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NEO Research Project in Korea

NEO Research Project in Korea. Wonyong Han 1 , Yong- Ik Byun 2 , Hong- Suh Yim 1 , Young-Jun Choi 1 , Hong- Kyu Moon 1 & NESS Team 1 Korea Astronomy and Space Science Institute (KASI ) 2 Yonsei University. Contents 1. Brief History 2. Ystar-Neopat Program 3. Ness program

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NEO Research Project in Korea

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  1. NEO Research Project in Korea Wonyong Han1, Yong-Ik Byun2, Hong-Suh Yim1, Young-Jun Choi1, Hong-KyuMoon1 & NESS Team 1Korea Astronomy and Space Science Institute (KASI) 2Yonsei University

  2. Contents 1. Brief History 2. Ystar-Neopat Program 3. Ness program 4. Future work

  3. 1. Brief History

  4. 1998~1999 (Preparation) 1998 :YUO1 started YSTAR2 program and developed 50-cm wide-field telescope systems for detection and monitoring optical brightness variations and moving objects. 1999 :KASI3formed a task force named NEOPAT4 and started NEO follow-up observation using their 0.6-m and 1.8-m optical telescopes. 1Yonsei University Observatory, 2Yonsei Survey Telescopes for Astronomical Research 3Korea Astronomy and Space Science Institute, 4Near-Earth Object PATrol

  5. 2000~2005 (YSTAR-NEOPAT Program) The Korean Ministry of Science and Technology awarded a research grant to the KASI NEOPAT group to establish the National Research Lab (NRL)for NEO survey. ` NEOPAT and YSTAR groups started to work together in order to combine their expertise and resources. In late 2003, our 1st telescope, started regular operation in Sutherland, South Africa. In late 2005, we commissioned 2nd telescope in Siding Spring Observatory, Australia.

  6. 2007~ (NESS Program) KASI started 2nd generationNEOPAT program : NESS (Near Earth Space Survey) This program is to develop new 0.6 robotic telescopes for stereo observations. And also to develop stable technology of automaticobservatory for network & stereo observations. `

  7. 2. YSTAR-NEOPAT Program

  8. TELESCOPE SYSTEM : T1-T2 0.5 meter aperture FOV 1.73  1.73 deg with 2k CCD Reaches ~ 17th mag with 60 sec exposures High speed mount, 10 deg/sec

  9. AWS Sky Monitor Computer Enclosure Observatory System

  10. Internet MASTER SCOPE SKYCCD Gateway Web Server Firewall Telescope Control Dome Control Sky Monitor GPS Receiver Weather Station HUB MAINCCD WEBCAM CCD Control 4 Security Cameras DATA PROCESS Data Storage Data Analysis Computer System

  11. South Africa Station, Sutherland (April, 2002)

  12. Australia Station, Siding Spring (December 2004) AustrailiaStation, Siding Spring (Januanry, 2005)

  13. Prepare by Y. H. Bae DATA PIPELINE : FindMovers On-Site computers run near real-time image processing and discovery routines. For each NEO candidate, a stamp animation and report file is created and forwarded to Korea for visual confirmation. South Africa Station

  14. Prepare by Y. H. Bae New Variable Stars • Found a few hundred of variable stars • not previously catalogued (paper in preparation)

  15. Prepare by Y. H. Bae Moving Objects • Number of Nights : 73 • Number of Mover Candidates : 1029 • Peak Magnitude : R~15 • Peak Velocity : ~0.2deg/day Number of candidates Number of candidates Velocity (deg/day) R magnitude

  16. 3. Near Earth Space Survey

  17. Prepare by Y. H. Bae New 0.6m telescope systems

  18. Automatic/Robotic Observatory • Our strategy is focused to increase sky coverage • by employing multiple telescopes • Automatic Observatory is the best and only solution to operate multiple telescopes with small man power • We have developed the s/w for automatic observations, automatic data processing and • self-protection in emergency. • Please see the Poster • “The Small Fast Robotic Observation System”

  19. Network Observation • Multiple telescopes placed in different longitudes • allow continuous observations for a given target • Network Observation is a powerful tool of time series monitoring for variables stars, NEO photometry and intraday variability of many celestial objects. • Please see the Poster • “The Network Observation • Using Several Robotic Telescopes”

  20. Stereo Observation Stereo Observation is to observe to the same target at the same time by telescopes in different locations. For nearby targets such as NEO, stereo observations provide accurate orbital elements quickly by direct distance estimates. The accuracy and range of distance measurements depend on the separation of two (or more) telescopes. • Please see the Poster • “Stereo Observations for Near Earth Space Survey”

  21. 4. Future Work

  22. Near Earth Space Survey (NESS) Network of Automatic Observatories T3 Daejeon T1 Sutherland T2 Siding Spring

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