Various information from different detection methods

1. Various information from different detection methods MPIA-Student-Workshop, Italy

2. André Outline • Introduction • Indirect detection techniques • Radial Velocity • Astrometry • Transit • Microlensing • Direct detection techniques • Reflected starlight • Imaging FLO MPIA-Student-Workshop, Italy

3. Introduction • so far 215 planets are detected (23.03.2007) • 21 multiple systems • first announcements: Peter van de Kamp (18.04.1963) • Astrometric study of Barnard‘s star from plates taken • with the 24-inch Sproul refractor(AJ, vol. 68, 515) • BUT: 1952 by Otto Struve: • Proposal for a project of high-precision stellar radial • velocity work (The Observatory, No. 870) • first detections: • 1995 by Mayor & Queloz: 0.5 MJupiter • P = 4.2 days around 51 Peg MPIA-Student-Workshop, Italy

4. Orbital parameters Period P Semi-mayor axis a Eccentricity e Inclination i Argument of perihelion ω Longitude of the acsending node Ω True anomaly T Time of periapsisτ MPIA-Student-Workshop, Italy

5. Indirect techniques - radial velocity measurements • 203 planets 175 Planetary systems, 20 systems with > 1 planet 94,4% • Doppler Wobble • Hot Jupiters mostly MPIA-Student-Workshop, Italy

6. RV time series of the young G0V star ιHor Kürster et al. 2000, A&A 353, L33 Requirements • High measurement precision ~ 1m - 20 cm/s • Stability over ~ 10 years • Derived orbital parameters • P, e, a, T, ω Msini MPIA-Student-Workshop, Italy

7. - Astrometry • So far 8 planets: • Gl 876: 2 planets • 55 Cnc: 4 planets • ε Eri • Wobble around center of mass due to planet • Law of the lever: Θs = mp/ms. ap/d • Limits: 1-2 mas (ground based) 0.1 mas (HST FGS) • need for interferometrie for high precision PRIMA • Constraints: nearby stars, not too close to the star • can derive inclination and mass of planetary companion MPIA-Student-Workshop, Italy

8. 2008 2007 What do I observe? • I see the overlay of three different motions: • Proper motion MPIA-Student-Workshop, Italy

9. 2008 2008 2007 What do I observe? • I see the overlay of three different motions: • Proper motion • Parallax MPIA-Student-Workshop, Italy

10. 2008 2007 20 What do I observe? • I see the overlay of three different motions: • Proper motion • Parallax • Planetary signal • need to measure all 3 motions accuratly • Derived parameters: α, i, Ω, μ, π, T true mass of companion MPIA-Student-Workshop, Italy

11. Jupiter as an example For a star at 10 pc distance: MPIA-Student-Workshop, Italy

12. And what about AO effects? • maybe there remains a residual defocus or other distortions • one need a reference pattern of background-stars to determine the • platescale and changes due to instrumental effects MPIA-Student-Workshop, Italy

13. And what about AO effects? • maybe there remains a residual defocus or other distortions • one need a reference pattern of background-stars to determine the • platescale and changes due to instrumental effects • but the background-stars can have their own pm and parallax MPIA-Student-Workshop, Italy

14. Transits Venustransit June 2004 MPIA-Student-Workshop, Italy

15. Transits • Photometric detection • Depth of lightcurve yields planet-radius (~ 1% for Jupiter) Tres-1 HD209458 MPIA-Student-Workshop, Italy

16. Transit • Parameters derived: P, T0, i ~ 90°, Rp/RS • Together with the mass of the planet from RV measurements one can derive the density of the planet MPIA-Student-Workshop, Italy

17. Microlensing • Principle: MPIA-Student-Workshop, Italy

18. D. Bennett Microlensing • Principle: • Magnification due to Star and planet acting as lenses MPIA-Student-Workshop, Italy

19. Microlensing • Principle: • Magnification due to Star and planet acting as lenses • First planet: Bond et al. (04.2004) MPIA-Student-Workshop, Italy

20. BUT: • No way of confirmation • Single event • Short timescale: hours - days • Results: 4 detections as of today MPIA-Student-Workshop, Italy

21. MPIA-Student-Workshop, Italy