PLAnetary Transits and Oscillations of stars H. Rauer 1 , C. Catala 2 , D. Pollacco 3 , S. Udry 4 and the PLATO Team 1: Institut für Planetenforschung, DLR and TU Berlin 2: Observatoire de Paris, LESIA 3: Univ. Belfast 4: Obs. Geneva http://www.oact.inaf.it/plato/PPLC/Home.html M-class mission candidate in ESA Cosmic Vision Program;
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PLAnetary Transits and Oscillations of stars H. Rauer 1, C. Catala 2, D. Pollacco 3, S. Udry 4 and the PLATO Team 1: Institut für Planetenforschung, DLR.
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PLAnetary Transits and Oscillations of stars
H. Rauer1, C. Catala2, D. Pollacco3, S. Udry4 and the PLATO Team
1: Institut für Planetenforschung, DLR and TU Berlin2: Observatoire de Paris, LESIA
3: Univ. Belfast4: Obs. Geneva
http://www.oact.inaf.it/plato/PPLC/Home.html
M-class mission candidate in ESA Cosmic Vision Program;In competition for launch in 2018
PLATO Science Objective
> measurement of radius and mass, hence of planet mean density
> measurement of age of host stars, hence of planetary systems
Transits: Planetary Parameters• Key Tool
Mostly geometry
radius of planet/star, inclination.
Kepler’s 3rd law => semi-major axis
FF
RPlR
2
Only needed physics: limb darkening
Sun + Jupiter : ~ 1% dip Sun + Earth : ~ 0.01% dip
CoRoT 7bCoRoT 7bKepler 4bKepler 4b
GJ1214bGJ1214b
GJ436bGJ436b
Detection range of transit surveysDetection range of transit surveys
Space surveys
Ground-based
surveysTrES-4b
HAT-P-7b
HD149026b
CoRoT-2b
HAT-P-12b
HAT-P-11b
PLATO Survey of 1RE rocky planets in habitable zones of all late type stars
News:• Now includes M dwarfs• M stars lower intrinsic
brightness (local) and very red
• PLATO can work as faint as I~15-16 mag with little blending in most cases
• 6000 M stars per pointing • RV signal larger
Groundbased follow-up- Vigorous follow-up needed- Most important aspect = radial velocity monitoring
planet confirmation and mass measurement
Planet Distance (AU)
RV Amp. (m/s)
Jupiter 1 28.4
Neptune 0.1 4.8
Neptune 1 1.5
SuperEarth 0.1 1.4
SuperEarth 1 0.5
Earth 1 0.1
- stellar intrinsic « noise »: oscillations, granulation, activity- need to apply proper averaging technique- time consuming- in practice limited to bright stars
PLATO
CoRoT - Kepler
telescope diameter needed to confirm earth-like planet
Very wide field + large collecting area :multi-instrument approach
on board data treatment: 1 DPU per camera 1 ICU
optical field 37°
4 CCDs: 45102 18m « normal » « fast »
focal planes
FPA
356 mm
S-FPL51
N-KzFS11 CaF2(Lithotec)
S-FPL53
L-PHL1
KzFSN5
164.
6 m
m
optics
fully dioptric, 6 lenses
Orbit around L2 Lagrangian point, 6-year nominal lifetime
Concept of overlapping line of sights
4 groups of 8 cameras with offset lines of sightoffset = 0.35 x field diameter
8 8
8 8
16
16
16 16
2424
2424
32
Optimization of number of stars at given noise level AND of number of stars at given magnitude
37°
50°
Kepler
CoRoT CoRoT
Basic observation strategyObservation strategy:1. two long pointings : 3 years or 2 years2. « step&stare » phase (1 or 2 years) : N fields 2-5 months each
PLATO
PLATO
Kepler
CoRoT CoRoT
>40% of the whole sky !
Basic observation strategyObservation strategy:1. two long pointings : 3 years or 2 years2. « step&stare » phase (1 or 2 years) : N fields 2-5 months each
Assumptions:- each star has one and only one planet in each cell - planet is detected if a transit signal AND a radial velocity signal are measured- intrinsic stellar « noise » is taken into account
Expected number of confirmed planets
lower right corner of the (orbit,mass) plane = terrestrial planets in the HZ, not covered by Kepler, will be explored by PLATO thanks to its priority on bright stars
-
Wagner et al. 2009, also: Valencia et al. 2007
standard error bar
Compare exoplanets with predictions of models with various compositions and structures
error bar dominated by error of host stars characteristics
Impact of radius and mass measurement
-
Wagner et al. 2009, also: Valencia et al. 2007
5%
10%
10%
5%
maximum acceptable error bars
standard error bar
Compare exoplanets with predictions of models with various compositions and structures
Impact of radius and mass measurement
error bar dominated by error of host stars characteristics
- constraints on planet interiors- radii and masses atmospheres- diversity
-
Wagner et al. 2009, also: Valencia et al. 2007
5%
10%
10%
5%
maximum acceptable error bars
PLATO error bar
standard error bar
Compare exoplanets with predictions of models with various compositions and structures
Impact of radius and mass measurement
PLATO: compare Earth-like exoplanets with age scale of Earth
- precision better than timescale planet
evolution
- targets of future characterization
dated by PLATO (Earth-like, but also
Neptunes, hot Jupiters…)
Impact of age measurement
place exoplanetary systems in evolutionary context
MagnetosphereCarbon-silicate cycle
Oxygen riseOzone layer
Proto Earth
Objective: Detect and characterize planetary systems, particularly earth-like in habitable zone
Techniques: detection by transits + asteroseismology of host stars + ground based spectroscopy
Instrument: Multi-telescopes very wide field of view
Targets: > 20,000 bright cool dwarfs (noise < 2.7 10-5 in one hr) > 50,000 bright cool dwarfs (mv<11)
> 6,000 very nearby M dwarfs > 230,000 cool dwarfs (mv<13,noise < 8.0 10-5 in one hr )
Observing strategy: 2 long runs (2-3 years) + several short runs