10.06.2005ESA-ESO WG: Extra-solar Planets1 ESA-ESO Working Group on Extra-solar Planets Report and Recommendations F. Kerber, ECF

10.06.2005 ESA-ESO WG: Extra-solar Planets 1

ESA-ESO Working Group on ESA-ESO Working Group on Extra-solar PlanetsExtra-solar Planets

Report and Recommendations

F. Kerber, ECF

Faculty meeting, 10.06.2005

ESA-ESO WG: Extra-solar Planets F. Kerber, page 2

Joint Working GroupsJoint Working Groups

Extra-solar Planets– M. Perryman, O. Hainaut, June - Dec 2004

Synergies between Herschel and ALMA – T. Wilson, in progress

Survey of the field:– review of methods used and envisaged– survey of associated instrumentation– summary of targets, capabilities, limitations



CompositionComposition

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)



Section 1: An IntroductionSection 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



Section 1: Current statusSection 1: Current status

Statistics (Dec 2004):– 135 planets, 119

systems (12 multiple, 2 triple, 1 transiting)

– five additional confirmed transits: OGLE/TrES + 1 microlensing



1997 ESO Working Group (App: C)1997 ESO Working Group (App: C)

Radial Velocity– Dedicated spectrograph with 1 m/s (HARPS)– Iodine cell for UVES, extension to IR: CRIRES

Narrow angle astrometry– VLTI: ATs and PRIMA

Microlensing– Dedicated 2.5 m on Paranal (VST)– 16k x 16k CCD (OmegaCam)

Direct Detection– High order AO/coronograph (Planetfinder)

Paresce, Renzini et al. 1997



Period 2005-2015: GroundPeriod 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



Summary of Prospects 2005-15 (Tab 5)Summary of Prospects 2005-15 (Tab 5)

Mass 2004 2010 2010 2008 2010 2015 2016 2016

(Jupiter) Radial Velocity

(ground)

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

2015-2025: 100-m OWL2015-2025: 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) Earth-like Jupiter-like

Imaging Spectroscopy Imaging Spectroscopy

30 d (pc) 10 0 70 5

N (stars) 22 0 6800 3

60 d (pc) 22 0 120 18

N(stars) 210 0 35000 170

100 d (pc) 40 15 500 35

N(stars) 1200 67 2500000 860



2015-2025 - Space: Darwin2015-2025 - 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



2015-2025 - Space: Darwin2015-2025 - 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?



TPF and BeyondTPF 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



ESA Themes Beyond 2015ESA 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

Schedule of Some Major FacilitiesSchedule of Some Major Facilities2000 2004 2008 2012 2016 2020

Gaia

TPF/Darwin

Very large telescopes(CELT, OWL)

Very large spacearrays

KeplerCorot

SIM

TPF-C

Europe

US



Detections and Follow-UpDetections 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 ?




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)






Astrophysical Characterisation: Host StarsAstrophysical 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



Recommendations (1/3)Recommendations (1/3)

1. ESA:1. Eddington: provide clear message to community2. Gaia: impact on field is a strong function of

accuracy3. Darwin: phase development with TPF-C in 20144. JWST: importance of transit capabilities5. Themes 2015: encourage innovative mission

proposals




2. ESO:1. Improve radial velocity detection limits2. Spectroscopic survey of nearby host stars3. Improve visible/infrared transit instrumentation4. Evaluate follow-up needs on small to large telescopes5. Consider OWL as a search / follow-up facility6. Investigate astrometric capabilities of OWL




3. ESA-ESO Joint Initiatives:1. Radial velocity follow-up of COROT/Kepler candidates2. Radial velocity follow-up of Gaia candidates3. Photometric transit monitoring of high-mass candidates4. Observing time support for preparatory observations5. Consider GENIE-like instrument at Dome C6. Coordination of amateur networks for transits7. Cooperation of solar system and exoplanet communities8. Coordinate public communication discovery aspects



Implementation: first stepsImplementation: first steps

Rec. 2.2 Spectral survey of nearby host stars – Estimate of time required

– Draft implementation plan

Fischer & Valenti 2005




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)




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




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)



CoRoTCoRoT

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



http://www.eso.org/gen-fac/pubs/esaesowg/

http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=36935

Available at ESO and ESA websites:

astro-ph/0506163

Documents

10.06.2005ESA-ESO WG: Extra-solar Planets1 ESA-ESO Working Group on Extra-solar Planets Report and Recommendations F. Kerber, ECF