ESA-ESO Working Group on
Extra-solar Planets
Report and Recommendations
F. Kerber, ECF
10.06.2005
ESA-ESO WG: Extra-solar Planets
1
Joint Working Groups

Extra-solar Planets
–

Synergies between Herschel and ALMA
–

M. Perryman, O. Hainaut, June - Dec 2004
T. Wilson, in progress
Survey of the field:
–
–
–
review of methods used and envisaged
survey of associated instrumentation
summary of targets, capabilities, limitations
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ESA-ESO WG: Extra-solar Planets
F. Kerber, page 2
Composition





Chair:
Michael Perryman (ESA)
Co-chair:
Olivier Hainaut (ESO)
Members:
Dainis Dravins (Lund), Alain Léger (IAS), Andreas
Quirrenbach (Leiden), Heike Rauer (DLR)
ECF support: Florian Kerber, Bob Fosbury
Experts: François Bouchy (Marseilles, COROT), Fabio Favata (ESA,
Eddington), Malcolm Fridlund (ESA, Darwin, GENIE), Roberto Gilmozzi
(ESO, OWL), Anne-Marie Lagrange (Grenoble, Planet Finder), Tsevi
Mazeh
(Tel Aviv, Transits), Daniel Rouan (Meudon, GENIE),
Stephane Udry (Genève, Radial velocity), Joachim Wambsganss
(Heidelberg,Microlensing)
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Section 1: An Introduction

Objectives of the searches:
– characterising and understanding the planetary population
– understanding the formation and evolution of planets
– search for biological markers and life

Survey methods:
– radial velocity, astrometry, photometry, direct imaging, microlensing,
miscellaneous

Accuracy limits from ground and space:
– photometry/astrometry: atmosphere; granular flows and star spots
– radial velocity: atmospheric circulation and oscillations
– conclusions: fundamental limits are not yet firmly understood
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Section 1: Current status

Statistics (Dec 2004):
– 135 planets, 119
systems (12 multiple, 2
triple, 1 transiting)
– five additional
confirmed transits:
OGLE/TrES + 1
microlensing
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1997 ESO Working Group (App: C)

Radial Velocity
–
–

Narrow angle astrometry
–

VLTI: ATs and PRIMA
Microlensing
–
–

Dedicated spectrograph with 1 m/s (HARPS)
Iodine cell for UVES, extension to IR: CRIRES
Dedicated 2.5 m on Paranal (VST)
16k x 16k CCD (OmegaCam)
Direct Detection
–
High order AO/coronograph (Planetfinder)
Paresce, Renzini et al. 1997
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Period 2005-2015: Ground

Radial velocity: 18 surveys, targeting 1 m/s
•
•
•
•

HARPS: leading instrument for radial velocity work
promises to reach a few Earth mass planets
will follow-up COROT detection
ESO: UVES, CRIRES: extension to IR
Transit surveys: 30 surveys ongoing
• results are expected to accelerate as temporal baseline increases
• four discoveries using 1.3-m OGLE; 1 with 10-cm TrES-1

Imaging/other:
• ESO activities: NAOS-CONICA, PRIMA, VLTI, Planet Finder, ALMA
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Summary of Prospects 2005-15 (Tab 5)
Mass
(Jupiter)
2004
2010
Radial Velocity
(ground)
2010
2008
2010
2015
2016
2016
Transits
(ground)
COROT
Kepler
SIM
Gaia
(astrom)
Gaia
(photom)
1-10
90
250
1000
5-15
20000
200
15000
3000
0.1-1
30
200
0
50-150
10000
50
5000
0
0.01-0.1
0
20
0
10-30
1000
20
0
0
< 0.01
0
0
0
0-3
0-500
0-5
0
0
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2015-2025: 100-m OWL


S/N=10: imaging (35 mag, 1 hr); spectroscopy (30 mag, 3 hr)
Detectability considers:
–
–
–
–
target Strehl ratios of 90% over 1-5 m
magnitude/separation (Table 6); planet detectable if beyond 5/D
number of target stars calculated from D
integration time  D– 4 (hence 30 m : 100 m = 123 times longer)
D(m)
30
60
100
Earth-like
Jupiter-like
Imaging
Spectroscopy
Imaging
Spectroscopy
d (pc)
10
0
70
5
N (stars)
22
0
6800
3
d (pc)
22
0
120
18
N(stars)
210
0
35000
170
d (pc)
40
15
500
35
1200
67
2500000
860
N(stars)
2015-2025 - Space: Darwin

Darwin (4 telescopes with B = 50–100 m):
– infrared: contrast, sample size, biomarkers, technology precursor
– detection phase: 2 years; spectroscopy follow-up: 3 years
– targets: 200 nearby stars covering CO2, H2O, O3, CH4

Integration times (hr): detection at S/N = 5, spectra at S/N = 7:
Stellar type
10 pc
20 pc
30 pc
G2V
18-33
28-54
109-173
K2V
4-9
26-37
104-157
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2015-2025 - Space: Darwin
• GENIE:
– nulling interferometer developed by ESO-ESA for VLTI
– targets the demonstration of technology required for
Darwin, and…
– scientific pre-cursor for Darwin survey (zodiacal
emission) in southern hemisphere
– will require of order 50 nights on UTs or ATs at 3.6 m
– operational by mid-2008?
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TPF and Beyond

TPF (NASA, April 2004):
–
–
–
–

6–8  3.5 m2 coronograph over 0.6–1.06 m in 2014
full search: 32 nearby stars, incomplete search 80–130 stars
free-flying interferometer, with ESA, before 2020
scientific and technical precursors: listed in Appendix A
Beyond 2025 (Appendix B):
– larger ‘life finders’ for improved S/N spectroscopy
– planet imagers (resolution of surface): distant visions only
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ESA Themes Beyond 2015

Astronomy Working Group, 19 October 2004:
– recognition of roles of COROT and Gaia
– confirmation of Darwin-type mission around 2015
– next steps: census of terrestrial planets within 100 pc, e.g.
astrometry
– re-iterates support of a rapid implementation of Eddington
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Schedule of Some Major Facilities
2004
2000
Corot
2008
2012
2016
2020
Kepler
Gaia
SIM
TPF-C
TPF/Darwin
Very large telescopes
(CELT, OWL)
Europe
US
Very large space
arrays
Detections and Follow-Up

Two types of planets (cf Figure 7):
– high-mass (Jupiter), where follow-up is ‘easy’
• large numbers: thousands to tens of thousands over 2008–2015
• ground radial velocity and transit surveys
• space transit surveys (Kepler) + astrometry and photometry (Gaia)
– low-mass (up to a few Earth mass), where follow-up is
problematic:
• from COROT and Kepler
• TPF-C general instrument ?
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ESA-ESO WG: Extra-solar Planets
F. Kerber, page 15
Detections and Follow-Up

Provides statistics of high-mass, low-mass, nearby stars:
– particularly important for Darwin preparations

Detections by method X, require follow-up by methods Y and Z:
–
–
–
–
–
rejection of false positives
characterisation of mass
transit spectroscopy - transit photometry
role of amateurs: TrES-1 observed by 5 groups, some sequential P=3.04d
multiple observations of transits: timing >> detection of lesser mass planets in
systems (Holman & Murray 2005)
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ESA-ESO WG: Extra-solar Planets
F. Kerber, page 16
Detections and Follow-Up
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Astrophysical Characterisation: Host Stars


Thousands of planetary systems should be known by 2010-15
Characterisation for formation/evolution requires (Section 4):
–
–
–
–
–
–


photometry: Teff, log g, metallicity, micro-variability (Gaia, LSST, etc)
spectroscopy at R = 20–60,000: Teff, log g, [Fe/H] (Section 4.4.1)
spatial distribution, kinematics, environment, e.g. wrt LSR (Gaia)
kinematic radial velocities, probably improved compared to Gaia
improvement in some fundamental physical data – VO (Section 4.7.1)
fundamental planetary data (Section 4.7.2)
Some of the necessary follow-up and characterisation studies will
be undertaken through the normal development of the field
Some may benefit from pro-active effort by ESA and ESO
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ESA-ESO WG: Extra-solar Planets
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Recommendations (1/3)
1. ESA:
1. Eddington: provide clear message to community
2. Gaia: impact on field is a strong function of
accuracy
3. Darwin: phase development with TPF-C in 2014
4. JWST: importance of transit capabilities
5. Themes 2015: encourage innovative mission
proposals
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Recommendations (2/3)
2. ESO:
1.
2.
3.
4.
Improve radial velocity detection limits
Spectroscopic survey of nearby host stars
Improve visible/infrared transit instrumentation
Evaluate follow-up needs on small to large
telescopes
5. Consider OWL as a search / follow-up facility
6. Investigate astrometric capabilities of OWL
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F. Kerber, page 20
Recommendations (3/3)
3. ESA-ESO Joint Initiatives:
1.
2.
3.
4.
5.
6.
7.
8.
Radial velocity follow-up of COROT/Kepler candidates
Radial velocity follow-up of Gaia candidates
Photometric transit monitoring of high-mass candidates
Observing time support for preparatory observations
Consider GENIE-like instrument at Dome C
Coordination of amateur networks for transits
Cooperation of solar system and exoplanet communities
Coordinate public communication discovery aspects
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Implementation: first steps

Rec. 2.2 Spectral survey of nearby host stars
– Estimate of time required
– Draft implementation plan
Faculty meeting, 10.06.2005
ESA-ESO WG: Extra-solar Planets
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Implementation: first steps

Rec. 2.5/2.6 OWL as search/follow-up facility
– ESO: Instrument concept studies; D’Odorico
– T-OWL: thermal IR imager (spectrograph)
• Lenzen (MPIA Heidelberg), Käufl (ESO)
– EPICS: NIR Camera-Spectrograph
• Hubin (ESO), SWG (Chair/Co-chair: Kasper, Kerber)
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Implementation: first steps

Rec. 3.6 Amateur Network
for transits (section 4.7.3)
– Cost efficient way to increase
follow-up capabilities
– Interesting hook for outreach
– Contact with amateur groups;
AGAPE (ESO)
– Draft project plan available
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ESA-ESO WG: Extra-solar Planets
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Implementation: first steps

Rec. 3.1, 3.4 COROT/Kepler preparatory obs &
follow-up
– Request from ESA received for COROT
– Analysis of requirements from COROT underway
– NASA-ESA WG Planet Finding Data Archive (Kerber)
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CoRoT

CNES (plus partners), launch Q3 2006
– Asteroseismology and Extra-solar planets
– FOV 2.6º, Galactic (anti-)center for 5 months, 5000-10000
target stars, high sampling rate (512s)
– accuracy: 7·10-4 at V=15 mag in 1 hr > transits of rocky
planets (a few 10s)

Need for characterization of fields and follow-up
– Photometry, Spectroscopy, RV measurements
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ESA-ESO WG: Extra-solar Planets
F. Kerber, page 26
Available at ESO and ESA websites:
http://www.eso.org/gen-fac/pubs/esaesowg/
http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=36935
astro-ph/0506163
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F. Kerber, page 27