1. Detecting Exoplanets Ma Bo, Department of Astronomy, Nanjing University

2. Candidates detected (342) by radial velocity 316by radial velocity by Transiting methods 58 by microlensing 8by microlensing by imaging 11by imaging by timing 7by timing

3. Radial Velocity ( 51 Pegasi in 1995)51 Pegasi reflex motion of the host star using pulsar timing or precision Doppler measurements

4. Transiting Method periodic dimming of the parent star as the planet transits in front

5. Microlensing planet-induced perturbations to microlensing light curves in which the host star acts as the primary gravitational lens

6. Inverse ray-shooting method （ Kayser1986 ） 和正向计算的方法比较 Lense planeAmplification image

7. Discovery of a Jupiter/Saturn Analog Could this be explained by a planet/satellite pair?

8. Timing method (for pulsar) pulses arrive at the telescope with a tiny, variable delay caused by planets around

9. Direct imaging (first at 2005) First direct imaging of a giant planet around a brown dwarf

10. Detection Limits for Planets Around Solar-Like Stars

11. Future space missions Space Interferometry Mission Kepler Terrestrial Planet Finder (TPF)

12. About Kepler System Characteristics: Spacebased Photometer: 0.95-m aperture Primary mirror: 1.4 meter diameter, 85% light weighted Detectors: 95 mega pixels (42 CCDs with 2200x1024 pixels) Bandpass: 430-890 nm FWHM Dynamic range: 9th to 16th magnitude stars Fine guidance sensors: 4 CCDs located on science focal plane Attitude stability: <9 milli-arcsec, 3 sigma over 15 minutes.

13. The End Thank you! Good Luck to Kepler and Man Utd! Welcome to Old Trafford, Inter Milan!