1. Mapping the Realm of Hot Jupiters Bun’ei Sato, Shigeru Ida （ Titech ）, Eri Toyota （ Kobe Univ. ）, Masashi Omiya （ Tokai Univ. ）, Debra Fischer （ SFSU ）, Greg Laughlin （ UC Santa Cruz ）, Paul Butler （ Carnegie Inst. of Washington ）, Geoff Marcy （ UC Berkeley ）

2. Mapping the Realm of Hot Jupiters Doppler search for Hot Jupiters with Subaru/HDS, Keck, Magellan （ N2K consortium ） Doppler search for Hot Jupiters with Subaru/HDS, Keck, Magellan （ N2K consortium ） Hunting “transiting” planets Hunting “transiting” planets Since 2004, 14 planets were discovered from N2K Since 2004, 14 planets were discovered from N2K 2 transiting planets （ HD149026b, HD17156b ） from Subaru !! 2 transiting planets （ HD149026b, HD17156b ） from Subaru !! Many planet-candidates are waiting for follow-up Many planet-candidates are waiting for follow-up Subaru intensive program Subaru intensive program S06A （ 10 nights ）, S06B （ 10 nights ） S06A （ 10 nights ）, S06B （ 10 nights ） Determine orbital parameters of planet-candidates making use of long time-baseline Determine orbital parameters of planet-candidates making use of long time-baseline

3. Hot Jupiters Giant planets in short-period orbits Giant planets in short-period orbits P ＜ 14d: ~70 HJ so far (30 are from transit surveys) P ＜ 14d: ~70 HJ so far (30 are from transit surveys) Frequency ~ 1% Frequency ~ 1% High-probability transit candidates High-probability transit candidates information about planet itself （ radius, internal structure, atmosphere, etc. ） information about planet itself （ radius, internal structure, atmosphere, etc. ） ex) HD149026b has an extraordinary huge solid core (Sato et al. 2005) ex) HD149026b has an extraordinary huge solid core (Sato et al. 2005) Tracers of multi-planet systems Tracers of multi-planet systems resonant configuration resonant configuration orbital evolution of planetary systems orbital evolution of planetary systems Test case of planet formation theory Test case of planet formation theory migration, tidal circularization,,, migration, tidal circularization,,,

4. N2K Consortium Search for Hot Jupiters around next 2000 solar-type stars Search for Hot Jupiters around next 2000 solar-type stars Keck （ USA ）、 Magellan （ Chile ）、 Keck （ USA ）、 Magellan （ Chile ）、 Subaru （ Japan ） Aiming to detect 60 Hot Jupiters and 5-6 transiting planets Aiming to detect 60 Hot Jupiters and 5-6 transiting planets Precise Doppler measurement Precise Doppler measurement using Iodine absorption cell Current precision with HDS Current precision with HDS ~4 m/s （ short-term ） ~4 m/s （ short-term ） ~10 m/s （ long-term ） ~10 m/s （ long-term ）

5. Strategy Database of 14,000 stars Database of 14,000 stars ・ V ＜ 10.5, d ＜ 110 pc, FGK V,IV ・ metalliicty, activity, binary,,, High priority to metal-rich stars High priority to metal-rich stars Detection probability from Monte Carlo Simulation ３＋１ nights observation ３＋１ nights observation ・ Identify candidates in 3 consecutive nights ・ RMS ＞ 20 m/s → follow-up ・ RMS ＞ 20 m/s → follow-up ・ RMS ＜ 20 m/s → drop ・ RMS ＜ 20 m/s → drop ・ Confirm candidates after 1 more night in 1 month later （ 0.5M J ） P=0.03x10^2[Fe/H]

6. Status: Keck & Magellan Magellan Keck 600 stars 12 planets (6 hot Jupiters) 30 more planet candidates 3 nights/yr 380 stars 20 planet candidates 3-4 nights/yr

7. Status: Subaru 635 stars >3 times: 512 stars >3 times: 512 stars <2 times: 123 stars <2 times: 123 stars S04A （ 4 nights ）S04A （ 4 nights ） S04B （ 4 nights ）S04B （ 4 nights ） S05B （ 5 nights ）S05B （ 5 nights ） S06A （ 10 nights ）S06A （ 10 nights ） 6 （ Jun. ） +4 （ Jul. ） 6 （ Jun. ） +4 （ Jul. ） S06B （ 10 nights ）S06B （ 10 nights ） 10 （ Dec. ） 10 （ Dec. ） find planet candidates confirm orbital parameters （ and find new planet candidates ） S08A （ 1.5 nights ）S08A （ 1.5 nights ） follow-up planet candidates

8. Metallicity: All N2K Targets Fischer et al. in preparation Nobs = 188 1291 stars 88 planets expected P=0.03x10^2[Fe/H]

9. Metallicity: Subaru Targets Fischer et al. in preparation Nobs = 188 504 stars 30 planets expected P=0.03x10^2[Fe/H]

10. RV Variations: Subaru Targets 471 stars 64 stars （ 20<σ RV <200 m/s ） -2 published planets -HD149026, HD17156 -3 strong planet-candidates at present -15 stars showing intermediate- to long-term trend (planet or SB) -20 possible planet-candidates -Others (active stars etc.)

11. Planet Candidates from Subaru P~35d P~700d P~500d Green:Keck Red ： Subaru

12. P=21.2 d K 1 =275 m/se=0.67 M p sini=3.1 M JUP a=0.15 AU HD 17156 （ G0V, V=8.2 ） M 1 =1.2M , R 1 =1.47R  [Fe/H]=0.24, Age=5.7Gyr Periastron distance 0.05 AU q=a （ 1-e ） =0.05 AU Tidal force from the central star Green:Keck Red ： Subaru HD17156b Mercury Fischer et al. 2007, ApJ, 669, 1336 Eccentric Short-Period Planet: HD 17156 b Planet evolving to a hot Jupiter?

13. Eccentricity Distribution of Exoplanets HD 17156 b q=0.05 AU circularized

14. Formation of Hot Jupiter Orbital Migration Orbital Migration migration due to interaction with disk migration due to interaction with disk small eccentricity small eccentricity Sling-shot Scenario Sling-shot Scenario gravitational interaction between planets gravitational interaction between planets one planet scattered close to the central star (with large eccentricity) becomes a hot Jupiter due to tidal force from the central star one planet scattered close to the central star (with large eccentricity) becomes a hot Jupiter due to tidal force from the central star

15. Aug. 16, 2008 Web release (homepage of Subaru)

16. Transit Detection in HD17156 Transit depth ～ 0.6 ％ Barbieri et al. 2007, A&A, 476, L13 Sep. 9-10, 2007 (UT) Amateur in Italy R planet  1.15±0.11R JUP Two of the two planets found by Subaru are transiting ones !!

17. Sky Projected Angle between Stellar Spin Axis and Planetary Orbital Axis ： λ λ=0°λ=60°λ=30° Stellar spin axis is on YZ-plane Ohta et al. 2005 Gaudi & Winn 2007 RM effect  λ and V s sinI s Rossiter-McLaughlin Effect

18. Previous Observations λ（°）λ（°） Mp（MJ）Mp（MJ） a （ AU ） eReference HD209458-4.4±1.40.660.04740.015Winn et al. 2005 HD189733-1.4±1.11.130.03120.001Winn et al. 2006 HD1475061.2±13.48.00.06860.5Winn et al. 2007 HD149026-12±150.350.04320Wolf et al. 2007 TrES-130±210.760.03940Narita et al. 2007 ｜ λ ｜ =0 ～ 30° No large misalignment

19. Photometric and Spectroscopic Observations of HD17156 by Osamu Oshima at Kurashiki-shi Planet radius/Stellar radius ＝ 0.08462  1.21±0.12R J Narita et al. PASJ, submitted Orbital Period =21.2162±0.0036 d 11 Nov. 2007

20. RM effect  λ=62±25° ＠ OAO/HIDES ● 岡山、 ▲ すばる、 ■ ケック λ=60° Narita et al. PASJ, submitted

21. HD17156 λ（°）λ（°） Mp（MJ）Mp（MJ） a （ AU ） eRef. HD209458-4.4±1.40.660.0470.015Winn et al. 2005 HD189733-1.4±1.11.130.0310.001Winn et al. 2006 HD1475061.2±13.48.00.0690.5Winn et al. 2007 HD149026-12±150.350.0430Wolf et al. 2007 TrES-130±210.760.0390Narita et al. 2007 HD1715662±253.130.150.67 First possible candidate with large spin-orbit misalignment

22. Summary & Future Prospects 2 planets have been found so far from Subaru 2 planets have been found so far from Subaru both of them are transiting ones, and they are unique and give big impact on planet formation theory both of them are transiting ones, and they are unique and give big impact on planet formation theory Metallicity database of all the N2K targets will be published soon Metallicity database of all the N2K targets will be published soon Improvement of RV precision of HDS is still required Improvement of RV precision of HDS is still required ~10 m/s offset between observing runs ~10 m/s offset between observing runs Continuous observations are necessary to investigate cause of RV variations for 40 more candidates Continuous observations are necessary to investigate cause of RV variations for 40 more candidates Queue-observations are helpful Queue-observations are helpful Ex.) 1-2 hours x many days Ex.) 1-2 hours x many days