1. 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

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

3. 1. Brief History 1. Brief History

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

5. NEOPAT (NRL) 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. 2000~2005 (YSTAR-NEOPAT Program)

6. ` KASI started 2 nd generation NEOPAT 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 automatic observatory for network & stereo observations. 2007~ (NESS Program)

7. 2. YSTAR-NEOPAT Program 2. YSTAR-NEOPAT Program

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

9. Sky Monitor AWS Enclosure Computer Observatory System

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

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

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

13. 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. Prepare by Y. H. Bae South Africa Station

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

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

16. 3. Near Earth Space Survey

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

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 4. Future Work

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