaining the engine revolution at 600 r. p. m. (Fig. 8-B) whereas the noise pressures at the observation points Nos.6,7,8,9 and 10 of 10 m depth underwater were 64,75,55,58,58 and 52 dB respectively(Fig.8-A).

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A diagram of the new TRAO observation system

  • Kang, Hyunwoo;Lee, Changhoon;Jung, Jae Hoon;Kim, Young Sik;Jeong, Il-Gyo
    • The Bulletin of The Korean Astronomical Society
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    • v.40 no.2
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    • pp.55.1-55.1
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    • 2015
  • Taeduk Radio Astronomy Observatory (TRAO) is about to jump with new system - 16 beams array receiver with low noise temperature, new observation system on VxWorks OS, and FX spectrometer for 32 input signals. We serve a quite obvious diagram to understand new TRAO observation system. This diagram will be quick guide for manager and observer.

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