• Proceedings of the Korean Institute of Navigation and Port Research Conference
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• v.2
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• pp.251-254
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• 2006

A precise real-time method of using the IGS ultra rapid products (IGU) and the GPS broadcast ephemeris to calculate the VRS orbit corrections was presented here which was suited for GPS/VRS reference station network based positioning. Test data acquired from both the SGRSN (Sichuan GPS Reference Station Network) and SCIGN (Southern California integrated GPS network) were used to evaluate the performance of the modeling techniques. The new method was proven to be more precise and reliable compared with the existing conventional network-based orbit error interpolation method. It was shown that 0.004ppm relative accuracy was reached, namely the influence from the orbit bias for the RTK positioning within 100km area can be of sub-millimeter level.

• Proceedings of the Korean Institute of Navigation and Port Research Conference
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• v.2
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• pp.9-14
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• 2006

Galileo is the European Global Navigation Satellite System, under civilian control, and consists on a constellation of medium Earth orbit satellites and its associated ground infrastructure. Galileo will provide to their users highly accurate global positioning services and their associated integrity information. The elements in charge of the computation of Galileo navigation and integrity information are the OSPF (Orbit Synchronization Processing Facility) and IPF (Integrity Processing Facility), within the Galileo Ground Mission Segment (GMS). Navigation algorithms play a key role in the provision of the Galileo Mission, since they are responsible for computing the essential information the users need to calculate their position: the satellite ephemeris and clock offsets. Such information is generated in the Galileo Ground Mission Segment and broadcast by the satellites within the navigation signal, together with the expected a-priori accuracy (SISA: Signal-In-Space Accuracy), which is the parameter that in fault-free conditions makes the overbounding the predicted ephemeris and clock model errors for the Worst User Location. In parallel, the integrity algorithms of the GMS are responsible of providing a real-time monitoring of the satellite status with timely alarm messages in case of failures. The accuracy of the integrity monitoring system is characterized by the SISMA (Signal In Space Monitoring Accuracy), which is also broadcast to the users through the integrity message.

• Journal of The Korean Astronomical Society
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• v.18 no.1
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• pp.1-13
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• 1985

We present the data of photoelectric photometric observations of BW Vul carried out for four nights during the period of $1982{\sim}1984$. The light curves with asymmetric shape show a stillstand on the ascending branch at phase of ${\phi}{\approx}0.85$ just before the maximum light, and also the ampitude and shape of light curves are changed from night to night. Using all the published data, a new ephemeris of maximum time is derived, in which the period of light variation is $P=0^d.20102977$ and its increasing rate is 2.2 see/century.

• Journal of Astronomy and Space Sciences
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• v.15 no.1
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• pp.69-74
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• 1998

Two colour(B & V) photoelectric observations of EB-type eclipsing binary GO Cyg were carried out for 15 nights during October and December 1996. Three new times of minimum derived from our own observations are presented. With these and previously published times, the period variation is studied, and a continuous period increase of $dP/dt{\approx}1.51{\times}10^{-7}d/yr$ is estimated from the quadratic ephemeris.

• 한국지형공간정보학회:학술대회논문집
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• 2002.03a
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• pp.9-16
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• 2002

본 연구에서는 광주를 고정으로 전라남도 4점과 전라북도 5점으로 삼각망을 구성하고 각 측점에서 관측한 데이터를 방송력과 정밀력을 이용하여 기선 해석을 실시하고 기선거리별 궤도력의 영향을 통계학적으로 비교 분석하여 전라남북도에 이르는 GPS관측망의 궤도력에 따른 각 기선별 오차분포를 정량화 할 수 있었고, 정밀력을 이용한 기선해석은 기준 공분산 값이 모두 1 미만으로 나타나 두 지역간의 지역적 변환계수와 지구중심절대좌표를 선정함에 있어 과대오차를 현저히 줄일 수 있었다.

• The Bulletin of The Korean Astronomical Society
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• v.46 no.1
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• pp.49.1-49.1
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• 2021

SomangNet team aims to make use of small- to medium-sized telescopes for photometric follow-up observations of transiting extrasolar planets orbiting a bright host star. Newly discovered transiting planets need frequent monitoring in order to maintain knowledge of the transit ephemeris. DOAO 1.0 m telescope and CBNUO 0.6 m telescopes are used for our monitoring. We will present some preliminary results of our observations and analysis.

• Journal of Astronomy and Space Sciences
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• v.24 no.4
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• pp.417-430
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• 2007

The selection of ground stations is one of the essential process of IGS (International GNSS Service) products. High quality GPS data should be collected from the globally distributed ground stations. In this study, we investigated an effect of ground station network selection on GPS satellite ephemeris. The GPS satellite ephemeris obtained from the twelve ground station networks were analyzed to investigate the effect of selection of ground stations. For data quality check, the observations, the number of cycle slips, and multipath of pseudoranges for L1 and L2 were considered. The ideal network defined by Taylor-Karman structure and SOD (Second Order Design) were used to obtain the optimal ground station network.

• Journal of Satellite, Information and Communications
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• v.10 no.4
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• pp.128-135
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• 2015

Currently we have an electro-optical space object monitoring system (OWL-Net) developed by the Korea Astronomy and Space Science Institute as the only ground-based on orbit space object tracking capability in Korea. This system can produce the ephemeris of domestic satellites and survey the geosynchronous orbit region. As the number of observation objects increases and the operation condition get worse, a low budget dedicated monitoring telescope capable of full time geosynchronous orbit region survey can support an effect operation of the OWL-Net. In this study, we analyze the requirements of a low-budget dedicated optical monitoring system for geosynchronous orbit region without the degradation of observation quality to increase the risk of corrupted ephemeris.

• Journal of Astronomy and Space Sciences
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• v.22 no.3
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• pp.197-210
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• 2005

Results of 7 nights of CCD VR photometry of the intermediate polar 1RXS J062518.2+733433 obtained at the Korean 1.8m telescope are reported. The corrected ephemeris for the orbital minimum is BJD (Orb.min) = 2453023.6159(42)+0.1966431(33) (E-1735). The corrected ephemeris for the spin maximum is BJD (spin max) = 2452893 78477 (10)+0.01374116815 (17) (E-15382) (cycle numbering corresponds to that of Staude et al.2003). The variations of the shape of the individual spin variations are highly correlated in V and R. The phase of the spin maximum is found to be dependent on the orbital phase. The corresponding semi-amplitude of sinusoidal variations of phase is $0.11{\pm}0.03.$ This new phenomenon is explained by the changing viewing conditions of the accreting magnetic white dwarf, and should be checked in further observations this star and for other intermediate polars. To avoid influence of this effect on the analysis of the long-term spin period variations, the runs of at least one orbital period are recommended. Results of time series analysis are presented in tables.

• Journal of Advanced Navigation Technology
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• v.20 no.5
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• pp.433-439
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• 2016

Several low-cost global navigation satellite system (GNSS) receivers do not support general range-domain correction, and DGNSS-CP (differential GNSS) method had been suggested to solve this problem. It improves its position accuracy by projecting range-domain corrections to the position-domain and then differentiating the stand-alone position by the projected correction. To project the range-domain correction, line-of-sight vectors from the receiver to each satellite should be calculated. The line-of-sight vectors can be obtained from GNSS broadcast ephemeris data or satellite direction information, and this paper shows positioning performance for the two methods. Stand-alone positioning result provided from Septentrio PolaRx4 Pro receiver was used to show the difference. The satellite direction information can reduce the computing load for the DGNSS-CP by 1/15, even though its root mean square(RMS) of position error is bigger than that of ephemeris data by 0.1m.