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Mapping the Realm of Hot Jupiters

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 ）.

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Mapping the Realm of Hot Jupiters

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  1. Mapping the Realm ofHot 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） • Hunting “transiting” planets • Since 2004, 14 planets were discovered from N2K • 2 transiting planets （HD149026b, HD17156b） from Subaru !! • Many planet-candidates are waiting for follow-up • Subaru intensive program • S06A（10 nights）, S06B（10 nights） • Determine orbital parameters of planet-candidates making use of long time-baseline

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

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

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

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

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

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

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

  10. RV Variations: Subaru Targets 471 stars 64 stars （20<σRV<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 Green:KeckRed：Subaru P~700d P~500d

  12. Eccentric Short-Period Planet: HD 17156 b HD 17156 （G0V, V=8.2） M1=1.2M, R1=1.47R [Fe/H]=0.24, Age=5.7Gyr P=21.2 d K1=275 m/s e=0.67 Mpsini=3.1 MJUP a=0.15 AU Green:KeckRed：Subaru Periastron distance q=a（1-e）=0.05 AU Mercury Tidal force from the central star Planet evolving to a hot Jupiter? HD17156b Fischer et al. 2007, ApJ, 669, 1336

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

  14. Formation of Hot Jupiter • Orbital Migration • migration due to interaction with disk • small eccentricity • Sling-shot Scenario • 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

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

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

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

  18. Previous Observations ｜λ｜=0～30° No large misalignment

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

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

  21. HD17156 First possible candidate with large spin-orbit misalignment

  22. Summary & Future Prospects • 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 • Metallicity database of all the N2K targets will be published soon • Improvement of RV precision of HDS is still required • ~10 m/s offset between observing runs • Continuous observations are necessary to investigate cause of RV variations for 40 more candidates • Queue-observations are helpful • Ex.) 1-2 hours x many days

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