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Extrasolar Planets & The Power of the Dark Side. David Charbonneau California Institute of Technology www.astro.caltech.edu/~dc. Fermilab – 24 April 2002. Gravitational Wobble. Gravitational Wobble. First Planet Detected 51 Pegasi – November 1995. - PowerPoint PPT Presentation
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Extrasolar Planets &Extrasolar Planets &The Power of the Dark SideThe Power of the Dark Side
David CharbonneauDavid Charbonneau
California InstituteCalifornia Institute
of Technologyof Technology
www.astro.caltech.edu/~dcwww.astro.caltech.edu/~dc
Fermilab – 24 April 2002
Gravitational WobbleGravitational Wobble
Gravitational WobbleGravitational Wobble
First Planet DetectedFirst Planet Detected51 Pegasi – November 199551 Pegasi – November 1995
First Planet System DetectedFirst Planet System DetectedUpsilon Andromedae – April 1999Upsilon Andromedae – April 1999
Used with permission of the artist.
The Radial Velocity SurveysThe Radial Velocity Surveys
Masses of Extrasolar PlanetsMasses of Extrasolar Planets
Close-In Extrasolar Giant PlanetsClose-In Extrasolar Giant Planetsand Planetary Migrationand Planetary Migration
Protoplanetary DisksProtoplanetary DisksAround Young StarsAround Young Stars
D. Padgett (IPAC/Caltech), M. McCaughrean (A I Potsdam), C. Burrows (STScI), K. Stapelfeldt (JPL/Caltech)
Transits:Transits:A Little Closer To Home…A Little Closer To Home…
Where will you be June 8, 2004?
Transit CharacteristicsTransit Characteristics ProbabilityProbability
pptt = R = Rstarstar / a / a
= 0.1= 0.1
DepthDepthI / I = (RI / I = (Rplpl / R / Rstarstar))22
= 0.01= 0.01
PeriodPeriodP = 3 – 7 daysP = 3 – 7 days
DurationDurationt = 3 hourst = 3 hours
The Observational ChallengeThe Observational Challenge
The fraction of stars with transits is:The fraction of stars with transits is:
f = ff = fss f fMSMS f fCEGPCEGP p ptt
ffss = fraction of stars that are single = fraction of stars that are single = 0.5= 0.5
ffMSMS = fraction of those on the main sequence = fraction of those on the main sequence = 0.5= 0.5
ffCEGPCEGP = fraction of those that have a close-in planet = fraction of those that have a close-in planet = 0.01= 0.01
pptt = fraction of those with an inclination to transit = fraction of those with an inclination to transit = 0.1= 0.1
Need to look at 4000 stars to find 1 that transits.Need to look at 4000 stars to find 1 that transits. Need to sample often compared to transit duration.Need to sample often compared to transit duration. Need 1% accuracy for a 3Need 1% accuracy for a 3 detection of a 2 hour transit. detection of a 2 hour transit. Need to look on sky for at least 1 orbital period.Need to look on sky for at least 1 orbital period.
Require 1,000,000 15-minute samples Require 1,000,000 15-minute samples with 1% accuracy to detect one transit.with 1% accuracy to detect one transit.
The STARE ProjectThe STARE Project
Delivers high-cadence time series photometry on roughly 30,000 stars (9 < V < 13) in a typical field centered on the galactic plane.
We obtain sufficient precision on 5,000 stars to detect a close-in Jupiter-sized companion.
The Search Is On!The Search Is On!
The Benefits of a NetworkThe Benefits of a Network
HD 209458 bHD 209458 bThe First Transiting PlanetThe First Transiting Planet
The Effects of Stellar InsolationThe Effects of Stellar Insolation
Burrows et al. (2000)
The Effects of a Planetary CoreThe Effects of a Planetary Coreand Tidal Dissipationand Tidal Dissipation
Bodenheimer et al. (2001)
Radial Velocity with Orbit RemovedRadial Velocity with Orbit Removed
G. Marcy et al. (2000)
STARE PhotometrySTARE Photometryof HD 209458of HD 209458
HST STIS PhotometryHST STIS Photometryof HD 209458of HD 209458
Unphased HST STIS PhotometryUnphased HST STIS Photometryof HD 209458of HD 209458
Planetary SatellitesPlanetary Satellitesfrom Photometric Residualsfrom Photometric Residuals
Planetary SatellitesPlanetary Satellitesfrom Transit Timingfrom Transit Timing
Transmission SpectroscopyTransmission Spectroscopy
Brown (2001)
A Prediction of Sodium AbsorptionA Prediction of Sodium Absorption
Hubbard et al. (2001)
Detection of anDetection of anExtrasolar Planet AtmosphereExtrasolar Planet Atmosphere
STIS Transmission SpectrumSTIS Transmission SpectrumBANDPASSESBANDPASSES
STIS Transmission SpectrumSTIS Transmission SpectrumDATADATA
STIS Transmission SpectrumSTIS Transmission SpectrumDATADATA
STIS Transmission SpectrumSTIS Transmission SpectrumTHEORYTHEORY
STIS Transmission SpectrumSTIS Transmission SpectrumNEAR FUTURENEAR FUTURE
Reflected LightReflected Light
Combination of:Combination of: Transiting planet with a well-Transiting planet with a well-
determined value for the radiusdetermined value for the radius Excellent photometric Excellent photometric
precision with STISprecision with STIS Desire to measure the Desire to measure the
planetary albedo, pplanetary albedo, p
We have 20 orbits of STIS data (290 – 1030 nm) spanning 4 times of secondary eclipse. The photon noise limit of these data would permit a detection threshold of p = 0.1, averaged over the entire bandpass.
These data will allow us to quantify the net energy deposition into the planet.
The Kepler ProjectThe Kepler Project
The Kepler ProjectThe Kepler ProjectParameter SpaceParameter Space
The Kepler ProjectThe Kepler ProjectTechnology DemonstrationTechnology Demonstration
The Kepler ProjectThe Kepler Project