• Title/Summary/Keyword: LAM

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Performance analysis for Ground Position Accuracy Test of MLAT (MLAT 지상 위치정확도 시험에 대한 성능 분석)

  • Koo, Bon-soo;Jang, Jae-won;Kim, Woo-riul;Kim, Tae-sik
    • Journal of Advanced Navigation Technology
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    • v.21 no.4
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    • pp.325-331
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    • 2017

  • As a GPS stability problem arises, MLAT system is spotlighted as an alternative technology of ADS-B. MLAT system has a high position accuracy as much as ADS-B. Also, MLAT receives the mode A,C,S, and 1090ES(ADS-B) signals from the mounted aircraft transponder. MLAT receives signals from several receiver units and calculates aircraft positions. MLAT has ADS-B level positioning accurarcy using GPS and can calculate the position information with objects independently. According to global environment changes, Local area multiltilateration(LAM) surveillance system is under development for moving vehicles and aircraft detection in airport. These are still under testing in Tae-an Airfield. In the paper, we analyzed the performance by comparing the calculated position data from MLAT to RTK. In order to confirm the position accuracy of MLAT and the deviation of position data between fixed target and moving target on the ground during the field test in Tae-an Airfield.

  • https://doi.org/10.12673/jant.2017.21.4.325 인용 PDF KSCI

GALAXY SED FITTING

  • Denis, Burgarella;Mederic, Boquien;Veronique, Buat;Laure, Ciesla;Yannick, Rhoelly
    • Publications of The Korean Astronomical Society
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    • v.32 no.1
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    • pp.205-208
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    • 2017

  • Modelling and fitting the spectral energy distribution (SED) of galaxies or regions of galaxies is one of the most useful methods available to the astronomer nowadays. By modelling the SEDs and comparing the models to the observations, we can collect important information on the physical processes at play in the formation and evolution of galaxies. The models allow to follow the evolution of the galaxies from their formation on. The versatility of code is crucial because of the diversity of galaxies. The analysis is only relevant and useful if the models can correctly reproduce this diversity now and across (as best as possible) all redshifts. On the other hand, the code needs to run fast to compare several million or tens of millions of models and to select the best (on a probabilistic basis) one that best resembles the observations. With this important point in mind, it seems logical that we should efficiently make use of the computer power available to the average astronomer. For instance, it seems difficult, today, to model and fit SEDs without a parallelized code. We present the new Python version of CIGALE SED fitting code and its characteristics. CIGALE comes in two main flavours: CIGALE Classic to fit SEDs and CIGALE Model to create spectra and SEDs of galaxies at all redshifts. The latest can potentially be used in conjunction with galaxy evolution models of galaxy formation and evolution such as semi-analytic ones.

  • https://doi.org/10.5303/PKAS.2017.32.1.205 인용 PDF KSCI