Transcript Ground support for MONS/COROT from OSN

PlanetVision: Belgian-Spanish
project for the characterization of
planetary systems, stars and
planets
A. Moya and H. Deeg et al. (Spain)
C. Aerts and J. De Ridder et al. (Belgium)
N. Santos et al. (Portugal)
H. Kjeldsen et al. (Denmark)
L. Kiss et al. (Hungary)
General context
1) Understand the origin and structure of the
diversity of planetary systems found
2) Is there life outside the Solar System?
3) Steps planned already:
I. Search for exoplanets
II. Accurate characterization of these
systems, habitability studies
III. Search for biomarkers
“An European roadmap for
exoplanets” (Exoplanet Roadmap Advisory
Team, October 2010)
History of project
1) 2010/11: informal discussions in Spain to lead
space project, topic exoplanet & astero science
(Andy Moya & Hans Deeg + industrials)
2) Contact with C. Aerts in June 2011 to consider
bilateral project: PlanetVision as answer to future
S-mission call of ESA
3) First specs defined over summer (incl. Joris
De Ridder, CoRoT and Kepler heritage)
4) Delegations + ESA meet in Madrid & Brussels,
Oct. 2011, Jan. 2012
5) 2011/12: Discussions with Swiss-led consortium
but mission concepts judged too ≠
Current situation
~ 700 exoplanets known
First planets touching habitable zone
found in 2010 and 2011
Current situation
~ 600 discovered from ground
~ 450 discovered with RV (poor information)
~170 with transits: mass, size, etc. known:
1) ~ 50 from space (high accuracy)
2) ~ 120 from ground (low accuracy)
The focus in exoplanets is changing
from discovering to understanding.
Current research issues
a) Exoplanet’s nature: density, surface properties,
atmospheric properties
b) Planetary orbits: Historical evolution, effects
due to other bodies
c) Host stars: Evolution, chemical composition,
accurate physical characteristics
There is only one thoroughly studied
case: The Solar System.
Current situation
Transits
2
F RP 



F 
R
 *
Direct imaging
(age)
Radial
Velocity
M

P

RV
f
M
 *
Current situation
Homogeneous studies of transiting extrasolar
planets. IV. Thirty systems with space-based
light curves
Southworth, J., 2011, arXiv:1107.1235
Mean errors
M*
R*
ρ*
Age
Mp
Rp
9,3%
7%
13.7%
150%
10.6%
7.1%
Errors of MP and RP dominated by errors of M* and R*
Current situation
Almost a 47% have mV<8, a 72% have mV<10
PlanetVision:
Scientific
project
Scientific project
Data acquisition technique:
Observation of temporal series of
high-precision multicolor photometry
Scientific project
Scientific methods:
1)Exoplanet science: Led by Spain
1) Asteroseismology: Led by Belgium
Goal: Bright stars with planets
(Specs defined for mv<8)
Exoplanet’s photometry: Transits, eclipses,
reflected light
PlanetVision complements space
observations (CoRoT, Kepler) and improves
ground-based observations
- Consistent high-precision photometry in 3 color
bands for bright targets (cf. EChO preparation)
- Long observations with high duty cycle
- flexibility in targets to observe:
· Large range of brightness admissible,
· Entire sky accessible,
· High temporal resolution possible
Exoplanet’s photometry: Transits, eclipses,
reflected light
The more transits are observed, the greater
the accuracy of the characterization
Exoplanets science: Objectives
1) Characterization of planetary systems
already known
A.
B.
C.
D.
Improving planet and star system parameters
Studies about the planet atmospheres
Detection of further bodies in transiting systems
Studies on planet host stars
2) Discovering of new planets
A. Verification of candidates coming from other
instruments
B. Direct discovery of new transits
Exoplanets science: Objectives
3) Study of planets WITHOUT known transits
A. Detection of reflected planetary light
B. Search for transits of RV planets
High precision photometry with at least three
different photometric bands, pointing flexibility,
very high duty cycle.
Asteroseismology
Something similar happens in the stars
Asteroseismology
Real cases
From Asteroseismology
μ Arae
Very accurate determination Y=0.30±0.01, Age=6.3±0.8 Gyr
From asteroseismology
•1 planet (Transit)
•Kepler observations
•solar-like modes
Work:
Christensen-Dalsgaard et al.,
2010
Age=2.14 ± 0.26 Gyr
Mean density=0.2712 ± 0.0032 g cm-3
Uncertainty Rp changes
3% → 0.5%
From asteroseismology
Precision obtained with Kepler
An uniform asteroseismic analysis of 22
solar-type stars observed with Kepler
Mathur et al., 2012, A&A, in press
Individual
frequencies not
resolved
Individual
frequencies
resolved
Mass
5%
1%
Radius
2%
1%
Age
10%
2.5%
Asteroseismology: Objectives
Precise stellar densities permit improvement of
planet parameters
1) Accurate characterization of the physical
properties of the star (mass, radius, age,
chemical composition,…)
2) Improve our understanding of the stellar
structure and evolution
3) Understand the planetary systems origin and
evolution
4) Discovering new planets (timing)
Asteroseismology
Consequences of observing stellar pulsations
Error
(with asteroseismology + Gaia)
Preliminary requirements
1) Photometric precision of 50 ppm with
integrations of 10 min, stars mv<8
2) To be able to monitore any position in the sky
at least at once during the year
3) Flexible duration of the monitoring between 3
hours and 3 months
4) Three well separated photometric bands
5) FOV > few to tens of sq deg (tbd)
6) Temporal resolution as short as 1s should be
available
7) Duty cycle > 90% (95%), minimizing periodic
gaps between 0.002-10 mHz
8) High dynamic range
Preliminary design
Payload:
1) 3-6 Telescopes (tbd)
2) 15-30 cm primary each (tbd)
3) Backside-illuminated CMOS + NIR
detectors, each telescope separately
Specs and observing strategy, field
selection, all to be
fine-tuned using the PLATO simulator tool
(already developed in Leuven)
Preliminary observation strategy
Dedicated observations for individual objects
or small groups
Platform: Ingenio
Ingenio is a mission for the
optical observation of the Earth.
This mission has already almost all the
required characteristics (pointing, size, cost,
data transmission, etc.)
Orbit: Likely an ETO, as
Kepler, Spitzer,...
Platform: Ingenio
~2.5 m
1.5 m
Dimensions
1.5 m
Approximate weight:
800 kg
Time schedule
phase
t0
t0+1
+2
+3
+4
+5
+6
+7
0/A
B
C/D
Laun.
Exploit.
= expected launch of M3 (approx)
+8
+9
+10
Phase 0 objectives
1. Scientific consortium consolidation
2. Accurate determination of the
scientific requirements
3. First approach to the satellite system
Phase 0 main actions
1. Direct contacts
2. Workshop
3. Technical support.
PlanetVision
in context:
other
missions
The project in context
Main objective: Accurate determination of
physical properties of planets already
discovered from ground.
Main characteristics:
1)Pointing flexibility
2)Different photometric bands
Unique project at the present time
PlanetVision in context: other missions
Future space projects: EChO and Plato
PLAVI is needed by EChO, since they need accurate physical properties
of the planets they plan to study.
PLAVI will deliver the much needed bright tarjets for EChO
The Spanish
and Belgian
scientific
communities
Belgian scientific community
Exoplanetary science and asteroseismology
ROB (Peter de Cat)
ULg (M.A. Dupret)
ULB (Alain
Jorissen)
BISA (Frank
Daerden, Severine
Robert)
Some 50
Belgian
scientists
KUL (Conny Aerts,
Joris De Ridder)
FUNDP (Anne
Lemaitre)
Spanish scientific community
Exoplanetary science and asteroseismology
U Vigo (Ana Ulla)
ICE, CSIC (M. LópezMorales)
CAB, INTA-CSIC (Andrés Moya,
David Barrado, Miguel Mas,
Enrique Solano)
UV (Juan Fabregat)
Some 40
Spanish
scientists
IAA, CSIC (Rafael Garrido,
J.C. Suárez, P.J. Amado)
IAC (Hans Deeg
and Pere Pallé)
Portuguese, Danish and Hungarian
scientific communities
CAUP (Mario Monteiro,
Nuno Santos)
University of Aveiro
(Alexandre Correia,
Helena Morais)
University of Århus (Hans
Kjeldsen, Joergen
Christensen-Dalsgaard)
Observatory of Konkoly
(Laszlo Kiss, Robert
Szabo)
Thanks!