planetary transits and oscillations of stars · planetary transits and oscillations of stars...
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PLATO PLAnetary Transits and Oscillations of Stars revealing the interior of planets and stars completing the age of planet discovery for Earth-sized planets constraining planet formation Heike Rauer and the PLATO team The PLATO Consortium: 501 members from 23 countries (European, Brazil, US, Chile, Canada, Australia)
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Techniques: - photometric transits - asteroseismology - ground based spectroscopy for radial velocity
PLATO : - very large samples of bright stars - continuous photometric monitoring from space, in the visible - ultra-high precision - very wide field
The PLATO mission
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Accuracy for an Earth around a solar-like star: * planet radius up to 2% * planet mass up to 10% * age known to 10% And much better for larger planets!
Example: Kepler-10b
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PLATO current status
• PLATO consortium applied to ESA to enter the M3 competition. • PLATO already finished mission studies during M2 competition. • The PLATO consortium will be re-adjusted to fit the M3
timeline (launch 2022/24) • The science case is refined in the context of the 2022/24
launch perspective, taking into account recent Kepler and rv-survey results
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Planet Detections
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Planet Detections
Focus of interest for future space-based transit missions: Detect terrestrial planets up tp the HZ of solar-like stars
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Planet diversity
Fressin et al. 2011 Gautier et al. 2012
• Future transit surveys need to • detect Earth-sized planets • characterize their radius and mass with high accuracy
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Planet diversity
Planets and moons in the Solar System
Meaningfiul constraints on planet interior require High accury on radius (2%) and mass (10%)
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Planet diversity and planet formation
Rocky and icy planets
Gas giants
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Planet diversity and planet formation
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Planets larger than the critical mass accrete H, He and develop into gas giants.
Planet diversity and planet formation
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Planets larger than the critical mass accrete H, He and develop into gas giants.
Planet diversity and planet formation
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Planet free region?
Planet diversity and planet formation
Our current understanding of planet formation predicts fast gas envelope accretion beyond 10-15 Mearth
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Circles: upper mass limits available only! Real planet masses are likely to be much lower.
Planet diversity and planet formation
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• Do massive rocky planets exist? • What is the critical mass for giant planet formation? • Does it depend on the disc (e.g. dust/gas ratio)?
? Objects with upper mass limits only orbit faint stars (~15 mag). Need to observe brighter stars.
Planet diversity and planet formation
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• What is the diversity of Earth-sized planets? • Does it depend on orbital distance, stellar type, etc.?
?
Objects with upper mass limits only orbit faint stars (~15 mag). Need to observe brighter stars.
Planet diversity and planet formation
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PLATO
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Selection of science cases: • Detect Earth-sized planets in the habitable zone with known radii
and masses, including planets orbiting solar-like stars.
• Obtain statistical significant numbers of characterized small planets at different orbits, stars, …
• Determine the critical mass for gas giant growth
• Study planet interior composition and structure including terrestrial objects
• Study planetary systems
• Determine accurate ages of planet systems
• Provide small terrestrial planets around bright stars as targets for atmosphere spectroscopy
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Currently little overlap between current transit and rv surveys
• Planet radii are obtained by transit observations
• Planet masses can be
derived by radial velocity measurements
• Transits are detected in broad-band (white light) photometry
• Radial velocity measurements require high-resolution spectroscopy –> much tighter limit on target brightness
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Currently little overlap between current transit and rv surveys
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Need to detect transiting planets around bright stars!
Provide targets for
spectroscopy characterization!
Region of interest for atmosphere characterization
Currently little overlap between current transit and rv surveys
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PLATO instrumental concept - 32 « normal » cameras :
cadence 25 sec - 2 « fast » cameras : cadence 2.5 sec, 2 colours - pupil 120 mm
- dynamical range: 4 ≤ mV ≤ 16
Very wide field + large collecting area : multi-instrument approach
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Organization of Groundbased follow-up
Tautenburg 2m OHP 2m
Mercator 1.2m
NOT 2.5m
ESO 2.2m
Euler 1.2m
US: several 2m
1-2m-class telescopes: 3-10m/s giant planets on short/medium orbits 100 nights/year x 6 years 6 telescopes
HARPS ESO 3.6m
HARPS-N TNG 3.5m
NTT 3.5m AAT 4m
4m-class telescopes: 1-2 m/s giant planets on long orbits super-earths on short/medium orbits 100 nights/year x 6 years 4 telescopes
Espresso VLT 8m
HET 10m
Keck 10m
GTC 10m
8m-class telescopes: < 50cm/s super-earths on long orbits, earths on short/medium orbits earths on long orbits @ brightest stars 40 nights/year x 6 years 1 telescope
Carmenes CA 3.5m
Crires VLT 8m
Spirou CFH 3.6m
Infrared facilities: 1-2 m/s earths around late K - M dwarfs 40 nights/year x 6 years 3 telescopes
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Current transiting planet findings
- high accuracy determination of radius and mass - bright hosts stars - very few such targets expected from Kepler
Confirmed planets and Kepler candidates
Kepler candidates are above mV=11 RV confirmation is very difficult no confirmed earth-like planet in HZ expected from Kepler
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PLATO planets versus current transiting planet findings
- high accuracy determination of radius and mass - bright hosts stars - very few such targets expected from Kepler
PLATO confirmed planet yield for <11mag PLATO will provide a large sample of terrestrial planets, down to Earth size, with highly accurate mass and radius around bright stars up to the habitable zone.
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Magnitude range of PLATO planets
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The PLATO legacy - a huge sample of characterized planets with known mass, radius and age, including terrestrial planets in the HZ of solar-like stars
- planets surrounding stars bright enough for detailed follow-up
pioneers true comparative planotology and taxonomy of planet systems
A huge complementary science program:
- 1,000,000 of high-precision photometric stellar lightcurves
- 85,000 of these stars will allow for astroseismic characterization
- in synergy with Gaia: mass, age, rotation, distance, luminosity, radius
a breakthrough in stellar physics (e.g. stellar structure and evolution, internal mixing processes, stellar rotation, ages of globular clusters, young open clusters)
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PLATO Selection of science cases: • Detect Earth-sized planets in the habitable zone with known radi
and masses, including planets orbiting solar-like stars.
• Obtain statistical significant numbers of characterized small planets at different orbits, stars, …
• Determine the critical mass for gas giant growth
• Study planet interior composition and structure including terrestrial objects
• Study planetary systems
• Determine accurate ages of planet systems
• Provide small terrestrial planets around bright stars as targets
for atmosphere spectroscopy