Mapping the Realm of Mapping the Realm of Hot Jupiters Jupiters - PowerPoint PPT Presentation

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

Mapping the Realm of Hot Jupiters Jupiters Mapping the Realm of Hot � Doppler search for Hot Doppler search for Hot Jupiters Jupiters with with � Subaru/HDS HDS, Keck, Magellan , Keck, Magellan （ N2K consortium consortium ） Subaru/ （ N2K ） � Hunting Hunting “ “transiting transiting” ” planets planets � � Since 2004, Since 2004, 7 7 planets were discovered from N2K planets were discovered from N2K � � 1 transiting planet 1 transiting planet （ HD149026b ） ） from Subaru from Subaru （ HD149026b � � ~ ~45 45 more planet more planet- -candidates not yet confirmed candidates not yet confirmed � � Subaru intensive program Subaru intensive program � � S06A S06A （ 10 nights ） , S06B S06B （ 10 nights ） （ 10 nights ） , （ 10 nights ） � � Determine orbital parameters of planet Determine orbital parameters of planet- -candidates candidates � making use of long time- -baseline baseline making use of long time � New planets confirmed New planets confirmed �

Hot Jupiters Jupiters Hot � Giant planets in short Giant planets in short- -period orbits period orbits � � P P ＜ 14d 、 M p sin i i ＞ 0.5M J ： ~ ~20 20 ％ ％ of of exoplanets exoplanets ＜ 14d 、 M p sin ＞ 0.5M J ： � � High High- -probability transit candidates probability transit candidates � � information about planet itself information about planet itself （ radius, internal （ radius, internal � structure, atmosphere, etc. ） structure, atmosphere, etc. ） � Tracers of multi Tracers of multi- -planet systems 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,,, �

Transiting Planets Transiting Planets Infrared emission Infrared emission Secondary Secondary Provide information on planet Provide information on planet Eclipse Eclipse from planets from planets itself which can’ ’t be obtained t be obtained itself which can from Doppler observations from Doppler observations temperature, temperature, atmosphere, atmosphere, Planetary radius Planetary radius albedo,,, ,,, albedo Transmission Transmission density, internal structure density, internal structure spectroscopy spectroscopy w/ or w/o solid core ） （ w/ or w/o solid core ） （ elements in elements in atmosphere atmosphere Rossiter effect effect spin- -orbit alignment orbit alignment Rossiter spin

HD 149026 HD 149026 Transit planet from Subaru, Keck, Transit planet from Subaru, Keck, P=2.8766 d Fairborn （ V=8.2 ， G0IV ） Fairborn （ V=8.2 ， G0IV ） K=43.3 m/s e=0 ・ M M p p sin sin i i = = 0.36 0.36 ± ± 0.0 0.03 3 M M J → 1.2 M 1.2 M SAT ・ UP → JUP SAT R p = 0.725 ± 0.05 R R J 0.86 R R SAT ・ R p = 0.725 ± 0.05 → 0.86 ・ UP → JUP SAT i = 85.3 = 85.3 ± 1.0 °） （ i ± 1.0 °） （ 70M M E solid core 70 E solid core Sato et al. 2005 Support core- -accretion scenario as accretion scenario as Support core Photometry planet formation mechanism planet formation mechanism However, the origin of such a huge However, the origin of such a huge core is still unknown core is still unknown Sato et al. 2005

Key: Key: Detection of transiting planets in bright stars Detection of transiting planets in bright stars V<10 ） ） for precise follow for precise follow- -up observations up observations （ V<10 （ • HD209458 HD209458 （ V=7.7 ） , HD149026 （ V=8.2 ） , HD189733 HD189733 • （ V=7.7 ） , HD149026 （ V=8.2 ） , （ V=7.7 V=7.7 ） ） , HAT , HAT- -P P- -1 1 （ （ V=10 V=10 ） ） （ • Transit systems from photometric survey Transit systems from photometric survey （ OGLE, TrES TrES, , • （ OGLE, WASP,, ） ） are too faint are too faint （ V=14- -16 16 ） ） for Doppler follow for Doppler follow- -up up WASP,, （ V=14 • Small transit depth of HD149026 would have been Small transit depth of HD149026 would have been • missed by current transit survey. Precise ephemeris is missed by current transit survey. Precise ephemeris is crucial to detect such a small variation. crucial to detect such a small variation. “Doppler survey Doppler survey → → Hot Jupiter Hot Jupiter → → Transit Transit” ” “ is the most efficient at present is the most efficient at present

N2K Consortium N2K Consortium � Keck Keck （ USA ）、 Magellan （ Chile ）、 � （ USA ）、 Magellan （ Chile ）、 Subaru （ Subaru （ Japan Japan ） ） � Search for Hot Search for Hot Jupiters Jupiters around around � next 2000 solar- -type stars type stars next 2000 solar � Aiming to detect Aiming to detect 60 60 Hot Hot Jupiters Jupiters � and 5 5 ～ 6 transiting planets transiting planets and ～ 6 � Precise Doppler measurement Precise Doppler measurement � using Iodine absorption cell using Iodine absorption cell � Current precision with HDS Current precision with HDS � ~3 m/s （ short- -term term ） ~3 m/s （ short ） ~10 m/s （ long- -term term ） ~10 m/s （ long ）

Group Members Group Members � Bun Bun’ ’ei ei Sato Sato （ （ PI PI ） ・・・ Observation Observation 、 、 Reduction Reduction 、 、 Analysis Analysis ）・・・ � � Shigeru Ida Shigeru Ida ・・・ Theory ・・・ Theory � � Eri Eri Toyota, Masashi Toyota, Masashi Omiya Omiya ・・・ Observation 、 Reduction 、 ・・・ Observation 、 Reduction 、 � Analysis Analysis � Debra Fischer Debra Fischer （ PI of N2K N2K ） Observation 、 Analysis （ PI of ）・・・ ・・・ Observation 、 Analysis � � G Greg reg Laughlin Laughlin ・・・ ・・・ Theory Theory � � P Paul aul Butler Butler ・・・ Reduction 、 Analysis ・・・ Reduction 、 Analysis � � G Geoff eoff Marcy Marcy � Graduate students ） � （ （ Graduate students ） � � Transit Network in Japan & USA Transit Network in Japan & USA � � Greg Henry Greg Henry （ （ USA USA ） ） � � Jun Jun- -ichi ichi Watanabe Watanabe （ （ NAOJ NAOJ ） ） , Osamu , Osamu Oshima Oshima （ （ Kamogata Kamogata High High- - � School ） , Shin- -ichiro ichiro Ishiguma Ishiguma （ Kobe Univ. ） , et al. School ） , Shin （ Kobe Univ. ） , et al.

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

HDS Observation HDS Observation =3500- -6100 6100 Å λ =3500 Å λ � � R~45,000 R~45,000 � � SN~150 for V~8 with 80s exp. SN~150 for V~8 with 80s exp. Iodine Cell � � in front of the RV precision using Iodine Cell RV precision using Iodine Cell � � slit of HDS � ~3 m/s ~3 m/s （ within the same run ） （ within the same run ） � （ since Jun. � ~10 m/s ~10 m/s （ long- -term term ） （ long ） � 2006 ） � systematic error between pre systematic error between pre- - � and post- -I I 2 cell replacement and post 2 cell replacement (and pre- - and post and post- -earthquake) earthquake) (and pre >100 stars/night >100 stars/night HD9407 （ RV Std. ） � � Observations are now almost Observations are now almost � � fully automated fully automated � observers only need change observers only need change � exposure time exposure time σ＝ 9.8 m/s � great effort by great effort by Tajitsu Tajitsu- -san san �