exoplanet science
DESCRIPTION
Exoplanet Science. Don Pollacco QUB. Overview. PLATO’s objectives and space Work packages in the definition phase Timescales and aims of the definition phase. PLATO Space. Exoplanet Objectives. Detection and Characterisation of Earth Analog systems - PowerPoint PPT PresentationTRANSCRIPT
Exoplanet Science
Don Pollacco QUB
Overview
• PLATO’s objectives and space
• Work packages in the definition phase
• Timescales and aims of the definition phase
PLATO Space
Exoplanet Objectives• Detection and Characterisation of Earth Analog systems
• Search for exoplanets around the brightest stars of solar type at all orbital periods and with all physical sizes
• Search for exoplanets around nearby M-type dwarfs with all physical sizes and at all orbital periods, including at orbital distances such that these planets fall within the habitable zones of these very cool stars
• Search for and characterization of exoplanets with a wide variety of sizes, masses and orbits around bright stars
• Full characterization of very bright stars, of all masses and ages, using seismic analysis
5
Reminder: Planet diversity
• Transit fractional radius (relative to host star) inclination.
• RV planetary mass
• 2 solid planets: - CoRoT-7b : Period ~ 0.85 d - MEarth-1b: Period ~ 1.50 d
=> Diversity
Transiting planets
Rad
ius
(Ear
th U
nits
)
ESA Cosmic Vision Dec 1 2009 PLATO: PLAnetary Transits and Oscillations of stars
CoRoT, M-Dwarf surveys
PLATO Planets
• Bright hosts => can be used for many types of follow-up eg atmospheric analysis
• Planets around the nearest hosts (eg 5th Mag G stars, M dwarfs etc) will be prized targets – maybe even direct imaging/spectroscopy
• Bulk composition and diversity
Definition Work Structure
• Structure based on CoRoT, Kepler and ground based experiences/discussions
• Work Packages are mix of mission (eg algorithm development/specification) and “pure” science
• In general recognized experts involved
Exoplanet ScienceD.Pollacco
Exoplanet ScienceD.Pollacco
Light Curve FilteringA.Lanza
Light Curve FilteringA.Lanza
Planet Detection MethodsJ.Cabrera
Planet Detection MethodsJ.Cabrera
Planet Candidate RankingM.Deleuil
Planet Candidate RankingM.Deleuil
Transit Fitting Tools
M.Gillon
Transit Fitting Tools
M.Gillon
PLATA Data Specific Science
D.Pollacco
PLATA Data Specific Science
D.Pollacco
PLATO Interpretation Specific Science
H.Rauer
PLATO Interpretation Specific Science
H.Rauer
Interface to Other WP and PDC
N.Santos
Interface to Other WP and PDC
N.Santos
110 000
111 000 112 000 113 000 114 000 115 000 116 000 117 000
Astrophysical NoiseS.Aigrain
Astrophysical NoiseS.Aigrain
Residual Instrumental
NoiseF.Faedi
Residual Instrumental
NoiseF.Faedi
111 100
111 200
General Planet detection Tools
J.Cabrera
General Planet detection Tools
J.Cabrera
Reflected Light detection
I.Snellen
Reflected Light detection
I.Snellen
Single Transit detectionD.Pollacco
Single Transit detectionD.Pollacco
Other detection methodsR.Silvotti
Other detection methodsR.Silvotti
Ranking ProceduresA.Cameron
Ranking ProceduresA.Cameron
False Positive identification
M.Deleuil
False Positive identification
M.Deleuil
Astrophysical mimics
A.Cameron
Astrophysical mimics
A.Cameron
Transit modeling
S.Csizmadia
Transit modeling
S.Csizmadia
Orbital parameters
M.Deleuil
Orbital parameters
M.Deleuil
112 100
112 200
112 300
112 400
113 100
113 200
113 300
114 100
114 200
Multi-body Systems
S.Desidera
Multi-body Systems
S.Desidera
Planet-Star interaction
S.Mathis
Planet-Star interaction
S.Mathis
M-dwarfs as planet hostsP.Wheatley
M-dwarfs as planet hostsP.Wheatley
Planetary System Characterisation
A.Sozzetti
Planetary System Characterisation
A.Sozzetti
Spectroscopic Noise sources
C.Watson
Spectroscopic Noise sources
C.Watson
Environments of HZ planetsH.Lammer
Environments of HZ planetsH.Lammer
Atmospheres of planetsF.Selsis
Atmospheres of planetsF.Selsis
Mass-Radius Terrestrial
planetsF.Soht
Mass-Radius Terrestrial
planetsF.Soht
Planet formation and orbital evolution
R.Nelson
Planet formation and orbital evolution
R.Nelson
Mass-Radius Gas Giants
T.Guillot
Mass-Radius Gas Giants
T.Guillot
115 100 116 100
115 200
115 300
112 500 116 500
115 400
116 200
116 300
116 400
Light Curve filtering
Concerned with identification and filtering of astrophysical noise (spots etc) and any residual instrumental noise
Transit Detection
Much work already done
Need to optimize and apply to more unusual situations (multi-body systems)
Examine timing capabilities and parameter space
Candidate Ranking
Given the pressure there will be on follow-up observations and in particular the RV facilities, then this is important.
Need to develop efficient ranking procedures
Transiting modelling
Extensive work already in the literature
But need to examine the validity of various techniques (eg small planet approximation) in the PLATO domain
“Near-data” sciencedevelopment
Science areas that will help either in modelling of PLATO related data (eg astrophysical noise effecting RV determination)
Science Interpretation
Areas of “pure” science that PLATO will impact on greatly.
There are (many) others….
Interface specifications
An extremely important work package
This specifies the requirements from other (non esp) areas needed to deliver the exoplanet parameters to the required level of accuracy
Definition Phase Aims• Very preliminary report to ESP PDC (for scaling
purposes) - asap
• Full (literature) review - April 2011. This is to update/inform documentation for implementation phase.
• Recommendations for improvements, developments and optimizations - December 2011