HR 8799 (HD 218396)

Observations with MOST + ground based multi-site campaign

Observations with MOST + ground based multi-site campaign

André-Nicolas Chené (NRC/HIA/CGO)~35 co-authors…

André-Nicolas Chené (NRC/HIA/CGO)~35 co-authors…

HR 8799 (HD 218396)HR 8799

(HD 218396)

CollaboratorsCollaborators• Canada

– Gordon Walker (UBC)– André-Nicolas Chené (HIA)– Christian Marois (HIA)– David Bohlender (HIA)– Stephenson L. S. Yang (UVic)

• Germany– Artie P. Hatzes (Tautenburg)– Michael Hartmann (Tautenburg)– Holger Lehmann (Tautenburg)

• Chile– Christian Nitschelm

(Antofagasta)

• U.S.A.– Bruce Macintosh (LLNL)– Josh Isaacs (LLNL)– Carl Melis (U Cal.)– Jason Rowe (AMES)

• Canada– Gordon Walker (UBC)– André-Nicolas Chené (HIA)– Christian Marois (HIA)– David Bohlender (HIA)– Stephenson L. S. Yang (UVic)

• Germany– Artie P. Hatzes (Tautenburg)– Michael Hartmann (Tautenburg)– Holger Lehmann (Tautenburg)

• Chile– Christian Nitschelm

(Antofagasta)

• U.S.A.– Bruce Macintosh (LLNL)– Josh Isaacs (LLNL)– Carl Melis (U Cal.)– Jason Rowe (AMES)

• Belgium– Peter De Cat (RBO)– Duncan J. Wright (RBO)– Connie Aerts (Leuven)– Tijl Verhost (Leuven)– Paul Beck (Leuven)– Steven Bleomen (Leuven)– Josefa Montalban (Liège)– Mehdi-Pierre Bouadib (Liège)– Andrea Miglio (Liège)– Marc-Antoine Dupret (Liège)

• Japan– Eiji Kambe (OAO)

• France– Philippe Mathias (OCA)

• MOST team

• Belgium– Peter De Cat (RBO)– Duncan J. Wright (RBO)– Connie Aerts (Leuven)– Tijl Verhost (Leuven)– Paul Beck (Leuven)– Steven Bleomen (Leuven)– Josefa Montalban (Liège)– Mehdi-Pierre Bouadib (Liège)– Andrea Miglio (Liège)– Marc-Antoine Dupret (Liège)

• Japan– Eiji Kambe (OAO)

• France– Philippe Mathias (OCA)

• MOST team

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Fit of the OrbitFit of the Orbit

(Konopacky et al. in prep)(Konopacky et al. in prep)

Best fit

Stable orbit

Spectra of the planetsSpectra of the planets

1 x 20 min. raw cube 1 x 20 min. cube after speckle removal

NIRC2 image showing OSIRIS FOV

The System’s AgeThe System’s Age

• Age determined:– Galactic space motion– Color-magnitude diag.

• BUT:– Single field-star Bootis

• Age determined:– Galactic space motion– Color-magnitude diag.

• BUT:– Single field-star Bootis

b

c d

(Marois et al. 2008)

The System’s AgeThe System’s Age

• HR 8799 is a -Dor variable (has g-modes (and p-modes ???))

• In-depth asteroseismologic modeling of the host star will be used to derive an independent age of the system.

• HR 8799 is a -Dor variable (has g-modes (and p-modes ???))

• In-depth asteroseismologic modeling of the host star will be used to derive an independent age of the system.

Photometry of HR 8799Photometry of HR 8799

• Zerbi et al. (1999)– a) Window function– b) folded light-

curves

• Zerbi et al. (1999)– a) Window function– b) folded light-

curves

f1 = 1.9791 d-1

f2 = 1.7268 d-1

f3 = 1.6498 d-1

f4 = 0.2479 d-1

a)a)

b)b)Associated with Associated with gg-modes-modes

HR 8799 with MOSTHR 8799 with MOST

• Confirmed 3 first freq. published by Zerbi

(1999)

• + 38 other freq.

• Confirmed 3 first freq. published by Zerbi

(1999)

• + 38 other freq.

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HR 8799 with MOSTHR 8799 with MOST

• Granulation?• Granulation?

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« Nah… » - Jason Rowe

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Spectroscopy of HR 8799

Spectroscopy of HR 8799

• Full mode determination is impossible with broad-band photometry only (sensitive to small values of l)

• The determination of both l and m requires high resolution, high signal-to-noise spectroscopic monitoring

• Full mode determination is impossible with broad-band photometry only (sensitive to small values of l)

• The determination of both l and m requires high resolution, high signal-to-noise spectroscopic monitoring

HJD 2449957 +

181.24185.26185.27185.29187.25397.59399.64401.56402.64403.53404.54406.56407.51410.52435.40436.41441.43448.45449.57470.44522.35524.29525.25530.31531.28

Spectroscopy of HR 8799

Spectroscopy of HR 8799

• Mathias et al. (2004)• Mathias et al. (2004)

a)a)

b)b)

• Zerbi et al. (1999)• Zerbi et al. (1999)

Multi-Site CampaignMulti-Site Campaign

OAO (JPN)OAO (JPN)

Lick (USA)Lick (USA)

DAO (CND)DAO (CND)

OHP (Fr)OHP (Fr)

Mercator (Es)Mercator (Es)

Taut (D)Taut (D)

+ many others+ many others with ROB!with ROB!(e. g. Xinglong, (e. g. Xinglong, BAO, La Silla, …)BAO, La Silla, …)

Multi-Site CampaignMulti-Site Campaign

• Continuous monitoring - 2 weeks

• Time span over ~2 years!!!– R=50-60 000 on ~4000-8000 Å

• Continuous monitoring - 2 weeks

• Time span over ~2 years!!!– R=50-60 000 on ~4000-8000 Å

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Multi-Site CampaignMulti-Site Campaign

•15-day sample of contig. obs.

(OAO, Lick, Taut., DAO)

•15-day sample of contig. obs.

(OAO, Lick, Taut., DAO)

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Multi-Site CampaignMulti-Site Campaign

• Using only ~900 spectra obtained last September (many more spectra to come)

• Using only ~900 spectra obtained last September (many more spectra to come)

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The model(s)The model(s)

• Nothing that I can present yet…

– Two teams are working on it.

• Nothing that I can present yet…

– Two teams are working on it.QuickTime™ and a

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The model(s)The model(s)

• Fairly well studied

• Inclination must be small (<20˚)

• Fairly well studied

• Inclination must be small (<20˚)

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The model(s)The model(s)

• Shows X-ray variations!!!– Due to stellar spots?

• Shows X-ray variations!!!– Due to stellar spots?

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(Robrade & Schmitt 2010)

The modelsThe models

• Moya (s) et al. 2010:• Moya (s) et al. 2010:

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Moya (s) et al. 2010Moya (s) et al. 2010

What they prefer At the limit

What they prefer At the limit

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Chené et al. 2010…Chené et al. 2010…

Stay tuned!Stay tuned!

The ENDThe END

Thank you very much

Thank you very much

André-Nicolas Chené (NRC/HIA/CGO)

~35 co-authors…André-Nicolas Chené (NRC/HIA/CGO)

~35 co-authors…