transiting extrasolar planets recent progress, xo survey, and the future christopher j. burke
TRANSCRIPT
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Transiting Extrasolar PlanetsRecent Progress, XO Survey, and the Future
Christopher J. Burke
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Solar SystemHas Predominately
Circular Orbits
Top View
Side View
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Planet Formation
NASA/JPL-Caltech/R. Hurt (SSC)
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ExceptionsNon-circularEccentricity
PlutoSedna
Nasa/CaltechCourtesy of Windows to the Universe, http://www.windows.ucar.edu
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~200 Extrasolar Planets
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● >7% stars have Jupiter mass planets within 5 AU● 1.2% stars have Hot Jupiter planets● Most planets have a>1 AU
Fischer & Valenti 2005
Metallicity Correlation
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● Multi-planet systems common (>30%) Wright et al. (2006) ● Low mass planets more common than high mass planets.
●5.5 Earth mass planet Beaulieu et al. (2006)
NASA/JPL-Caltech/T. Pyle (SSC)
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How do you detect planets?Radial Velocity Technique
Only Measure Planet Mass
Doppler Shifted Light
©Think Quest
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flux
time
Transit Technique
Extrasolar Planet Detection
Δf = (Rp/R*)2
~1%
Measure Radius!!
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Charbonneau et al. 2006, Brown et al. 2001
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Core Dominated
Inflated Radius
70 Mearth
coreSato et al. (2005) & Fortney et al. (2005)
Difficult to explain
Charbonneau et al. 2006
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● Highly accurate radii● Stellar limb darkening
What do we learn fromTransiting Planets?
Dan Bruton
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HD 209458b
Knutson et al. (2006)
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● Highly accurate planet radii● Stellar limb darkening● Characterize planet atmosphere
Transmission spectroscopyNa, H, C, O detection HD 209458
Charbonneau et al. (2002), Vidal-Madjar (2003, 2004)
What do we learn fromTransiting Planets?
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Compare SpectraOut of Transit
In Transit Vidal-Madjar (2003)
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Vidal-Madjar (2003)
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● Highly accurate planet radii● Stellar limb darkening● Characterize planet atmosphere
Phased light curve – optical
What do we learn fromTransiting Planets?
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Albedo <0.25 Rowe et al. (2006)will soon reach ~0.1 limits
Hot Jupiter planets are dark!
Reflected Light
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● Highly accurate planet radii● Stellar limb darkening● Characterize planet atmosphere
Secondary Eclipse – IR Test planet atmosphere models
What do we learn fromTransiting Planets?
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NASA/JPL-Caltech/R. Hurt (SSC)
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Constrain atmosphere metallicity, clouds, redistribution of heat, perhaps CO & H
2O
Disentagling these effects may be difficult
Burrows et al. (2006)
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Motivated to find bright transiting planets
XO Transit SurveyPI Peter McCullough
Jeff ValentiKen Janes, Boston U
Jim Heasley, U of HawaiiChris Johns-Krull, Rice U
Extended Team Professionals & “Amateurs”
Ron Bissinger, CAMike Fleenor, TNCindy Foote, UTEnrique Garcia, SpainBruce Gary, AZ
Paul Howell, MEFranco Malia, Italy Gianluca Masi, ItalyTonny Vanmunster, Belgium
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Haleakala, Maui
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Baker Nunn Observatory 1957Built to track satellitesin particular Sputnik
www.ifa.hawaii.edu/users/steiger/post_cook.htm
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Today houses XO
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Every 10 min7.2o x 63o strip
10 cm aperture
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Why have so few transits been found?● Only 1.2% stars have Hot Jupiter planets● The probability for a Hot Jupiter to transit ~10%● Most stars are too big (sub-giant or giant)
In magnitude limited survey only 10% of stars are dwarfs Gould & Morgan (2003)
● There are many objects that mimica transit signal
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Transit ImpostersTransit surveys yield 10/1 false positives
● Dwarf star eclipsing a subgiant/giant● Grazing eclipsing binary● Triple star / blend diluted deep eclipse● Brown dwarfs
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Transit Imposters
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96 MJup
Brown dwarf same radius as planet!
Radial Velocity Followup Required!
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How does XO deal with imposters
Stellar spectral type estimate
Photometric catalogs - Tycho, 2MASS, TASS
Transit duration, depth, and periodconsistent with a planet orbiting the estimated stellar spectral type
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Closer stars Higher Proper Motion
1955 1993 2000
NASA/IPAC Infrared Science Archive
DSS1 DSS2 2MASS
Discriminate dwarfs from giants
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XO's Extended Team
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Blending
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Triple Stars
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XO has timeon the Hobby-EberlyTelescopefor precisionRV
ConfirmedXO-1bas a bona fideplanet
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Future of Extrasolar Planets
HARPS now achieves 20 cm/s RV stability over several days
ESO La Silla 3.6m
Pont priv. comm. (2006)
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Space Based Transit Searches
COROT – Launched Dec. 26
27cm primary2.5 year duration
150 day continuous
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KEPLER – Nov. 2008
1.4m primary4 year duration fully continuous42 CCDs to fill 1.2o diameter FOV
100,000 stars V<15.0
Space Based Transit Searches
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Precision Transit Timing
Sensitive to moons, rings, stellar spots
Can detect Earth mass planets in resonance
XO Future
XO-2b, XO-3b, XO-4b,...
Expansion to 3+ mounts in 2007