hr 8799 (hd 218396)
DESCRIPTION
HR 8799 (HD 218396). Observations with MOST + ground based multi-site campaign. André-Nicolas Chené (NRC/HIA/CGO) ~35 co-authors…. Collaborators. Belgium Peter De Cat (RBO) Duncan J. Wright (RBO) Connie Aerts (Leuven) Tijl Verhost (Leuven) Paul Beck (Leuven) Steven Bleomen (Leuven) - PowerPoint PPT PresentationTRANSCRIPT
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…