By using the Optical Wide-field Patrol (OWL) network developed by the Korea Astronomy and Space Science Institute (KASI) we generated the right ascension and declination angle data from optical observation of Low Earth Orbit (LEO) satellites. We performed an analysis to verify the optimum number of observations needed per arc for successful estimation of orbit. The currently functioning OWL observatories are located in Daejeon (South Korea), Songino (Mongolia), and Oukaïmeden (Morocco). The Daejeon Observatory is functioning as a test bed. In this study, the observed targets were Gravity Probe B, COSMOS 1455, COSMOS 1726, COSMOS 2428, SEASAT 1, ATV-5, and CryoSat-2 (all in LEO). These satellites were observed from the test bed and the Songino Observatory of the OWL network during 21 nights in 2014 and 2015. After we estimated the orbit from systematically selected sets of observation points (20, 50, 100, and 150) for each pass, we compared the difference between the orbit estimates for each case, and the Two Line Element set (TLE) from the Joint Space Operation Center (JSpOC). Then, we determined the average of the difference and selected the optimal observation points by comparing the average values.

1. INTRODUCTION
 2. OPTICAL WIDE FIELD PATROL NETWORK(OWL-NET)
 3. POST CORRECTION OF OPTICALOBSERVATION DATA BY OWL-NET
 4. METHODS OF ORBIT DETERMINATION ANDRESULTS
 5. SUMMARY
 ACKNOWLEDGMENTS
 REFERENCES

• Maru Park(Department of Astronomy and Space Science, Chungbuk National University, Cheongju 28644, Korea, Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Jung Hyun Jo(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea, Korea University of Science and Technology, Daejeon 34113, Korea) Corresponding Author
• Sungki Cho(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea, Korea University of Science and Technology, Daejeon 34113, Korea)
• Jin Choi(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea., Korea University of Science and Technology, Daejeon 34113, Korea)
• Chun-Hwey Kim(Department of Astronomy and Space Science, Chungbuk National University, Cheongju 28644, Korea)
• Jang-Hyun Park(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Hong-Suh Yim(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Young-Jun Choi(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Hong-Kyu Moon(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Young-Ho Bae(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Sun-Youp Park(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Ji-Hye Kim(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Dong-Goo Roh(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Hyun-Jung Jang(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Young-Sik Park(Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)
• Min-Ji Jeong(Department of Astronomy and Space Science, Chungbuk National University, Cheongju 28644, Korea, Korea Astronomy and Space Science Institute, Daejeon 34055, Korea)