Status of RV Sub-Catelogy

Norio Narita (NAOJ)Yasuhiro H. Takahashi (Univ. of Tokyo)

Bun’ei Sato (Titech) Ryuji Suzuki (NAOJ)

and SEEDS/HiCIAO/AO188 teams

RV Internal Category

• F (Famous): nearby bright well-known stars with planets

• FM (Famous M stars): nearby well-known M stars with planets

• T (Transit): with transiting planets

• E (Eccentric): with eccentric (e>0.7) planets

• L (Long-term): with long-term RV trend

• G (Giants): GK giant stars with planets and long-term RV trend

Motivation of Each Internal Category

• Famous Systems

– They are famous and well investigated

• Eccentric and Transiting Systems

– To constrain planetary migration models

• Long-term and Giants

– To constrain orbits and mass of outer bodies

Target Name Reduction Results Follow-up/Publish Plan

HAT-P-7 (T) done 2 possible companions Narita et al. (2010)

55 Cnc. (F) done No companion --

HAT-P-13 (T) done 1 faint object Follow-up this year

HD81040 (E) done No companion --

HD68988 (L) done 2 background stars --

WASP-33 (T) done 1 bright object Follow-up next winter

ups And. (F) done 1 faint object Follow-up this year

WASP-14 (T) done 1 bright object Follow-up next year

tau Boo. (F) done 1 background/1 binary LoI(pub) submitted

GJ436 (FM) done 2 suspicious objects Follow-up this year

RV sub-category status 1/3

Target Name Reduction Results Follow-up/Publish Plan

HIP54195 (E) done 3 faint/1 bright objects Follow-up next year

HAT-P-14 (T) done 2 objects LoI(pub) submitted

TrES-4 (T) done 2 bright objects LoI(pub) submitted

GJ1214 (FM) done no companion --

tau Boo. (F) done 1 background/1 binary LoI(pub) submitted

HAT-P-11 (T) done several background LoI(pub) submitted

WASP-17 (T) done 3 bright objects LoI(pub) submitted

GJ581 (FM) done no companion --

WASP-15 (T) done no companion LoI(pub) submitted

18 Del. (G) In progress 1 faint object LoI(pub) submitted

RV sub-category status 2/3

Target Name Reduction Results Follow-up/Publish Plan

HAT-P-6 (T) In progress 4 objects --

HAT-P-17 (T) In progress No object/poor data --

WASP-8 (T) In progress 1 object --

HD8673 (E) In progress 1 object SCExAO follow-up needed

eps Eri. (F) in progress -- --

KOI-42 (T) In progress 1 object --

RV sub-category status 3/3

Ongoing Publication Plan

• tau Boo. : Takahashi et al.

• early results for transiting systems: Narita et al.

• summary paper for each internal category: TBD

Various Migration Models

consider gravitational interaction between

disk-planet (disk-planet interaction models)

• e.g., Ida & Lin papers

planet-planet (planet-planet scattering models)

• e.g., Chatterjee et al. 2008, Nagasawa et al. 2008

planet-binary companion (Kozai migration)

• e.g., Wu & Murray 2003, Fabrycky & Tremaine 2007

How can we discriminate those models by observations?

Diagnostics to discriminate migration models

small eccentricity and obliquitydisk-planet interaction

large eccentricity or obliquityplanet-planet scattering

Kozai migration

orbital eccentricityby radial velocity

spin-orbit alignment angleby the RM effect

Two Models Need Outer Massive Body

ejected planet/BD

captured planets

companion

star

orbit 1: low eccentricity and high inclination

orbit 2: high eccentricity and low inclination

binary orbital plane

outer planet/BD

Can we discriminate two models?

• Planet-Planet scattering

• Kozai migration

Additional information from direct imaging!

Search for outer massive bodies is important toconstrain migration mechanisms for each system

First/Second Year Targets

We focused on tilted and eccentric transiting planetary systems 10+ tilted transiting systems observed

Here we present a summary of early results and 2 cases with 2nd

epoch observations

9 Results at a Glance

First/Second Year Results9 out of 10 systems have companion candidates

high frequency of detecting candidate companions

Caution: this is only 1 epoch -> follow-up needed

Message to transit/secondary eclipse observers

Be careful about contamination of candidate companions,

even they are not real binary companions

sometimes they may affect your results

2nd epoch observations are ongoing

e.g., HAT-P-7 and HAT-P-11

First Application: HAT-P-7

not eccentric, but retrograde (NN+ 2009, Winn et al. 2009)

very interesting target for direct imaging observation

NN et al. (2009) Winn et al. (2009)

HAT-P-7 has a likely CPM Companion

2009 August H band: NN et al. (2010)2011 August Ks band

We have obtained J, H, Ks, L’ band images to determine spectral type

Possible additional planet ‘HAT-P-7c’

HJD - 2454000

Winn et al. (2009c) 2008 and 2010 Subaru data

(unpublished)2007 and 2009 Keck data

Long-term RV trend ~20 m/s/yr is ongoing from 2007 to 2010

constraint on the mass and semi-major axis of ‘c’

(Winn et al. 2009)

Additional Body Restricts Kozai migration

In the presence of ‘c’the Kozai migration caused by the companion cannot occur in this system

Kozai migration allowed

Kozai migration forbidden

Summary for the HAT-P-7 case

We detected two binary candidates and one is a likely CPM

companion

BUT the Kozai migration was excluded in the presence of the

additional body

planet-planet scattering appears plausible

HAT-P-11 (1st epoch)

Several companion candidates detected

HAT-P-11 (2nd epoch)

BUT they did not pass the common proper motion test!

Summary for the HAT-P-11 case

We detected several companion candidates in 1st epoch

2nd epoch follow-up suggests they are not a real companion

planet-planet scattering appears plausible

Conclusions for Transiting Systems

We found high frequency of detecting candidate companions

Caution: this is only 1 epoch

Further follow-up observations are important

Be careful for contamination of companion candidates

Depth of transit/secondary eclipse may be affected, even

they are not real companions

SEEDS observations will allow us to constrain migration models

We can present additional information for a frequency of p-p

scattering and Kozai migration