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Astronomy Group, Department of Physics, University of Warwick
PMC SCIENCE MANAGEMENT
WORK PACKAGE DESCRIPTIONS
DEVELOPMENT
Name & Society
Prepared by
Date
Signature
1st September
2015
Don Pollacco
PSM Coordinator
David J. A. Brown
PSM Project Office
Approved by
Authorized by
ARCHIVING:
Heike Rauer
PLATO mission Consortium Lead
1st September
2015
1st September
2015
Don Pollacco
PSM Coordinator
Limited Diffusion
DOCUMENT HANDLED IN CONFIGURATION: No
Public x
PSM WPDs
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Table of Contents
PSM Coordination
PSM WP 100 000
12
PSM Project Office
PSM WP 101 000
13
PSM Coordination Team
PSM WP 103 000
14
Exoplanet Science Coordination
PSM WP 110 000
15
Coordination of Tools for Lightcurve Filtering
PSM WP 111 000
16
Specification of Tools for Lightcurve Filtering
PSM WP 111 100
17
Specification of Tools for Detecting and Filtering Residual Instrumental Noise
PSM WP 111 200
18
Specification of Planet Detection Tools
PSM WP 112 000
19
Transit Detection Tools
PSM WP 112 100
20
Detection of Single and Unusual Transit Events
PSM WP 112 200
21
Detection of Exoplanet Systems via Reflected Light
PSM WP 112 300
22
Other Detection Methods
PSM WP 112 400
23
Eclipse Timing Variations in Eclipsing Binaries
PSM WP 112 420
24
Phase Variations in Pulsating Stars
PSM WP 112 430
25
Multi-Planet Systems
PSM WP 112 500
26
Photometric Detection of Circumbinary Planets
PSM WP 112 510
27
Planets in Trojan Orbits
PSM WP 112 520
28
Exomoons and Binary Planets
PSM WP 112 530
29
PSM WPDs
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Other Multiple Systems
PSM WP 112 540
30
Transit Time Variations and Transit Duration Variations (TTV / TDV)
PSM WP 112 600
31
TTV / TDV Detection
PSM WP 112 610
32
TTV / TDV Modelling
PSM WP 112 620
33
Specification of Procedures to Rank Planet Candidates
PSM WP 113 000
34
Rank Planet Candidates
PSM WP 113 100
35
Specification for Space Based False Positive Identification Through Centroid Analysis
PSM WP 113 200
36
Astrophysical False Positives
PSM WP 113 300
37
Specification of Transit Fitting Tools
PSM WP 114 000
38
Specify Transit Curve Modelling Tools
PSM WP 114 100
39
Specify Tools for Accurate Orbital Period Determination
PSM WP 114 200
40
Rossiter-McLaughlin Modelling Tools
PSM WP 114 300
41
Development of PLATO Data Specific Science
PSM WP 115 000
42
Astrophysical Noise Sources and Their Impact on RV Determination
PSM WP 115 100
43
Improved Planetary System Characterisation
PSM WP 115 200
44
Planet-Star Interactions
PSM WP 115 300
45
Transits of Close-in Objects
PSM WP 115 400
46
Non-Transiting Planets via REBs
PSM WP 115 500
47
Development of PLATO Interpretation Specific Science
PSM WP 116 000
48
PSM WPDs
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Compositions & Formation of Gas & Ice Giants
PSM WP 116 100
49
The Mass-Radius Relationship for Terrestrial Planets
PSM WP 116 200
50
Planetary Formation and Orbital Evolution
PSM WP 116 300
51
Protoplanetary Disc Models
PSM WP 116 310
52
Disc-Planet Interactions
PSM WP 116 320
53
The Assembly of Planetary Systems
PSM WP 116 330
54
The Post-Formation Long-Term Dynamical Evolution of Planetary Systems
PSM WP 116 340
55
Planet Formation and Evolution in Binary Systems
PSM WP 116 350
56
Influence of Birth Environment on the Formation and Evolution of Planetary Systems
PSM WP 116 360
57
Post-Main Sequence Evolution of Planetary Systems
PSM WP 116 370
58
Statistical Comparison Between Theory and PLATO Data
PSM WP 116 380
59
Atmospheres of PLATO Terrestrial Planets
PSM WP 116 400
60
PLATO Habitable Zone Planets
PSM WP 116 500
61
Environments of PLATO HZ Planets
PSM WP 116 510
62
Astrophysical Factors Influencing Habitability of PLATO Planets
PSM WP 116 520
63
Climate / Atmospheres of PLATO Habitable Zone Planets
PSM WP 116 530
64
Dynamical Interactions in Multi-Planet Systems
PSM WP 116 600
65
Long-Term Dynamical Evolution of Planetary Systems
PSM WP 116 610
66
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Stability and Resonances in Multi-Planet Systems
PSM WP 116 620
67
Tidal Dissipation and Evolution of Multi-Planet Systems
PSM WP 116 630
68
Rotational Evolution of Planets in Multiple Systems
PSM WP 116 640
69
Planetary Ephemerides of PLATO Systems
PSM WP 116 650
70
Specifications for Interface to Other PSM WPs and PDC
PSM WP 117 000
71
Stellar Science Coordination
PSM WP 120 000
72
Stellar Models
PSM WP 121 000
73
1D Stellar Models
PSM WP 121 100
74
Very Low-Mass Stellar Models
PSM WP 121 110
75
Low Mass Stellar Models
PSM WP 121 120
76
Theoretical Oscillation Frequencies
PSM WP 121 130
77
Transport Processes
PSM WP 121 200
78
PMS Evolution
PSM WP 121 300
79
2D / 3D Stellar Evolution Models
PSM WP 121 400
80
Evolution of Stars in Multiple Systems
PSM WP 121 500
81
Non-Seismic Diagnostics and Model Atmospheres
PSM WP 122 000
82
1D Model Atmospheres
PSM WP 122 100
83
3D Model Atmospheres
PSM WP 122 200
84
Fundamental Stellar Parameters
PSM WP 122 300
85
PSM WPDs
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Limb Darkening
PSM WP 122 400
86
Interstellar Extinction
PSM WP 122 500
87
Stellar Activity and Rotation
PSM WP 123 000
88
Spot Models
PSM WP 123 100
89
Surface Convection (1D & 3D)
PSM WP 123 200
90
Models of Rotational Evolution and Gyrochronology
PSM WP 123 300
91
Dynamos and Differential Rotation
PSM WP 123 400
92
Tools to Measure Rotational Modulation
PSM WP 123 500
93
Stellar Rotation from Transits
PSM WP 123 600
94
Seismic Diagnostics
PSM WP 124 000
95
Forward Approaches
PSM WP 124 100
96
Inverse Techniques
PSM WP 124 200
97
Acoustic Glitches
PSM WP 124 300
98
Determination of Stellar Parameters
PSM WP 125 000
99
Scaling Laws
PSM WP 125 100
100
Incorporating Classical Parameters
PSM WP 125 200
101
Seismic Parameters
PSM WP 125 300
102
Open Clusters
PSM WP 125 400
103
PSM WPDs
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Mode Physics
PSM WP 126 000
104
Mode Amplitude and Near-Surface Effects on Mode Parameters
PSM WP 126 100
105
Mode Line-Width
PSM WP 126 200
106
Intensity-Velocity Relation
PSM WP 126 300
107
Seismology of Magnetic Activity
PSM WP 126 400
108
Seismic Constraints From Aging Stars
PSM WP 127 000
109
Stellar Models of Evolved Stars
PSM WP 127 100
110
Seismic Diagnostics for Evolved Stars
PSM WP 127 200
111
Constraints on Main-Sequence Stars
PSM WP 127 300
112
Power Spectrum Fitting Tools
PSM WP 128 000
113
Average Seismic Parameters
PSM WP 128 100
114
Mode Fitting Tools
PSM WP 128 200
115
Solar-Like Stars
PSM WP 128 210
116
Solar-Like Stars with Planets
PSM WP 128 220
117
Multiple Stars
PSM WP 128 230
118
Ensemble Fit
PSM WP 128 240
119
Fitting Tools for Evolved Stars
PSM WP 128 250
120
Interfaces
PSM WP 129 000
121
Target / Field Characterization and Selection
PSM WP 130 000
122
PSM WPDs
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Project Office Assistant
PSM WP 130 100
123
Catalogues Analysis
PSM WP 131 000
124
Gaia Catalogues Analysis
PSM WP 131 100
125
Astrometric Analysis
PSM WP 131 110
126
Photometric Analysis
PSM WP 131 120
127
Spectroscopic Analysis
PSM WP 131 130
128
Gaia Parameters Extraction
PSM WP 131 140
129
PLATO-Gaia Simulations
PSM WP 131 150
130
Other Large Catalogues Analysis
PSM WP 131 200
131
Photometric and Astrometric Catalogues
PSM WP 131 210
132
M-Dwarfs
PSM WP 131 220
133
M-Dwarfs as Planet Hosts
PSM WP 131 221
134
Stellar Activity
PSM WP 131 230
135
Binary Systems
PSM WP 131 240
136
Large Spectroscopic Catalogues
PSM WP 131 250
137
Known and Candidate Exoplanets
PSM WP 131 260
138
Single Target Additional Data
PSM WP 131 300
139
High Resolution and Deep Imaging
PSM WP 131 310
140
PSM WPDs
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Spectroscopic Data
PSM WP 131 320
141
Preparatory Observations
PSM WP 131 330
142
K2 Data
PSM WP 131 400
144
TESS Data
PSM WP 131 500
145
Contaminant Analysis
PSM WP 131 600
146
Contaminant Modelling Tool
PSM WP 131 610
147
Gaia Analysis of Contaminants
PSM WP 131 620
148
Contaminant Analysis From Other Catalogues
PSM WP 131 630
149
Field and Target Selection
PSM WP 132 000
150
Field Selection
PSM WP 132 100
151
Target Selection and Prioritisation
PSM WP 132 200
152
PLATO Field Contaminants
PSM WP 132 300
153
Single Target Contaminants
PSM WP 132 310
154
False Alarm Probability
PSM WP 132 320
155
Interface to Other PSM WPs and PDC
PSM WP 133 000
156
Interface to Other PSM WPs
PSM WP 133 100
157
Interface to PDC
PSM WP 133 200
158
Interface Gaia-PLATO
PSM WP 133 300
159
Interface to PLATO CCD Image Simulator
PSM WP 133 400
160
PSM WPDs
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Interface to TOU
PSM WP 133 500
161
Coordination of PLATO Follow-Up Observations
PSM WP 140 000
162
Strategy and Operation Preparation
PSM WP 141 000
163
Target Distribution Requirements
PSM WP 141 100
164
Aids for Optimizing Photometric and Spectroscopic Measurements
PSM WP 141 200
165
Information Transfer
PSM WP 141 300
166
Planet Yield Determination
PSM WP 141 400
167
Radial Velocity Follow-up
PSM WP 142 000
168
Radial Velocity Computation and Global Analysis Tools
PSM WP 142 100
169
First Radial Velocity Screening [≥ 10 m/s]
PSM WP 142 200
170
Intermediate Precision Radial Velocity Follow-Up [3-5 m/s]
PSM WP 142 300
171
Very High-Precision RV Measurements [≤ 1 m/s]
PSM WP 142 400
172
Infrared Radial-Velocity Measurements
PSM WP 142 500
173
Time Critical Photometry
PSM WP 143 000
174
Photometry Specific Tools
PSM WP 142 100
175
Photometric Follow-Up with Small Telescopes
PSM WP 143 200
176
Standard Photometric Observations
PSM WP 143 300
177
Very High Precision Photometric Observations
PSM WP 143 400
178
PSM WPDs
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High Angular Resolution Imaging
PSM WP 144 000
179
Imaging Analysis Tools
PSM WP 144 100
180
Single-Epoch Seeing-Limited Imaging
PSM WP 144 200
181
Reconnaissance High Resolution Imaging
PSM WP 144 33
High Contrast Imaging
PSM WP 144 400
182
183
Candidate Classification
PSM WP 144 500
184
Additional Exoplanet Follow-Up
PSM WP 145 000
185
Transmission Spectroscopy Follow-Up
PSM WP 145 100
186
Secondary Eclipse and Phase-Variation Spectroscopy
PSM WP 145 200
187
Developing Techniques for Atmosphere Characterization
PSM WP 145 300
184
Rossiter-McLaughlin Observations
PSM WP 145 400
189
Additional Long Term Follow-Up (RV and Transit Timing)
PSM WP 145 500
190
Spectroscopy
PSM WP 146 000
191
Activity Indicators and Doppler Information on Active Stars
PSM WP 146 100
192
Tools for Spectral Classification
PSM WP 146 200
193
Infrared Spectroscopy
PSM WP 146 300
194
Spectropolarimetric Follow-Up
PSM WP 146 400
195
Performance Assessment & FU Efficiency
PSM WP 147 000
196
Interfaces to Other PSM WPs and PDC
PSM WP 148 000
197
PSM WPDs
DEVELOPMENT
Complementary Science
PSM WP 160 000
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PSM WPDs
DEVELOPMENT
PSM Coordination
Leader: Don Pollacco
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PSM WP 100 000
Development phase
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco
Objectives:
Overall coordination of PMC Science Management activities.
Tasks:
1.
2.
3.
4.
5.
6.
7.
Coordinate activities of PSM team
Coordinate its interfaces with the PDC, the PLATO instrument and ESA
Ensure the required PDC input and documentation is delivered on time with the requested quality level
Organization of regular meetings of the PSM coordination team
Organization of workshop to involve the scientific community into PSM activities
Overlook PR-activities by EPO
Report on PSM activities to PCL, PMC board, and ESA
Input:
1. Activities and reports from PSM task coordinators
2. Documentation of results obtained
Dependencies:
Close interactions foreseen with the PDC Coordination and the PSM Coordination Team (WP 103 000) & with all
sub-packages in WP 110, 120, 130, 140, and 160
Output:
1. Specifications and data input to PDC
2. Coordinated PR and EPO activities
Deliverables:
1.
Reports from each PSM work packages listing recommendations for implementation within PDC
2.
Input to PDC catalogues
Milestones:
12/2016: Organize PMC Science Conference
09/2016: Ground Segment Requirement Review (GSRQR)
04/2017-05/2017: Internal PMC Product Design Review (PDR)
03/2020: Delivery of preliminary reports, specifications of algorithms and first data input to PDC
09/2018: Ground Segment Design Review (GSDR)
09/2022: Ground Segment Implementation Review (GSIR)
12/2022: Final reports and improved specifications, final pre-launch PDC input catalogue data to PDC
06/2023: Ground Segment Readiness Review (GSRR)
Risks:
1.
Late delivery of any of the outputs from PSM work packages will impact on the work of the PDC
2.
Late delivery of field characterization tasks will impact target field selection for PLATO.
PSM WPDs
DEVELOPMENT
PSM Project Office
Leader: David J. A. Brown
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PSM WP 101 000
Development phase
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. J. A. Brown
Objectives:
Support coordination of the PSM activities.
Tasks:
1.
2.
3.
4.
Organization of PSM meetings, teleconferences, etc.
Organization of workshop with scientific community
Editing of PSM documentation
Interface between WP 100 000, WP 103 000, and sub-packages
Input:
Organizational requests from PSM
Dependencies:
Close interactions foreseen with the WP 100 000 and WP 103 000.
Output:
1. Organization of meetings, teleconferences, etc.
2. Preparation of PSM documents
Deliverables:
Documentation of the PSM activities
Milestones:
12/2016: Organize PMC Science Conference
09/2018: Ground Segment Requirement Review (GSRQR)
09/2019: Internal PMC Product Design Review (PDR)
03/2020: Delivery of preliminary reports, specifications of algorithms and first data input to PDC
09/2021: Ground Segment Design Review (GSDR)
09/2022: Ground Segment Implementation Review (GSIR)
12/2022: Final reports and improved specifications, final pre-launch PDC input catalogue data to PDC
06/2023: Ground Segment Readiness Review (GSRR)
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
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PSM Coordination Team
Leader: Don Pollacco
Rev.: 5
Development phase
PSM WP 103 000
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco; PSM coordination team members
Objectives:
Coordinate and review PSM and PDC activities
Tasks:
1.
Review the progress of the SPM during the development phases by regular telephone conferences and
meetings
2.
Coordinate the science specifications and priorities between each SPM task needed to achieve the
science goals
3.
Agree on the final science specifications to be implemented in the PDC
4.
Prepare and review the documents including final specifications and inputs for the PDC (first full draft by
mid-2015 with later upgrades where needed
5.
Review the implementation of PSM specifications and input at the PDC
Input:
1. Activities and reports from PSM task coordinators
2. Documentation of results obtained
3. Report on implementations in PDC
Dependencies:
Close interactions foreseen with the WP 100 000 and all its sub-packages.
Output:
1. Verified specifications and input for the PDC
2. Review documents
Deliverables:
Documentation on the activities of the PSM.
Milestones:
12/2016: Organize PMC Science Conference
09/2018: Ground Segment Requirement Review (GSRQR)
09/2019: Internal PMC Product Design Review (PDR)
03/2020: Delivery of preliminary reports, specifications of algorithms and first data input to PDC
09/2021: Ground Segment Design Review (GSDR)
09/2022: Ground Segment Implementation Review (GSIR)
12/2022: Final reports and improved specifications, final pre-launch PDC input catalogue data to PDC
06/2023: Ground Segment Readiness Review (GSRR)
Risks:
Late delivery of any of the outputs from the PSM will impact on the work of the PDC
PSM WPDs
DEVELOPMENT
Exoplanet Science Coordination
Leader: Don Pollacco
Development phase
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PSM WP 110 000
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco
Objectives:
Coordination of exoplanet work packages for input to PDC.
Tasks:
1.
Liaise with work package coordinators over progress in meeting their objectives
2.
Liaise and respond to the PMC Science Management Coordinator over project requirements
3.
Attend meetings (etc.) as required
Input:
1.
PLATO Red Book
2.
Scientific literature
3.
Scientific specifications from the sub packages
4.
Scientific validation and update on the algorithms by the Exoplanet Science sub packages
Dependencies:
All sub-packages
Output:
1.
Successful completion of exoplanet work packages as input to PDC
2.
Scientific specification for both algorithm & tools
Deliverables:
Reports from each work packages listing recommendations for performance evaluation and improvements
during development phase.
Milestones:
04/2017: Delivery of initial set of scientific specifications to the PDC
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Late delivery of any of the outputs from these work packages will impact on the work of the PDC.
PSM WPDs
DEVELOPMENT
Coordination of Tools for Lightcurve Filtering
Leader: Antonino F. Lanza
Development phase
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PSM WP 111 000
04/2016 — 12/2023
Institution: INAF-Catania (Italy)
Key Personnel: A. F. Lanza; S. Aigrain (Oxford); F. Faedi (Warwick)
Objectives:
To coordinate work packages looking at noise sources (both astrophysical and instrumental) in the PLATO
photometry. To deliver algorithms and specifications to reduce the impact of noise on transit detection and
modelling.
Tasks:
1.
Continue the evaluation of scientific literature on this topic (including new works from CoRoT and Kepler)
2.
Assessment of algorithm descriptions and their requirements
3.
Methods to test the implemented algorithms
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
Simulated PLATO data
Dependencies:
WP 111 100, WP 111 200, PLATO End-to-End Simulator
Output:
1.
Understanding of stellar noise on PLATO photometry and its impact on transit detection and modelling
in collaboration with WP 112 000 and 114 000
2.
Transfer of information through WP 117 000
Deliverables:
1.
Reports on algorithms and specifications.
2.
Reports on tests performed as algorithms and their implementation evolve.
Milestones:
04/2017: Delivery of Initial Set of scientific specifications to the PDC
04/2018: Review and scientific validation implementation of algorithms done in the PDC
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
If astrophysical noise is not properly treated, small planets will only be detectable in the quietest of systems, i.e.,
with a solar-like level of stellar activity, and more transits will be required for detection. A good instrumental
characterization is required to fully understand residual instrumental effects.
PSM WPDs
DEVELOPMENT
Specification of Tools for Lightcurve Filtering
Leader: Suzanne Aigrain
Development phase
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PSM WP 111 100
04/2016 — 12/2023
Institution: Oxford University (UK)
Key Personnel: S. Aigrain; 1 postdoc (Oxford)
Objectives:
To understand and minimize the impact of stellar noise on transit detection with PLATO through the evaluation
and development (as necessary) of light curve filtering algorithms
Tasks:
1.
Continued evaluation of scientific literature (including unpublished works from CoRoT and Kepler)
2.
Development and testing of algorithms for different types of variability
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
Simulated PLATO data
Dependencies:
1.
PLATO End-to-End Simulator
Output:
1.
Understanding of stellar noise on PLATO transit photometry
2.
Scientific specifications for noise handling algorithms
Deliverables:
1.
Report on WP activity
2.
Algorithm(s) for implementation by PDC
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
If this is not understood, small planets will only be detectable in the quietest of systems, and more transits will be
required for detection.
PSM WPDs
DEVELOPMENT
Specification of Tools for Detecting and Filtering
Residual Instrumental Noise
Leader: Don Pollacco
Development phase
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PSM WP 111 200
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco; F. Faedi (Warwick)
Objectives:
To simulate the effect of systematic noise arising in the PLATO instrument itself and its effects on transit
detection. To adapt and optimize mitigation techniques outlined earlier. This WP will also produce test data to be
used by other exoplanet WPs for benchmarking the PDC Exoplanet software.
Tasks:
1.
Optimization of algorithms via the analysis of light-curves residuals after de-trending.
2.
Develop and assessment of algorithms for different types of systematic noise sources.
3.
Develop test data to be used in benchmarking (and testing) the PDC exoplanet software.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
CoRoT and Kepler datasets
Dependencies:
Exchange of information and coordination with WP 112 and WP 114, PLATO End-to-End Simulator
Output:
Mitigation of the effects of residual instrumental noise on PLATO photometry. For example residuals correlation
with colour, magnitude, time scale of observation. Test for the optimal de-trending technique.
Deliverables:
1.
Report on status and tests of algorithms
2.
Report on bench mark datasets
Milestones:
12/2016: Results from the use of Kepler data to assess the algorithm performance for PLATO
04/2017: Production of specification for bench mark and identification of existing and synthetic datasets
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
If residual systematic noise is not well understood and removed, it could affect significantly the detection of small
transit signals in particular on long time scales (fewer transits) making Earth-analogue hard to identify in the data
(one transit detection).
PSM WPDs
DEVELOPMENT
Specification of Planet Detection Tools
Leader: Juan Cabrera
Ref.: PLATO-UWA-PSMWPD-001
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PSM WP 112 000
Development phase
04/2016 — 12/2023
Institution: DLR (Germany)
Key Personnel: J. Cabrera; NN (DLR)
Objectives:
Coordination of the activities of the sub-work packages related to planet detection by different methods.
Coordination of the exchange of information among the sub-WP. Coordination of the exchange of information
between the sub-WP and the PSM structure. Coordination of the specifications of the simulated data that will be
used for the tests of the algorithms. See that reports, algorithms, and specifications are delivered on time.
Tasks:
1.
Liaise with sub-work package leaders
2.
Liaise with Exoplanet coordinator
3.
Responsible for reports and algorithms from sub-work packages
Input:
1.
Scientific literature
2.
PLATO Red Book
3.
Current PLATO performance estimation
4.
PLATO Specifications
5.
Simulated PLATO light curves
Dependencies:
Close interactions foreseen with the WP 111 000; 113 000; 114 000 and sub-WPs, PLATO End-to-End
Simulator
Output:
Scientific specifications of planet detection algorithms and strategies for PDC
Deliverables:
Reports from sub-work packages and scientific specifications of transit detection tools
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Planet detection is a key area for the success of PLATO. Ability and efficiency of planet detection will be
impaired without an optimized solution for PLATO data sets.
PSM WPDs
DEVELOPMENT
Transit Detection Tools
Leader: Juan Cabrera
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 21/200
PSM WP 112 100
04/2016 — 12/2023
Institution: DLR (Germany)
Key Personnel: J. Cabrera; NN (DLR); S. Aigrain (Oxford); R. Alonso (IAC); A. Bonomo (INAF-Torino);
Carone (Leuven); S. Carpano (ESTEC/ESA); P. Eigmüller (DLR); A. Ofir (Weizmann); M. Pätzold (Köln)
L.
Objectives:
Transit detection algorithms (TDA) are mathematical tools that take as input stellar light curves (LC) and provide
as output a statistic that evaluates the presence of a transit-like signature in the LC. There is abundant literature
referring to the TDA tools and the different approaches in the analysis of the data followed by ground-based and
space-based surveys. The objectives of the WP 112 100 are to find out which approach and which TDA or set of
TDAs apply better to the PLATO observing strategy guaranteeing that the requirements for the success of the
PLATO mission are fulfilled.
Taking as an input the study done during the definition phase, the objectives of the WP 112 100 will be to design
the transit detection strategy, identifying the particular challenges from the experience acquired during the
CoRoT and Kepler missions, to assess the capabilities of the existing TDA and deciding which improvements
have to be developed, and to provide the PDC with a set of tested tools for their implementation.
Tasks:
1.
Design a realistic transit detection test on simulated PLATO data, including the most updated
knowledge on the expected levels of stellar and instrumental residuals in the cleaned light curves. The test will
scientifically validate the capabilities of several TDA
2.
Coordinate a taskforce who will analyse the results of the transit detection test, study the performances
of the different TDA, propose modifications and optimizations
3.
Document the results of the tests and propose the PDC an strategy for transit detection and a set of
TDA for their implementation
4.
Advise the PDC in the implementation of the recommended strategy and TDA. Assess that the quality
levels required are achieved. Provide new input if needed
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
PLATO specifications and simulated PLATO light curves
Dependencies:
WP 110, WP 116, WP 160, WP 112, PLATO End-to-End Simulator
Deliverables:
Report and scientific specifications of transit detection tools
Milestones:
04/2017: Delivery of Initial Set of scientific specifications to the PDC
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specs in compliance with the PDC development plan
Risks:
Transit detection is a key area for the success of PLATO. Ability and efficiency of transit detection will be
impaired without an optimized solution for PLATO data sets.
PSM WPDs
DEVELOPMENT
Detection of Single and Unusual Transit Events
Leader: Don Pollacco
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 22/200
PSM WP 112 200
Development phase
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco; F. Faedi (Warwick); J. Cabrera (DLR); A. Erikson (DLR)
Objectives:
Reliable detection (or at least significance) from single and unusual transit events
Light-curve properties: knowledge of advanced de-trending techniques, and of methods for analysing de-trended
light curves, is crucial for the detection of individual transits; residual correlated noise (or variability) could
prevent detection of individual, shallow signals, or oddly shaped events. Light curve morphology: an individual
transit is temporally short compared to the out-of-transit lightcurve. Use the properties of the transit signal
(shape, depth, timescale of ingress and egress, and duration) to define and build detection criteria. Identification
using Blind Correlation Plots: (detection of individual events is independent of periodicity) for example compare
the mean flux level to the rapid changes during ingress / egress, over a range of trial durations. Test for a
degree of correlation of the observations over the expected / desired transit durations. Isolate possible in-transit
points from out-of-transit points; estimate a per-point transit probability using the out-of-transit flat light-curve.
Detection algorithms: test detection limits and algorithm performance using synthetic PLATO light curves.
Assess detection probability of single and unusual events for a range of observation timespans, expected orbital
periods, and host spectral types, accounting for different possible residual noise levels.
Tasks:
1.
Assessment of current transit detection techniques for small planets and / or noisy stars.
2.
Detection algorithm development, and algorithm optimisation.
3.
Determination of statistic of detection reliability for single and unusual events.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
Simulated PLATO light curves
Dependencies:
Exchange of information and coordination with WP 111 000, WP 114 000, PLATO End-to-End Simulator
Output:
Scientific specifications for algorithms to detect (or at least statistically rank) transits from single, or unusually
shaped, events and / or at low signal to noise.
Deliverables:
Report on status and scientific tests of algorithms.
Milestones:
04/2017: Delivery of initial set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Ability and efficiency of transit detection will be impaired without an optimized solution for PLATO datasets.
PSM WPDs
DEVELOPMENT
Detection of Exoplanet Systems via Reflected Light
Leader: Ignas Snellen
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 23/200
PSM WP 112 300
04/2016 — 12/2023
Institution: University of Leiden (Netherlands)
Key Personnel: I. Snellen
Objectives:
Detection of planets through their orbital phase variations, either from varying reflected light or thermal
contributions.
Tasks:
1.
Evaluate the scientific literature on phase variations and especially on their recovery in the presence of
systematic noise from the host star and likely noise sources from the spacecraft.
2.
Conduct tests on data readily available from other space missions (CoRoT/Kepler) and simulated data
3.
Develop and test an algorithm given above knowledge
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
Simulated PLATO light curves
Dependencies:
Discussions with WP 111, PLATO End-to-End Simulator
Output:
1.
Detection of planets through their phase variations
2.
Increase in PLATO planet catch
Deliverables:
Report and scientific specifications of algorithms
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
The detection of phase variations offers a further technique to discover exoplanets in large numbers.
For each planet detected through transit detection there will be tens maybe hundreds that will display orbital
phase variations. However, the concept is not proven yet, and could be hampered by intrinsic stellar variability
on similar timescales as the orbital period of the planet.
PSM WPDs
DEVELOPMENT
Other Detection Methods
Leader: Roberto Silvotti
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 24/200
PSM WP 112 400
Development phase
04/2016 — 12/2023
Institution: INAF-Torino (Italy)
Key Personnel: R. Silvotti; V. Nascimbeni (INAF-Padova); S. Dreizler (Göttingen); S. Schuh (MPSSR);
Burleigh (Leicester); Sz. Csizmadia (DLR); F.V. Hessman (Göttingen)
M.
Objectives:
Comprehensive study of planet detection through other methods, in particular those based on timing:
WP 112 600 (transit time variations and transit duration variations, TTV/TDV); WP 112 420 (eclipse timing
variations in eclipsing binaries, circumbinary planets), and WP 112 430 (phase variations in pulsating stars).
Extend PLATO discovery space to potentially very small planets/moons and to relatively unexplored types of
stars.
Tasks:
1.
Coordination of WPs 112 420, 112 430.
2.
Coordination of interfaces with WP 112 500 (Multi-planet Systems), WP 367 400 (Circumbinary Planet
Parameters), and relevant sub-WPs of WP 160.
3.
Coordination/collection of reports and requirements from sub-WP and delivery to WP 112 000
coordinator and PDC.
Input:
1.
Scientific literature, own expertise
2.
PLATO Definition Phase Documentation
3.
Current PLATO performance
4.
Simulated PLATO light curves
Dependencies:
Coordination with WP 112 500 (Multi-planet Systems), WP 145 500 (Additional Long Term Follow-up (RV and
Transit Timing)), WP 367 400 (Circumbinary Planet Parameters), and relevant sub-WPs of WP 160. PLATO
End-to-End Simulator
Output:
1.
Well-tested science case with feedback for PDC.
2.
Definition of preparatory and follow-up observations.
Deliverables:
1.
Observing plan for preparatory observations.
2.
Reports/documents and requirements for PDC (specifications of algorithms).
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2017: Science case tested with existing data (ground based, CoRoT, Kepler, Plato simulations)
04/2018: Observing plan for preparatory observations
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Time sampling is a critical issue and can limit the minimum detectable mass of planets/moons.
PSM WPDs
DEVELOPMENT
Eclipse Timing Variations in Eclipsing Binaries
Leader: Stefan Dreizler, Sonja Schuh
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 25/200
PSM WP 112 420
04/2016 — 12/2023
Institution: Georg-August University Göttingen (Germany)
Key Personnel: S. Dreizler; S. Schuh; F.V. Hessman (Göttingen); R. Silvotti (INAF-Torino)
Objectives:
To use PLATO photometry to detect planets by means of eclipse timing variations in eclipsing binaries
(circumbinary planets). Extend PLATO discovery space to relatively unexplored types of stars.
Tasks:
1.
2.
3.
4.
5.
Perform test analyses with existing (Kepler/CoRoT) and simulated data.
Critically test analysis tools.
Define and perform preparatory and follow-up observations.
Assess false positive scenarios.
Write relevant documents/reports.
Input:
1.
Scientific literature, own expertise
2.
Light curve processing
3.
Stellar parameters
4.
Current PLATO performance
5.
PLATO Simulated light curves
Dependencies:
Coordination with WP 112 500 (Multi-planet Systems), WP 367 400 (Circumbinary Planet Parameters), PLATO
End-to-End Simulator
Output:
1.
Well-tested science case with feedback for PDC.
2.
Definition of preparatory and follow-up observations.
Deliverables:
1.
Observing plan for preparatory observations.
2.
Reports/documents and requirements for PDC (scientific specifications of algorithms).
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2017: Science case tested with existing data
04/2018: Observing plan for preparatory observations
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Time sampling is a critical issue and can limit the minimum detectable mass of planets.
PSM WPDs
DEVELOPMENT
Phase Variations in Pulsating Stars
Leader: Roberto Silvotti
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 26/200
PSM WP 112 430
04/2016 — 12/2023
Institution: INAF-Torino (Italy)
Key Personnel: R. Silvotti; S. Schuh (Göttingen); M. Burleigh (Leicester)
Objectives:
To use PLATO photometry to detect planets by means of pulsation phase variations in pulsating stars, in
particular compact pulsators (white dwarfs, hot subdwarfs), thanks to their short periods down to few minutes.
Extend PLATO discovery space to relatively unexplored types of stars.
Tasks:
1.
2.
3.
4.
5.
Perform test analyses with existing (Kepler/CoRoT) and simulated data.
Critically test analysis tools.
Define and perform preparatory and follow-up observations.
Assess false positive scenarios.
Write relevant documents/reports.
Input:
1.
Scientific literature, own expertise
2.
Light curve processing
3.
Stellar parameters
4.
Current PLATO performance
5.
PLATO Simulated light curves
Dependencies:
Coordination with relevant sub-WPs of WP 160. PLATO End-to-End Simulator
Output:
1.
Well tested science case with feed-back for PDC
2.
Definition of preparatory and follow-up observations
Deliverables:
1.
Observing plan for preparatory observations
2.
Reports/documents and requirements for PDC (algorithms)
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2017: Science case tested with existing data
04/2018: Observing plan for preparatory observations
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Time sampling is a critical issue and can limit the minimum detectable mass of planets.
PSM WPDs
DEVELOPMENT
Multi-Planet Systems
Leader: Silvano Desidera
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 27/200
PSM WP 112 500
Development phase
04/2016 — 12/2023
Institution: INAF-Padova (Italy)
Key Personnel: S. Desidera; G. Picogna (INAF-Padova)
Objectives:
Comprehensive study of planet occurrence in multi-body systems (either binary or multiple stars, or multiple
planets), and their photometric detectability using PLATO (algorithms, targets)
Tasks:
1.
Coordination of WP 112 510, 112 520, 112 530, 112 540
2.
Coordination of interfaces with WP 112 400 on timing detections of multi-planet systems
3.
Collection of reports and requirements from sub-WP and delivery to WP 112 000 coordinator
Input:
1.
Scientific literature
2.
PLATO Definition Phase documentation
3.
PLATO Simulated light curves
Dependencies:
Coordination with WP 112 400 needed, PLATO End-to-End Simulator
Output:
1.
Reports on detectability of planets in multiple systems with PLATO
2.
Detection algorithms for photometric detections of multi-planet systems
3.
Target and target parameters
Deliverables:
Interim Report, Final Report, Requirements for PDC (detection algorithms), Requirements for PIC (targets and
their parameters)
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Photometric Detection of Circumbinary Planets
Leader: Hans J. Deeg
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 28/200
PSM WP 112 510
04/2016 — 12/2023
Institution: IAC (Spain)
Key Personnel: H.J. Deeg; 1 postdoc
Objectives:
1.
Preparation for detection/characterization of circumbinary planets, primarily from PLATO photometric
data, towards a maximisation in the numbers and variety of circumbinary planets detected.
2.
Implications in mission design/protocols for observing/data-handling and maximizing science return.
3.
Optimization of existing or newly developed detection methods.
4.
Preparation to coordinate detection effort during flight phase, and its publication and dissemination.
Tasks:
1.
Continued review of the scientific literature and consequent adaptation of WP objectives and methods.
2.
Sample definition: definition of expected sample for circumbinary planet searches (e.g. sample size and
characteristics). It consists in an initial estimate for the sample, which will be refined and updated alongside the
evolution and eventual freezing of PLATO mission specs.
3.
Detection methods:
a.
Initially: revision of existing methods and algorithms. This includes: evaluation of their sensitivity,
requirements onto PLATO data; need for auxiliary data; potential results
b.
Selection of methods and development/implementation in PLATO data analysis protocol.
c.
Testing of these methods with simulated data and definition of their performance.
d.
Feedback to PMC Science coordination about design aspects that may allow an optimization of the
mission towards the WP objectives
4.
Definition of auxiliary data that will be needed: revising their availability in literature or databases or
defining the observations required from other instruments (ground or space).
Input:
1.
Scientific literature, PLATO Definition Phase docs and estimation of PLATO performance
2.
Ongoing progress from: WP 112 100, 112 300, 112 400, other WP’s related to Eclipsing Binaries
Dependencies:
Specification of PLATO mission parameters, performance and data format, PLATO End-to-End Simulator
Output:
1.
Ongoing review of circumbinary planet detections and methods
2.
Development of protocol to detect and characterize circumbinary planets, including: data processing
and detection algorithm; definition of additional data that are needed;
3.
Framework for interactive tools for detection of circumbinary planets and archiving of results.
Deliverables:
Report; detection algorithms; publications of algorithms and their expected detection performance
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specs in compliance with the PDC development plan
Risks:
Unknown abundance of circumbinary planets does not permit that their discovery will be guaranteed.
PSM WPDs
DEVELOPMENT
Planets in Trojan Orbits
Leader: Francesco Marzari
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 29/200
PSM WP 112 520
04/2016 — 12/2023
Institution: University of Padova (Italy)
Key Personnel: F. Marzari; G. Picogna (INAF-Padova)
Objectives:
Study of potential occurrence of Trojan planets (either co-orbital companions of planets or in binary systems)
and of their detectability using PLATO.
Tasks:
1.
Continued review of the scientific literature in this area.
2.
Identify selection criteria for binary systems candidates to host Trojan planets (suitable values of mass
ratio and eccentricities leading to stable tadpole orbits)
3.
Develop in depth formation scenarios for Trojan planets that may help in candidate selection
4.
Elaborate strategies for detecting Trojan companions to transiting extrasolar planets. These methods
are based either on direct photometric detection at transit of the Trojan planet or on long-term monitoring of the
parent planet orbit looking for gravitational perturbations by an unseen Trojan companion.
5.
Other Science development needed to fully exploit PLATO data.
Input:
1.
Scientific literature
2.
PLATO Definition Phase documentation
3.
Simulated PLATO light curves
Dependencies:
Detectability of Trojan planets using timing techniques considered in WP 112 400, PLATO End-to-End Simulator
Output:
Ongoing review of published knowledge. Selection criteria for binary systems candidates to host Trojan planets.
Stability analysis of Trojan planets with chaos indicator like Laskar's frequency map analysis or Fast Lyapunov
indicators. Algorithms for photometric detection of Trojan planets Algorithms for analysis of the orbits of
photometrically detected planets looking for gravitational signatures of a lower mass Trojan companion.
Deliverables:
Reports, computer codes, detection algorithms, requirements for target selection and target parameters.
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Unknown abundance of Trojan planets does not permit that their discovery will be guaranteed.
PSM WPDs
DEVELOPMENT
Exomoons and Binary Planets
Leader: Gyula Szabo
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 30/200
PSM WP 112 530
04/2016 — 12/2023
Institution: Konkoly Observatory (Hungary)
Key Personnel: G. Szabo; A. E. Simon (Konkoly)
Objectives:
The main task of this WP in the development phase is to develop tools that will enable us to identify binary
exoplanets and moons orbiting extrasolar planets directly from the raw photometric data. According to pilot
experiments with simulated data, PLATO will be able to detect exomoons down to those similar in size to the
largest moons in our Solar System. Algorithms will be applied to all transiting planets and candidates identified
by PLATO, thus the input catalogue of objects will be compiled in the operational phase.
Tasks:
1.
2.
3.
4.
5.
6.
Define the characteristics of systems which have a detectable exomoon in PLATO data
Development of detection tools of binary planets
Development of detection tools of exomoons in the averaged folded light curves (Algorithm 1)
Development of detection tools of exomoons in the scatter peak of folded light curves (Algorithm 2)
Development of detection tools in the case of several moons orbiting the same planet
Science development needed to fully exploit PLATO data
Input:
1.
Scientific literature
2.
PLATO Definition Phase documentation
Dependencies:
Interface with WP 112 400 for the detection of exomoons using timing, PLATO End-to-End Simulator
Output:
1.
Specification of those planets which host detectable exomoons with Algorithms 1 and 2
2.
Specification of detectable systems with several moons
3.
Detection probabilities and false alarm rates of various moons in many multiple systems based on
simulated transit observations.
4.
Ongoing review of published knowledge.
5.
Development of theory (as required) to fully exploit PLATO data in this area.
Deliverables:
Reports, detection algorithms, requirements for target selection and target parameters.
Milestones:
12/2016: End of the development and test of the simulators
12/2017: End of the development and test of the detection algorithms for single moons
12/2018: End of the development and test of the detection algorithms for several moons
12/2018: End of the development and test of the detection algorithms for binary planets
03/2019: Delivery of interim reports, detection algorithms and requirements on target and parameters
12/2019: Specification of systems with a single moon in terms of detection efficiency and false alarm probability
12/2020: Full specification of detectability, including binary planets and systems with several moons
09/2023: Delivery of final report on WP activity
Risks:
Unknown abundance of exomoons and binary planets does not permit that their discovery will be guaranteed.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 31/200
Other Multiple Systems
Leader: Silvano Desidera
Rev.: 5
Development phase
PSM WP 112 540
04/2016 — 12/2023
Institution: INAF-Padova (Italy)
Key Personnel: S. Desidera; G. Picogna (INAF-Padova); F. Marzari (INAF-Padova)
Objectives:
Study of planet occurrence in multi-body systems (either binary or multiple stars, or multiple planets), excluding
those that are the subject of specific WPs (circumbinary planets, Trojan planets, exomoons and binary planets)
and their photometric detectability using PLATO (algorithms, targets)
Tasks:
1.
Review of planet occurrence in multi-body systems (either binary or multiple stars, or multiple planets),
excluding those that are the subject of other WPs (circumbinary planets, Trojan planets, exomoons and binary
planets).
2.
Study of potential effect on their detectability in photometric and spectroscopic data (except for detection
based on timing techniques, that are included in WP 112 400).
3.
Identification of science development needed to fully exploit PLATO data
4.
Identification of algorithms for photometric identification of multi-planet systems in their various
configurations
5.
Identification of targets for searches of multi-planet systems in their various configurations
Input:
1.
Scientific Literature
2.
PLATO Definition Phase documentation
3.
Simulated PLATO light curves
Dependencies:
Coordination with WP 112 400 on synergy between photometric and timing methods to detect multi-body
systems, PLATO End-to-End Simulator
Output:
Review of published knowledge. Simulations, Detection algorithms, Development of theory (as required) to fully
exploit PLATO data in this area.
Deliverables:
1.
Reports on detectability of planets in multiple systems with PLATO
2.
Detection algorithms for photometric detections of multi-planet systems
3.
Target and target parameters
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 32/200
Transit Time Variations and Transit Duration
Variations (TTV / TDV)
Leader: Valerio Nascimbeni
Rev.: 5
PSM WP 112 600
Development phase
04/2016 — 12/2023
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni; Sz. Csizmadia (DLR); G. Piotto (INAF-Padova); R. Silvotti (INAF-Torino)
Objectives:
To coordinate the activities of sub-work packages WP 112 610 (TTV / TDV Detection) and WP 112 620 (TTV /
TDV Modelling), investigating the impact and potential of transit timing variations (TTVs) and transit duration
variations (TDVs) on photometric observations of PLATO planetary systems. Coordination of information
exchange between the sub-WPs. Coordination of information exchange between the sub-WPs and WP 112 000,
and the wider PSM structure. To deliver reports, algorithms and specifications for the detection and modelling of
both TTVs and TDVs.
Tasks:
1.
2.
3.
4.
Liaise with sub-work package leaders
Liaise with Exoplanet coordinator
Liaise with leader of WP 112 000
Responsible for reports and algorithms from sub-work packages
Input:
1.
Scientific literature
2.
PLATO red book
3.
Current PLATO performance estimates
4.
PLATO specifications
5.
Simulated PLATO light curves
6. Kepler, CoRoT, K2 observations of TTVs
Dependencies:
Coordination with WP 112 500 (Multi-planet Systems), coordination with WP 145 500 (Additional Long Term
Follow-up: RV and Transit Timing), coordination with WP 112 000 (Specification of Planet Detection Tools),
PLATO End-to-End Simulator
Output:
1.
Well-tested science case and best-suited algorithms with feedback for PDC.
2.
Definition of preparatory and follow-up observations.
Deliverables:
1.
Observing plan for preparatory observations.
2.
Reports/documents and requirements for PDC (specifications of algorithms).
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2017: Science case tested with existing data
04/2018: Observing plan for preparatory observations
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Low risk
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 33/200
TTV / TDV Detection
Leader: Valerio Nascimbeni
Rev.: 5
PSM WP 112 610
Development phase
04/2016 — 12/2023
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni; Sz. Csizmadia (DLR); G. Piotto (INAF-Padova); R. Silvotti (INAF-Torino)
Objectives:
To use PLATO photometry to measure planetary masses and to detect additional planets, moons, Trojans and
sub-stellar companions by means of: (1) transit time variations (TTV) and (2) transit duration variations (TDV) of
already identified planetary transits. This will extend the PLATO discovery space to potentially very small
planets/moons, and make the follow-up easier.
Tasks:
1.
2.
3.
4.
Perform test analyses with existing (Kepler/CoRoT/K2) and simulated data.
Critically test analysis tools.
Define and perform preparatory and follow-up observations.
Write relevant documents/reports.
Input:
1.
2.
3.
4.
5.
6.
7.
8.
Scientific literature
Light curve processing
Stellar parameters
Current PLATO performance estimates
Simulated PLATO light curves
PLATO red book
PLATO specifications
Kepler, CoRoT, K2 observations of TTVs
Dependencies:
Algorithms of transit/ephemeris fitting from WP 114 100 and 114 200, coordination with WP 145 500 (Additional
Long Term Follow-up: RV and Transit Timing), PLATO End-to-End Simulator
Output:
1.
Well-tested science case and best-suited detection algorithms with feedback for PDC.
2.
Definition of preparatory and follow-up observations.
Deliverables:
1.
Observing plan for preparatory observations.
2.
Reports/documents and requirements for PDC (specifications of algorithms).
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2017: Science case tested with existing data
04/2018: Observing plan for preparatory observations
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Low risk
PSM WPDs
DEVELOPMENT
TTV / TDV Modelling
Leader: Rosemary Mardling
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 34/200
PSM WP 112 620
Development phase
04/2016 — 12/2023
Institution: Geneva University (Switzerland)
Key Personnel: R. Mardling;
Objectives:
TBD
Tasks:
1.
TBD
Input:
1.
TBD
Dependencies:
Coordination with WP 112 500 (Multi-planet Systems), algorithms of transit/ephemeris fitting from WP 114 100
and 114 200, coordination with WP 145 500 (Additional Long Term Follow-up (RV and Transit Timing)), PLATO
End-to-End Simulator
Output:
1.
TBD
Deliverables:
1.
TBD
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2017: Science case tested with existing data
04/2018: Observing plan for preparatory observations
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
TBD
PSM WPDs
DEVELOPMENT
Specification of Procedures to Rank Planet
Candidates
Leader: Magali Deleuil
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 35/200
PSM WP 113 000
04/2016 — 12/2023
Institution: Laboratoire d'astrophysique de Marseille (France)
Key Personnel: A. Bonomo (INAF-Torino); M. Deleuil + temporary
Objectives:
Coordination of sub-work packages related to planet ranking procedures and algorithms
Delivery of specification to PDC
Tasks:
1.
Liaise with sub-work package leaders
2.
Liaise with Exoplanet Coordinator and PMC Science Management Coordinator as required
3.
Responsible for reports and algorithms from sub-work packages
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
Dependencies:
Reports from each work packages listing recommendations for implementation within PDC
Output:
Procedure for full ranking of candidates for follow-up observations
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Low risk
PSM WPDs
DEVELOPMENT
Rank Planet Candidates
Leader: Andrew Collier Cameron
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 36/200
PSM WP 113 100
04/2016 — 12/2023
Institution: St Andrews University (UK)
Key Personnel: A. Collier Cameron
Objectives:
To specify an algorithm to be implemented by the PDC allowing the production of a list of planet candidates (and
their likelihoods)
Tasks:
1.
Continued review of the scientific literature
2.
Specify a procedure to produce a ranked list of candidates as a function of planet mass, determined
from the results from lightcurve modelling and centroid fitting.
3.
Algorithm specification and test for above
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
Dependencies:
PLATO End-to-End Simulator
Output:
Report to work package leader
Deliverables:
Report and specifications of algorithms
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
If this work is not undertaken then the efficiency of planet detection/confirmation will decline. Less efficient use
of limited follow-up observation resources
PSM WPDs
DEVELOPMENT
Specification for Space Based False Positive
Identification Through Centroid Analysis
Leader: Magali Deleuil
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 37/200
PSM WP 113 200
04/2016 — 12/2023
Institution: Laboratoire d'astrophysique de Marseille (France)
Key Personnel: M. Deleuil; A. Bonomo (INAF-Torino); J.-M. Almenara (LAM); C. Moutou (LAM) + temporary
Objectives:
To improve the quality of PLATO planet candidates by rejection of imposters as determined by their centroided
positions and lightcurves. Use as background eclipsing binary rejection technique.
Tasks:
1.
Continued review of scientific literature
2.
Review of centroiding and lightcurve measuring methods
3.
Specification and test of algorithms for centroiding lightcurves and mimic rejection
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
Dependencies:
PLATO End-to-End Simulator
Output:
Development of criteria and algorithms for centroid filtering.
Deliverables:
Report and specifications of algorithms
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
If this work is not undertaken then the efficiency of planet detection/confirmation will decline. Less efficient use
of limited follow-up observation resources
PSM WPDs
DEVELOPMENT
Astrophysical False Positives
Leader: Andrew Collier Cameron
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 38/200
PSM WP 113 300
04/2016 — 12/2023
Institution: St Andrews University (UK)
Key Personnel: A. Collier Cameron
Objectives:
To identify the list of astrophysical phenomena that can minim a planetary transit. To produce a procedure to
identify those objects effected.
Tasks:
1.
Continued review of the scientific literature.
2.
Critically examine likely and unlikely astrophysical false positives that could be present in PLATO data
including grazing and blended stellar binaries and blended transiting gas-giant systems.
3.
Find a mitigation procedure combining astrometric and photometric catalogue data with lightcurve
modelling, to allow the most efficient identification of these objects with the minimal use of ground based
telescope time.
4.
Specify and test an algorithm to apply above technique
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
Dependencies:
PLATO End-to-End Simulator
Output:
Procedure and algorithm for efficient mimic detection and mitigation.
Deliverables:
Report and algorithms
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
This WP directly affects the efficiency of the ground based follow up project and that of confirming planets.
PSM WPDs
DEVELOPMENT
Specification of Transit Fitting Tools
Leader: Szilard Csizmadia
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 39/200
PSM WP 114 000
Development phase
04/2016 — 12/2023
Institution: DLR (Germany)
Key Personnel: Sz. Csizmadia; N.N. (DLR); A. Bonomo (INAF-Torino); M Gillon (Liège)
Objectives:
Coordinating the definition and development of a prototype for the PLATO Eclipse Fitting Tool PEFT, in
coordination with the leaders of the sub-work packages WP 114 100 and WP 114 200.
PEFT will have 3 purposes:
- To help assessing the planetary nature of periodic signals found in PLATO data.
- To deduce the posterior distributions for the eclipse parameters of confirmed planets.
- To study astrophysical effects linked to the detected planets.
For details, see the document 'WP 114 000. Design specifications for PEFT, the PLATO Eclipse Fitting Tool.’
Tasks:
1.
2.
3.
4.
5.
6.
Liaise with leaders of sub-work packages WP 114 100 and WP 114 200.
Liaise with the leader of the work package WP 113 000, as PEFT will be used to rank the candidates.
Liaise with Exoplanet Coordinator and PMC Science Management Coordinator as required.
Development of a PEFT prototype.
Responsible for reports and algorithms from sub-work packages.
Responsible for delivery of a PEFT prototype to PDC.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
Simulated PLATO light curves
Dependencies:
WP 111, WP 112, PLATO End-to-End Simulator
Output:
Optimal tools to be used with PLATO data.
Deliverables:
Reports giving algorithms + models description and listing recommendations for implementation within PDC.
PEFT software.
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Low quality planetary parameters due to inadequate codes, or inappropriately applied.
PSM WPDs
DEVELOPMENT
Specify Transit Curve Modelling Tools
Leader: Szilard Csizmadia
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 40/200
PSM WP 114 100
04/2016 — 12/2023
Institution: DLR (Germany)
Key Personnel: Sz. Csizmadia; N.N. (DLR); A. Bonomo (INAF-Torino); M Gillon (Liège)
Objectives:
Specify the tools used in transit modelling
Tasks:
1.
Review of scientific literature
2.
Evaluate the suitability of commonly used simplifications (e.g. small planet approximation)
3.
Evaluate the suitability of different fitting techniques (e.g. Markov Chain Monte Carlo routines, Genetic
algorithms etc.)
4.
Specification and test of algorithms to be used and their extremes of applicability.
5.
Tests on simulated data.
6.
Assemble a team for the task
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
Simulated PLATO light curves
Dependencies:
Close interaction foreseen with the relevant tasks within WP 110, 113, 114, PLATO End-to-End Simulator
Output:
Transit fitting algorithms and their optimized areas of applicability.
Deliverables:
Report and algorithms
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
This WP will be one of the key tasks for PLATO to create L2-products. Poorly chosen algorithms, badly defined
procedures and unforeseen scientific/procedural problems will cause delay in the delivery of products.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 41/200
Specify Tools for Accurate Orbital Period
Determination
Leader: Magali Deleuil
Rev.: 5
Development phase
PSM WP 114 200
04/2016 — 12/2023
Institution: Laboratoire d'astrophysique de Marseille (France)
Key Personnel: M. Deleuil; A. Bonomo (INAF-Torino)
Objectives:
Specify period finding techniques and the generation of orbital ephemeris for single and multiple stars.
Tasks:
1.
2.
3.
4.
5.
Review of scientific literature
Evaluate the suitability of commonly used period determination techniques
Evaluate the suitability of commonly used methods of orbital ephemeris generation
Extension of the above (and evaluation) to binary and multiple star systems
Specification and test of algorithms for above.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
4.
Commonly available codes within the PLATO community or freely available
Dependencies:
WP 112, PLATO End-to-End Simulator
Output:
Ability to produce accurate ephemeris for single and multiple systems.
Deliverables:
Report and specifications of algorithms
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC.
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Non-optimized orbital solutions will lead to inaccurate ephemeris. This will make the follow-up radial velocity
observations inefficient.
PSM WPDs
DEVELOPMENT
Rossiter-McLaughlin Modelling Tools
Leader: Guillaume Hébrard
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 42/200
PSM WP 114 300
04/2016 — 12/2023
Institution: IAP/OHP (France)
Key Personnel: G. Hébrard; F. Bouchy (LAM-CNRS); A. Collier Cameron (St Andrews); M. Gillon (Liège);
Lecavelier (IAP); A. Santerne (Porto/CAUP); A. Triaud (Toronto)
A.
Objectives:
Exploration of models and algorithms for Rossiter-McLaughlin analysis
Tasks:
1.
Define and develop the algorithms and tools to compute the Rossiter-McLaughlin (RM) effect, in
classical way from radial velocity measurements and tomographic way from spectral line profile variation
analysis.
2.
Evaluate the prospects for differential RM (as a function of wavelength) for atmosphere characterization.
3.
Specify the tools for the analysis.
Input:
1.
Estimation of the planet population detected by PLATO, with their basic physical properties (mass and
radius)
2.
The physical properties of their host stars, in particular their project rotational velocity vsini
3.
Different available tools for RM analysis
Dependencies:
WP 142 XXX, WP 145 400, WP 145 100, WP 144 XXX, WP 114 000, PLATO End-to-End Simulator
Output:
Specifications of fitting tools to be included in the PLATO Eclipse Fitting Tool
Deliverables:
Report and specifications algorithms
Milestones:
04/2017: Delivery of Initial Set of scientific specifications
04/2018: Review and scientific validation implementation of algorithms done in the PDC
09/2018 – 09/2023: Cyclic updates on the scientific specifications in compliance with the PDC development plan
Risks:
Low Risk
PSM WPDs
DEVELOPMENT
Development of PLATO Data Specific Science
Leader: Don Pollacco
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 43/200
PSM WP 115 000
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco
Objectives:
Development of exoplanet science topics that impact on the analysis and subsequent follow-up of PLATO data.
Tasks:
1.
Liaise with sub-work package leaders
2.
Liaise with Exoplanet Coordinator and PMC Science Management Coordinator as required
3.
Responsibly for reports from sub-work packages
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current PLATO performance estimation
Dependencies:
WP’s in this branch
Output:
Continued review of current state of knowledge and identification of important areas for future progress
Deliverables:
Reports from each sub-work package
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
Astrophysical Noise Sources and Their Impact on RV
Determination
Leader: Chris Watson
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 44/200
PSM WP 115 100
04/2016 — 12/2023
Institution: Queens University Belfast (UK)
Key Personnel: C. Watson; 1 postdoc (QUB)
Objectives:
Understand the effects that astrophysical noise such as star spots and granulation has on the radial velocity
follow-up required – especially for low mass planets. Develop and outline mitigation procedures, thereby
enhancing the efficiency of the PLATO ground-based follow-up mission and broadening its span.
Tasks:
1.
2.
3.
4.
5.
Continued review of the scientific literature in this area.
Model astrophysical noise and quantify its impact across the PLATO discovery regime.
Algorithm development for spot jitter mitigation and follow-up optimization.
Investigate granulation jitter reduction techniques specifically for low-mass planet detection.
Identify further areas requiring science development to fully exploit PLATO data.
Input:
1.
Scientific literature and PLATO Red Book.
2.
Current estimation of PLATO performance and ground-based facility capabilities.
Dependencies:
WP 140, WP 111, PLATO End-to-End Simulator
Output:
Review of current state of knowledge in this topic and identify areas that potentially impact PLATO. Report on
potential noise mitigation procedures and reassess impact areas previously identified.
Deliverables:
Reports & specifications of noise reduction algorithms and/or strategies for ground-based follow-up.
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activities.
04/2017: Report on starspot jitter removal methods (larger planets around young/active stars).
04/2019: Interim report on granulation noise impact on radial velocity follow-up of smaller planets.
04/2022: Final report on mitigation procedures for granulation and impact for detecting small planets.
12/2023: Report on prioritizing & filtering strategies, and expected follow-up efficiency of PLATO overall.
Risks:
Reduced ground-based follow-up efficiency leading to increased pressures on ground-based facilities & overall
reduction in the scientific impact of PLATO. Successful completion of this WP will enable increased small planet
detection through efficiency savings in follow-up observations & enhanced detectability of more active systems
than is currently envisaged. This will also lead to improved prioritisation of targets suitable for follow-up, further
minimising pressure on ground-based facilities.
PSM WPDs
DEVELOPMENT
Improved Planetary System Characterisation
Leader: Alessandro Sozzetti
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 45/200
PSM WP 115 200
04/2016 — 12/2023
Institution: INAF-Torino (Italy)
Key Personnel: A. Sozzetti; 1 postdoc (INAF-Torino)
Objectives:
To take advantage of the synergy between PLATO data and any other available spectroscopic, astrometric, and
photometric info (across a broad range of wavelengths), both from the ground and in space, for improved
modelling of the system architecture but also for betterment of the stellar primary characteristics. During
implementation phase, (simulated) data from other sources will be combined with simulated PLATO data
demonstrating expected system improvements. Where applicable, observing programs will be proposed to
advance the synergetic effort ahead of PLATO launch.
Tasks:
1.
Continued review of the scientific opportunities presented from and instrumentation at current and future
facilities
2.
Use of simulated data to define comparison metrics for demonstrating the potential advantages and
improvements on planetary systems characterization from combined datasets
3.
Specification of an algorithm showing the use of external data within the different types of PLATO
planets (e.g., Gaia astrometry for large planets detected as transiting within the PLATO datasets etc.)
Input:
1.
Scientific literature
2.
Simulated (and actual) data from ground-based and space-borne facilities devoted to exoplanet
detection
3.
PLATO Red Book
4.
Current estimation of PLATO performance, via detailed simulations
Dependencies:
WP 140, WP 111, PLATO End-to-End Simulator
Output:
Simulation results on the synergy between PLATO and other planet-hunting facilities. Algorithm demonstrating
areas of applicability as a function of systems’ architecture and datasets combination. Where applicable,
observational data on PLATO targets ahead of mission launch.
Deliverables:
Detailed report with global review of published knowledge and simulation results on the synergy between
PLATO and other planet-hunting facilities. Specifications of algorithm demonstrating areas of applicability as a
function of systems’ architecture and datasets combination.
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
Planet-Star Interactions
Leader: Stéphane Mathis
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 46/200
PSM WP 115 300
04/2016 — 12/2023
Institution: CEA/DSM/LESIA - CNRS (France)
Key Personnel: S. Mathis; I. Pagano (INAF-Catania); F. Remus (Paris/CEA/DSM); A.-S. Brun (CEA-CNRS); G.
Scandariato (INAF-Catania); 1 postdoc
Objectives:
Detailed investigation on the gravitational and magnetic star-planet interactions: study of tidal interactions, of the
impact of stellar activity on planetary environments, and of magnetic couplings such as stellar wind-planetary
magnetosphere interactions and young star-disk couplings.
Tasks:
1.
Continued review of the scientific literature in this area.
2.
Science developments needed to fully exploit PLATO data: general study of tidal interactions between
planets and their host stars and of their consequences on planet and host star characteristics and dynamical
evolution; general study of magnetic interactions between planets and their host stars and young stars and
disks.
3.
Identify the main analysis tools required to extract the star-planet interaction signatures from the PLATO
light curves of planetary systems hosting Jovian planets in close-by orbits.
4.
Specify the algorithms required to extract the star-planet interaction signatures from the PLATO light
curves.
Input:
1.
Scientific literature
2.
PLATO Red Book
3.
Current estimation of PLATO performance
Dependencies:
WP 140, WP 111, PLATO End-to-End Simulator
Output:
1.
Ongoing review of published knowledge
2.
Development of theory (as required) to fully exploit PLATO data in this area
3.
Development of numerical codes (as required) to fully exploit PLATO data in this area
Deliverables:
Report, scientific publications, numerical codes and specifications of algorithms.
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of the mission.
PSM WPDs
DEVELOPMENT
Transits of Close-in Objects
Leader: Carole Haswell
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 47/200
PSM WP 115 400
04/2016 — 12/2023
Institution: The Open University
Key Personnel: C Haswell
Objectives:
Study extremely close-in bodies including very hot Jupiters (e.g. WASP-12b), disintegrating rocky planets (e.g.
KIC 1255b) and sub-planetary-sized bodies (e.g. exocomets around 51 Peg and older stars) in planetary
systems. Examine and exploit their potential for informing theories of planet formation and evolution, and
develop techniques for determining planetary compositions using mass loss from these objects. Generate
statistical predictions for the frequency of these objects and their transit characteristics, and thus assess the
benefits and drawbacks of various PLATO observing strategies.
Tasks:
1. Review of relevant scientific literature.
2. Observations and modelling of transits of these bodies.
3. Observations, modelling and characterization of circumstellar gas and dust lost from close-in orbiting bodies.
4. Calculate statistical predictions for the occurance of undiscovered close-in bodies around PLATO targets.
5. Use archive and freshly acquired stellar spectroscopy to produce quantitative probability predictions for
likelyhood of close-in bodies around individual stars within PLATO field.
Input:
1.
2.
3.
4.
5.
6.
Scientific literature
PLATO Red book
Current estimates of PLATO performance
Tools and techniques developed for analysis of mass loss in WASP-12b, KIC 1255b and similar objects
Observations of known and suspected extremely close-in planetary and sub-planetary-sized bodies.
Archive high resolution stellar spectra from instruments such as HARPS, SOPHIE, HIRES, MIKE
Dependencies:
Interaction with WP 116 200 is expected.
Output:
1. Prioritisation of targets within the PLATO field.
2. Population characterisation: Knowledge of the number and size distribution of extremely close-in orbiting
bodies.
3. Tools and techniques for constraining the composition of close-in bodies from suitable transmission
spectroscopy and photometry of transiting material lost from disrupting/evaporating planets
Deliverables:
Catalogue of confirmed and candidate hosts of mass-losing close-in bodies.
Interim and final reports.
Milestones:
07/2017: Delivery of interim report
04/2024: Delivery of final report on activity
Risks: Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Non-Transiting Planets via REBs
Leader: David Barrado
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 48/200
PSM WP 115 500
04/2016 — 12/2023
Institution: Centro de Astrobiología, INTA-CSIC (Spain)
Key Personnel: D. Barrado; H. Bouy (CAB, INTA-CSIC); N. Huélamo (CAB, INTA-CSIC); M. Morales-Calderón
(CAB, INTA-CSIC); J. Lillo-Box (CAB, INTA-CSIC)
Objectives:
Detection of non-transiting planets via beaming and ellipsoidal effects in the light curve (REBs).
Tasks:
1.
Preparation of the detection and modelling of the out-of-transit region of the light-curves to look for the
ellipsoidal and beaming effects, both able to provide the mass of the surrounding planets for non-transiting
systems.
2.
Development of the statistical algorithm to analyse the high-spatial resolution images to be obtained once
the planet host candidates are available. Strategy to prioritize the candidates. Feedback on task #1.
Input:
Task 1 - Current PLATO performance estimate. Kepler (and CHEOPS) light curves.
Task 2 - Simulated high-resolution images to test the algorithm. Application of the algorithm to already existing
high-resolution images from different ground-based instruments to test the algorithm.
Dependencies:
Task 1 - WP 111 000, 112 100, 112 300, 112 400, 114 000, 123 100, 125 000, 141 400.
Task 2 - WP 112 000, 113 000, 132 100, 143 000.
Output:
Task 1 - Expected efficiency finding non-transiting planets.
Task 2 - Algorithm to analyse the high-spatial resolution images.
Deliverables:
Task 1 - Detection and modelling algorithms and planet yield estimate based on REBs. Report on findings.
Task 2 - Report and algorithm.
Milestones:
Task 1:
12/2017 Algorithm verification and delivery to PDC for implementation.
12/2020 Re-evaluation with CHEOPS data
Task 2:
12/2018 Algorithm verification and delivery to PDC for implementation.
Risks:
Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
Development of PLATO Interpretation Specific
Science
Leader: Heike Rauer
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 49/200
PSM WP 116 000
04/2016 — 12/2023
Institution: DLR (Germany)
Key Personnel: H. Rauer
Objectives:
Development of exoplanet science topics that impact on the interpretation of PLATO data.
Tasks:
1. Liaise with sub-work package leaders
2. Liaise with Exoplanet Coordinator and PMC Science Management Coordinator as required
3. Responsibly for reports from sub-work packages
Input:
1.
Scientific literature
2.
PLATO Red Book
3.
Current estimation of PLATO performance
Dependencies:
WP 110, PLATO End-to-End Simulator
Output:
Continued review of current state of knowledge and identification of important areas for future
Deliverables:
Reports from each sub-work package
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
Rev.: 5
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 50/200
Compositions & Formation of Gas & Ice Giants
Leader: Tristan Guillot
Rev.: 5
Development phase
PSM WP 116 100
04/2016 — 12/2023
Institution: OCA/CNRS (France)
Key Personnel: T. Guillot; M. Havel (OCA)
Objectives:
Understand the expected impact of PLATO photometry on the mass vs. radius relationship of gas giants and its
implications for their structure, composition and formation.
Tasks:
1.
Develop software enabling a routine, homogeneous calculation of the evolution of exoplanets (gas to ice
giants) to be discovered by PLATO
2.
Develop expertise for a statistical analysis of the data
3.
Link planet evolution/structure/composition with up-to-date formation scenarios.
Input:
1.
CESAM/CEPAM stellar & planet evolution codes
2.
Scientific literature
3.
PLATO Red Book
Dependencies:
WP 110, PLATO End-to-End Simulator
Output:
Scientific analysis ‘pipeline’ including data analysis method and modelling software
Deliverables:
Reports, data analysis method, planet evolution modelling tool.
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 51/200
The Mass-Radius Relationship for Terrestrial Planets
Leader: Frank Sohl
Rev.: 5
Development phase
PSM WP 116 200
04/2016 — 12/2023
Institution: DLR (Germany)
Key Personnel: F. Sohl; N.N. (DLR)
Objectives:
Investigate the expected use of PLATO photometry and ground-based radial velocity observations for structural
and compositional models of solid exoplanet interiors as inferred from corresponding mass vs. radius
relationships.
Tasks:
1.
Continued review of the scientific literature in this area
2.
Construction of depth-dependent interior structure models of solid exoplanets (including CoRoT and
Kepler results)
3.
Science development needed to fully exploit PLATO data
Input:
1.
Scientific literature
2.
PLATO Red Book
3.
Current estimation of PLATO performance
4.
Commonly available codes within the PLATO community or freely available
Dependencies:
WP 110, PLATO End-to-End Simulator
Output:
1.
Ongoing review of published knowledge
2.
Development of theory (as required) to fully exploit PLATO data in this area
Deliverables:
Report
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of the mission.
PSM WPDs
DEVELOPMENT
Planetary Formation and Orbital Evolution
Leader: Richard Nelson
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 52/200
PSM WP 116 300
04/2016 — 12/2023
Institution: Queen Mary, University of London (UK)
Key Personnel: R. Nelson; O. Gressel (NBI); W. Kley (Tuebingen); A. Johansen (Lund); Y. Alibert (Bern);
Morbidelli (OCA); M. Davies (Lund); M. Wyatt (IoA, Cambridge); C. Mordasini (Bern)
A.
Objectives:
Simulate the formation and orbital evolution of planetary systems to mimic the expected PLATO population.
Consider range of environments, including binary stars and stellar clusters, and their impact on formation and
post-formation evolution. Prepare statistical analysis tools for comparing simulations with data.
Tasks:
1.
Continued review of relevant scientific literature
2.
Development of planet formation and migration theory, and models for long-term orbital evolution,
covering planets with full range of masses in a broad range of environments
3.
Code development to enable global models of planet formation and long-term evolution to be performed
4.
Run suites of simulations to generate synthetic planetary populations; calibrate against CoRoT and
Kepler data using statistical analysis tools
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
Dependencies:
Close interactions foreseen with the all subpackages within WP 116, and WP 112 500, WP 115 200, WP 115
300, WP 115 400
Output:
1.
New theoretical insights into mechanisms of planet formation, migration and long-term dynamical
evolution
2.
Synthetic planet populations generated using state-of-the-art theoretical models
3.
Ongoing review of published knowledge
4.
Software tools for simulating formation and orbital evolution of planetary systems in global context
Deliverables:
End-to-end planetary formation and orbital evolution simulation tools, calibrated against CoRoT and Kepler
Synthetic planetary populations in anticipation of launch and data collection
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Protoplanetary Disc Models
Leader: Oliver Gressel
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 53/200
PSM WP 116 310
04/2016 — 12/2023
Institution: Niels Bohr Institute (Denmark)
Key Personnel: O. Gressel; S. Fromang (AIM); S.J. Paardekooper (QMUL); B. Bitsch (Lund); A. Morbidelli
(OCA); L. Mayer (Zürich); R. Alexander (Leicester); M. Flock (AIM); H. Latter (Cambridge); G. Lodato (Milan);
D. Forgan (St Andrews); K. Rice (Edinburgh); E. Szuszkiewicz (Szczecin); P. Loren (Exeter); M. Bate (Exeter);
J. Papaloizou (Cambridge); C. Surville (MPIA); H. Meheut (AIM); G. Ogilvie (Cambridge); E. Vorobiev (Vienna);
G. Lesur (Grenoble); F. Meru (IoA, Cambridge); S. Charnoz (AIM); C. Clarke (IoA, Cambridge);
C. Dullemond
(Heidelberg); R. Nelson (QMUL)
Objectives: Develop state-of-the-art simulations of protoplanetary discs (PPDs) that incorporate the most up-todate chemical and physical processes. Model development will require inclusion of non-ideal MHD effects, selfgravity, thermal/radiative processes, photoevaporation and chemistry to examine evolution of discs through their
complete life-cycles and to assess role of disc evolution in the formation and evolution of planets.
Tasks:
1.
2.
3.
4.
Continued review of scientific literature
Development of theoretical understanding of protoplanetary disc evolution
Code development to enable ever more sophisticated global models of PPDs to be computed
Run suites of calculations to simulate disc evolution and assess influence of planet formation
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Observational data from ALMA etc.
Dependencies:
Close interaction foreseen with WP 116 320, WP 116 330, WP 116 350 and WP 116 360
Output:
New theoretical insight into (magneto-) hydrodynamic stability of discs, the role of self-gravity, formation and
evolution of vortices, and long-term evolution due to stellar irradiation.
Simulations of discs that provide insight into role of disc evolution on the formation and evolution of planets at all
stages of the disc life-cycle
Deliverables:
Sophisticated protoplanetary disc models, calibrated against observations of PPDs obtained e.g. by ALMA
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
02/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks: Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Disc-Planet Interactions
Leader: Wilhelm Kley
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 54/200
PSM WP 116 320
Development phase
04/2016 — 12/2023
Institution: University of Tuebingen (Germany)
Key Personnel: W.Kley; S.J. Paardekooper (QMUL); F. Marzari (INAF-Padova); A. Morbidelli (OCA);
A.
Johansen (Lund); B. Bitsch (Lund); R. Alexander (Leicester); A. Crida (OCA); M. Flock (AIM); A. Pierens (LAB);
G. Lodato (Milan); C. Baruteau (IRAP); E. Szuszkiewicz (Szczecin); O. Gressel (NBI);
N.
Madhusudhan (IoA, Cambridge); P. Loren (Exeter); M. Bate (Exeter); J. Papaloizou (Cambridge); F. Meru (IoA,
Cambridge); S. Charnoz (AIM); C. Migaszewski (NCU); C. Terquem (Oxford); Y. Alibert (Bern);
C.
Mordasini (Bern); R. Nelson (QMUL)
Objectives: To study in detail the physics of disc-planet interaction for young planets that are embedded in the
protoplanetary disc. The goal is to create a suite of simulations under different physical conditions to provide
simplified expression for migration and mass growth that can be used in other models that study the evolution of
planets to compare with the expected PLATO sample.
Tasks:
1.
Continued review of relevant scientific literature
2.
Development of disc-planet simulations using realistic disc models that include all relevant physics
3.
Extend and improve existing numerical modelling approaches to cover local to global length scales.
4.
Run 2D and 3D simulations for an extended set of parameters and develop adapted scaling functions to
be used in other approaches in order to construct estimates for the expected PLATO sample
5.
Perform multi-planet simulations and study their emerging system architecture and long term evolution
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
4.
Commonly available codes within the PLATO community or freely available
Dependencies:
Close interactions foreseen with all subpackages within WP 116.
Output: New theoretical insights into physical mechanisms of planet migration in discs
Increased knowledge about the long-term evolution of planets and planetary systems
Important input for population synthesis modellers
Publication of obtained results in peer-reviewed journals
Deliverables:
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks: Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
The Assembly of Planetary Systems
Leader: Yann Alibert & Anders Johansen
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 55/200
PSM WP 116 330
04/2016 — 12/2023
Institution: University of Bern (Switzerland) & Lund University (Sweden)
Key Personnel: Y. Alibert; A. Johansen; R. Helled (Tel-Aviv); Z. Leinhardt (Bristol); A. Morbidelli (OCA);
B.
Bitsch (Lund); L. Mayer (Zürich); R. Alexander (Leicester); H. Latter (Cambridge); C. Baruteau (IRAP);
D.
Forgan (St Andrews); E. Lopez (Edinburgh); N. Madhusudhan (IoA, Cambridge); J. Papaloizou (Cambridge); F.
Meru (IoA, Cambridge); S. Nayakshin (Leicester); C. Mordasini (Bern); C. Dullemond (Heidelberg); R. Nelson
(QMUL)
Objectives:
Develop comprehensive models of planetary system formation for comparison with the PLATO data.
Tasks:
1.
2.
3.
4.
Continued review of relevant scientific literature
Addressing formation based on core-accretion and disk-instability models
Code development to enable global models of planet formation
Run population synthesis models providing predictions for the architecture of planetary systems
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
Dependencies:
Close interactions foreseen with the all subpackages within WP 116, in particular with WP 116 310, WP 116 320
(input), WP 116 340 (output) and WP 116 380
Output:
1.
End-to-end planet formation models
2.
Synthetic planet populations generated using state-of-the-art theoretical models
3.
Ongoing review of published knowledge
4.
Software tools for simulating formation of planetary systems in global context
Deliverables:
End-to-end planetary formation simulation tools
Synthetic planetary populations in anticipation of launch and data collection
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
The Post-Formation Long-Term Dynamical Evolution
of Planetary Systems
Leader: Alessandro Morbidelli
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 56/200
PSM WP 116 340
04/2016 — 12/2023
Institution: Observatoire de la Cote d’Azur (France)
Key Personnel: A. Morbidelli; D. Veras (Warwick); F. Marzari (INAF-Padova); K. Rice (Edinburgh);
K.
Gozdziewski (NCU); C. Migaszewski (NCU); E. Szuszkiewicz (Szczecin); G. Ogilvie (Cambridge); C. Agnor
(QMUL); A. Bonsor (Bristol); Y. Alibert (Bern); C. Mordasini (Bern); R. Nelson (QMUL)
Objectives: Simulate the orbital evolution of planetary systems after the removal of the disk of gas, in order to
mimic the expected PLATO population.
Tasks:
1.
Continued review of relevant scientific literature
2.
Run suites of simulations using as initial conditions the planetary orbits issued from studies of planet
formation and evolution in gas-disk, to understand the long-term evolution of these systems, the change of
architecture through dynamical instability phases and tidal interactions, the final distributions for mature systems
3.
Investigate the role of planetesimals in the long-term evolution of planetary systems
4.
Compare the outcomes with known planetary systems discovered from existing surveys
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Planetary systems issued from WP 116 320 & 330
Dependencies:
Close interactions foreseen with the all subpackages within WP 116
Output:
1.
New theoretical insights into mechanisms leading to planet instabilities and on the long-term evolution of
planetary systems
2.
Transformation of the planetary systems as they emerge from the gas-disk phase into mature planetary
systems for main sequence stars.
3.
Ongoing review of published knowledge
Deliverables:
Scientific publication of results
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Planet Formation and Evolution in Binary Systems
Leader: Richard Nelson
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 57/200
PSM WP 116 350
04/2016 — 12/2023
Institution: Queen Mary, University of London (UK)
Key Personnel: R. Nelson; S. J. Paardekooper (QMUL); R. Helled (Tel-Aviv); Z. Leinhardt (Bristol);
F.
Marzari (INAF-Padova); R. Alexander (Leicester); A. Pierens (LAB); G. Lodato (Milan); K. Gozdziewski (NCU);
W. Kley (Tuebingen)
Objectives: To develop models of planet formation and evolution in binary systems, including both circumbinary
planets and planetary systems with external binary companions. The models will consider all phases of
planetary formation, and the long-term evolution after disc dispersal. A major goal is to make predictions about
the population of circumbinary planets that will be observed by PLATO, and to make predictions about the
influence that external companions will have on the PLATO planet population.
Tasks:
1.
Review of relevant scientific literature
2.
Code development for running simulations of planet formation in binary systems
3.
Performing simulations that examine formation, migration and growth of planets in binaries during the
phase when the protoplanetary disc is present according to various scenarios (core accretion, gravitational
fragmentation, etc.)
4.
Simulations that examine long-term dynamical evolution with different binary configurations
5.
Compare simulation results with existing data (e.g. Kepler data) for calibration
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
4.
Disc models from WP 116 310
Dependencies:
Close interaction with WP 116 310, WP 116 320, WP 116 330, WP 116 340, WP 116 380, WP 112 510
Output:
Formation models of circumbinary planets and planets with external binary companions
Results on the long-term dynamical evolution of planets in binary systems
Software tools for simulating planet formation and evolution in binaries.
Deliverables:
Synthetic planet populations in anticipation of launch
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks: Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
Influence of Birth Environment on the Formation and
Evolution of Planetary Systems
Leader: Melvyn Davies
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 58/200
PSM WP 116 360
04/2016 — 12/2023
Institution: Lund University (Sweden)
Key Personnel: M. Davies; R. Church (Lund); Z. Leinhardt (Bristol); E. Vorobiev (Vienna); A. Mustill (Lund); I.
Bonnell (St Andrews); J. Dale (USM); F. Meru (IoA, Cambridge); G. Rosotti (IoA, Cambridge); C. Clarke (IoA,
Cambridge)
Objectives:
A comprehensive analysis of how birth environments (e.g. density and mass of birth cluster) modify the
properties of the planetary population.
Tasks:
1.
Review of relevant scientific literature
2.
Development of theory of effects of close encounters on protoplanetary discs in the birth environments
of their host stars.
3.
Development of theory of close encounters and other processes affecting planetary systems in the birth
environments of their host stars.
4.
Simulations of the evolution of protoplanetary discs and young planetary systems in stellar birth
environments
Input:
1.
Scientific literature
2.
PLATO red book
3.
Current estimates of PLATO performance
Dependencies:
Close interactions foreseen with all sub-subpackages within WP 116 300 particularly with WP 116 330 and WP
116 340
Output:
New theoretical insights into processes affecting protoplanetary discs and planetary systems in clusters.
Models of the effects of encounters on planetary populations.
Ongoing review of published knowledge.
Deliverables:
Quantified effects of encounters/irradiation on protoplanetary discs and planetary systems within birth clusters.
2018: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2019: Delivery of interim reports
12/2024: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Post-Main Sequence Evolution of Planetary Systems
Leader: Mark Wyatt
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 59/200
PSM WP 116 370
04/2016 — 12/2023
Institution: University of Cambridge (UK)
Key Personnel: M. Wyatt; D. Veras (Warwick); E. Villaver (UAM); M. Davies (Lund); A. Mustill (Lund);
Migaszewski (NCU); A. Bonsor (Bristol)
C.
Objectives:
Model the evolution of the planetary systems known to exist around main sequence stars as the stars evolve
into the post-main sequence phase, and to ascertain the detectability with PLATO of this population at different
evolutionary phases
Tasks:
1.
Continued review of relevant scientific literature
2.
Development of theory for planetary system evolution that takes account of stellar evolution into the
post-main sequence phase
3.
Simulations of detectability of post-main sequence planetary systems with PLATO
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
Dependencies:
Close interactions with many sub-packages within WP 116 300, particularly WP 116 340 and 380
Output:
1.
New theoretical insights into the evolution of planetary systems in the post-main sequence phase
2.
Ongoing review of published knowledge
3.
Simulations of observability of post-main sequence planetary systems with PLATO
Deliverables:
1.
2021: Interim report on scientific activity
2.
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Statistical Comparison Between Theory and PLATO
Data
Leader: Christoph Mordasini
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 60/200
PSM WP 116 380
04/2016 — 12/2023
Institution: University of Bern (Switzerland)
Key Personnel: C. Mordasini; Y. Alibert (Bern); A. Johansen (Lund); M. Davies (Lund); R. Church (Lund);
Alexander (Leicester); E. Lopez (IoA, Cambridge); C. Migaszewski (NCU); A. Mustill (Lund); S. Nayakshin
(Leicester); R. Nelson (QMUL)
R.
Objectives:
Extraction of predicted statistics from theoretical models, and preparation of the statistical comparison with the
PLATO data. Identification of quantitative measures of the level of agreement between statistical predictions by
the models and the PLATO data, to be used for refinement of the theoretical investigations post-launch.
Tasks:
1.
Continued review of relevant scientific literature
2.
Determination of key statistical quantities for the comparison: distributions of radii, periods, masses,
eccentricities, inclinations, multiplicity, etc. and correlations between these quantities.
3.
Code development to enable quantitative statistical comparison between results of different theoretical
models and PLATO data (Kolmogorov-Smirnov tests, correlation coefficients etc.)
4.
Preparation of a library of simulated planetary systems from different planet formation and evolution
models (core accretion, gravitational instability, etc.).
5.
Potentially: development of an interactive online interface for efficient upload of simulated planetary
systems prepared by other WPs into the library; associated unified online statistical analysis tools.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
4.
Statistical predictions from theoretical models
Dependencies:
Close interactions foreseen with the all subpackages within WP 116, in particular with WP 116 330, WP 116 340
(input), WP 116 350, and WP 116 360 (input)
Output:
1.
Preparation for the assessment of the theoretical descriptions by comparison with PLATO data
2.
Ongoing review of published knowledge
3.
Software tools for statistical comparison and library of synthetic planetary systems
Deliverables:
Numerical tools to perform statistical comparison between models and PLATO data
Test of the tools on simulated PLATO data as well as on CoRoT and KEPLER data
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks: Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 61/200
Atmospheres of PLATO Terrestrial Planets
Leader: John Lee Grenfell
Rev.: 5
Development phase
PSM WP 116 400
04/2016 — 12/2023
Institution: DLR (Germany)
Key Personnel: J. L. Grenfell; H. Rauer (DLR); F. Selsis (Bordeaux, CNRS)
Objectives:
Examination of current exoplanet model atmospheres for the expected population of terrestrial planets that
PLATO will be sensitive to.
Estimation of the likelihood of detection with other facilities such as the E-ELT or the JWST.
Tasks:
1.
Continued review of the scientific literature in this area
2.
Science development needed to fully exploit PLATO data
Input:
1.
Review of the scientific literature in this area
2.
PLATO Red Book
3.
Current estimation of PLATO performance
Dependencies:
WP 110, PLATO End-to-End Simulator
Output:
1.
Ongoing review of published knowledge.
2.
Development of theory (as required) to fully exploit PLATO data in this area.
Deliverables:
Report
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
PLATO Habitable Zone Planets
Leader: Manuel Güdel / Helmut Lammer
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 62/200
PSM WP 116 500
04/2016 — 12/2023
Institution: University of Vienna (Austria) / Space Research Institute, Austrian Academy of Sciences (Austria)
Key Personnel:
Objectives:
Tasks:
Input:
Dependencies:
Output:
Deliverables:
Milestones:
Risks:
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 63/200
The Environments of PLATO Habitable Zone Planets
Leader: Helmut Lammer
Rev.: 5
Development phase
PSM WP 116 510
04/2016 — 12/2023
Institution: Space Research Institute, Austrian Academy of Sciences (Austria)
Key Personnel: H. Lammer; 2 co-workers (SRI, AAS)
Objectives:
Evaluation of likely environmental (stellar and planetary) conditions for habitable zone planets typical of those
expected in the PLATO surveys.
Tasks:
1.
Continued review of the scientific literature in this area
2.
Science development needed to fully exploit PLATO data
Input:
1.
Scientific literature
2.
PLATO Red Book
3.
Current estimation of PLATO performance
Dependencies:
WP 110, PLATO End-to-End Simulator
Output:
1.
Ongoing review of published knowledge.
2.
Development of theory (as required) to fully exploit PLATO data in this area.
Deliverables:
Report
Milestones:
06/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
DEVELOPMENT
Astrophysical Factors Influencing Habitability of
PLATO Planets
Leader: Manuel Güdel
Institution: University of Vienna (Austria)
Key Personnel:
Objectives:
Tasks:
Input:
Dependencies:
Output:
Deliverables:
Milestones:
Risks:
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 64/200
PSM WP 116 520
04/2016 — 12/2023
PSM WPDs
DEVELOPMENT
Climate / Atmospheres of PLATO Habitable Zone
Planets
Leader: John Lee Grenfell
Institution: DLR (Germany)
Key Personnel:
Objectives:
Tasks:
Input:
Dependencies:
Output:
Deliverables:
Milestones:
Risks:
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 65/200
PSM WP 116 530
04/2016 — 12/2023
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 66/200
Dynamical Interactions in Multi-Planet Systems
Leader: Jacques Laskar
Rev.: 5
Development phase
PSM WP 116 600
04/2016 — 12/2023
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: J. Laskar; A. Correia (Aveiro); G. Boué (IMCCE); A. Fienga (OCA)
Objectives:
Develop the tools and theory for a better understanding of the orbital and rotational evolution of multi-planet
systems in order to be ready for the analysis and interpretation of the PLATO data. Consider the constraints that
can be raised by dynamical evolution for an improved analysis of the PLATO data.
Tasks:
1.
Continued review of relevant scientific literature
2.
Development of planetary systems evolution with an emphasis on close in planets and resonant
systems.
3.
Code development to enable PLATO data analysis together with dynamical constraints.
4.
Understanding of the various dissipative effects of importance for the dynamical evolution and structure
of multi planet systems, including orbital and rotational motion.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
4.
Input from the results of the KEPLER and CHEOPS mission and Earth based observations.
Dependencies:
Close interactions foreseen with the subpackages within WP 112, WP 113, WP 114, WP 115, WP 116
Output:
1.
New theoretical insights on planetary systems long-term evolution when considering both orbital and
rotational motions.
2.
New insights on the role of resonances in multi-planet systems.
3.
Ongoing review of published knowledge
Deliverables:
1.
Software tools for the analysis of PLATO data with dynamical constraints, benchmarked with Kepler and
CHEOPS
2.
Interim report on scientific activity
3.
Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Long-Term Dynamical Evolution of Planetary
Systems
Leader: Jacques Laskar
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 67/200
PSM WP 116 610
04/2016 — 12/2023
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: J. Laskar
Objectives: Develop criterions for forecasting the long-term dynamical stability of multi-planet systems.
Tasks:
1.
2.
3.
4.
Continued review of relevant scientific literature.
Develop software for a fast prediction of long-term stability of planetary systems.
Investigate the role of resonances in the long-term evolution of planetary systems.
Use as test beds the planetary systems from existing surveys.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Input from the results of the KEPLER and CHEOPS mission and Earth based surveys.
Dependencies: Interactions foreseen with the all subpackages within WP 116, and with WP 115 300
Output:
1.
New theoretical insights into mechanisms leading to long-term instabilities in planetary systems.
2.
New criterions for forecasting long-term stability from the PLATO observed configuration.
3.
Ongoing review of published knowledge
Deliverables:
Scientific publication of results
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Stability and Resonances in Multi-Planet Systems
Leader: Jacques Laskar
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 68/200
PSM WP 116 620
04/2016 — 12/2023
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: J. Laskar
Objectives: Develop the theoretical tools and software for a better understanding of the global dynamics of
multi-planet systems in presence of resonance or not.
Tasks:
1.
Continued review of relevant scientific literature.
2.
Develop theory for the analysis of the resonant structure of planetary systems dynamics. Evaluate the
impact on observational data. Consider the case of 1:1 resonances.
3.
Develop software tools for analysis of the global dynamics in the vicinity of observed configuration.
4.
Investigate the role of resonances in the long-term evolution of planetary systems.
5.
Use as test beds the planetary systems from existing surveys.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Input from the results of the KEPLER and CHEOPS mission and Earth based surveys.
Dependencies: Interactions foreseen with the all subpackages within WP 116 and WP 115 300
Output:
1.
New theoretical insights into resonant dynamics in planetary systems.
2.
New software tools for studying the global dynamics for the PLATO observed systems.
3.
Ongoing review of published knowledge
Deliverables:
Scientific publication of results
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Tidal Dissipation and Evolution of Multi-Planet
Systems
Leader: Alexandre C. M. Correia
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 69/200
PSM WP 116 630
04/2016 — 12/2023
Institution: University of Aveiro (Portugal)
Key Personnel: A. Correia
Objectives:
Develop the tools and theory for a better understanding of the tidal dissipation and evolution of multi-planet
systems in order to be ready for the analysis and interpretation of the PLATO data. Determine additional
constraints for the PLATO planets that will be inferred from the observed tidally evolved configurations
Tasks:
1.
Continued review of relevant scientific literature
2.
Develop a library of routines designed to simulate long-term tidal evolution of planets in multi-planet
systems using different rheological models
3.
Investigate the role of orbital architecture and internal structure on the long-term tidal evolution of multiplanet systems in order to search for constraints the planets to be observed
4.
Run the code on known planetary systems discovered from existing surveys
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Current estimates of PLATO performance
Dependencies:
Close interactions foreseen with all sub-packages within WP 116, and WP 114 200, WP 115 200, and WP 115
300.
Output:
1.
A library dedicated to the analysis of the long-term tidal evolution of planets in multiple systems
2.
New theoretical insight on planetary evolution in multiple systems depending on different orbital
architectures and internal structures
3.
Ongoing review of published knowledge
4.
Deliverables:
Scientific publication of results
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Rotational Evolution of Planets in Multiple Systems
Leader: Gwenaël Boué
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 70/200
PSM WP 116 640
Development phase
04/2016 — 12/2023
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: G. Boué
Objectives: Have an efficient library to analyse the rotation motion of the planets that will be detected by
PLATO.
Tasks:
1.
Continued review of relevant scientific literature
2.
Develop a library of routines designed to simulate the short term and the long term rotation of planets in
multi-planet systems either in or outside spin-orbit resonance
3.
Investigate the role of orbital architecture and internal structure on the long term evolution of planetary
spin axis
4.
Run the code on known planetary systems discovered from existing surveys
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Input from the results of the KEPLER and CHEOPS mission and Earth based surveys.
Dependencies: Close interactions foreseen with the all subpackages within WP 116
Output:
1.
A library dedicated to the analysis of the rotational dynamics of planets in multiple systems
2.
New theoretical insight on planetary rotation evolution in multiple systems with different orbital
architectures
3.
Ongoing review of published knowledge
Deliverables:
Scientific publication of results
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 71/200
Planetary Ephemerides of PLATO Systems
Leader: Agnes Fienga
Rev.: 5
Development phase
PSM WP 116 650
04/2016 — 12/2023
Institution: Observatoire de la Côte d’Azur (France)
Key Personnel: A. Fienga
Objectives: Develop a planetary ephemerides database for PLATO multi-planet systems.
Tasks:
1.
2.
3.
4.
Continued review of relevant scientific literature.
Develop software for a fast elaboration of planetary ephemerides for the PLATO multi-planet systems.
Investigate best representation for exoplanet ephemerides.
Use as test beds the planetary systems from existing surveys.
Input:
1.
Scientific literature
2.
PLATO Red book
3.
Input from the results of the CHEOPS mission and Earth based surveys.
Dependencies: Interactions foreseen with the all subpackages within WP 116 600
Output:
1.
New theoretical insights for planetary ephemerides elaboration for large number of planetary systems.
2.
Elaboration of a database for ephemerides of known planetary systems.
3.
Ongoing review of published knowledge
Deliverables:
Scientific publication of results
Database for the planetary ephemerides of selected planetary systems.
2021: Interim report on scientific activity
2023: Final report on scientific activity
Milestones:
03/2021: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
DEVELOPMENT
Specifications for Interface to Other PSM WPs and
PDC
Leader: Nuno Santos
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 72/200
PSM WP 117 000
04/2016 — 12/2023
Institution: CAUP (Portugal)
Key Personnel: N. Santos; D. Pollacco (Warwick)
Objectives:
To specify required data needed from other (primarily stellar) work packages and its method of retrieval and use.
Assessment of required data accuracy to reach mission goals.
Tasks:
1.
Continued review of scientific literature.
2.
Assessment of required input stellar data needed per system and evaluation of its quality. Identify further
observations if required (either on PLATO or other facilities).
3.
Evaluation of stellar parameters from asteroseismology
4.
Evaluation of stellar evolution models and in particular stellar ages and relationships with observational
parameters.
5.
Specifications of parameters (and their errors) to be included in database. Assess most important
parameters that could aid the database design.
6.
Specify design of most useful tools to aid data-mining the archive.
Input:
1.
Scientific literature
2.
PLATO Red Book
3.
PLATO current performance
4.
PLATO work packages WP 121/122/124/125/126/127/128/129
Dependencies:
Stellar work packages WP 121/122/124/125/126/127/128/129
Output:
Report specifying form of interface to PDC. Also contains details of required data and accuracy needed.
Deliverables:
Report
Milestones:
01/2019: Delivery of interim reports
12/2023: Delivery of final report on WP activity
Risks:
Efficiency of planet detection and confirmation will be seriously impaired if this work package is not successfully
completed.
PSM WPDs
DEVELOPMENT
Stellar Science Coordination
Leader: Marie-Jo Goupil
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 73/200
PSM WP 120 000
04/2016 — 12/2023
Institution: Observatoire de Paris (France)
Key Personnel: M.J. Goupil; K. Belkacem (LESIA, Paris)
Objectives:
Coordination of the works of the work packages WP 121 000 to WP 129 000.
Tasks:
1.
Ensure that the necessary work is done by the Stellar Science WPs on time and the outputs have the
requested quality level
2.
Organization of working and review meetings gathering the leaders of the WPs
3.
Delivery of scientific specifications for both algorithms and tools
4.
Review scientific validation
Input:
1.
Scientific specifications from the sub-packages WP 121 000 to WP 129 000.
2.
Scientific validation and update of the algorithms by the Stellar Science WP 121 000 to WP 129 000.
Dependencies:
Input and output from PDC (WP 370) and PSM (WP 100, WP 110, WP 130, WP 160); PLATO End-to-End
Simulator.
Output:
1.
Validated stellar models.
2.
Scientific specifications for algorithms and tools related to the accurate characterisation of stars from the
core program.
Deliverables:
Reports, algorithms and tools
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Delivery of first generation of validated models and procedures related to the characterization of host
stars
05/2022: Delivery of second generation of validated models and procedures related to the characterization of
host stars
Risks:
Acceptable risks of delay for delivering second generation of stellar models and frequencies
PSM WPDs
DEVELOPMENT
Stellar Models
Leader: Marc-Antoine Dupret
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 74/200
PSM WP 121 000
Development phase
04/2016 — 12/2023
Institution: University of Liège (Belgium)
Key Personnel: M-A Dupret; A. Noels (Liège); R. Scuflaire (Liège); key personnel of WP 121 100 to WP 121
500
Objectives: To provide grids of high quality stellar models and their pulsation frequencies specifically for the
stars belonging to the core program.
Tasks:
Coordination of works from work packages WP 121 100 to WP 121 500.
1.
Provide grids of state-of-the-art stellar models produced by selected, accurate and tested stellar
evolution codes (WP 121 100), from very low mass (WP 121 110) to intermediate mass (WP 121 120), including
the PMS phase (WP 121 300), along with their pulsation frequencies (WP 121 130);
2.
Develop improved descriptions for the constitutional physics of stars with specific emphasis on transport
processes of chemicals and angular momentum (WP 121 200) and through 2-3-D simulations of rotation (WP
121 400), convection (WP 122 100 and WP 123 200) and the influence of binarity (WP 121 500);
3.
Implement these improved descriptions in stellar evolution codes;
4.
Test these improvements with available (CoRoT and Kepler) data.
5.
Impact of the improvement on the accuracy of stellar ages.
Input:
1.
Existing stellar model grids and evolutionary codes, legacy from CoRoT similar work (ESTA),
2.
Existing 2D/3D hydro codes; results from hydro-simulations
Dependencies:
1.
Input from WP 121 200, 300, 400 and WP 122 000, WP 123 200, WP 127 100 for WP 121 100
2.
WP 121 200 and 500 are connected
Output:
Grids of first generation stellar models, evolutionary tracks and oscillation frequencies.
Deliverables:
Updated validated stellar model grids, evolutionary tracks and oscillation frequencies, with full documentation.
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Grids of first generation of validated stellar models
05/2022: Grids of second generation of validated stellar models
Risks: None
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 75/200
1D Stellar Models
Leader: Yveline Lebreton
Rev.: 5
PSM WP 121 100
Development phase
04/2016 — 12/2023
Institution: Observatoire de Paris, GEPI (France)
Key Personnel: Y. Lebreton; S. Cassisi (INAF-Teramo); J. Montalban (INAF-Padova); J.C. Suárez (Granada);
P. Ventura (INAF-Rome); J.P. Marques (IAS-Orsay)
Objectives: Provide grids of high quality stellar models and associated frequencies.
Tasks:
1.
Provide grids of models from very low mass to intermediate mass stars covering evolutionary stages
from pre main sequence to sub-giant stages.
2.
Implement in stellar evolution codes (1) the angular momentum and/or chemical elements transport
induced by rotation and/or waves with improved transport coefficients, and (2) an improved description of
convective core overshooting (3) an improved description of surface convection.
3.
Compare representative sets of models computed by the different groups participating to the project
4.
Provide the oscillation spectra associated to the models and computed by different oscillation codes.
Perform seismic tests.
5.
Test the implementation by modelling stars in open clusters, binaries and stars with available seismic
data.
Input:
1.
Existing stellar evolutionary codes appropriate to calculate PMS, MS, subgiant branch stellar models.
2.
Existing stellar oscillation codes.
3.
Model atmospheres to be used as boundary conditions (from WP 122 000).
4.
Improved formulations for heat, chemical element and angular momentum transport from WP 121 200,
WP 121 300, 127 100 and from WP 122 000 (model atmospheres) and WP 123 200 (surface convection).
Dependencies: WP 121 200, WP 121 300 and WP 122 000, WP 123 200, WP 127 100
Output:
Grids of stellar models, evolutionary tracks and oscillation frequencies.
Deliverables:
Stellar model grids, evolutionary tracks and oscillation frequencies, with full documentation.
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Grids of first generation of validated stellar models
05/2022: Grids of second generation of validated stellar models
Risks:
None. The group has a wide expertise in stellar models and oscillation computation. They have participated
actively to several studies of detailed comparisons of related codes. Main tools are available.
PSM WPDs
DEVELOPMENT
Very Low-Mass Stellar Models
Leader: Santi Cassisi
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 76/200
PSM WP 121 110
Development phase
04/2016 — 12/2023
Institution: INAF - Astronomical Observatory of Teramo (Italy)
Key Personnel: S. Cassisi; M. Salaris (INAF-Teramo); A. Pietrinferni (INAF-Teramo)
Objectives: Provide a detailed characterization of both the structural and evolutionary properties of Very Low
Mass stars (VLM) stellar objects with mass lower than about 0.5Msun from the Pre-Main Sequence to the start
of core H-burning. This objective will be achieved by computing detailed, state-of-the-art stellar evolution
models.
Tasks:
1.
Compute grids of updated stellar models for very low mass stars (M <0.5Msun) with existing
evolutionary codes adapted for this type of stars;
2.
Improve the physical framework used by the evolutionary code;
Input:
1.
A release of some preliminary sets of stellar models;
2.
Relevant data concerning some physical inputs: Equation of State, conductive opacity, nuclear reaction
rates, surface boundary conditions
3.
Evolutionary code and numerical tools for extracting the structural and evolutionary properties of the
various stellar models.
Dependencies:
This WP is strongly related with many other WPs of the “global” WP 121 such as WP 121 100, WP 121 200, WP
121 300, WP 121 400, and WP 127 300
Output:
Grids of updated stellar models for very low mass stars
Deliverables:
Reports and stellar models
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Grids of first generation of validated stellar models
05/2022: Grids of second generation of validated stellar models
Risks:
The researchers involved in this task have a long-standing expertise in the computation of state-of-art stellar
models, and the WP program builds up on a well-known approach so no risks are expected. However, some
limitations in the release of the final models grid could be possible in case of failure of major progress in the
WPs aimed to improve the physical scenario;
PSM WPDs
DEVELOPMENT
Low Mass Stellar Models
Leader: Josefina Montalban
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 77/200
PSM WP 121 120
04/2016 — 12/2023
Institution: University of Padova (Italy)
Key Personnel: J. Montalban; Y. Lebreton (Paris, GEPI); J-P Marques (IAS-Orsay); A. Palacios (Montpellier);
P. Eggebenger(Geneva); A. Noels (Liège); P. Ventura (INAF-Rome); S. Cassisi (INAF-Teramo)
Objectives: Provide grids of high quality 1D stellar models for low/intermediate mass main sequence (MS) and
subgiant stars as specified during the definition phase.
Tasks:
1.
Keeping updating the physical description of low/intermediate mass stellar models in dedicated
evolutionary codes
2.
Studying the effects of rotation and correlated rotational mixing in the results obtained with codes which
do not include them yet in connection with WP 121 200
3.
Testing the theoretical evolutionary framework on suitable empirical data: star clusters and eclipsing
binaries
4.
Comparing models computed by the different groups participating to the project
Input:
1.
Existing grids of models.
2.
Relevant data concerning some physical inputs: Equation of State, radiative and conductive opacity,
nuclear reaction rates, boundary conditions from atmosphere models (WP 122 000)
3.
Evolutionary code and numerical tools for extracting the structural and evolutionary properties of the
various stellar models.
Dependencies:
WP 121 120 is part of WP 121 100. Inputs from WP 122 000 and WP 121 200
Output:
Package of grids of updated 1-D stellar models for main sequence and subgiant stages. The stellar parameter
domain will cover masses between 0.7 and that corresponding to spectral type F5 in the MS, and a large range
of chemical compositions. Evolutionary tracks and stellar structure files will be provided in a standard format for
oscillation computation. A documented user guide providing a detailed description of the content of grids and of
the physical description assumed in the model computation.
Deliverables: Grids of stellar models: evolutionary tracks and stellar structure files for main sequence and subgiant stages, and the corresponding documentation.
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Grids of first generation of validated stellar models
05/2022: Grids of second generation of validated stellar models
Risks: Acceptable risks
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 78/200
Theoretical Oscillation Frequencies
Leader: Juan Carlos Suárez
Rev.: 5
Development phase
PSM WP 121 130
04/2016 — 12/2023
Institution: Universidad de Granada (Spain)
Key Personnel: J.C. Suárez; A. García Hernández (Porto); J.R. Rodón (IAA-CSIC)
Objectives: To select an oscillation code to be used for obtaining the oscillation frequencies of every model of
the grids. To calculate these frequencies. To study the impact of the differences observed when different
oscillation codes are used in the estimation of the stellar parameters.
Tasks:
1.
Test the impact of the choice of the pulsation code on the mode frequencies.
2.
Test how the differences in the frequencies coming from the different oscillation codes impact on the
estimate of stellar parameters.
3.
Define the standard physical and mathematical inputs for the calculation of the oscillation frequencies of
the models grids. Select the code to be used for the systematic calculation of the frequencies.
4.
Calculate the oscillation frequencies of every model of the grids.
Input:
1.
Models from the grid obtained in the WP 121 100
2.
Outputs from the different oscillation codes included in the study, and information about their general
characteristics.
3.
The code finally selected for the calculation of the frequencies.
Dependencies:
1.
WP 121 130 is part of WP 121 100.
2.
Inputs from WP 121 110 and WP 121 120.
3.
Interactions with the WP 124 200.
Output:
An estimate of the impact of the frequency differences obtained with different codes. A set of physical and
mathematical procedures selected to obtain the complete grid of frequencies. A complete set of frequencies for
every model of the grid.
Deliverables:
A complete set of frequencies for every model of the grids.
Milestones:
12/2017: Provide a reference oscillation code and frequencies associated with the first generation of models.
Definition of the set of oscillation codes to be part of the comparison study.
2018: Selection of the final code and estimation of its performances.
2019-2023: Systematic calculation of the frequencies of the models.
Risks: Acceptable risks
PSM WPDs
DEVELOPMENT
Transport Processes
Leader: Ana Palacios
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 79/200
PSM WP 121 200
04/2016 — 12/2023
Institution: Université de Montpellier (France)
Key Personnel:
A. Palacios; C. Charbonnel (Geneva); S. Mathis (CEA); J.P. Marques (IAS- Orsay); N. Lagarde (Birmingham); V.
Prat (MPA – Garching); O. Richard (Montpellier); P. Eggenberger (Geneva); F. Lignières (IRAP)
Objectives:
Improve the modelling of (non-standard) transport processes of heat, angular momentum and nuclides in 1D
stellar evolution codes. The transport generated by turbulence, waves and magnetic fields will be reviewed to
this end
Tasks:
1.
Review and evaluate existing theoretical models for transport processes
2.
Review and explore the interplay between transport processes
3.
Identify the processes requiring further modelling based on the results obtained from the CoRoT and
Kepler missions.
4.
Provide theoretical formulations and prescriptions adapted to stellar evolution codes (according to the
available manpower)
5.
Test the new formulations in a stellar evolution code that already implements rotation
6.
Select the processes and formulations we should include in the seismic analysis
7.
Study of the impact of these improvements on the accuracy of age determination
Input:
Existing stellar model grids and evolutionary codes (STAREVOL, GENEC, CESTAM).
Existing asteroseismic constraints
Dependencies:
1D stellar models (WP 121 100) and WP 121 500
Output:
1.
Document that lists and describes the physical ingredients related to transport of chemical elements, heat
and angular momentum that must be implemented in (the second generation of) 1D stellar models;
2.
Estimates of uncertainties due to these processes if they are not implemented will be included;
3.
Formulations of transport mechanisms that can be implemented in 1D stellar evolutionary code (output for
WP 121 100).
Deliverables:
Reports
Milestones:
12/2017: Review of transport processes and existing theoretical models
06/2018: Review of existing implementations and recommendations of usage
12/2018: Recommendations for implementation for first generation of validated stellar models
06/2019: Provide new theoretical formulations; Select the processes and formulations we should include in the
seismic analysis
Until launch: Follow up to help with implementation by WP 121100 and coordination with WP 121 000 and
propose modifications if required
Risks: Acceptable risk
PSM WPDs
DEVELOPMENT
PMS Evolution
Leader: Joao Pedro Marques
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 80/200
PSM WP 121 300
Development phase
04/2016 — 12/2023
Institution: Université de Paris-Sud (France)
Key Personnel: J. P. Marques; F. Palla (INAF-Arcetri); M. Marconi (INAF-OAC); E. Tognelli (Rome); P. G.
Prada Moroni (Pisa); S. Degl’Innocenti (Pisa)
Objectives: To build computation tools which provide PMS stellar models with rotation profiles that are as
realistic as possible.
Tasks:
1. Implementation of seismically validated improvements of the physical description of PMS models in PMS
evolutionary codes.
2. Implementation of more realistic initial conditions in PMS evolutionary codes.
3. Computation of improved PMS models covering the low mass star domain.
4. Impact of these improvements on the structure and rotation profile of stars belonging to the core program.
Input:
Existing stellar evolutionary codes (FRANEC, CESTAM).
Dependencies:
Input from WP 121 100, WP 121 200, WP 123 300 and WP 123 400. Output to WP 121 100.
Output:
1.
Grids of improved PMS models covering the low mass stars domain.
2. Recommendation for implementation on 1D evolutionary codes.
Deliverables:
Grids of PMS models.
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Grids of first generation of validated stellar models
05/2022: Grids of second generation of validated stellar models
Risks: Acceptable risks
PSM WPDs
DEVELOPMENT
2D / 3D Stellar Evolution Models
Leader: Michel Rieutord
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 81/200
PSM WP 121 400
Development phase
04/2016 — 12/2023
Institution: IRAP (France)
Key Personnel: M. Rieutord; B. Dintrans (IRAP); F. Lignières (IRAP); J. Ballot (IRAP); L. Jouve (IRAP)
Objectives: The objective of the WP is to deliver very precise stellar models that can be used by the
exoplanetary science team. Indeed, the determination of the bulk parameter of a star (age, mass, etc.) from e.g.
asteroseismic data needs a very good preliminary model of the star. This is compulsory to identify the
eigenmodes that are observed. Such good models require at least two spatial dimensions to properly include the
effects of rotation. We therefore propose to deliver models at the state-of-the-art level, which can be combined
to the best oscillation codes, which already exist and will just need slight adaptations, out of which the most
precise stellar parameters can be drawn.
Tasks:
1.
2.
3.
4.
5.
Deliver 2D evolution codes with more and more refined physics
Deliver transport prescriptions based on 3D magneto-hydrodynamic simulations
Deliver the associated oscillation codes that are able to use the 2D evolutionary models
Evaluate the limits of 1D model
Organize the scientific community to make an efficient use of the new tools
Input:
Existing models
Dependencies:
WP 121 100, WP 122
Output:
Models of stars at any rotation rate including state-of-the-art models of transport processes.
Deliverables:
At each milestone a numerical code will be delivered, with its associated oscillation code.
Milestones:
12/2017: Models describing chemically homogeneous fast rotating stars
06/2019: Models including nuclear evolution and fast rotation
12/2020: Models including angular momentum loss, nuclear evolution and fast rotation
12/2022: Models including a self-consistent atmosphere
Risks:
Risks come from the stability of the algorithms, which may not be able to cover all the mass range. These
potential difficulties may require further studies of the numerical algorithms and delay the delivery of codes.
PSM WPDs
DEVELOPMENT
Evolution of Stars in Multiple Systems
Leader: Stéphane Mathis
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 82/200
PSM WP 121 500
04/2016 — 12/2023
Institution: CEA/DSM/IRFU/Service d’Astrophysique / Laboratoire Dynamique des Etoiles et de leur
Environnement (France)
Key Personnel: S. Mathis; M. Guenel (CEA); P.-A. Desrotour (CEA); P. Beck (CEA); A. Palacios (Montpellier);
J.P. Marques (IAS); C. Damiani (IAS); J. Ballot (IRAP); C. Charbonnel (Geneva); G. Meynet (Geneva); P.
Eggenberger (Geneva); L. Siess (ULB Brussels); C. Aerts (KU Leuven); A. Tkachenko ( Leuven)
Objectives: Stars could have companions, either planets or stellar objects (stars or compact objects). If
companions are close enough to the host star, the evolution of the system is modified by tidal (and MHD)
interactions and possible mass transfers. The study of stars in multiple systems is thus very important both for
star-planet and for close binary/multiple star studies in PLATO.
Tasks:
1.
Study of tidal large-scale flows in stellar interiors (equilibrium tide); study of low-frequency oscillations
(inertial, gravito-inertial) excitation by the tidal potential (dynamical tide); study of the tidal kinetic energy
(equilibrium & dynamical tides) dissipation and of the induced exchanges of angular momentum between the
host star and companions (scaling laws as a function of stellar parameters); determination of the characteristic
time-scales (circularization, synchronization, spin alignment).
2.
Study of couplings between internal transport processes (WP 121 200) with tidal (and MHD) interactions
and possible mass transfers. Study of the induced modification of stellar evolution.
3.
Implementation of binarity/multiplicity in dynamical stellar evolution codes, in which transport processes
are already included; associated grids computation (third generation).
4.
Study of the asteroseismic signatures of the dynamical tide and of the perturbations/excitation of
acoustic and mixed modes by tides; corresponding Hare and Hound exercises.
5.
Study of the observational signatures of the impact of interactions in multiple systems on stellar
evolution; corresponding Hare and Hound exercises.
Input:
1.
Existing dynamical stellar evolution codes (WP 121 100 - 200).
2.
Inputs, results and developments achieved by working groups on transport processes (WP 121 200),
2D and 3D stellar structure and global angular momentum evolution (WP 121 400), and Planet-Star interactions
(WP 115 300), Model of rotational evolution and gyrochronology (WP 123 300), Multiple stars (128230).
Dependencies:
WP 115 300, WP 121 XXX, WP 123 300, WP 128 230.
Output:
1.
Prediction of asteroseismic and complementary observational signatures of the interactions between
stars and companions.
2.
Integrated star-planetary systems or close binary stars modelling with treating angular momentum
exchanges from the core of the star to its external environment (interface with WP 115 300).
Deliverables:
Characterization of the asteroseismic signatures of tidal interactions; observational signatures of the impact of
interactions in multiple systems on stellar evolution; dynamical models of stars interacting with a companion,
which take into account transport processes, and consequences for stellar mass, age, and radius; constraints on
the age by the orbital properties (circularization) and the spins state (synchronization and alignment).
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Grids of first generation of validated stellar models
05/2022: Grids of second generation of validated stellar models
Risks: Acceptable risks
PSM WPDs
DEVELOPMENT
Non-Seismic Diagnostics and Model Atmospheres
Leader: Thierry Morel
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 83/200
PSM WP 122 000
04/2016 — 12/2023
Institution: University of Liège (Belgium)
Key Personnel: T. Morel (Liège)
Objectives: Develop new generations of state-of-the-art 1D/3D stellar model atmospheres and compute
improved grids of limb-darkening coefficients. Specify procedures for an accurate determination of the
fundamental parameters (e.g., Teff, radii, and chemical abundances) based on non-seismic diagnostics (e.g.,
ground-based data, Gaia parallaxes). Coordinate activities of WP 122 100 to WP 122 500.
Tasks:
1.
Ensure no overlap and efficient coordination of the activities performed within the sub-packages.
2.
Develop grids of 1D and 3D model atmospheres with updated physics.
3.
Compute new grids of limb-darkening coefficients.
4.
Implement optimised procedures and develop automated tools for the determination of the stellar
parameters (e.g., Teff, radii) and chemical abundances with an accuracy matching the PLATO scientific
requirements.
5.
Compute 3D/non-LTE corrections for the abundances of individual lines, continua and centre-to-limb
variations.
6.
Estimate interstellar extinction towards the line of sight for each target.
7.
Ensure close coordination and efficient data exchange with other relevant WPs outside WP 122 000
(listed in Dependencies section below)
8.
Investigate the need for additional ground-based or space observations.
Input: Input from sub-packages
Dependencies: Input/output from and to PDC (WP 350 000) and PSM (WP 121 000, WP 123 000, WP 125
000, WP 127 000, and WP 131 000)
Output:
1.
New grids of 1D/3D model atmosphere and limb-darkening coefficients. Libraries of high-resolution,
synthetic spectra and spectrophotometric data.
2.
Procedures for the determination of the stellar parameters (e.g., Teff, radii, and chemical abundances)
corrected for 3D/non-LTE effects.
Deliverables:
Successive generations of updated grids of 1D/3D model atmospheres and limb-darkening coefficients.
Automated tools for the determination of the stellar parameters.
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: Acceptable risks.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 84/200
1D Model Atmospheres
Leader: Bertrand Plez
Rev.: 5
Development phase
PSM WP 122 100
04/2016 — 12/2023
Institution: Université de Montpellier, CNRS (France)
Key Personnel: B. Plez; F. Allard (Lyon); P. Barklem (Uppsala); M. Bessell (RSSA, ANU); L. Casagrande
(MSO, ANU); B. Edvardsson (Uppsala); U. Heiter (Uppsala); C. Helling (St Andrews); D. Homeier (Lyon);
M.
Ireland (RSSA, ANU); O. Kochukhov (Uppsala); J. Linsky (Boulder); S. Meszaros (Gothard); C. Barban (LESIA)
Objectives: Improve our knowledge of stellar photospheres for PLATO targets (i.e., FGK dwarfs and subgiants,
M dwarfs). Ensure that we have the best possible description of their atmospheres, necessary for the accurate
characterisation of their output spectra, limb-darkening, and internal structure boundary condition. Provide the
grid of model atmospheres to be used for the analysis of PLATO data.
Tasks:
1.
Compare families of 1D model atmospheres.
2.
Verify model atmospheres and opacities using high-resolution observations of benchmark stars.
3.
Address defects in physical ingredients and recipes used in present models, e.g., opacity data.
4.
For very cool M dwarfs, account for dust formation, and non-homogeneity of dust distribution.
5.
Examine the adequacy of the description of the deeper layers of model atmospheres, to be used as
boundary condition for interior models.
6.
Compute a complete grid of 1D model atmospheres covering the parameter space of stars observed
with PLATO (i.e., FGK dwarfs and sub-giants, M dwarfs).
7.
Create a database, for seismic studies, that contains the output of the theoretical calculations (e.g., 1D
model atmospheres and associated model fluxes).
Input: Spectroscopic and spectrophotometric observations of FGKM stars. Astrometry from Gaia. Improved
molecular and atomic line lists
Dependencies: Other WP 122 000 sub-packages, WP 121 000, WP 123 000, WP 127 000, and WP 131 000
Output:
Grids of updated 1D models, and predicted detailed spectra, assessment of their quality viz. observations.
Procedures for estimating stellar parameters of reference FGKM stars.
Deliverables:
Detailed report on accomplished work and reasons for the choices that were made.
Full grid of model atmospheres for FGKM stars in 1D.
Milestones:
01/2019: Complete an accuracy assessment for photometry/spectrophotometry of sources with the appropriate
brightness range
07/2019: Perform a comparison of model atmospheres for our purposes: MARCS; Kurucz; Phoenix etc.
07/2020: Obtain/calculate the final1D model atmospheres for PLATO targets
Risks: Availability of input data (opacities), securing funding for postdocs or PhD students that will do part of
the work
PSM WPDs
DEVELOPMENT
3D Model Atmospheres
Leader: Martin Asplund
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 85/200
PSM WP 122 200
04/2016 — 12/2023
Institution: Australian National University (Australia)
Key Personnel: M. Asplund; F. Allard (Lyon); L. Bigot (Nice); A. Chiavassa (Nice); R. Collet (Canberra);
Homeier (Lyon); Z. Magic (MPA); F. Thévenin (Nice) ; R. Trampedach (Boulder)
D.
Objectives:
Develop 3D hydrodynamical stellar model atmospheres of late-type stars (spectral type FGKM, dwarfs and
subgiants) for a wide range of stellar parameters (effective temperature, surface gravity, metallicity) targeted by
PLATO. Continuously improve 3D model atmospheres to ensure highest accuracy and reliability in derived
stellar parameters and chemical compositions.
Tasks:
Compute dense grid of 3D stellar model atmospheres for all stellar parameters
Input:
Existing atmosphere models
Dependencies:
Other WP 122 000 sub-packages, WP 121 000, WP 123 000, and WP 127 000
Output:
First grid of highly realistic 3D hydrodynamical stellar model atmospheres for a very wide range of parameters
corresponding to late-type stars
Deliverables:
Reports
Milestones:
01/2018: Complete first grid of 3D stellar model atmospheres at solar and low metallicity
01/2019: Complete final dense grid of 3D stellar model atmospheres for all stellar parameters
06/2019: Compute 3D LTE spectral line formation for wide range of elements and transitions
06/2019: Compute continuum centre-to-limb variations using 3D models
01/2020: Photometric and spectroscopic stellar parameter estimations using 3D models
01/2021: Systematic 3D non-LTE for all stellar parameters
01/2022: Further refinements in 3D stellar model atmospheres and non-LTE spectrum calculations
Risks: Some delay can occur to reach these ambitious goals in a timely manner, depending on the available
manpower.
PSM WPDs
DEVELOPMENT
Fundamental Stellar Parameters
Leader: Carlos Allende Prieto
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 86/200
PSM WP 122 300
04/2016 — 12/2023
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: C. Allende Prieto; A. Amarsi (ANU); M. Ammler-von-Eiff (MPSSR); P. Barklem (Uppsala);
M. Bergemann (MPIA); C. del Burgo (INAOE); L. Casagrande (ANU); L. Fossati (Argelander); J. I. González
Hernández (IAC); L. Koesterke (Texas); K. Lind (Uppsala); L. Mashonkina (Moscow); Y. Maqueo Chew (UNAM);
T. Merle (ULB); R. Monier (Meudon); D. Mourard (Nice); N. Nardetto (Nice); A. Sozzetti (Torino)
Objectives:
Assess the limitations and accuracy of the different methods to determine fundamental stellar parameters (Teff,
BC, radius, chemical abundances, etc.) for FGKM stars observed by PLATO, based on photometric and
spectroscopic observations, including astrometry to be provided by Gaia. Identify the preferred protocol to derive
fundamental parameters and chemical abundances for targets of interest. Provide model fluxes covering the
parameter space of the FGKM stars observed by PLATO.
Tasks:
1.
Design an optimal protocol to infer stellar parameters for PLATO targets, that takes into account 3D/nonLTE effects and benefits from the availability (except for M stars) of accurate seismic parameters (e.g., surface
gravity).
2.
Compute 1D and 3D model fluxes including non-LTE corrections.
3.
Create a database, for seismic studies, that contains the output of the theoretical calculations (e.g.,
model fluxes for FGKM stars).
4.
Create a database, for seismic studies, that contains preliminary parameters for the FGKM stars based
on ground-based and Gaia data.
Input:
Spectrophotometry from HST and Gaia, astrometry from Gaia, spectroscopy from ground-based surveys, stellar
angular diameters from ground-based interferometers, stellar structure models, atomic and molecular data, 1D
and 3D model atmospheres.
Dependencies:
Other WP 122 000 sub-packages, WP 125 000, and WP 131 000
Output: Model fluxes for FGKM stars. Preliminary stellar parameters of PLATO targets.
Deliverables: Documents describing the studies performed.
Milestones:
12/2015: Provide the final analysis protocol to derive fundamental parameters for Plato targets
Risks: None
PSM WPDs
DEVELOPMENT
Limb Darkening
Leader: Antonio Claret
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 87/200
PSM WP 122 400
Development phase
04/2016 — 12/2023
Institution: IAA (Spain)
Key Personnel: A. Claret; C. Barban (LESIA); J. D. do Nascimento Jr. (Natal); B. Plez (LUPM); L. Bigot (Nice);
D. Mourard (Nice); N. Nardetto (Nice); M.P. Di Mauro (Rome); Y. Unruh (Imperial College London); N. Krivova
(Göttingen); S. Solanki (Göttingen)
Objectives:
Determine with precision the limb-darkening distribution of the host stars. Identify and quantify the sources of
uncertainties in masses, radii and effective temperatures of the host stars, due to limb-darkening.
Tasks:
Computation of limb-darkening coefficients. The comparison of eclipsing binary data with theoretical predictions
involving atmosphere models seems to indicate some discrepancies between the theoretical and observational
data. Such disagreements may be related to intrinsic problems in either the atmosphere models or in the
numerical methods adopted. In order to investigate the causes of these discrepancies, we plan to compute limbdarkening (LDC) and gravity-darkening (GDE) coefficients for several atmosphere models: ATLAS, PHOENIX,
1D MARCS, 3D Stagger models and, possibly, a version of spherical ATLAS. The calculations will be performed
for the photometric system of PLATO (to be defined), as well as for the most commonly used passbands
(uvbyUBVRIJHK, Sloan, etc.) by adopting least-squares and flux conservation methods. This will make our
calculations useful not only for the PLATO mission.
Input:
Grids of atmosphere (specific intensities)
Dependencies:
Other WP 122 000 sub-packages
Output:
Series of grids of limb- and gravity-darkening coefficients computed by adopting different numerical methods.
Such calculations will be available for several passbands.
Deliverables:
Distribution of the grids of limb- and gravity-darkening coefficients. Parts of these grids (PHOENIX models:
effective temperatures in the range 1500-10000 K) were already published during the 2012-2013 period.
Milestones:
12/2017: First sets of limb darkening coefficients computed with the involved codes for comparison tests
12/2020: Comparisons, tests, improvements scientific specifications
06/2021: Delivery of the first sets of validated limb darkening coefficients
12/2023: Update of the model atmospheres and computations of corresponding updated limb darkening
coefficients
Risks: Some acceptable delay in the delivery of validated limb-darkening and gravity-darkening coefficients can
arise from delay in the computations of the proper model atmospheres
PSM WPDs
DEVELOPMENT
Interstellar Extinction
Leader: Douglas Marshall
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 88/200
PSM WP 122 500
Development phase
04/2016 — 12/2023
Institution: Université Paris Diderot / CEA (France)
Key Personnel: D. Marshall; S. Sale (Oxford); J. Linsky (Colorado); R. Hanson (MPIA); K. Dobashi (Tokyo.); J.
Montillaud (Franche-Comté); E. Amores (Estadual de Feira de Santanta)
Objectives:
Provide values of anticipated extinction along different lines of sight. Ensure that interstellar extinction is handled
properly to enable precision estimates of stellar parameters.
Tasks:
1.
2.
3.
4.
Take responsibility for ensuring that extinction simulations are done as required
Investigate the use of Gaia reddening, including using the diffuse interstellar band at 862 nm
Advise on strategies for obtaining more precise extinction estimates from follow-up data
Evaluate uncertainties on extinction estimates
Input:
Gaia reddening, ground-based spectroscopic data
Dependencies:
Other WP 122 000 sub-packages, WP 131 000
Output:
Extinction maps. Extinction estimate for each source.
Deliverables:
Reports, and software test reports
Milestones:
12/2017: Preliminary set of specifications for the PDC will be available
09/2020: A first full set of specifications for the PDC should be available
12/2022: Updates on the specifications
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Stellar Activity and Rotation
Leader: Antonino Francesco Lanza
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 89/200
PSM WP 123 000
04/2016 — 12/2023
Institution: INAF-Osservatorio Astrofisico di Catania (Italy)
Key Personnel: A.F. Lanza; B. Mosser (OBSPM); M. Pinsonneault (Ohio State); S. Messina (INAF-Catania); F.
Kupka (Vienna); A. S. Brun (CEA); A. Valio (Mackenzie)
Objectives:
To coordinate the development and definition of the methods to study the impact of stellar activity on stellar
science and define the methods to measure and study stellar rotation and magnetic fields in late-type stars.
Development of physical models for a better understanding of the interplay between convection, rotation and
magnetic fields in stars.
Tasks:
1.
To communicate and coordinate the contributions from and to other WPs for the determination of the
stellar parameters and of the parameters of the planetary systems, with an emphasis on stellar rotation period,
surface differential rotation, filling factor of stellar magnetic fields, star-planet magnetic interactions;
2.
To coordinate the development of the models for surface convection in late-type stars with and without the
effects of magnetic fields, hydromagnetic models for stellar differential rotation, dynamo action, and the
evolution of the rotation under the action of stellar magnetized winds;
3.
To coordinate the study and development of new methods for reaching the above objectives.
Input:
Stellar atmosphere models from Stellar Science WP 122 000, interior models from WP 121 000, CoRoT or
Kepler data, synthetic data, stellar parameters (effective temperature, gravity, chemical composition,
rotation period, chromospheric activity indexes, asteroseismic age).
Dependencies:
WP 121 000, WP 122 000 and sub-packages.
Output:
Procedures for the analysis of stellar magnetic activity, rotation and surface magnetic fields to derive constraints
on basic stellar parameters and pursue a better understanding of the interplay between convection, rotation and
magnetic fields in stars with and without exoplanets.
Deliverables:
Specification of tools to analyse stellar activity in late-type stars and the interplay of convection, rotation and
magnetic fields in individual objects as well as in samples of given ages; constraints on basic stellar parameters,
notably rotation, differential rotation, and the broad distribution and filling factor of magnetic active regions.
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Tests on simulated data and on CoRoT and Kepler light-curves of selected active targets; tests of the
physical models implemented in numerical codes
05/2022: Update of the modelling algorithms and codes, tests and analysis of the results in order to establish the
final procedures for the PLATO mission
Risks: No general risks are foreseen; specific risks are detailed in each WP description.
PSM WPDs
DEVELOPMENT
Spot Models
Leader: Benoît Mosser
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 90/200
PSM WP 123 100
Development phase
04/2016 — 12/2023
Institution: Observatoire de Paris (France)
Key Personnel: B. Mosser; F. Baudin (IAS); R. García (CEA); A.-M. Lagrange (Grenoble) ; N. Meunier
(Grenoble) ; D. Barrado (CSIC-INTA)
Objectives:
To specify and test methods and algorithms for the measurement of the spot distribution, in close relation with
the stellar activity and rotation measurements and analysis methods and algorithms.
Tasks:
1.
Specify the methods and algorithms needed for the spot modelling
2.
Specify the methods and algorithms needed for interacting with the rotation and activity measurements
3.
Specify the way to ensure the adequacy of the spot modelling for measuring the relevant parameters
4.
Specify the modelling of solar activity (the Sun as a star) by comparison of radial velocity, photometry
and astrometric signals due to solar activity to prepare the comparative study of Plato and follow-up groundbased data
5.
Test the above procedures with synthetic data
Input:
Stellar atmosphere models from Stellar Science WP 122, WP 122 300, CoRoT and Kepler data, synthetic data,
stellar characteristics (effective temperature, gravity, chemical composition, rotation period, chromospheric
indexes, asteroseismic age); solar activity measurements
Dependencies:
WP 121, WP 122, WP 125 and sub-packages
Output:
Procedures for the fitting of the spot distribution, results from tests on synthetic and CoRoT/Kepler data;
specifications for PDC WP 374 200
Deliverables:
Spot modelling and reliable output parameters (rotation rate, spot lifetimes, spot longitudes and latitudes,
amplitude of differential rotation, activity cycles, age estimates based on the activity level)
Milestones:
12/2018: First specifications
2020:
Tests on simulated data and on CoRoT and Kepler light curves of selected active targets
12/2022: Refinement of the modelling algorithms and codes, performing of tests and analysis of the relative
results for the establishment of the final procedures for the PLATO mission.
Risks:
Difficulty to determine the adequate model depending on the level of stellar activity, on the rotation rate and on
the SNR.
PSM WPDs
DEVELOPMENT
Surface Convection (1D & 3D)
Leader: Friedrich Kupka
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 91/200
PSM WP 123 200
04/2016 — 12/2023
Institution: University of Vienna (Austria)
Key Personnel: F. Kupka; K. Belkacem (LESIA, Paris); E. Caffau (GEPI, Paris); H.-G. Ludwig (Heidelberg); R.
Samadi (LESIA, Paris)
Objectives:
The surface activity of the host stars has to be understood when analysing and interpreting data of PLATO. WP
123 200 is dedicated to investigate the properties of surface convection, in particular of stellar granulation, which
contributes to the activity mechanisms operating at stellar surfaces and has to be characterized for PLATO as a
function of spectral type. One has to construct 1D models and 3D numerical simulations of convection for the
parameter regime of interest. This is particularly important for stars with a solar-like surface convection zone,
where granulation provides a major contribution to the stellar background variability signal.
Tasks:
The main tasks to be performed in this WP are the following:
1.
Development of numerical codes for the computation of the theoretical contribution of granulation to
observed intensity and its signature in power spectra;
2.
Test of the codes and their theoretical basis; this includes comparing 1D model and different 3D
simulation codes and their predictions for the granulation background;
3.
Computing expected granulation contributions as a function of spectral type.
Input:
Models of granulation developed for use with PLATO data.
Dependencies:
WP 121 000, WP 122 000 and sub-packages.
Output:
For further application within the data analysis for PLATO this WP will provide model grids of the theoretical
contributions of granulation to the intensity and its signature in power spectra as a function of the spectral type
of the host star.
Deliverables:
Granulation model.
Milestones:
09/2020: Delivery of first generation of validated models and procedures related to the characterization of host
stars
12/2022: Delivery of second generation of validated models and procedures related to the characterization of
host stars
Risks:
The necessary numerical simulations may turn out to be more expensive in terms of computing time required, if
additional physical processes such as magnetic fields will have to be taken into account in the granulation
model. However, such additional computing resources can be expected to become also more affordable during
the next few years.
PSM WPDs
DEVELOPMENT
Models of Rotational Evolution and Gyrochronology
Leader: Marc Pinsonneault
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 92/200
PSM WP 123 300
04/2016 — 12/2023
Institution: Ohio State University (USA)
Key Personnel: M. Pinsonneault; J.-D. do Nascimento Jr. (Natal); A. Palacios (Montpellier); J. Guzik (los
Alamos)
Objectives: Studying angular momentum evolution of PLATO stars and inferring ages from their measured
rotation rates.
Tasks:
1.
Defining distinct rotation-age relationships appropriate for both unevolved and evolved low mass stars
using pre-PLATO data.
2.
Empirically constrain these relationships and quantify their uncertainties.
3.
Develop working models for the loss and transport of angular momentum.
4.
Explore mixing as a diagnostic of angular momentum transport.
5.
Infer seismic diagnostics of internal stellar rotation.
Input:
PLATO data
Dependencies:
Input from and output from PDC (WP 370) and PSM (WP 100, WP 130, WP 160); PLATO End-to-End Simulator
Output:
Updated stellar models; working prescriptions for age as a function of rotation, evolutionary state, mass, and
composition
Deliverables:
Reports and updated stellar models
Milestones:
12/2018: First specifications
12/2020: Tests on the models and application to simulated and observational data;
12/2022: Refinement of the modelling algorithms and codes, performing of tests and analysis of the relative
results for the establishment of the final procedures for the PLATO mission.
Risks: Minimal risks
PSM WPDs
DEVELOPMENT
Dynamos and Differential Rotation
Leader: A. S. Brun
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 93/200
PSM WP 123 400
04/2016 — 12/2023
Institution: IRFU/SAp, UMR AIM, CEA-Saclay (France)
Key Personnel: A. S. Brun
Objectives: Most stars rotate and exhibit a large diversity of magnetic fields. It is believed that dynamo action,
i.e. the complex, nonlinear interplay between, convection, large scale flows (differential rotation and meridional
circulation) and magnetic fields, is the source of the magnetism of solar like stars and M dwarfs, the main stellar
targets of PLATO. Being able to constrain all these MHD processes is crucial to our understanding of stars and
their impact on their environment. Seismic inversions of the extent of convective envelope, the surface and
internal profiles of large scale flows and of proxies of the magnetic activity confronted to multi-D simulations and
scaling laws/regime diagrams will help reaching this goal.
Tasks:
•
Assessment of software developments for providing rotation and magnetic modulation of light curves as
a function of spectral types
•
Definition of output variables to help in the Hare & Hound tests for the PDC pipeline
•
Production of light curves variability due to magnetic activity, differential rotation and convection
•
Start coordination of theoretical and modelling effort of stellar rotation proxy for solar-like stars
•
Start coordination of theoretical and modelling effort of stellar dynamo and magnetic activity proxies
•
Start multi-D numerical simulations of convection, rotation, turbulence & magnetism of solar like stars
•
Code maintenance and development
•
Regular reports on WP progress, participation to PSM meetings
Input:
•
Seismic inversion of internal rotation profile (WP 125 000)
•
Extent of convective envelope (WP 126 000), 1-D stellar state (WP 121 100) for 3-D models
•
Proxies of magnetic activity (WP 125 000)
Dependencies: WP 120 000 and sub-WPs
Output: (WP 121 000, 124 000, 127 000)
•
Impact of magnetism, convection and rotation on light curves as a function of spectral type
•
Scaling laws of differential rotation and activity levels as a function of spectral type
•
Provide light curves for Hare & Hound test in PDC pipeline
•
Realistic 3-D Simulations of some PLATO targeted stars to be used as test bed
•
Turbulent convective spectra for waves excitation
Deliverables:
Participation to Hare & Hound PSM and test by providing light curves for various stellar spectral types, First set
of light curves, spectra (turbulent and of gravity modes) and 3-D models by June 2020, second set after
observations become available
Regular reports of advancement of WP, regular meeting with PSM WP and sub-WP leaders
Milestones:
12/2017: Assessment of software development to provides light curves for Hare & Hound PDC test
12/2018: Production of light curves for Hare & Hound tests in PDC pipeline
12/2019: Start development of multi-D MHD models of generic PLATO stars
12/2019: Production of turbulent spectra for various spectral types to asses modes visibility
12/2020: Start ab-initio simulations of gravity modes in solar like stars and sub giants
12/2023: Determination of key stellar parameters for optimization of PLATO stellar targets
Regular intervals: Regular reports of advancement of WP, regular meeting with PSM WP and sub-WP leaders
Risks: lack of precision of inverted convection extent, differential rotation profiles and magnetic activity
PSM WPDs
DEVELOPMENT
Tools to Measure Rotational Modulation
Leader: Sergio Messina
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 94/200
PSM WP 123 500
04/2016 — 12/2023
Institution: INAF-Catania (Italy)
Key Personnel: S. Messina; T. Granzer (AIP); K. G. Strassmeir (AIP); M. Schuessler (MPSSR); N. Meunier
(Grenoble); A.-M. Lagrange (Grenoble); M. Ammler von Eiff (MPSSR); D. Barrado (CSIC-INTA)
Objectives:
To study, develop and test methods and algorithms for the measurement of the rotational modulation of the
optical flux of the stars in close relation with the stellar activity and spectroscopic rotation measurements,
analysis methods and algorithms.
Tasks:
1.
Develop the methods and algorithms needed for the detection and analysis of the rotational modulation of
the flux
2.
Develop the methods and algorithms needed for exploiting the information from activity models;
3.
Derive the stellar rotation period, estimate of the surface differential rotation, spot lifetimes
4.
Derive the procedures to use spectroscopic rotation measurements to improve and check results;
5.
Test the above procedures with synthetic data
Input:
1.
Stellar optical light curves
2.
Stellar spectral type
3.
Spot models from Stellar Science WP 123 100
4.
CoRoT or Kepler data
5.
Synthetic time series
Dependencies:
WP 120 000 and sub-WPs
Output:
Procedures for the detection and the analysis of the rotational modulation and to measure the rotation period,
results from tests on synthetic and CoRoT/Kepler data;
Deliverables:
Rotation period, amplitude of the surface differential rotation; lifetime of the active regions; correlation between
rotation and activity level; correlation between rotation and age;
Milestones:
12/2018: First specifications
2020:
Tests on the models and application to simulated and observational data;
12/2022: Refinement of the modelling algorithms and codes, performing of tests and analysis of the relative
results for the establishment of the final procedures for the PLATO mission.
Risks:
Optical flux modulation dominated by starspot evolution rather than rotational modulation; this can be checked
using spot models of WP 123 100; active regions lifetime significantly shorter than the rotation period; effects
due to activity cycles;
PSM WPDs
DEVELOPMENT
Stellar Rotation from Transits
Leader: Adriana Valio
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 95/200
PSM WP 123 600
04/2016 — 12/2023
Institution: CRAAM, Mackenzie University (Brazil)
Key Personnel: A. Valio
Objectives:
1.
Determine the rotation period of a star through the detection of spots on its surface. The period will be
determined by following the spots position through time. The spots longitude is determined from the light curve
during planetary transits. As the planet eclipses its host star, features on the stellar surface such as a spot may
be occulted. When this happens, a small variation in intensity may be detected. By modelling this “bump” during
the transit light curve it is possible to infer the position (latitude and longitude) of the spot and also its size and
brightness with respect to the stellar disk intensity. This method can also be applied to binaries, and not only
star-planet systems, provided that the stellar companion is small, or even a brown dwarf.
2.
Estimate the stellar differential rotation. If the average rotation period of the star is known, or the
rotation period at different latitudes from multiple transiting planets, then by assuming a solar like differential
rotation profile, or another given one, it may be possible to determine the differential rotation profile of the star.
Also possible to use in multi planet systems with eclipses at different latitudes of the star.
Tasks:
1.
Spot detection: identify intensity variations in the transit light curves due to spots;
2.
Spot modelling: fit the intensity variation by a model to infer the spots characteristics such as position
(latitude and longitude), relative intensity, and size;
3.
Rotation period: identify the same spot on later transits to determine the stellar rotation period;
4.
Differential rotation: from the period estimates obtained from spots at different latitudes on the stellar
surface, i.e., from the modelling of in- and out-of-transit light curves, calculate the differential rotation profile of
the star.
Input:
Computer codes to detect and model the spots; Model data; CoRoT and Kepler light curves.
Dependencies:
WP 120 000 and sub-WPs
Output:
Refined routines optimized for estimating the rotation period and the differential rotation profile of stars with
transiting companions, which may be a planet, a brown dwarf or a dwarf star.
Deliverables:
Stellar rotation period at different latitudes of the star, also star spots physical characteristics such as sizes and
temperatures. More precise planet radius, once the stellar activity has been accounted for.
Milestones:
12/2018: First specifications
2020:
Tests on the models and application to simulated and observational data;
12/2022: Refinement of the modelling algorithms and codes, performing of tests and analysis of the relative
results for the establishment of the final procedures for the PLATO mission.
Risks: Low, since this technique has already been proven to be effective with CoRoT and Kepler observations
PSM WPDs
DEVELOPMENT
Seismic Diagnostics
Leader: Margarida Cunha
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 96/200
PSM WP 124 000
Development phase
04/2016 — 12/2023
Institution: Universidade do Porto, CAUP (Portugal)
Key Personnel: M. Cunha; I. Roxburgh (QMUL); D. Reese (Birmingham); S. Deheuvels (OMP, IRAP)
Objectives: To coordinate the development and validation of the algorithms to be delivered to the PDC, with
regards to the inverse, glitch-related, and forward procedures that are to be adopted for the determination of the
mass, radius and age of the core program stars, as well as additional information on their internal structure and
dynamics.
Tasks:
1.
Overall coordination of the development and comparison tests that shall be undertaken within WP 124
100, WP 124 200, and WP 124 300, regarding the selected forward, inverse, and glitch-related procedures. This
will include an evaluation of the connection between the outputs of WP 124 100 and the inputs required by WP
124 200 and WP 124 300. One must verify, in particular, under which conditions the precision on the stellar
parameters obtained in WP 124 100 is sufficient, when the solution is to be used as a first guess for the
inversions.
2.
Overall coordination of the tests on the algorithms to be developed under WP 124 100, WP 124 200 and
WP 124 300 and delivered to the PDC.
3.
Overall coordination of the validation of the algorithms implemented by the PDC, concerning forward,
inverse, and glitch-related procedures.
Input:
Data from CoRoT and Kepler for test and validation of operations; PLATO simulated data; procedures
developed in WPs 124 100 to 124 300; Grids of models and stellar evolution codes, seismic, and non-seismic
parameters to be provided by WPs 121 000, WP128 000, and WP 122 000, respectively.
Dependencies:
Input from WPs 121 000, 122 000, and 128 000;
Input from and output to WPs 124 100 to 124 300 and WP 120 000
Output:
Outputs from the development phase of WP 124 100, WP 124 200, and WP 124 300
Deliverables:
1.
Algorithms for the adopted forward procedures;
2.
Algorithms for the adopted inverse procedures;
3.
Algorithms for the adopted glitch-related procedures;
4.
Report on the results of the evaluation to be carried out under task 1.
Milestones:
05/2016: Delivery of tested forward and inverse procedures to be adopted as a first generation data analysis.
05/2017: Algorithms for second generation of forward and inverse procedures fully developed;
05/2020: Delivery of second generation of forward and inverse algorithms fully validated.
05/2022: Updating of validated second generation of forward and inverse algorithms if necessary
Risks: Acceptable: forward, inverse, and glitch-related procedures already exist and their intrinsic accuracy is
not too far from the level required for Plato data analyses.
PSM WPDs
DEVELOPMENT
Forward Approaches
Leader: Ian Roxburgh
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 97/200
PSM WP 124 100
Development phase
04/2016 — 12/2023
Institution: Queen Mary University of London (UK)
Key Personnel: I. Roxburgh; S. Vorontsov (QMUL); M. Cunha (Porto); M. Bazot (Porto)
Objectives: To develop and validate forward procedures capable of delivering the mass, radius and age of the
core program stars with an accuracy requested by exoplanet studies as well as information on their internal
structure and dynamics. The procedures will focus on low mass, main sequence stars, of spectral type F to M.
Tasks:
1.
Compare several forward modelling approaches for the determination of stellar parameters and
associated uncertainties on the stellar mass, radius and age. All approaches make use of a grid of stellar
evolutionary models and have been used in the context of the Kepler mission. The comparison between these
methods will be based on targets with the characteristics of those to be observed by PLATO and will take into
account the aspects of the models that are most likely to introduce systematic errors in the results, for a full
characterization of the final uncertainties on the derived parameters.
2.
Further development in order to optimize the outcome of the analysis, when applied to PLATO targets.
3.
Develop a forward modelling tool aimed at an in-depth asteroseismic exploitation of the data on a
particular selection of PLATO targets. The tool must explore both fully and in a global manner the parameter
space, without being limited by a pre-computed grid. This will include a global search approach coupled to a
local, finer search.
4.
Carry out tests to validate the implementation of the tools defined above by the PDC
Input:
Forward methods identified for further testing and development. Grids of models, stellar evolution codes and
seismic and non-seismic parameters.
Dependencies:
Input from and output to WP 124 000
Output:
Adopted forward procedures and associated codes, as well as new estimates of the precisions expected on the
parameters at each level.
Deliverables:
1.
Report on the results of the comparison carried out in task 1;
2.
Detailed description of the fully developed procedure to be applied in the level 1 analysis;
3.
Detailed description of the fully developed procedure to be applied in the level 2 analysis.
Milestones:
06/2019: Identification of final forward procedure to be adopt in level 1 analysis
06/2020: Forward procedure for level 1 fully adapted
01/2021: Forward procedure for level 2 fully developed
12/2022: Forward tools fully validated
Risks: Acceptable; forward procedures already exist and their intrinsic accuracy is not too far from the level
required for Plato data analyses.
PSM WPDs
DEVELOPMENT
Inverse Techniques
Leader: Daniel Reese
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 98/200
PSM WP 124 200
Development phase
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: D. Reese; G. Buldgen (Liège); I. Roxburgh (QMUL); S. Deheuvels (OMP, IRAP)
Objectives: To develop inverse methods that can provide total mass, internal density profile and other
information on the core program stars. The adopted procedures will focus on low mass, main sequence stars
from F to M spectral types.
Tasks:
1. Classical inversion methods
a.
Tests and validation on simulated data and real data from CoRoT and Kepler missions
b.
Improvements of the inversion procedures if necessary to obtain better precisions.
2. Model independent inversion methods
a.
Tests and validation on simulated data and real data from CoRoT and Kepler missions
b.
Improvements of the inversion procedures if necessary to obtain better precisions.
Input:
Inversion methods identified for testing and further development. Stellar models, seismic and non-seismic
parameters. Outputs from forward modelling.
Dependencies:
Input from and output to WP 124 000
Output:
Inversion procedures and codes
Deliverables:
Comprehensive descriptive documents on the adopted inverse methods, procedures and algorithms as well as a
user-friendly guide and estimates of the expected precisions.
Milestones:
12/2017: First version of algorithms for inversion
01/2018-07/2020: Tests on simulated data and real data from CoRoT and Kepler missions. Improvements of
the inversion procedures if necessary
07/2020-12/2020: Delivery of second generation of validated inversion procedures
01/2021-12/2023: Updating and further tests
Risks: Acceptable; inversion procedures already exist and have been tested. Their adaptation to foreseen
PLATO data to reach the requested precision is not too demanding on theoretical developments.
PSM WPDs
DEVELOPMENT
Acoustic Glitches
Leader: Sébastien Deheuvels
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 99/200
PSM WP 124 300
Development phase
04/2016 — 12/2023
Institution: Observatoire Midi-Pyrénées, IRAP (France)
Key Personnel: S. Deheuvels; M. Monteiro (CAUP); M. Cunha (Porto); J. Ballot (IRAP); D. Reese (Birmingham)
Objectives: To develop and validate procedures capable of extracting the properties of acoustic glitches inside
stars from the frequencies of the observed oscillation modes. This will provide additional constraints on stellar
models, thus leading to better estimates of the mass, radius and age of the core program stars.
Tasks:
1.
Test different existing methods designed to estimate in a model-independent way the depths of two major
acoustic glitches, namely the base of the convective envelope and the second helium-ionization zone. Such
methods have already been validated in the context of the Kepler mission. Their efficiency will be compared for
stellar models representative of Plato targets in order to establish an optimal procedure.
2.
Develop of a tool to estimate the size of the convective cores (the boundary of the core also creates an
acoustic glitch) of main sequence stars through grid modelling. The grids must be computed using different
evolutionary codes in order to estimate systematic effects. The grid characteristics (mesh, ranges…) that are
needed to measure the core size will be estimated. A better knowledge of the extension of convective cores will
yield better estimates of the age of the exoplanet host stars.
3.
Explore the possibility to estimate the abundance of helium in the convective envelope using the signature
in the mode frequencies of the second helium ionization zone, as could be done for some Kepler targets. This
would provide additional constraints on stellar models.
4.
Determine the characteristics of Plato targets (stellar parameters, signal-to-noise ratio of oscillation
modes) for which the procedures from tasks 1, 2, and 3 can be applied.
5.
Carry out tests to validate the tools implemented following the recommendations of tasks 1, 2, and 3.
Input:
Methods previously applied to extract the depths of acoustic glitches in the Kepler mission. Stellar evolution
codes and grids of models. Estimates of stellar fundamental parameters along with corresponding uncertainties
and properties of the oscillation modes.
Dependencies:
Input from and output to WP 124 000
Output:
Detailed procedures to extract the depths of acoustic glitches from the oscillation mode frequencies, to estimate
the size of convective cores through grid modelling, and to estimate the He abundance in the envelope.
Deliverables:
1.
Description of the algorithms to be implemented to apply the selected procedures for task 1
2.
Description of the algorithms to be implemented to apply the selected procedures for task 2
3.
Description of the algorithms to be implemented to apply the selected procedures for task 3
4.
Characteristics of the grids of models needed to estimate the size of convective cores
Milestones:
12/2020: Description of the algorithms for task 1
12/2021: Description of the algorithms for task 2
12/2022: Description of the algorithms for task 3
12/2023: Characteristics of the grids of models needed to estimate the size of convective cores
Risks: Acceptable: glitch-related procedures already exist and have been tested. Their adaptation to foreseen
PLATO data is not too demanding on theoretical developments.
PSM WPDs
DEVELOPMENT
Determination of Stellar Parameters
Leader: Jørgen Christensen-Dalsgaard
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 100/200
PSM WP 125 000
04/2016 — 12/2023
Institution: Aarhus University (Denmark)
Key Personnel: J. Christensen-Dalsgaard; Hans Kjeldsen (Aarhus); B. Chaplin (Birmingham)
Objectives:
This WP must coordinate the work in order to provide to the PDC procedures that deliver masses, radii, ages,
and chemical composition of stars of the core program with the precision required by the exoplanet WPs, and
with reliable statistical characterization. Maintain close coordination with the activities under WP 121 000 (Stellar
models) to ensure that reliable modelling tools are used in the analysis of the data. Maintain close coordination
with WP 125 200 to ensure that optimal modelling tools are used for determination of 'classical' parameters
under WP 125 200. Maintain close coordination with WP 125 300 to ensure that optimal seismic tools are used
for determination of seismic parameters.
Tasks:
1.
Coordination of the work done by WP 125 100 to 125 400
2.
Make sure that the quality of the outputs from WP 125 100 to 125 400 match the specified requirements
3.
Establish procedures for utilizing the asteroseismic insights obtained through the analysis of PLATO
data to improve the determination of stellar parameters.
Input:
Results from WP 125 100 – 125 400
Dependencies:
1.
WP 121 000, WP 122 000, WP 123 000, WP 124 000, WP 126 000.
2.
Output to PDC (WP 370 000) using WP 129 000
Output:
Optimized procedures to determine accurate masses, radii, ages, chemical composition as well as specification
of probability density functions, including correlations, that satisfy the exoplanet requirements, with full
documentation of the procedures
Deliverables:
Optimized procedures to determine accurate masses, radii, ages, chemical composition as well as specification
of probability density functions, including correlations, that satisfy the exoplanet requirements, with full
documentation of the procedures
Milestones:
05/2016: Delivery of the first set of specifications to the PDC.
05/2019: Critical status review of all activities.
05/2022: Delivery of procedures, documentation and test results, including publication in the scientific literature.
Risks: Acceptable risks
PSM WPDs
DEVELOPMENT
Scaling Laws
Leader: Andrea Miglio
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 101/200
PSM WP 125 100
Development phase
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: A. Miglio; K. Belkacem (LESIA, Paris); J. Montalban (INAF-Padova); B. Mosser (OBSPM) I.W.
Roxburgh (QMUL)
Objectives: This WP must provide prescriptions to compute mass and radius based on scaling relations using
combinations of seismic and non-seismic pieces of information. It must also provide the uncertainties on the
derived quantities due to underlying simplifying assumptions.
Tasks:
1.
Validation of the scaling relations by comparison with detailed numerical computation of stellar models
and oscillation frequencies (outcome of WP 121 100), and predictions of mode amplitudes (WP 126 100)
2.
Empirical calibration of the scaling relations using CoRoT, Kepler, K2, and ground-based observations
of stars with available independent mass/radius estimates (detached eclipsing binaries, stars in clusters, nearby
stars with precise interferometric and Gaia’s astrometric constraints)
3.
Final assessment of the star parameter uncertainties
4.
Development of optimized procedures to implement computations of stellar parameters and their
uncertainties obtained from use of scaling laws
Input:
1.
Grids of stellar models (from WP 121 100), predictions of mode amplitudes (from WP 126 100)
2.
Astronomical literature, Gaia’s parallaxes when available
3.
Available CoRoT, Kepler, and ground-based data.
Dependencies:
Input from WP 121, WP 126, WP 128, and WP 370
Output:
Optimized and validated procedures to determine accurate masses, radii, ages, chemical composition as well as
uncertainties that satisfy the exoplanet specifications
Deliverables:
Optimized and validated procedures to determine accurate masses, radii as well as uncertainties that satisfy the
exoplanet specifications, with full documentation
Milestones:
06/2017: Initial planning meeting
06/2018: Start of tests on artificial and existing data
2019 – 2022: Yearly progress meetings
12/2022: Delivery of procedures, documentation and test results
Risks: Acceptable. Some of the necessary scaling laws already exist and will be operational. The absolute
precision of the output will have nevertheless to be estimated when used with actual PLATO data
PSM WPDs
DEVELOPMENT
Incorporating Classical Parameters
Leader: Sofia Feltzing
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 102/200
PSM WP 125 200
04/2016 — 12/2023
Institution: Lund Observatory, Lund University (Sweden)
Key Personnel: S. Feltzing
Objectives:
Develop procedures to incorporate reliable information about classical stellar properties in the analysis to
determine stellar parameters. These properties include effective temperature, luminosity, radius, composition
from ground-based photometry and spectroscopy and, in particular, from the Gaia observations, expected to be
available when PLATO is launched. The analysis must make use of optimal stellar atmosphere modelling for the
interpretation of the observations. Procedures must be included for full statistical analysis, allowing
determination of error properties of the inferred quantities.
Tasks:
Interface between WP 125 000 and other WP such as classical stellar parameters from ground-based
observations and from Gaia (WP 122 000), and models (WP 121 000).
Input:
WP 122 000, WP 121 000
Dependencies:
WP 121 000, WP 122 000, WP 125 000 and sub-packages
Output:
Reports on testing the determination of classical stellar parameters, including evaluation of internal consistency
and consistency with independent asteroseismic analyses as applied, e.g., to Kepler data
Deliverables:
Procedures, with documentation, for determining stellar parameters for the different relevant classes of stars,
including also recommendations for required support observations.
Milestones:
07/2017: Initial planning meeting
2017-2019: Evaluation of potential procedures and resources
2018-2023: Ground-based support observations
2019-2022: Yearly meetings to discuss progress
12/2022: Delivery of procedures documentation and test results
Risks: Access to required observing facilities.
PSM WPDs
DEVELOPMENT
Seismic Parameters
Leader: Christoffer Karoff
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 103/200
PSM WP 125 300
Development phase
04/2016 — 12/2023
Institution: Aarhus University (Denmark)
Key Personnel: C. Karoff
Objectives:
Based on procedures from 125 100 and 125 200, combine the results in procedures to determine the desired
properties of the stars (mass, radius, age, composition etc.) in an optimal fashion, including also a study of the
benefit of including individual frequencies in the analysis. Procedures must be included for full statistical
analysis, allowing determination of error properties of the inferred quantities. As a side benefit, information
should be extracted which documents, in a statistically solid fashion, errors in the underlying stellar models, to
be used in updating the modelling and hence reducing the systematic errors in the inferred stellar parameters.
Tasks:
1.
Establish procedures to determine stellar parameters (mass, radius, age, composition, etc.) from seismic
parameters (frequency separations and individual frequencies) and classical parameters (effective temperature,
luminosity, composition, etc.) with realistic error estimates.
2.
Interface between WP 125 000 and other WP such as seismic observables, including individual
frequencies (WP 124 000), and models (WP 121 000)
Input:
From WP 125 100 (mainly model grids), WP 125 200 (mainly effective temperature, luminosity, composition,
etc.) and WP 124 000 (mainly individual frequencies).
Dependencies:
Input from WP 124 000 and WP 121 000
Output:
Documented tests of the resulting procedures, applied both to realistic artificial data and to the reanalysis of
appropriate Kepler data.
Deliverables:
Procedures and documentation for the optimized determination of seismic parameters.
Milestones:
09/2017: Planning meeting of the activities during the implementation phase, with PDC WP 374 000 (Stellar
modelling tools)
09/2021: Start of testing of procedures within the PDC, particularly WP 374 000, using realistic artificial data.
09/2022: Critical status review of all activities.
09/2023: Delivery of procedures, documentation and test results, including publication in the scientific literature.
Risks: Acceptable risk
PSM WPDs
DEVELOPMENT
Open Clusters
Leader: Sarbani Basu
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 104/200
PSM WP 125 400
Development phase
04/2016 — 12/2023
Institution: Yale University (USA)
Key Personnel: S. Basu
Objectives:
Based on procedures from WP 125 100 and WP 125 200 (stellar models), and using input from WP 125 300
(seismic inputs), identify and develop the procedures that make use of the specific information provided from the
fact that stars are members of open clusters. This includes specific requirements on the 'classical' information
under WP 125 200.
Procedures will be included for full statistical analysis, allowing determination of error properties of the inferred
quantities. As a side benefit, information should be extracted which documents, in a statistically solid fashion,
errors in the underlying stellar models, to be used in updating the modelling and hence reducing the systematic
errors in the inferred stellar parameters, noting that internal consistency amongst cluster stars may be
particularly relevant for this.
Tasks:
Put a reasonably automated pipeline in place to input stellar grids as well as data (seismic and non-seismic) to
output basic properties of the stars, errors on the properties and error-correlations.
Determine how to find stars that should be investigated in detail and to determine the optimum distribution of
such stars across the cluster CMD to make reliable estimates of cluster parameters.
Input:
From WP 125 100 (model grids), WP 125 200 (mainly effective temperature, luminosity, composition)
Dependencies:
WP 121, WP 122, WP 123, WP 125 100, WP 125 200
Output:
Pipelines, together with instructions, to determine properties of stars in clusters
Deliverables:
Validated codes with documentation
Milestones:
07/2017: Initial planning meeting
12/2019: finish tests on simulated data
12/2022: Delivery of procedures documentation and test results
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 105/200
Mode Physics
Leader: Kevin Belkacem
Rev.: 5
PSM WP 126 000
Development phase
04/2016 — 12/2023
Institution: LESIA, Observatoire de Paris (France)
Key Personnel: K. Belkacem; F. Baudin (IAS)
Objectives:
Coordination of the mode physics sub-working groups in charge of providing realistic determination of mode
amplitudes and line-widths. The objectives are to provide realistic stellar light-curves (for use inside WP 120)
including oscillations as well as an estimation and modelling of sub-surface effects (e.g. turbulent pressure,
granulation, magnetic effects) on mode parameters. These developments will benefit from the CoRoT and
KEPLER legacy.
Tasks:
1.
Validation and calibration of the stellar light-curve simulator for H&H exercises inside the PSM, using
both CoRoT and Kepler available observations.
2.
Developments of methods and algorithms for correcting mode parameters (frequencies, line-width,
amplitude) from surface effects.
3.
Hare & Hound (H&H) exercises for optimizing the scientific return and target selection.
Input:
PLATO End-To-End simulator
Dependencies:
Input from and output from PLATO End-to-End Simulator, and from WP 126 100 to WP 126 400
Output:
1.
User manual of the stellar light-curve simulator,
2.
Realistic light-curves for the PLATO scientific community for H&H exercises,
3.
Algorithms for correcting stellar parameters from surface effects
Deliverables:
Algorithms for correcting stellar parameters from surface effects.
Milestones:
05/2016: Delivery of the first version of the stellar light-curve simulator.
05/2017: Validation and calibration of the stellar light-curve simulator using both CoRoT and Kepler available
observations.
05/2019: Developments of methods and algorithms for correcting mode parameters (frequencies, line-width,
amplitude) from surface effects.
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Mode Amplitude and Near-Surface Effects on Mode
Parameters
Leader: Réza Samadi
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 106/200
PSM WP 126 100
04/2016 — 12/2023
Institution: LESIA, Observatoire de Paris (France)
Key Personnel: R. Samadi; K. Belkacem (LESIA, Paris); H.-G. Ludwig (Heidelberg); L. Bigot (Nice);
Caffau (GEPI, Paris)
E.
Objectives:
1.
To develop tools and generate relevant set of data in order to derive realistic predictions of mode
amplitudes for stars of the core program;
2.
To develop realistic models of the near-surface effects, namely here the effects on the mode
frequencies of turbulent convection near the stellar surface;
3.
To compare our predictions with CoRoT and Kepler data
Tasks:
1.
Calculation of “patched” models (i.e. 1D global stellar with surface layers obtained from an associated
3D hydrodynamic model) for each set of 3D hydrodynamic models.
2.
Calculation of theoretical mode frequencies and amplitudes associated with each “patched” model.
3.
Development of a tool to derive mode amplitudes for any star within the domain covered by the grid of
3D models.
4.
Quantification of the near-surface effects using the grid of stellar models.
5.
Modelling the near-surface effects using either empirical or theoretical approach.
6.
Development of a method (e.g. scaling laws) to predict near-surface effects for within the domain
covered by the grid of 3D models.
7.
Comparison of our predictions with CoRoT and Kepler data.
Input:
1.
Grid of 3D hydrodynamic models for a large range in effective temperature, gravity and chemical
composition;
2.
Theoretical or empirical models of mode damping line-widths for a variety of stars (WP 126 200)
Dependencies: WP 126 200
Output:
1.
Grid of patched models;
2.
A numerical tool to predict mode amplitudes;
3.
Models of near-surface effects and associated numerical tool
Deliverables:
1.
Grid of patched models;
2.
A numerical tool to predict mode amplitudes;
3.
Models of near-surface effects and associated numerical tool
Milestones:
12/2018: Developments of an algorithm to interpolate the grid of 3D simulations so as to deduce superficial
layers of stellar 1D models
12/2019: Validation of task 1 on CoRoT and Kepler observations.
12/2021: Determination and modelling of surface effects on mode parameters (frequency, line-width, amplitude)
12/2023: Validation of task 3 on CoRoT and Kepler observations.
Risks: none
PSM WPDs
DEVELOPMENT
Mode Line-Width
Leader: Marc-Antoine Dupret
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 107/200
PSM WP 126 200
Development phase
04/2016 — 12/2023
Institution: University of Liège (Belgium)
Key Personnel: M.A. Dupret; M. Grosjean (Liège); K. Belkacem (LESIA, Paris)
Objectives:
This WP aims to improve the theoretical determination of mode line-width. A quantitative estimation of mode
line-widths of solar-like stars across the HR diagram will be provided. It is an important objective since the linewidth determines the mode detectability.
Tasks:
1.
Improvement of time-dependent convection models used to compute mode line-widths
2.
Computation of mode-linewidth in a sparse grid of stellar models
3.
Validation of the mode line-width modelling using available CoRoT and Kepler observations
Input:
Non-radial non-adiabatic oscillation code MAD
3D simulations of convection (WP 122 100 and WP 123 200)
Dependencies:
WP 126 000, WP 122 100 and WP 123 200
Output:
An improved code to compute mode line-widths of solar-like stars across the HR diagram
First generation grid of mode line-widths
Deliverables:
Validated mode line-width model.
Milestones:
01/2018: A model of mode line-width; it will have to take into account the variation of stellar properties across
the HR diagram.
01/2020: Validation of the mode line-width modelling using available CoRoT and Kepler observations
Risks: Minimal risks
PSM WPDs
DEVELOPMENT
Intensity-Velocity Relation
Leader: Günter Houdek
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 108/200
PSM WP 126 300
04/2016 — 12/2023
Institution: Aarhus University (Denmark)
Key Personnel: G. Houdek
Objectives:
Relation between mode Intensity and velocity: the CoRoT and Kepler mission taught us that a correct modelling
of mode amplitude and line-width is not sufficient to reproduce the observations. Indeed, the ratio between mode
intensity (luminosity) and velocity amplitudes is also needed. To progress on the knowledge of this ratio,
dominated by non-adiabatic effects, ground-based spectroscopic as well as photometric observations are
needed on the same targets. In addition, this work package aims to investigate the effect of adopting various
stellar atmospheres on the super-adiabatic outer stellar layers and consequently mode amplitude ratios.
Tasks:
1.
2.
A model for mode Intensity-Velocity relation, using both 1D and 3D simulations.
Testing and validation of this model using photometric data from CoRoT and Kepler, as well as
from ground-based (Doppler) observations of one the same stars.
Input:
Non-adiabatic oscillation code
Dependencies:
WP 126 000
Output:
A model for mode Intensity-Velocity relation.
Deliverables:
A model for mode Intensity-Velocity relation.
Milestones:
01/2018: A model for mode Intensity-Velocity relation, using both 1D and 3D simulations
12/2022: Validation using available photometric (CoRoT and/or Kepler) and ground-based (Doppler)
observations on the same stars and improvement if necessary
Risks:
Some delays can arise depending on the available ground-based observations.
PSM WPDs
DEVELOPMENT
Seismology of Magnetic Activity
Leader: Laurent Gizon
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 109/200
PSM WP 126 400
Development phase
04/2016 — 12/2023
Institution: Max-Planck-Institut für Sonnensystemforschung (Germany)
Key Personnel: L. Gizon; A. Bhagatwala (Stanford); S. Hanasoge (Princeton); H. Schunker (MPSSR)
Objectives:
Model and characterize the influence of magnetic fields on global mode frequencies in Sun-like stars. This
requires the development of a code to compute the interaction of seismic waves with surface magnetic activity
(starspots and active regions). Among various applications, we will then seek methods to infer the level of
surface magnetic activity from stellar-cycle frequencies variations, and methods to clean mode frequencies from
magnetic effects.
Tasks:
1. Develop a code for simulating wave propagation through 3D magnetized stellar interiors, which is capable of
running on massively parallel supercomputers and (most probably) based on the cubed- sphere model. This
code will be used to compute the influence of surface magnetism on low-degree modes (the forward problem). A
numerical code is required because the effects of the magnetic field are not small near the surface, i.e. first
order perturbation theory does not work.
2. Procurement of development system to validate code.
3. Technical validation of code.
4. Validation of concept using solar oscillations (explain low-degree solar frequency shifts from maps of surface
activity).
5. Characterization and parameterization of magnetic effects on oscillations.
6. Development of methods to clean frequencies from magnetic effects.
7. Development of methods to infer the magnetic field from stellar-cycle variations in mode frequencies.
Input:
1. Scientific literature.
2. Definition Phase activities: GLASS code.
3. Development system to validate MHD pulsation code.
Dependencies: WP 126 000, WP 123 000, WP 123 100, WP 123 400, WP 372 220
Output: Completion of tasks 2 to 7
Deliverables: Reports, MHD pulsation code, methods of analysis
Milestones:
01/2018-12/2018: Validation of the MHD code to model seismic wave propagation
01/2019-12/2019: Stellar-cycle variations of mode frequencies
01/2020-12/2020: Characterization and parameterization of magnetic effects on oscillations
01/2021-12/2021: Developments of methods to clean frequencies from magnetic effects
01/2022-07/2023: Developments of methods to infer the magnetic field from frequencies variations
Risks: Acceptable risk.
PSM WPDs
DEVELOPMENT
Seismic Constraints From Aging Stars
Leader: Benoît Mosser
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 110/200
PSM WP 127 000
04/2016 — 12/2023
Institution: Observatoire de Paris (France)
Key Personnel: B. Mosser; M. Barbieri (Obs. Cote d’Azur); A. Miglio (Birmingham); J. Montalban (INAFPadova); M.-A. Dupret (Liège); T. Morel (Liège); A. F. Lanza (INAF-Catania); A. Weiss (MPA Garching)
Objectives:
Evolved stars keep memory of the physical mechanisms taking place during the main sequence and sub-giant
phases. Due to their specific seismic properties, they can be used to probe more efficiently some of those
mechanisms than using main sequence seismic data.
This WP aims at coordinating the activities of stellar modelling, atmosphere parameter determination and
seismic tools specific for the case of red giants stars in order to provide:
- Procedures that deliver masses, radius, evolutionary state and chemical composition required by the WP
dedicated to exoplanets around red giant stars.
- Procedures that constraints stellar evolution for strengthening the properties of stars hosting planets at all
evolutionary stages
- Procedures that constraints stellar population for strengthening the properties of stars hosting planets at all
evolutionary stages
Coordination with the activities under WP 121 000 (stellar models), WP 123 (stellar activity), WP 122 (nonseismic diagnostics).
These developments will be built upon the CoRoT, Kepler, and K2 legacy
Tasks:
1.
Coordinate the work done by WP 127 100-300, 122
2.
Make sure that the quality of the outputs from WP 127 100-300 and 122 match the specified
requirements
3.
Establish procedures for utilizing the asteroseismic insights obtained through the analysis of PLATO
data to improve the determination of stellar parameters.
Input:
Available observations from CoRoT and Kepler data as learning sets
Dependencies:
WP 127 100, WP 127 200, WP 122, WP 121, WP 123, WP 128
Output:
Optimized procedures to determine accurate masses, radii, ages, chemical composition as well as uncertainties
that satisfy the exoplanet specifications, with full documentation of the procedures.
Deliverables: reports
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results.
Risks:
Minimal risks, owing to the experience gained with precursors (CoRoT, Kepler)
PSM WPDs
DEVELOPMENT
Stellar Models of Evolved Stars
Leader: Paolo Ventura
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 111/200
PSM WP 127 100
04/2016 — 12/2023
Institution: INAF-Roma (Italy)
Key Personnel: P. Ventura; P. Eggenberger (Geneva); P. Marigo (INAF-Padova); L. Girardi (INAF-Padova); A.
Bressan (INAF-Padova); E. Brocato (INAF-Teramo); G. Raimondo (INAF–Teramo), Y. Lebreton (GEPI, Paris); J.
Montalban (INAF-Padova); A. Noels (Liège); A. Palacios (Montpellier); S. Cassisi (INAF-Teramo)
Objectives:
Provide grids of high quality 1D stellar models for low and intermediate mass in the phases of red giant branch
(RGB) and core He-burning (He-B). These grids are an extension of those delivered by WP 121 100 for a
reduced set of stellar parameters and lower precision than that required for main sequence models. The domain
of mass and age will be determined by the constraints provided by the age of the universe and the maximum
luminosity for exoplanet transit detection in the framework of PLATO.
Tasks:
1.
Keeping updating the physical description red giant stellar models in dedicated evolutionary codes
2.
Inclusion of missing but necessary physical ingredients in evolutionary codes and computations of
improved stellar models
3.
Testing the theoretical evolutionary framework on suitable empirical data: star clusters and eclipsing
binaries;
4.
Comparing models computed by the different groups participating to the project
Input:
1.
Relevant data concerning some physical inputs: Equation of State, conductive opacity, nuclear reaction
rates; boundary conditions from atmosphere models
2.
Evolutionary code and numerical tools for extracting the structural and evolutionary properties of the
various stellar models.
3.
Dependencies:
WP 127 000 and WP 121 000
Output:
Package of available grids of updated stellar models for low mass red giant stars covering a large range of
chemical composition and with the required precision for oscillation computations. A documented user guide
providing a detailed description of the content of grids and of the physical description assumed in the model
computation.
Deliverables:
Grids of stellar models for red giant evolutionary phase. Evolutionary tracks and internal structure files in a
standard format (FGONG) for oscillation computations.
Milestones:
06/2017: First generation grid
12/2018: Provide preliminary grid of stellar models including effects of non-standard physics.
2019-23: Provide continuously improved stellar models and extend the parameter domains
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 112/200
Seismic Diagnostics for Evolved Stars
Leader: Andrea Miglio
Rev.: 5
Development phase
PSM WP 127 200
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: A. Miglio; S. Deheuvels (OMP, IRAP); M.-A. Dupret (Liège); P. Eggenberger (Geneva);
Silva Aguirre (Aarhus); J. Montalban (INAF-Padova)
V.
Objectives:
To develop seismic diagnostics specific to evolved stars that can provide precise stellar mass, age, radius and
properties of the stellar interior. This objective has three applications: providing accurate stellar parameters for
planetary host stars, understanding of stellar physics, and characterising stellar populations monitored by
PLATO. These developments build upon the CoRoT, Kepler, and K2 legacy.
Tasks:
1.
Compute adiabatic oscillation frequencies for models in the grid provided by WP 127 100
2.
Extend the validation and test of scaling relations (WP 125 100) to the case of evolved stars, using
models provided by WP 127 100
3.
Develop seismic diagnostic tools specific to evolved stars, that give reliable estimates of stellar
properties (mass, radius, age)
4.
Develop seismic tests of the internal structure of evolved stars, with the aim of adding accuracy to stellar
models, hence to the age determination of planetary host giants and main-sequence stars (WP 127 300).
5.
Comparison with hare and hound exercises of the results and the resulting precisions on the derived
quantities
6.
Development of optimised procedures to implement computations of stellar parameters and their
uncertainties
Input:
Grids of stellar models (from WP 127 100), available CoRoT, K2, and Kepler data.
Dependencies:
Input from WP 127 100
Output:
Optimised and validated procedures to determine accurate masses, radii, ages as well as uncertainties that
satisfy the exoplanet specifications.
Deliverables:
Optimised and validated procedures to determine accurate masses, radii, ages, chemical composition as well as
uncertainties that satisfy the exoplanet specifications
Milestones:
07/2017: Initial planning meeting
07/2023: Delivery of procedures, documentation and test results
Risks: Minimal risks
PSM WPDs
DEVELOPMENT
Constraints on Main-Sequence Stars
Leader: Josefina Montalban
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 113/200
PSM WP 127 300
04/2016 — 12/2023
Institution: University of Padova (Italy)
Key Personnel J. Montalban; A. Miglio (Birmingham); S. Deheuvels (OMP, IRAP); M.-A. Dupret (Liège);
Eggenberger (Geneva); V. Silva Aguirre (Aarhus); L. Girardi (INAF-Padova); A. Bressan (INAF-Padova);
Lebreton (GEPI, Paris); S. Cassisi (INAF-Teramo); A. Palacios (Montpellier)
P.
Y.
Objectives:
Deriving constraints on main-sequence stars from the comprehensive study of the observations of stellar
populations including all evolutionary stages
Tasks:
1.
Use stellar evolution models from WP 127 100
2.
Use adiabatic oscillation frequencies for models in the grid provided by WP 127 200
3.
Develop seismic diagnostic tools all along stellar evolution
4.
Use seismic diagnostics to constrain populations of stars from ensemble seismic properties
5.
Comparison with hare and hound exercises of the results and the resulting precisions on the derived
quantities
6.
Development of optimised procedures to implement computations of stellar parameters and their
uncertainties
Input:
Grids of stellar models from WP 127 100, seismic analysis from WP 127 200
Dependencies:
Input from WP 127 100 and 127 200; cross-check with WP 121
Output:
Optimised and validated procedures to constraints stellar models from the observation of ensemble properties
Deliverables:
Optimised and validated procedures to determine accurate masses, radii, ages, chemical composition of red
giant stars as well as uncertainties. Constraints on main-sequence stars.
Milestones:
07/2017: Initial planning meeting
07/2023: Delivery of procedures, documentation and test results
Risks: Minimal risks
PSM WPDs
DEVELOPMENT
Power Spectrum Fitting Tools
Leader: Bill Chaplin
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 114/200
PSM WP 128 000
Development phase
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: B. Chaplin
Objectives: Coordination of the work packages WP 128 100 through WP 128 250, which deal with the
application of data analysis techniques -- in particular "peak bagging" -- to the frequency-power spectra of the
lightcurves, in order to extract estimates of the seismic and background parameters.
Tasks: Coordination of the sub-packages under WP 128 000
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from Kepler, CoRoT and TESS
Dependencies: WP 128 000 is part of the Stellar Science work package
Output: Procedures for analysis of the frequency power spectra of target stars
Deliverables: Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Average Seismic Parameters
Leader: Rafael A. García
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 115/200
PSM WP 128 100
Development phase
04/2016 — 12/2023
Institution: IRFU/SAp, UMR AIM, CEA-Saclay (France)
Key Personnel: R. García; B. Chaplin (Birmingham); S. Hekker (MPSSR); D. Huber (Sydney); T. Kallinger
(Vienna); S. Mathur (SSI); B. Mosser (OBSPM); D. Stello (Sydney)
Objectives: To specify requirements and procedures for the estimation of average seismic parameters for solarlike oscillators
Tasks:
1.
Review of procedures developed for CoRoT, Kepler and TESS
2.
Scope out requirements for test sets comprised of artificial PLATO data and existing
Kepler Data; perform tests
3.
Describe fully automated procedures
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from CoRoT, Kepler and TESS
Dependencies: WP 128 100 is part of the Stellar Science work package
Output: Procedures for extracting average seismic parameters of targets
Deliverables: Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Mode Fitting Tools
Leader: Bill Chaplin
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 116/200
PSM WP 128 200
Development phase
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: B. Chaplin
Objectives: Coordination of the work packages WP 128 210 through WP 128 250 which are devoted to peakbagging, extraction of estimates of the seismic and background parameters from frequency-power spectra of the
lightcurves.
Tasks: Coordination of the sub-packages under WP 128 200
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from Kepler, CoRoT and TESS
Dependencies: WP 128 200 is part of the Stellar Science work package
Output: Procedures for fitting frequency-power spectra of targets
Deliverables: Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Solar-Like Stars
Leader: Bill Chaplin
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 117/200
PSM WP 128 210
Development phase
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: B. Chaplin; T. Appourchaux (IAS); J. Ballot (IRAP); T. Campante (Birmingham); G. Davies
(Birmingham); R. García (CEA); M. Lund (AAU); T. White (MPSSR)
Objectives: Specify optimal requirements, techniques and procedures for peak-bagging solar-type stars.
Tasks:
1.
2.
3.
4.
Review of procedures and codes developed for CoRoT, Kepler and TESS
Scope out requirements for test sets comprised of artificial PLATO data and existing
CoRoT and Kepler Data; perform tests
Development of fully automated procedures for peak-bagging
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from CoRoT, Kepler and TESS
Dependencies:
WP 128 210 is part of the Stellar Science work package
Output:
Procedures for fitting frequency-power spectra of targets
Deliverables:
Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Solar-Like Stars with Planets
Leader: Tiago Campante
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 118/200
PSM WP 128 220
Development phase
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: T. Campante; B. Chaplin (Birmingham); T. Appourchaux (IAS); J. Ballot (IRAP); E. Corsaro
(CEA); G. Davies (Birmingham); R. Handberg (AAU); M. Lund (AAU); T. White (MPSSR)
Objectives:
Specify any changes to peak-bagging procedures for solar-type stars required for targets with detected
candidate transiting planets
Tasks:
1.
2.
3.
Review of procedures and codes developed for Kepler and TESS
Scope out requirements for test sets comprised of artificial PLATO data and existing Kepler
Data; perform tests
Development of fully automated procedures for peak-bagging
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from Kepler and TESS
Dependencies:
WP 128 220 is part of the Stellar Science work package
Output: Procedures for fitting frequency-power spectra of targets
Deliverables: Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Multiple Stars
Leader: Guy Davies
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 119/200
PSM WP 128 230
Development phase
04/2016 — 12/2023
Institution: University of Birmingham (UK)
Key Personnel: G. Davies; B. Chaplin (Birmingham); T. Appourchaux (IAS); J. Ballot (IRAP); T. Campante
(Birmingham); M. Lund (AAU); T. White (MPSSR)
Objectives:
Specify any changes to peak-bagging procedures for solar-type stars when there is clear evidence of multiplicity
Tasks:
1.
Review of procedures and codes developed for Kepler and TESS
2.
Scope out requirements for test sets comprised of artificial PLATO data and existing Kepler Data;
perform tests
3.
Development of fully automated procedures for peak-bagging
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from Kepler and TESS
Dependencies: WP 128 230 is part of the Stellar Science work package
Output: Procedures for fitting frequency-power spectra of targets
Deliverables: Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Ensemble Fit
Leader: Jerôme Ballot
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 120/200
PSM WP 128 240
Development phase
04/2016 — 12/2023
Institution: IRAP (France)
Key Personnel: J. Ballot; T. Appourchaux (IAS); T. Campante (Birmingham); B. Chaplin (Birmingham);
G. Davies (Birmingham); R. García (CEA); M. Lund (AAU); T. White (MPSSR)
Objectives:
Specify additional techniques and procedures for fitting stars in clusters, i.e., to leverage the additional prior
constraints available on such stars
Tasks:
1.
Review of any relevant procedures developed for Kepler and TESS
2.
Scope out requirements for test sets comprised of artificial PLATO data and existing Kepler Data;
perform tests
3.
Development of fully automated procedures for peak-bagging
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from Kepler and TESS
Dependencies:
WP 128 240 is part of the Stellar Science work package
Output: Procedures for fitting frequency-power spectra of targets
Deliverables: Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Fitting Tools for Evolved Stars
Leader: Saskia Hekker
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 121/200
PSM WP 128 250
Development phase
04/2016 — 12/2023
Institution: MPSSR (Germany)
Key Personnel: S. Hekker; B. Chaplin (Birmingham); E. Corsaro (CEA); G. Davies (Birmingham), Y. Elsworth
(Birmingham); T. Kallinger (Vienna); B. Mosser (OBSPM); D. Stello (Sydney); T. White (MPSSR)
Objectives:
Specify special techniques and procedures needed to extract seismic parameters on the oscillations of evolved
solar-like oscillators (red giants)
Tasks:
1.
Review of procedures developed for CoRoT and Kepler
2.
Scope out requirements for test sets comprised of artificial PLATO data and existing Kepler Data;
perform tests
3.
Define and test fully automated procedures for peak-bagging
Input:
1.
PLATO Red Book and up-to-date data on expected photometric performance
2.
Results on artificial PLATO data
3.
Procedures/knowledge/experience from CoRoT and Kepler
Dependencies:
WP 128 250 is part of the Stellar Science work package
Output: Procedures for fitting frequency-power spectra of targets
Deliverables: Documentation on the procedures for implementation in the PDC
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2019: Intermediate delivery of procedures, documentation and test results
05/2022: Final delivery of the first generation of procedures, documentation and test results
Risks: None
PSM WPDs
DEVELOPMENT
Interfaces
Leader: Frédéric Baudin
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 122/200
PSM WP 129 000
Development phase
04/2016 — 12/2023
Institution: Institut d’Astrophysique Spatiale (France)
Key Personnel: F. Baudin; C. Barban (Lesia)
Objectives: Interface between Stellar Science and other WPs (specifically PDC and Exoplanet WPs), and
outreach activities related to the activities of the WP 120.
Tasks:
1.
Ensure no overlap exists between the different WP 120 and others
2.
Make sure that information from (to) the Stellar Science are transmitted to (from) the PDC
3.
Make sure that the methods developed in the Science Stellar are properly translated in PLATO
language and adapted to PLATO data
4.
Interface for outreach activities of WP 120
Input:
Models, prototyped algorithms and tools from WP 120 XXX (to be transmitted to PDC), potential outreach
material
Dependencies:
Output:
Validated specifications to be transmitted to PDC, outreach material from WP 120 ready for diffusion
Deliverables:
Reports and proposed validations of algorithms and tools
Milestones:
05/2016: Delivery of the first set of specifications to the PDC
05/2017: Delivery of first generation of validated models and procedures related to the characterization of host
stars
05/2022: Delivery of second generation of validated models and procedures related to the characterization of
host stars
Risks: None
PSM WPDs
DEVELOPMENT
Target / Field Characterization and Selection
Leader: Giampaolo Piotto
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 123/200
PSM WP 130 000
04/2016 — 12/2023
Institution: Università di Padova (Italy)
Key Personnel: G. Piotto
Objectives:
Coordinate all the WPs to deliver in due time the PLATO input catalogue with all relevant parameters for each
target.
Tasks:
1.
Support to the PSAT and PSM on the understanding of PLATO field and PLATO samples properties
2.
Select PLATO fields
3.
Define the list of parameters to be collected
4.
Provide the list of catalogues relevant for PIC
5.
Prepare the criteria for identification, selection and prioritization of the first observed field targets and
corresponding parameters
6.
Provide the criteria for contaminant list and properties selection
7.
Provide target false alarm probability
Input:
All catalogues/parameters gathered by WP 131 000 and WP 132 000
Dependencies:
Output of WP 131 000, WP 132 000
Output:
1.
LD and S&S proposal of the PLATO observing fields;
2.
Criteria for the identification, selection and prioritization of the first observed field targets and
corresponding parameters
Deliverables:
LD and S&S PLATO observing field coordinates. Criteria for PIC preparation for the first observing field
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-24m Validation of the PIC for the first observing field
L-18m Results of guest observer call added to the PIC
Risks:
Depends on Gaia output; in case of delay or failure from Gaia, the catalogue will rely on available
photometric/astrometric catalogues.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 124/200
Project Office Assistant
Leader: Valentina Granata
Rev.: 5
Development phase
PSM WP 130 100
04/2016 — 12/2023
Institution: Università di Padova (Italy)
Key Personnel: V. Granata
Objectives:
Support to the management of WP 130.
Tasks:
1.
2.
3.
4.
5.
6.
7.
8.
Support to organization of WP 130 team activities
Support to the organization of WP 130 team meetings and teleconferences.
Support to monitoring action items progress
Support to document preparation
WP 130 documentation management and archival
PLATO document tracking
Participation to PICs meetings and minute preparation
Participation to PSM teleconferences and minute preparation
Input:
•
•
•
•
PLATO Management Plan and PSM
PLATO Science Requirement Document
PDCR ESA review reports
Products and documentation of WP 131 000 and WP 132 000 and WP 133 000
Dependencies:
Output of WP 131 000, WP 132 000 and WP 133 000
Output:
Output of WP 131 000, WP 132 000 and WP 133 000
Deliverables:
WP 130 000 documentation
Milestones:
01/2018: Preparation of Reports defining preliminary parameters and specifications for first PLATO field
L-36m: Preparation of Reports defining criteria for selection and prioritization of the selected first observed field
L-30m: Preparation of Reports defining criteria for contaminants selection and false alarm probability
L-24m Preparation of Reports about validation of the PIC for the first observing field
L-18m Preparation of Reports about results of guest observer call added to the PIC
Risks:
None
PSM WPDs
DEVELOPMENT
Catalogues Analysis
Leader: Valerio Nascimbeni
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 125/200
PSM WP 131 000
04/2016 — 12/2023
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni
Objectives:
Coordinate the WP 131 100, 131 200, 131 300, 131 400, 131 500, 131 600 to collect relevant information and
define criteria allowing the characterization of stars that could be observed with PLATO. The resulting stellar
parameters will be the basis of the PLATO Input Catalogue (PIC) and lead to the selection of targets.
Tasks:
1.
Define the list of parameters to be collected
2.
Make sure the relevant information is searched for in all possible catalogues, and integrate the
information in a consistent way
3.
Follow the progress of the Gaia mission that should be the main contributor to the PIC
Input:
All catalogues and characterization criteria gathered by WP 131 100, 131 200, 131 300, 131 400, 131 500, 131
600
Dependencies:
Output of WP 131 100, 131 200, 131 300, 131 400, 131 500, 131 600 and all sub-packages therein
Output:
Final set of source catalogues, algorithms and criteria, adopted to extract astrophysical parameters of all the
stars of potential interest for the PIC.
Deliverables:
Documents reviewing the input catalogues, and describing the classification algorithms and criteria above.
Milestones:
L-24m: Final criteria for the characterization of the first PLATO field and preliminary criteria for the other fields
L-12m: Final criteria for the characterization of the whole PIC
Risks:
Depends on Gaia output (WP 131 100); in case of delay or failure from Gaia the catalogue will rely on catalogues
collected by WP 131 200 and 131 300, 131 400, 131 500, and 131 600.
PSM WPDs
DEVELOPMENT
Gaia Catalogue Analysis
Leader: Alessandro Sozzetti
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 126/200
PSM WP 131 100
04/2016 — 12/2023
Institution: INAF-Osservatorio Astrofisico Torino (Italy)
Key Personnel: A. Sozzetti; R. Smart (INAF-Torino)
Objectives:
The objective of this WP is to coordinate the analysis of all available information (astrometric, photometric, and
spectroscopic) initially from detailed simulations of Gaia observations and then from the Gaia early data releases
and final catalogue, to provide a highly complete reservoir of well-classified and well-parameterized nearby dwarf
stars from which to choose in order to populate the PLATO Input Catalogue.
Tasks:
Coordinate WP 131 110, WP 131 120, WP 131 130, and WP 131 140 activities
Input:
Output of WP 131 110, WP 131 120, WP 131 130, and WP 131 140
Dependencies:
WP 131 110, WP 131 120, WP 131 130, and WP 131 140
Output:
Communications to WP 133 200 for the definition of a finalized set of data products requirements ahead of the
publication of the Gaia early release catalogue. Communications with WP 131 300 for the purpose of
continuously refining and finalizing the list of target fields and the list of targets within each field based on the
improved assessment of the requirements on Gaia data products.
Deliverables:
Documents with detailed completeness assessments of nearby dwarf targets based on the combined analysis of
the Gaia early release catalogue. Detailed parameterization of potential targets criteria for PIC
Milestones:
06/2016: Final assessment of the combined analysis of WP 131 110, WP 131 120, WP 131 130, & WP 131 140
based on simulated Gaia data
12/2018: Final assessment of the combined analysis of WP 131 110, WP 131 120, WP 131 130, & WP 131 140
based on the Gaia early data release catalogues
12/2021: Final assessment of the combined analysis of WP 131 110, WP 131 120, WP 131 130, & WP 131 140
based on the Gaia final catalogue release
06/2022: Communications to WP 133 200 (finalized data products requirements based on the GAIA early release
catalogue) and WP 131 300 and WP 132 000 (finalized parameterization of potential PLATO targets criteria
based on the Gaia early data releases and final catalogue)
Launch: Communications to WP 133 200 (further refinements to data products requirements based on Gaia final
catalogue release, if applicable) and WP 131 300 and 132 000 (further refinements to parameterization of
potential PLATO targets criteria based on Gaia final catalogue release, if applicable)
Risks:
Biased completeness estimates due to significant discrepancies between the simulated performances of Gaia
astrometry, photometry and spectroscopy and the actual data quality assessed during mission operations
PSM WPDs
DEVELOPMENT
Astrometric Analysis
Leader: Mario G. Lattanzi
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 127/200
PSM WP 131 110
Development phase
04/2016 — 12/2023
Institution: INAF– Osservatorio Astronomico di Torino (Italy)
Key Personnel: M.G. Lattanzi; R. Smart (INAF-Torino); A. Sozzetti (INAF-Torino); 1 postdoc
Objectives:
Use of the Gaia Data Processing and Analysis Consortium released data for a robust assessment of the quality
of Gaia astrometry for the purpose of the definition of a PLATO Input Catalogue with a high degree of
completeness (i.e., minimizing the contamination from distant giants), and for the optimization of the PLATO
fields of view.
Tasks:
1.
General assessment of released Gaia astrometric data of the PLATO fields
2.
Independent assessment of the (e.g. parallax) error distributions as a function of longitude using the
GSR component of AVU operated at the Torino Gaia Data Processing Centre
3.
In-depth investigations of the quality of the astrometry for potential PLATO targets with parallax
estimates derived not as part of the main AGIS reduction pipeline
4.
Continued refinement of the reservoir of astrometrically selected objects for inclusion in the PIC using
data from subsequent data releases and the final Gaia catalogue
Input:
Released Gaia astrometric data
Dependencies:
Depends on Gaia
Output:
Estimates of the quality of parallax determination for nearby, bright dwarfs from analysis of Gaia astrometry at
the level of early data release and final catalogue, as a function of location in the sky and other relevant
parameters. Comparison metrics with dedicated simulations for PLATO fields and for the Kepler, K2, and TESS
fields
Deliverables:
Document with the assessment of the reliability/completeness of a high-accuracy astrometric catalogue of bright
nearby dwarfs based on early release and final catalogue Gaia data
Milestones:
06/2017: Estimates of Gaia astrometric performance using the first release catalogue
12/2018: Refined assessment of Gaia astrometric performance using the subsequent data releases
Launch: Astrometric selection procedures of objects for inclusion in the PIC using data from the Gaia original
release catalogue.
Risks:
Significant degradations in the post-commissioning Gaia astrometric performance estimates - LOW
PSM WPDs
DEVELOPMENT
Photometric Analysis
Leader: Simon Hodgkin
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 128/200
PSM WP 131 120
Development phase
04/2016 — 12/2023
Institution: Institute of Astronomy, Cambridge (UK)
Key Personnel: S. Hodgkin
Objectives:
Understanding, and in particular facilitating the use of Gaia photometry for the optimal selection of targets in the
PLATO fields (and how it can even help fine tuning the PLATO fields selection themselves). To this purpose, this
WP will examine the outputs of the Data Processing and Analysis Consortium and planned data release
schedule for Gaia. Right now this can be based on the GOG (Gaia Object Generator) software interface. The
Gaia data release schedule (beginning in the summer of 2016) ensures that, well in the advance of PLATO’s
launch, we will have the most precise all-sky catalogue available to provide a strong foundation for the PIC and
everything that depends on it.
Tasks:
1.
To ensure the correct elements and appropriate views of the Gaia simulated and released photometric
catalogue data (G-band and BP/RP) are accessible to the PIC. This needs full awareness of the requirements on
the PIC by other operational aspects (field selection, target selection, contamination analysis, planet candidate
environment analysis, candidate ranking and so on.)
2.
To ensure that GOG simulated fake variability (spots, transiting and eclipsing systems) can be included
in the PIC for objects of well-constrained effective temperature and radii.
3.
To extend this variability analysis to real Gaia Photometry, with real understanding of the Gaia stars as
the data are released (including luminosity class, parallax, binarity).
4.
Investigation of the usefulness and limitations of the Gaia data for lightcurve de-blending and Source
Environment Analysis.
5.
Preliminary selection of PLATO fields from the Gaia early release catalogue.
6.
Incorporate the results of subsequent Gaia releases
Input:
Simulated and early release Gaia photometric data
Dependencies:
Depends on Gaia
Output:
Description of the available photometric data to the PIC as a function of time from Gaia. Definition of the
expected photometric accuracy of, and of the ability to distinguish intrinsically variable stars in, the Gaia Early
Data Release and subsequent releases. Cycle progress reports and assurance reports to the PSM
Deliverables:
Documentation of the Gaia schema for the PIC Gaia photometry tables. Document an assessment of the
expected Gaia photometric performance based on the Gaia early release catalogue. Document completeness,
contamination and reliability of the photometric-based measurements from Gaia.
Milestones:
06/2016: Estimates of Gaia photometric performance based on simulations.
01/2017: Refined assessment of Gaia photometric performance using the early data release catalogue
Launch: Continued refinement of the reservoir of photometrically selected objects for inclusion in the PIC using
data from subsequent data releases.
Risks:
Evolution in the Gaia photometric performance
PSM WPDs
DEVELOPMENT
Spectroscopic Analysis
Leader: Alejandra Recio-Blanco
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 129/200
PSM WP 131 130
04/2016 — 12/2023
Institution: Observatoire de la Côte d'Azur (France)
Key Personnel: A. Recio-Blanco; P. de Laverny (Côte d’Azur); C. Soubiran (Bordeaux)
Objectives:
Understanding in detail how Gaia spectroscopy can be used towards the optimal selection of targets in the
PLATO fields (and how it can even help fine tuning the PLATO fields selection themselves). To this purpose, this
WP will examine the outputs of the Gaia/RVS Generalized Stellar Parameterizer-spectroscopy (GSP-spec)
algorithm of the Gaia Data Processing and Analysis Consortium.
Tasks:
1.
Selection of automated parameterization methods (MATISSE, DEGAS, GAUGUIN) to evaluate the Gaia
RVS constraints for the different types of stars, with particular interest in F-G-K stars in the V<11 magnitude
domain
2.
Evaluation and treatment of effective temperature vs. gravity degeneracies for the Gaia RVS data
3.
Tests of the algorithms with on large datasets of real spectra, including the Gaia RVS wavelength
domain and resolutions (AMBRE project)
Input:
Simulated Gaia spectra and real spectra including the RVS wavelength domain
Dependencies:
Depends on Gaia WP 823-0000
Output:
Constraints of Gaia spectroscopic data on stellar atmospheric parameters and chemical abundances
Deliverables:
Document with the assessment of the Gaia/RVS errors in stellar parameters for FGK stars
Milestones:
04/2016: Robust constraints from Gaia/RVS simulated data
09/2016: Tests with real GBOG data of the EPSL fields and comparison with the corresponding results from Gaia
RVS data. Comparison with results of the Gaia-ESO Survey data for the same targets.
04/2017: First real constraints from the Gaia/RVS intermediate results
09/2017: First internal evaluation of the Gaia/RVS parameters for stars included in the Gaia Data Release 1, in
particular the Hipparcos stars and the stars included in the Tycho catalogue.
09/2018: Robust constraints on Gaia/RVS characterisation using Gaia DR2 data.
01/2019: Report on the validation activities of Gaia/RVS parameterization
Launch: Final spectroscopic characterization of PLATO targets from the Gaia/RVS data and list of possible
PLATO targets for the PLATO fields
Risks:
Variations in the Gaia/RVS instrumental performances
PSM WPDs
DEVELOPMENT
Gaia Parameters Extraction
Leader: Alessandro Sozzetti
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 130/200
PSM WP 131 140
04/2016 — 12/2023
Institution: INAF-Osservatorio Astronomico di Torino (Italy)
Key Personnel: A. Sozzetti; M.G. Lattanzi (INAF-Torino); R. Smart (INAF-Torino); 1 postdoc
Objectives:
Definition and prioritization of the astrometric, spectroscopic, and photometric parameters from the Gaia early
data releases and final catalogue utilized for the purpose of the definition of the PLATO Input Catalogue and for
the optimization of the PLATO fields of view.
Tasks:
1.
Creation, software implementation and testing of an algorithm for cross-examination of the Gaia
astrometric, spectroscopic, and photometric information for the definition and prioritization of the set of
parameters utilized for the selection of PIC targets and PLATO fields of views, based on extensive GOG and
AGISLab simulations of the PLATO fields, and the completeness assessment from WP 131 110, WP 131 120,
and WP 131 130
2.
Adaptation of the algorithm for ingestion of, and extraction of the relevant parameters from, actual Gaia
early release and final catalogue data
Input:
1.
Simulated, early release and final Gaia data
2.
Input from WP 131 110, WP 131 120, and WP 131 130
Dependencies:
Depends on Gaia
Output:
Finalized and prioritized list of stellar parameters from Gaia astrometry, photometry, and spectroscopy to be
used for the selection of PIC targets and PLATO fields of view
Deliverables:
Documentation and software algorithms detailing the Gaia catalogue parameters definition and prioritization
criteria (e.g. cross-examination of Gaia error models) adopted for their finalization
Milestones:
11/2016: Algorithms definition
04/2017: Software implementation and testing of the algorithms
09/2017: Definition and prioritization of the required Gaia parameters based on the algorithms developed for
GOG/AGISLab simulations, and WP 131 110, WP 131 120, and WP 131 130 input
01/2018: Finalized definition and prioritization of the required Gaia parameters using the early data release
catalogue
Launch: Continued refinement of the prioritized list of Gaia parameters for dwarf stars to be potentially included
in the PIC using data from subsequent releases and the final catalogue
Risks:
Unavailability of the necessary catalogue parameters from Gaia astrometry, photometry and spectroscopy at the
level of early data releases and final catalogue - LOW
PSM WPDs
DEVELOPMENT
PLATO-Gaia Simulations
Leader: Holger Voss
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 131/200
PSM WP 131 150
04/2016 — 12/2023
Institution: University of Barcelona (Spain)
Key Personnel: H. Voss; X. Luri (UB), J.M. Carrasco (UB), F. Julbe (UB)
Objectives:
Implement additional elements into the Gaia Object Generator (GOG): a) to refine the error models of
astrometry, photometry and spectroscopy according to the real Gaia mission and the intermediate and final
catalogues (if available), b) to simulate PLATO targets from Gaia catalogues, and c) to become a tool for the
selection of PLATO target fields.
Tasks:
1. Derive transformations from Gaia photometry to PLATO photometry for the sources in the Gaia catalogue
to be updated during the development phase when the instrument is changing.
2. Implement error models in GOG according to the latest Gaia catalogue
3. Provide tools to evaluate the contribution of faint Gaia sources to the background level of the pixel
4. Develop GOG to become a tool for WP 131 110, WP 131 120, WP 131 130 and WP 131 140
5. Provide simulations for WP 131 110, WP 131 120, WP 131 130, WP 131 140.
6. Compile additional data (ground or space based) that may be needed to provide simulations for PLATO.
Input:
Gaia catalogue releases: astrometric, photometric and spectroscopic data
Gaia DPAC GOG tool for simulation
PLATO instrument definition (passband, sensitivity, QE and pixel sizes in particular) kept updated
5.
Dependencies:
Gaia Object Generator (owned by Gaia Data Processing and Analysis Consortium), WP 131110, WP 131120,
WP 131130 and WP 131140
Output:
1. PLATO predicted brightness for Gaia sources
2. GOG adapted to PLATO Input Catalogue construction
3. Simulations required to other WP for PIC definition for Gaia sources (astrometry, photometry, spectroscopy,
stellar parameters)
Deliverables:
Documentation on the tasks and outputs
Milestones:
09/2016: First error model from the Gaia first release (astrometry, G-band photometry)
03/2017: Updated error model from the Gaia second data release (astrometry, photometry)
06/2017: GOG version adapted to PLATO
07/2017: Start providing simulations of the defined fields for PLATO
03/2018: Updated error model from the Gaia third release (astrometry, photometry, spectroscopy, stellar
parameters)
2018-2023: Iterate with other WP (WP 131110, WP 131120, WP 131130 and WP 131140 in particular) requests
of simulations to define PIC.
2023: Updated error model from the Gaia final release (astrometry, photometry, spectroscopy, stellar
parameters)
Risks: Delays in the Gaia data releases (low).
PSM WPDs
DEVELOPMENT
Other Large Catalogues Analysis
Leader: Riccardo Claudi
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 132/200
PSM WP 131 200
04/2016 — 12/2023
Institution: INAF-Osservatorio Astronomico di Padova (Italy)
Key Personnel: R. Claudi; S. Benatti (INAF-Padova)
Objectives:
The objective of this WP is to coordinate the analysis of available photometric, astrometric and stellar activity
catalogues to define and to implement the tools and parameter for an optimal extraction of the 5 PLATO samples
of targets and the M-dwarf targets.
Tasks:
Coordination and management of the package
Input:
Available (and planned) catalogues for photometry, astrometry and activity for stars up to M spectral type
Dependencies:
Depends on other catalogues
Output:
Extraction of subgiants and dwarfs later than F5 up to M which will provide the basic input for “Target and Field
Selection” WP 132 000
Deliverables:
Catalogues of possible PLATO targets
Milestones:
09/2016: Optimal tools for the extraction of the PLATO targets and list of possible targets for PLATO long term
field
L-36m: Further photometric/astrometric characterization of PLATO targets, and list possible PLATO targets for
the remaining PLATO fields
Risks:
Available photometric/astrometric catalogues may not be sufficient to identify (with high completeness) all
PLATO targets, in particular for stars with V>11.0. Additional observations may be needed, and their costs must
be estimated
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 133/200
Photometric and Astrometric Catalogues
Leader: Valerio Nascimbeni
Rev.: 5
Development phase
PSM WP 131 210
04/2016 — 12/2023
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni; G. Piotto (Padova); S. Ortolani (Padova); 1 postdoc
Objectives:
Development of the optimal algorithms and criteria for the extraction of stellar parameters of all the stars which
can be considered for inclusion in the PIC, from the analysis of existing wide-field photometric and astrometric
catalogues.
Tasks:
1.
Test the classification techniques reviewed during the Definition Phase to determine the optimal criteria
for characterizing the potential PLATO targets
2.
Include in the analysis the photometric/astrometric data coming from new surveys which will have
become available, and re-assess the reliability (completeness and contamination levels) of the output data
3.
Implement software tools to provide a single, homogeneous final database of stellar parameters
4.
Cross-check the results with independent stellar parameter derived from Gaia (WP 131 100) or groundbased spectroscopic surveys (WP 131 250, 131 320) or additional observations (WP 131 330)
Input:
Existing and forthcoming wide-field photometric/astrometric catalogues
Dependencies:
For testing purposes: preliminary PLATO LD fields from WP 132 100
Output:
Criteria for the extraction of stellar parameters and the associated reliability diagnostics for every star of potential
interest for the PIC
Deliverables:
Document with the assessment of the reliability of the extracted stellar parameters, along with a detailed
description of the technique(s) and tools to be used to derive stellar classification
Milestones:
L-24m: freezing of the optimal extraction tools for the LD fields
L-12m: freezing of the optimal extraction tools for the S&S fields
Risks:
Available data could not be sufficient to cover the magnitude range of the PLATO Stellar Samples P1-P5 with the
required level of reliability. In particular, some risk exists for the fainter samples, P4 and P5.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 134/200
M-Dwarfs
Leader: Loredana Prisinzano
Rev.: 5
PSM WP 131 220
Development phase
04/2016 — 12/2023
Institution: INAF-Osservatorio Astronomico di Palermo (Italy)
Key Personnel: L. Prisinzano; L. Affer (INAF-Palermo); G. Micela (INAF-Palermo)
Objectives:
Optimal extraction of M-dwarf candidate targets in the PLATO Stellar Sample 4 within the PLATO fields selected
by WP 132 200, from the comparison of photometric catalogues and spectral classification tools
Tasks:
1.
Use the spectral classification tools chosen during the Definition Phase to select the sample of M-dwarf
targets from the available photometric catalogues
2.
Include M-dwarf fiducial candidates selected by available spectroscopic catalogues of M-dwarfs
3.
Include photometric data coming from new surveys which will have become available, to re-asses the
reliability (photometric errors, astrometric confusion, contamination level) of the output data
4.
Implement software tools to provide a single, homogeneous final catalogue of M-dwarfs
5.
Use of the first partial release of Gaia results to check and refine the M-dwarf sample
Input:
Existing and forthcoming photometric/spectroscopic/astrometric catalogues and PLATO fields selected by WP
132 200
Dependencies:
Selected PLATO fields from WP 132 200
Output:
Catalogue of M-dwarf candidate targets to be used for the PLATO Stellar Sample 4
Deliverables:
Report with description and discussion of the reliability of adopted input photometric catalogues and techniques
used to classify the candidates for the PLATO Stellar Sample 4
Milestones:
09/2016: Final re-assessment based on the best available spectral classification tools of the extracted M-dwarf
catalogue for the first PLATO long-duration field
L-36m: Refined first catalogue field, catalogue of M-dwarfs for the second PLATO long-duration field and for the
step & stare fields
Risks:
Available data could be contaminated by reddened early type stars and/or giants and/or pre-main sequence
objects.
PSM WPDs
DEVELOPMENT
M-Dwarfs as Planet Hosts
Leader: Peter Wheatley
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 135/200
PSM WP 131 221
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: P. Wheatley; 1 postdoc
Objectives:
Simulate the P4 sample of M-dwarfs detectable against jitter noise in the PLATO fields and thereby determine
the precise magnitude limits and numbers of faint targets to be monitored in each field (the P4 targets are
relatively faint, but provide a key component of the habitable planets detectable by PLATO, especially in the
step-and-stare phase). Liaise with PDC to assess impact on data reduction and analysis software set by this
uniquely faint sample, and update software requirements where necessary. Assess stellar activity and variability
of the P4 sample as an input to catalogue selection (WP 131 220). Determine the likely planet catch and
magnitude distribution of M-dwarf planet hosts and ensure that adequate and appropriate follow-up resources
are allocated to the confirmation of this small-planet sample (with priority given to the potentially habitable
planets).
Tasks:
1.
Ongoing review of the scientific literature and of ground-based follow-up facilities (especially IR
spectrographs capable of radial velocity confirmation of small planets around M-dwarf hosts).
2.
Simulate M-star population in each PLATO field, accounting for range of spectra and jitter noise.
3.
Simulations of likely planet catch and magnitude distribution of M-star planet hosts.
4.
Liaison with PDC on data reduction and analysis issues related to the faintness of the P4 sample.
5.
Feedback on the P4 selection criteria defined in WP 131 220.
6.
Analysis of follow-up resources needed to confirm terrestrial planets around M-star sample.
Input:
Scientific literature, PLATO Red Book, PLATO end-to-end simulator, P4 selection criteria from WP 131 220.
Dependencies:
Updated PLATO payload description from definition phase. P4 selection criteria from WP 131 220.
Output:
An understanding of the P4 M-dwarf target sample, including the impact of stellar activity and variability;
feedback on criteria for target selection (to WP 131 220); predictions of the likely numbers of small planets
detected; and an assessment of the resources needed for confirmation of this key planet sample.
Deliverables:
Reports on P4 M-dwarf target sample population and likely distributions of planet sizes, host star magnitudes
and variability characteristics.
Milestones:
04/2017: Delivery of interim report to Science Coordinator
04/2019: First field preliminary criteria defined by PIC team
12/2023: Delivery of final report on activity
Risks:
Inadequate understanding of the M-dwarf target population could result in non-optimal allocation of data
reduction/analysis resources and follow-up resources to the P4 sample, and the loss of small habitable planets
that could otherwise be discovered with PLATO.
PSM WPDs
DEVELOPMENT
Stellar Activity
Leader: Isabella Pagano
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 136/200
PSM WP 131 230
Development phase
04/2016 — 12/2023
Institution: INAF- Osservatorio Astronomico di Catania (Italy)
Key Personnel: I. Pagano; G. Leto (INAF-Catania); 1 postdoc; A.F. Lanza (INAF-Catania)
Objectives:
The final objective is the production of a catalogue of data useful to assess the activity level of the PLATO
candidate targets. The objective of the present phase is to extract from the literature the data on stellar activity as
defined during the definition phase, acquire new data on activity level for the targets not already characterized,
production the catalogue to be ingested by the PDC, and to maintain update the catalogue with new data from
the literature
Tasks:
1.
phase
2.
3.
4.
Extraction of data on stellar activity from the literature according to what defined during the definition
Acquisition and reduction of new data on activity level for the targets not already characterized
Production of the catalogue to be ingested by the PDC
Update of the catalogue with new literature data
Input:
1.
Data in literature
2.
Data from ad hoc observations is required by the results of the definition phase
Dependencies:
WP 133 000
Output:
A catalogue of data useful to assess the activity level of the PLATO candidate targets.
Deliverables:
A catalogue of data useful to assess the activity level of the PLATO candidate targets.
Updated release of the catalogue after its first release.
Milestones:
First release: to be agreed with PDC and interface package
Risks:
Acceptable risk
PSM WPDs
DEVELOPMENT
Binary Systems
Leader: Silvano Desidera
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 137/200
PSM WP 131 240
04/2016 — 12/2023
Institution: INAF—Osservatorio Astronomico di Padova (Italy)
Key Personnel: S. Desidera
Objectives: Provide census of stellar multiplicity of selected targets
Tasks:
1.
2.
3.
4.
5.
Provide census of eclipsing companions of selected targets from catalogues and literature
Provide census of spectroscopic companions of selected targets from catalogues and literature
Provide census of astrometric companions of selected targets from catalogues and literature
Provide census of visual companions of selected targets from catalogues and literature
Identify targets suitable for the search for circumbinary planets
Input:
Selected targets in each PLATO field from WP 132 000, info of individual targets from WP 131 000
Dependencies:
Input from WP 132 000 and WP 131 000, interface with WP 350 000 and WP 367 400 (circumbinary planets)
Output:
Data to WP 350 000, binarity information to WP 132 000 for priority definitions
Deliverables:
Document with specification of information to be provided
Data to be provided to the Ancillary Database (WP 350 000)
Milestones:
12/2017: Identification of information to be provided
L-72m: identify required information for the first PLATO field
L-36m: identify required information for the second PLATO field
Risks:
Limited risk (inclusion of targets unlikely of hosting planets due to dynamical influence of companions or more
challenging for planet identifications due to blending effects). Information from catalogues and literature more
important for the 1st PLATO field due to partial availability of Gaia data.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 138/200
Large Spectroscopic Catalogues
Leader: Ulisse Munari
Rev.: 5
Development phase
PSM WP 131 250
04/2016 — 12/2023
Institution: INAF-Osservatorio Astronomico di Padova (Italy)
Key Personnel: U. Munari
Objectives: Provide spectroscopic validation for targets to be observed by PLATO
Tasks:
RAVE has observed half-million and GALAH is currently observing one-million southern stars over the
magnitude range of interest for PLATO, deriving temperature, surface gravity, metallicity, alpha-enhancement,
microturbulence and rotational velocity, in addition to accurate chemical abundances of many key elements. By
accessing the RAVE and GALAH databases prior to continuing improving public releases and directly the
unpublished spectra, the PLATO input targets can be ranked according to the probability of success in meeting
mission specs.
Input:
RAVE and GALAH internal databases accessed thanks to “builder” status
Dependencies:
Selected PLATO fields and targets from WP 132 200
Output:
Validation of criteria for target selection from WP 132 200
Deliverables:
Validation of criteria for target selection from WP 132 200, high quality atmospheric parameters to assist in
analysis of spectral data secured by the PLATO ground-based segment and age determination
Milestones:
Depending from delivery of WP 132 200 products
Risks:
Minimal
PSM WPDs
DEVELOPMENT
Known and Candidate Exoplanets
Leader: Serena Benatti
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 139/200
PSM WP 131 260
04/2016 — 12/2023
Institution: INAF—Osservatorio Astronomico di Padova (Italy)
Key Personnel: S. Benatti; R. Claudi (INAF-Padova)
Objectives: Identification of known and candidate planets in the PLATO fields
Tasks:
- Gathering information on known Planets
- Gathering information on planet candidates
- Include photometric and spectroscopic data coming from new high Contrast Imaging surveys
- Include spectroscopic data coming from transit emission and absorption spectroscopy.
- Implement software tools to provide a simple homogeneous final catalogue for both known and candidate
planes.
Input:
- Existing and forthcoming planet catalogue and Candidate Planet catalogue
Dependencies:
-Selected PLATO Fields from WP 132 200
Output:
Catalogue of known and candidate planets
Deliverables:
- Software Tools
- Reports
- Catalogue
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
Risks:
Minimal
PSM WPDs
DEVELOPMENT
Single Target Additional Data
Leader: Isabelle Boisse
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 140/200
PSM WP 131 300
04/2016 — 12/2023
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: I. Boisse; F. Bouchy (IAP/OHP); M. Deleuil (LAM)
Objectives:
1.
Coordinate the development of the catalogue for individual stars of interest from the various WPs
2.
Validate the catalogue
Tasks:
Gather the outputs from WP 131 310, WP 131 320, WP 131 330
1.
Create a catalogue of stellar parameters derived from spectroscopic or imaging data analysis
2.
Check compliance of the catalogue with the specifications
3.
Validate the catalogue
4.
Validate regular updates
Input:
Catalogues with parameters and data (images and/or spectra) from WP 131 310, WP 131 320, WP 131 330
Dependencies:
Output of WP 131 310, WP 131 320 and WP 131 330
Output:
Catalogue of spectra and images with their characteristics (observatory, instrument, spectral resolution,
wavelength range, etc.) and their associated/derived stellar parameters to be provided to WP 131 000
Deliverables:
Milestones:
L-24m: delivery of criteria for the target selection for the first field. Refined criteria of the first PLATO field
Launch: delivery of criteria for target selection for the second field. Continuing refinements of the criteria.
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 141/200
High Resolution and Deep Imaging
Leader: Arthur Vigan
Rev.: 5
PSM WP 131 310
Development phase
04/2016 — 12/2023
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: A. Vigan; S. Desidera (INAF-Padova)
Objectives:
Identify high spatial resolution deep imaging available for the targets and collect relative astrometry and
photometry of stars close to the target (both physical companions and field stars). The data will be used to
characterize the environment of targets (location of potential contaminants, binarity) and will be further exploited
as part of the follow-up
Tasks:
1.
Identify high spatial resolution deep imaging available for the targets
2.
Collect relative astrometry and photometry of stars close to the targets
3.
Provide data to the Ancillary Database
Input:
Selected targets in each PLATO field from WP 132 000
Dependencies:
Input from WP 132 000, interface with WP 350 000 and WP 140 000
Output:
Data to WP 350 000
Deliverables:
Document with specification of information to be provided to the Ancillary Database
Data to be provided to the Ancillary Database (WP 350 000)
Milestones:
04/2017: Identification of information to be provided to Ancillary Database, format, etc.
L-24m: identify required information for the first PLATO field
L-24m: identify required information for the second PLATO field
Risks:
Minimal risk (ancillary information)
PSM WPDs
DEVELOPMENT
Spectroscopic Data
Leader: Isabelle Boisse
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 142/200
PSM WP 131 320
Development phase
04/2016 — 12/2023
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: I. Boisse
Objectives:
1.
Develop a catalogue for individual stars observed with ground-based spectrographs
2.
Validate the catalogue
Tasks:
1.
Gather spectra from ground-based facilities archives
2.
Create a catalogue of stars stellar parameters derived from spectroscopic data including radial velocity
measurements for stars with already known planets
3.
Check compliance of the catalogue with the specifications
4.
Validate the catalogue
5.
Validate regular updates
Input:
Catalogues from various observatory archives and/or scientific publications
Dependencies: WP 131 300
Output:
Catalogue of spectra with their characteristics (observatory, spectral resolution, wavelength range, etc.) and their
associated physical parameters to be provided to WP 131 000
Deliverables:
Catalogue of spectra with their characteristics (observatory, spectral resolution, wavelength range, etc.) and the
derived stellar parameters.
Milestones:
L-24m: delivery of criteria for the target selection for the first field. Refined criteria of the first PLATO field
Launch: delivery of criteria for target selection for the second field. Continuing refinements of the criteria.
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Preparatory Observations
Leader: Klaus G. Strassmeier
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 143/200
PSM WP 131 330
04/2016 — 12/2023
Institution: AIP (Germany)
Key Personnel: K. G. Strassmeier; T. Granzer (AIP); J. Weingrill (AIP); G. Bihain (AIP); S. A. Barnes (AIP); N.N.
Objectives:
Carry out a stellar-variability survey of the PLATO long–pointing fields
Tasks:
1.
Mate Zeiss BMK telescope with 10k-CCD system
2.
Adapt STELLA Control System SCS for the robotisation of the telescope
3.
Performance review of all hard- and software in Potsdam
4.
Adapt STELLA data-reduction pipeline for C-filter system and prepare positioning-input files
5.
Adapt building and infrastructure in Tenerife
6.
Deploy telescope and instrument from Potsdam/Germany to Tenerife/Spain
7.
Reintegrate telescope and instrument and commission both
8.
Performance review
9.
Start survey of initial northern PLATO field
10.
Maintain hard- and software on site and monitor data quality
11.
Manage and organize IT issues of data transfer and database (mass storage, community pre-access,
safety etc.)
12.
Optional: move telescope to a southern site and repeat the survey for the southern long-pointing field.
13.
Rebuild sites and ship telescope and instrument back to Germany (tbd).
Input:
Need to know the exact location of the field as soon as possible
Dependencies:
Survey starts first in the northern hemisphere.
Output:
A time-series of 200 CCD pointings of the full 2,300-sqrd PLATO FOV per every clear night with a pixel
resolution of 2.5”. Usage of all possible ≈1,300 hours per observing season would result in a total of ≈32,000
CCDs frames or ≈9TB of data per observing season.
Deliverables:
1.
Provide seasonal-long light curves of all targets between 8th-17th magnitude within the long-pointing
PLATO fields. Determine all eclipsing binaries in the field and extract a variability flag for all accessible stars on
the basis of their long-term brightness rms. Aim for at least n≈100 visits (maximum 160) per CCD field (i.e. per
star) in one ground-based observing season with a time resolution of one day. Expected photometric precision
ranges are from ≈1mmag for V<10thmag, 2-3mmag for 10-11mag, ≈5mmag for 11-12.5mag, up to ≈10mmag for
12.5-13.5mag. Faint limit is ≈16.5mag at ≈50mmag. It will also enable the determination of precise photometric
periods, in particular stellar rotation periods, and the expected degree of spot activity.
2.
Determine the target contamination down to 2.5ʺ″ for every PLATO pixel on the sky (pixel size of 15ʺ″).
Aim for a magnitude difference of 5 mag in V, i.e. contaminating targets down to V≈18mag from stacked images.
In principle, the CCD frames also allow an astrometric calibration.
3.
Cross correlate targets with 2MASS JH magnitudes if available and construct J,H vs. “C”-filter band
diagrams (basically R+I band). According to, e.g. Bilir et al. (2006a, AN 327, 72; 2006b, AN 327, 693; 2008,
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 144/200
MNRAS 384, 1178) it will allow a statistical separation of dwarfs from giants and a crude separation of early-type
from late-type stars.
Milestones:
2016-17: Preparation of site infrastructure and deployment of telescope to Tenerife
2019: Start of survey of northern long-pointing PLATO field
2021: Start of survey of southern long-pointing PLATO field
Risks:
Northern observing site has been chosen and legal processes started (no risks). Technical risks during transport
and assembly. Southern site has not been chosen yet, therefore optional at the moment.
PSM WPDs
DEVELOPMENT
K2 Data
Leader: Magali Deleuil
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 145/200
PSM WP 131 400
Development phase
04/2016 — 12/2023
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: M. Deleuil; I. Boisse (LAM); F. Bouchy (IAP/OHP); A. Vigan (LAM); D. Pollacco (Warwick)
Objectives:
1.
Develop a catalogue for individual stars and planets observed with K2 mission
2.
Validate the catalogue
Tasks:
1.
Gather K2 mission results from NASA archives and publications
2.
Create a catalogue gathering information on possible planetary companion, identified eclipsing binaries
and variable stars
3.
Check compliance of the catalogue with the specifications
4.
Validate the catalogue
5.
Validate regular updates
Input:
Catalogues from NASA archives and/or scientific publications
Dependencies:
WP 131 000
Output:
Catalogue of stars observed by K2 with their characteristics (time and duration of the K2 observations, related
publications, etc.) and the relevant parameters: presence of a companion, nature of the companion, variability of
the source, rotation period, etc. to be provided to WP 131 000
Deliverables:
Catalogue of stars observed by K2 with their characteristics (time and duration of the K2 observations, related
publication, etc.) and the relevant parameters: presence of a companion, nature of the companion, variability of
the source, rotation period, etc.
Milestones:
L-24m: delivery of criteria for the target selection for the first field. Refined criteria of the first PLATO field
Launch: delivery of criteria for target selection for the second field. Continuing refinements of the criteria.
Risks:
No risks identified
PSM WPDs
DEVELOPMENT
TESS Data
Leader: Magali Deleuil
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 146/200
PSM WP 131 500
Development phase
04/2016 — 12/2023
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: M. Deleuil; I. Boisse (LAM); F. Bouchy (IAP/OHP); A. Vigan (LAM); D. Pollacco (Warwick)
Objectives:
1.
Develop a catalogue for individual stars and planets observed with TESS mission
2.
Validate the catalogue
Tasks:
1.
Gather TESS mission results from NASA archives and publications
2.
Create a catalogue gathering information on possible planetary companion, identified eclipsing binaries
and variable stars
3.
Check compliance of the catalogue with the specifications
4.
Validate the catalogue
5.
Validate regular updates
Input:
Catalogues from NASA archives and/or scientific publications
Dependencies:
WP 131 000
Output:
Catalogue of stars observed by TESS with their characteristics (time and duration of the TESS observations,
related publications if any, etc.) and the relevant parameters: presence of a companion, nature of the companion,
variability of the source, rotation period etc. to be provided to WP 131 000
Deliverables:
Catalogue of stars observed by TESS with their characteristics (time and duration of the TESS observations,
related publication, etc.) and the relevant parameters: presence of a companion, nature of the companion,
variability of the source, rotation period etc.
Milestones:
L-24m: delivery of criteria for the target selection for the first field. Refined criteria of the first PLATO field
Launch: delivery of criteria for target selection for the second field. Continuing refinements of the criteria.
Risks:
No risks identified
PSM WPDs
DEVELOPMENT
Contaminant Analysis
Leader: Ulrich Kolb
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 147/200
PSM WP 131 600
04/2016 — 12/2023
Institution: The Open University (UK)
Key Personnel: U. Kolb
Objectives:
1.
Explore contaminant information of likely target sources in Gaia catalogue and other pertinent catalogues
2.
Create and calibrate a contaminant modeller that estimates contaminant effects for any source
Tasks:
Coordination and management of the package.
Input:
WP 131 000
Dependencies:
Output of WP 131 000; WP 132 000
Output:
Assessment of contaminant information in Gaia and other pertinent catalogues.
Deliverables:
Contaminant estimator tool
Milestones:
As specified in sub WPs
Risks:
Gaia catalogue analysis and contaminant projection relies on the soundness of Gaia data. Other catalogues are
incomplete for fainter contaminants.
PSM WPDs
DEVELOPMENT
Contaminant Modelling Tool
Leader: Ulrich Kolb
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 148/200
PSM WP 131 610
04/2016 — 12/2023
Institution: The Open University (UK)
Key Personnel: U. Kolb; P. Rowden (OU); A. Santerne (Porto)
Objectives:
1.
Explore contaminant information of likely target sources in Gaia catalogue and other pertinent catalogues
2.
Create and calibrate a contaminant modeller that estimates contaminant effects for any source
Tasks:
1.
Create contaminant modeller, using existing models (such as GUMS) where appropriate, to obtain a
generic synthetic Galactic blend/false positive model
a.
Review existing models and extract useful subroutines
b.
Establish types of false positives to be considered
c.
Establish Galactic population model for each type
d.
Create synthetic PLATO contaminants population
2.
Calibrate contaminant modeller against observed contaminants, in preparation for estimating false
positive probability of individual sources
Input:
WP 131 420 & 430
Dependencies:
WP 132 000
Output:
Theoretical model that underpins the pre-operation determination of false positive probability
Deliverables:
Numerical tool for false positive assessment of a potential target
Milestones:
04/2017: Complete first definition of input for population modelling tool
09/2018: First assembly of population modelling tool
09/2018: Calibration runs completed
09/2019: Refined tool completed
Risks:
Code calibration requires readiness of underlying catalogues
PSM WPDs
DEVELOPMENT
Gaia Analysis of Contaminants
Leader: Nick Walton
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 149/200
PSM WP 131 620
Development phase
04/2016 — 12/2023
Institution: Institute of Astronomy, University of Cambridge (UK)
Key Personnel: N. Walton; S. Hodgkin (IoA)
Objectives:
1.
Study contaminant statistics in Gaia catalogue
2.
Optimize computations of PLATO pixel contamination inferred from Gaia data
Tasks:
1.
Assess stellar motions and variability inferred from Gaia data for contaminating sources
2.
Develop algorithm to optimize calculation of contamination for a PLATO target
Input:
WP 131 120
Dependencies:
WP 131 610
Output:
1.
Optimised algorithm of likely contaminants of PLATO targets
2.
Calibrator data for WP 131 610
Deliverables:
Method for generating PLATO contamination information inferred from Gaia
Milestones:
09/2017: delivery of first calibrator data
04/2018: first definition of algorithms
2022: release of final algorithm (to coincide with Gaia final data release)
Risks:
Relies on soundness of Gaia data
Rev.: 5
PSM WPDs
DEVELOPMENT
Contaminant Analysis From Other Catalogues
Leader: Valerio Nascimbeni
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 150/200
PSM WP 131 630
04/2016 — 12/2023
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni; U. Kolb (OU); S. Hodgkin (IoA); K2 expert; LSST expert
Objectives:
Study contaminant statistics in pertinent catalogues other than Gaia, including K2, TESS and LSST.
Tasks:
1.
Develop procedure for contaminant extraction from respective catalogues
2.
Statistical analysis of contaminant properties
3.
Provide calibrator for contaminant modeller
Input:
WP 132 200, 400 & 500
Dependencies:
WP 132 610, WP 133 000
Output:
1.
Assessment of contaminant information from catalogues other than Gaia
2.
Calibrator data for WP 131 610
Deliverables:
Method for generating PLATO contamination information inferred from catalogues other than Gaia
Milestones:
09/2017: delivery of first calibrator data
04/2018: first definition of algorithms
04/2019: improved algorithms
2023: first assessment of and recommendations from LSST data
Risks:
Depends on success of TESS and timely operational start of LSST
PSM WPDs
DEVELOPMENT
Field and Target Selection
Leader: Ricardo Claudi
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 151/200
PSM WP 132 000
04/2016 — 12/2023
Institution: INAF- Osservatorio Astronomico di Padova (Italy)
Key Personnel: R. Claudi; S. Benatti (INAF-Padova)
Objectives:
Coordinate all the WPs to deliver PLATO field positions, and PLATO targets
Tasks:
1.
Select PLATO fields
2.
Select PLATO targets and deliver PIC to PDC
3.
Estimate completeness/contamination of the selected targets
Input:
WP 131 000, WP 132 000, PDC WP 343 000
Dependencies:
Output of WP 131 000, 132 000
Output:
PLATO fields and PLATO target catalogue
Deliverables:
PIC and PLATO fields
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-18m Results of guest observer call added to the PIC
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Field Selection
Leader: Sergio Ortolani
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 152/200
PSM WP 132 100
Development phase
04/2016 — 12/2023
Institution: Università di Padova (Italy)
Key Personnel: S. Ortolani; G. Piotto (Padova); C. Afonso; V. Nascimbeni (INAF-Padova)
Objectives:
Deliver PLATO fields
Tasks:
1.
2.
3.
4.
Analyse results from WP 131 000
Perform stellar crowding experiments
Analyse Galactic models
Select PLATO fields
Input:
WP 131 000
Dependencies:
Output of WP 131 000
Output:
PLATO fields position
Deliverables:
PLATO fields
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-18m Results of guest observer call added to the PIC
Risks:
Acceptable risk
PSM WPDs
DEVELOPMENT
Target Selection and Prioritisation
Leader: Valentina Granata
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 153/200
PSM WP 132 200
04/2016 — 12/2023
Institution: Università di Padova (Italy)
Key Personnel: V. Granata; S. Ortolani (Padova); G. Piotto (Padova); V. Nascimbeni (INAF-Padova); 1 postdoc
Objectives:
Deliver all relevant parameters for each target and their prioritisation
Tasks:
1.
Make sure the relevant information is searched for in all possible catalogues
2.
Study of the stellar population in the target volume and of the environment conditions
3.
Coordinate with PDC WP 343 000 for tools and algorithms to implement criteria for target parameters
into PIC
4.
Provide prioritisation criteria and stellar parameters
5.
Coordination of WP 132 410 and WP 132 420
Input:
All catalogues/parameters gathered by WP 132 000, PDC WP 343 000 tools and algorithms
Dependencies:
Output of WP 132 000, PDC WP 343 000, Gaia early release catalogues
Output:
Final criteria for targets/parameters of the PLATO input catalogue
Deliverables:
Final list of criteria for targets/parameters of the PLATO input catalogue
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-18m Results of guest observer call added to the PIC
Risks:
Depends on Gaia output; in case of delay or failure from Gaia mission, the catalogue will rely on available
photometric/astrometric catalogues, including some current ongoing wide field.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 154/200
PLATO Field Contaminants
Leader: Ulrich Kolb
Rev.: 5
Development phase
PSM WP 132 300
04/2016 — 12/2023
Institution: The Open University (UK)
Key Personnel: U. Kolb
Objectives:
1.
To inform field selection by population models of false positives
2.
To supply algorithms for calculating a false positive rate for all targets, on the basis of catalogue data and
supporting theoretical models
Tasks:
Coordination and management of the package.
Input:
Model specifications assembled in WP 131 600
Dependencies:
A close liaison with WP 113 000 and WP 111 000 and relevant sub-WPs is required
Output:
1.
A Galactic population model of sources giving rise to false positive signals, informing field selection
2.
A false positive probability tool for catalogue sources, to generate contaminant information for each
source.
Deliverables:
Code to obtain contaminant assessment on a source-by-source basis
Milestones:
As specified for WP 132 310 & WP 132 320
Risks:
Minimal risks
PSM WPDs
DEVELOPMENT
Single Target Contaminants
Leader: Ulrich Kolb
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 155/200
PSM WP 132 310
Development phase
04/2016 — 12/2023
Institution: The Open University (UK)
Key Personnel: U. Kolb; P. Rowden (OU); 1 postdoc
Objectives:
Conduct a statistical study of the abundance of astrophysical false positives in potential PLATO fields, as a
function of Galactic latitude and longitude, to inform target field selection.
Tasks:
1.
Tailor models from WP 131 600 to PLATO field geometry and differential sensitivity
2.
Study longitude and latitude dependence of overall false positive rate
Input:
Model specifications assembled in WP 131 600
Dependencies:
Output of WP 132 000
Output:
All-sky synthetic false positive population
Deliverables:
Independent assessment of global false positive content of any potential PLATO field
Milestones:
9/2018: Completion of limited population study to inform optimum latitude of first PLATO field
9/2020: Completion of extended population study, to inform selection of further fields
Risks:
None apparent.
PSM WPDs
DEVELOPMENT
False Alarm Probability
Leader: Alexandre Santerne
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 156/200
PSM WP 132 320
04/2016 — 12/2023
Institution: University of Porto (Portugal)
Key Personnel: A. Santerne; U. Kolb (OU)
Objectives:
Optimize the calculation of individual false positive probabilities for a given PLATO target or potential target,
taking into account both observed contaminant properties and theoretical models of the physical nature of
contaminants.
Tasks:
1.
Assimilate catalogue-specific information
2.
Assimilate model information
3.
Adapt PASTIS code to pre-operations mode
Input:
1.
Catalogue information gathered by WP 131 000
2.
Field positions selected by WP 132 000
Dependencies:
Output of WP 131 000 and WP 132 000
Output:
Algorithms for calculating the false positive probability given the source position and its contaminant
environment.
Deliverables:
Code
Milestones:
04/2017: first assembly of code completed
04/2019: first full working version released
2019-23: Further adaptations to coincide with output from WP 131 600
Risks:
None apparent.
PSM WPDs
DEVELOPMENT
Interface to Other PSM WPs and PDC
Leader: Silvano Desidera
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 157/200
PSM WP 133 000
Development phase
04/2016 — 12/2023
Institution: INAF- Osservatorio Astronomico di Padova (Italy)
Key Personnel: S. Desidera
Objectives:
The objective of this WP is to coordinate the activities of the Interface WP
Tasks:
Coordinate WP 133 100, WP 133 200, WP 133 300, WP 133 400, and WP 133 500 work
Input:
Definition Phase documentation
Dependencies:
Output of the WP 133 100, WP 133 200, WP 133 300, WP 133 400, and WP 133 500
Output:
Requirement documents and development phase reports
Deliverables:
Requirement documents
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-24m Validation of the PIC for the first observing field
L-18m Results of guest observer call added to the PIC
Risks:
Acceptable risk
PSM WPDs
DEVELOPMENT
Interface to Other PSM WPs
Leader: Silvano Desidera
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 158/200
PSM WP 133 100
04/2016 — 12/2023
Institution: INAF- Osservatorio Astronomico di Padova (Italy)
Key Personnel: S. Desidera
Objectives:
The objective of this WP is to coordinate the interfaces with the other science WP
Tasks:
Interface of WP 130 000 activities with WP 110 000, WP 120 000, WP 140 000, WP 160 000, and PLATO Endto-End Simulator
Input:
Definition Phase documentation
Dependencies:
Close interaction can be foreseen with WP 110 to 160
Output:
Collection of requirements from WP 110 000, WP 120 000, WP 140 000, and WP 160 000 for target selection
and target parameters to be included in PIC
Deliverables:
Requirement document for target and field selection and target parameters
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-24m Validation of the PIC for the first observing field
L-18m Results of guest observer call added to the PIC
Risks:
Interface problems, efficiency losses
PSM WPDs
DEVELOPMENT
Interface to PDC
Leader: Valentina Granata
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 159/200
PSM WP 133 200
Development phase
04/2016 — 12/2023
Institution: Università di Padova (Italy)
Key Personnel: V. Granata
Objectives:
The interface team will coordinate the exchange of data, information, requirements and progress reports between
the WP 130 team and the PDC (PLATO Data Centre), as formalized in the Interface Requirements Document
(IRD) and Interface Control Document (ICD).
The principal activity will be to coordinate and document the exchanges between the WP 130 and the Input
Catalogue team (IC) and the Ancillary Database Content Management (AD).
Tasks:
1.
Definition and maintenance of IRD and ICD
2.
Gather information and documentation on catalogues format, description, file specification, size and
target selection and characterization from PDC
3.
Transfer information on the criteria for target selection to IC team and provide their feedback to WP 130
4.
Collect and provide criteria to IC team.
5.
Monitor progress, ensuring that schedule requirements are maintained and identifying/ initiating any
change requests that may arise out of the interface requirements
6.
Gather information and documentation on additional data available in the Ancillary Database
7.
Provide feedback to Ancillary Database team
Input:
From WP 132 000: Criteria for field selection information
From WP 350 000: Information and documentation on additional catalogues
Dependencies:
Input from WP 132 000, WP 340 000, WP 350 000
Output:
To WP 340 000: criteria for target selection information
To WP 340 000: information and requirements for Ancillary Database catalogues
Deliverables:
Interface Requirements Document (IRD) and Interface Control Document (ICD)
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-24m Validation of the PIC for the first observing field
L-18m Results of guest observer call added to the PIC
Risks:
Minimal risk
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 160/200
Interface Gaia-PLATO
Leader: Nicholas Walton
Rev.: 5
PSM WP 133 300
Development phase
04/2016 — 12/2023
Institution: Institute of Astronomy, University of Cambridge (UK)
Key Personnel: N. Walton; D. W. Evans (IoA)
Objectives:
A range of information is required from Gaia in refining the input catalogue for PLATO. In particular the initial
positional, flux and early astrometric information from Gaia will be important in aiding the characterisation of the
PLATO target samples. This WP will define the required interfaces required by PLATO with Gaia and define the
implementation phase activities within the PSM to ensure these relevant programmatic interfaces. The interface
requirements activities will be complete at the time of the PLATO PSM/PDC CDR in 2016.
Tasks:
1.
2.
3.
4.
Evaluate time line for delivery of Gaia data products to PLATO
Determine availability of Gaia data products (via communication with Gaia DPAC)
Evaluate required technical interfaces to Gaia data
Report on requirements
Input:
1.
WP 133 300 Definition Phase report
2.
PLATO SIRD and SIP
Dependencies:
PSM WP 131 100 – science requirements interface
Output:
Cycle progress reports and assurance reports to the PSM
Deliverables:
07/2018: Gaia-PLATO (input catalogue) interface requirements document
07/2019: Revised Gaia-PLATO (input catalogue) interface requirements document
Milestones:
03/2019: Define parameters and specifications for the preliminary catalogue of the first PLATO field
12/2019: Final catalogue for the first PLATO field
06/2020: Proposal for selection of the second PLATO field
03/2021: Refined catalogue of the first PLATO field
09/2023: Preliminary catalogues for the second PLATO fields
Launch: Refined final catalogue for first PLATO field, preliminary catalogues for the other PLATO fields
Risks:
This WP will comply with the PSM RMP.
PSM WPDs
DEVELOPMENT
Interface to PLATO CCD Image Simulator
Leader: Luca Borsato
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 161/200
PSM WP 133 400
04/2016 — 12/2023
Institution: Università di Padova (Italy)
Key Personnel: L. Borsato
Objectives:
The objective of this WP is to coordinate the interfaces with the PLATO End-to-End Simulator, and the other
WPs for the Target/Field selection.
Tasks:
Interface of WP 130 000 activities with PLATO End-to-End Simulator
Input:
Collection of requirements from WPs for target/field selection WP 130 000
Dependencies:
PLATO End-to-End Simulator (development, updates, and bug-fixes of the Simulator and time to compute the
simulations)
Output:
Results of the simulations from the PLATO End-to-End Simulator
Deliverables:
Fits images and simulated light curves for defined fields
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-24m Validation of the PIC for the first observing field
L-18m Results of guest observer call added to the PIC
Risks:
Interface problems, misinterpretation of the simulations and expected photometric quality
PSM WPDs
DEVELOPMENT
Interface to TOU
Leader: Riccardo U. Claudi
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 162/200
PSM WP 133 500
Development phase
04/2016 — 12/2023
Institution: INAF-Osservatorio Astronomico Padova (Italy)
Key Personnel: R. Claudi
Objectives:
1.
Gather information on the optical performance of PLATO
2.
Gather information on the operation mode of PLATO
3.
Trading off between PIC and Telescope Optical Units Requirements
Tasks:
Manage the Interface with the TOU Design Work packages
Input:
Telescope Optical Unit (TOU)
Dependencies:
Performances of TOU
Output:
Limits for target parameters
Requirements on TOU performances
Deliverables:
Interface Requirement Document (IRD) and Interface Control Document (ICD) with TOU Reports
Milestones:
01/2018: Define parameters and specifications for the preliminary catalogue of the first PLATO field
06/2019: Proposal of the LD and S&S positions
L-36m Criteria for the identification, selection and prioritization of the selected first observed field targets and
corresponding parameters
L-30m Criteria for target contaminants selection and characterization; false alarm probability for each target
L-24m Validation of the PIC for the first observing field
L-18m Results of guest observer call added to the PIC
Risks:
Interface problems, misinterpretation of expected photometric quality
PSM WPDs
DEVELOPMENT
Coordination of PLATO Follow-Up Observations
Leader: Stéphane Udry
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 163/200
PSM WP 140 000
04/2016 — 12/2023
Institution: Geneva University (Switzerland)
Key Personnel: S. Udry (Geneva); NN (Geneva)
Objectives:
Coordination of the preparation for the follow-up observations of PLATO transit candidates.
Tasks:
1.
Management of WP 14X: Control that WP activities are progressing according to planning; facilitate
horizontal transfer of information; etc.
2.
Identify and list all the existing and in-development facilities that will be in operation during the PLATO
mission.
3.
If existing (and in development) facilities are not sufficient, define the strategy to build new facilities
or/and upgrade existing ones.
4.
Organize general meetings on FU-related activities
Input:
1.
Activities of FU WP’s and sub-WP’s
2.
PLATO-related activities at observing facilities (instrument and software developments)
3.
Dependencies:
WP 100 000, WP 110 000, WP 120 000, WP 130 000, WP 14X XXX, WP 160 000.
Output:
1.
Follow-Up coordination
2.
List of observing facilities
3.
FU observing strategy
Deliverables:
Report synthesizing the FU-activities for mid-term and end of development phase
Milestones:
03/2019: Preliminary agreement with major available observing facilities
03/2021: Specification of final observer interface
Risks:
Non-development or closing of foreseen observing facilities
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 164/200
Strategy and Operation Preparation
Leader: Don Pollacco
Rev.: 5
Development phase
PSM WP 141 000
04/2016 — 12/2023
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco
Objectives:
To coordinate work packages looking at the efficient spread of PLATO candidates to the available follow-up
facilities. To define aids to be used by observers for efficient assessment of observation quality. Recent results
have shown that the smallest planets will need almost real time follow-up observations for efficient detection.
This work package interfaces with the PDC through the ancillary database.
Tasks:
1.
Establish observation descriptors in terms of candidate priority and characteristics.
2.
Assess important criteria dictating which photometric or spectroscopic facility is used for a particular
object e.g., screening via AO imaging or other photometric technique, or reconnaissance spectroscopy (if not
unavailable).
3.
Establish PLATO observational aids to be used as facilities for assessing observation quality and its
flagging.
4.
Liaise with the PDC to establish which observatory products are to be returned to the Ancillary
Database.
5.
Liaise with representative from the Ancillary Database to establish observation descriptors as required
within the PDC and data format.
Input:
1.
Scientific literature
2.
PLATO Red book and current PLATO performance estimation.
3.
Current follow-up facility performance descriptions and software manuals.
Dependencies:
Exchange of information and coordination with all WP 140 packages along with the Ancillary Database WP 312
500. Report to WP 140 000 and also Science coordinator.
Output:
A methodology describing how and which PLATO candidates will be distributed to which follow-up facility both
for ground based photometric and spectroscopic observations. Return of observatory processed data to the
Ancillary Database for inclusion into the PDC.
Deliverables:
1.
Reports on algorithms and specifications.
2.
Reports on tests performed as algorithms and their implementation evolve.
Milestones:
01/2018: Establish critical parameters required for PLATO candidate follow-up.
01/2020: Establish methodology and algorithm required for efficient distribution of candidates through facilities.
01/2022: Produce dummy data sets and flush through process and return data sets to dummy Ancillary
Database. Evaluate performance and instigate and start updates.
12/2023: Final version of methodology.
Risks:
The efficient utilization of our follow-up facilities will be key to the success of PLATO. In efficient target
distribution will result in time wasted on astrophysical mimics or low quality targets. Poor matching will result in
low efficiency of planet confirmation and, in the worse case, low return in planet detection.
PSM WPDs
DEVELOPMENT
Target Distribution Requirements
Leader: Ignasi Ribas
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 165/200
PSM WP 141 100
04/2016 — 12/2023
Institution: Insititut de Ciències de l’Espai (Spain)
Key Personnel: I. Ribas; J. Colomé (ICE); F. Vilardell (ICE); E. Herrero (ICE); M. Perger (ICE); A. García-Piquer
(ICE); J. Guàrdia (ICE); J. Sanz (ICE)
Objectives:
To use information gained from CoRoT, Kepler and leading ground based surveys such as SuperWASP to
define the optimum follow-up strategy for PLATO candidates. To determine information needed to be passed to
follow-up facilities for successful and efficient observations.
Tasks:
1.
To examine the planet confirmation strategies of the leading surveys and determine an optimum
procedure for PLATO candidates.
2.
To define what information (and observation characterization aids) need to be made available to a given
follow-up facility.
Input:
1.
Scientific literature
2.
PLATO Red book and current PLATO performance estimation.
3.
Current follow-up facility performance descriptions and software manuals.
4.
Dependencies:
Exchange of information and coordination with all WP 140 packages. Link to WP 115 100 to ensure best-facility
and follow-up procedure given likely astrophysical noise conditions.
Output:
A methodology describing how the various PLATO candidates will be selected and then distributed to the bestsuited follow-up facility (based on likely planet/host star parameters) for both efficient ground-based photometric
and spectroscopic observations.
Deliverables:
Reports on current distribution techniques and PLATO specific requirements. Report on facility requirements.
Report and software defining the methodology of object distribution. Report on observation assessment tools.
Milestones:
12/2017: Evaluation of current follow-up strategies.
12/2018: Initial evaluation of follow-up facility requirements and observational aids.
07/2020: Preliminary outline of follow-up distribution strategy.
12/2023: Final report on activities, including results of tests of the final target distribution methodology.
Risks:
The efficient utilization of our follow-up facilities will be key to the success of PLATO. Use of the wrong
methodology will result in inefficient use of follow-up facility time and hence a low planet yield.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 166/200
Aids for Optimizing Photometric and Spectroscopic
Measurements
Leader: Josep Colomé
Rev.: 5
PSM WP 141 200
Development phase
04/2016 — 12/2023
Institution: Insititut de Ciències de l’Espai (Spain)
Key Personnel: J. Colomé; I. Ribas (ICE); F. Vilardell (ICE); E. Herrero (ICE); M. Perger (ICE); A. García-Piquer
(ICE); J. Guàrdia (ICE); J. Sanz (ICE)
Objectives:
To develop and install observation aids to optimize the development of real time selection of targets specifically
for any particular facility. These will be orientated towards improving the observation efficiency and will include
routines to help with ephemeris and orbit fitting etc.
Tasks:
1.
Review currently used tools at likely sites and determine their capabilities user friendliness and suitability
for PLATO candidates.
2.
Establish list of requirements given PLATO requirements.
3.
Compile the PLATO Observational Aid suite of tools and distribute around sites.
4.
Compile documentation to allow efficient maintenance of above.
Input:
1.
Scientific literature and instrumentation manuals.
2.
PLATO Red book and current PLATO performance estimation.
3.
Current follow-up facility performance descriptions and software manuals.
Dependencies:
Exchange of information and coordination with all WP 140 packages along with the Ancillary Database WP 312
500.
Output:
PLATO Observation Aids that will enable the observer to make best use of telescope time and assess the quality
of the data obtained.
Deliverables:
1.
Report on freely available observational orientated aids.
2.
Report with specification on useful aids that need to be developed.
3.
Observationally orientated aids development and deployment.
Milestones:
07/2017: Evaluation of freely available observational aids
07/2018: Establish specifications for needed aids
07/2020: First generation PLATO Observational Aids deployed and testing begins
07/2021: Review of testing period
07/2022: Second generation PLATO Observational Aids deployed and testing begins
Risks:
The efficient utilization of our follow-up facilities will be key to the success of PLATO. In efficient target
distribution will result in time wasted on astrophysical mimics or low quality targets. Poor matching will result in
low efficiency of planet confirmation and, in the worse case, low return in planet detection.
PSM WPDs
DEVELOPMENT
Information Transfer
Leader: Francesc Vilardell
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 167/200
PSM WP 141 300
Development phase
04/2016 — 12/2023
Institution: Insititut de Ciències de l’Espai (Spain)
Key Personnel: F. Vilardell; I. Ribas (ICE); J. Colomé (ICE); E. Herrero (ICE); M. Perger (ICE); A. García-Piquer
(ICE); J. Guàrdia (ICE); J. Sanz (ICE)
Objectives:
Deliver aids to provide follow-up observers with target information in a graphic web page. This is similar to the
“Variable Star Investigator” format used by the WASP consortium and others. This will also be the main method
for passing descriptive information (e.g. meteorological information) back to the Ancillary Database and PDC.
Tasks:
1.
Evaluate the WWW observer interfaces made available to us by third parties (e.g. WASP).
2.
Determine specifications for PLATO Observer interface, and assess needs of specific facilities and types
of observations.
3.
Develop and trial PLATO Observer Interface.
4.
Liaise with representative from the Ancillary Database to establish observation descriptors as required
within the PDC and data format.
Input:
1.
Scientific literature
2.
Available literature on third party Observer Interfaces.
3.
PLATO Red book and current PLATO performance estimation.
4.
Current follow-up facility performance descriptions and software manuals.
Dependencies:
Exchange of information and coordination with all WP 140 packages along with the Ancillary Database WP 312
500.
Output:
PLATO Observer Interface and Ancillary Database feedback tool
Deliverables:
Reports detailing the specification for the PLATO Observer Interface tailored to each facility or type of follow-up
observation. Methodology for feedback of descriptive information to the Ancillary Database.
Milestones:
07/2017: Preliminary evaluation of third party Observer interface software available to us.
12/2017: Specifications for generic PLATO Observer Interface
07/2018: Specifications for specific follow-up facilities as required.
07/2020: First release of PLATO Observer Interface.
Yearly (or as required) updates after this date
Risks:
The efficient utilization of our follow-up facilities will be key to the success of PLATO. Inefficient target
distribution will result in telescope time being wasted on astrophysical mimics or low quality targets. Poor
matching will result in low efficiency of planet confirmation and, in the worse case, low return in planet detection.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 168/200
Planet Yield Determination
Leader: Yann Alibert
Rev.: 5
Development phase
PSM WP 141 400
04/2016 — 12/2023
Institution: University of Bern (Switzerland)
Key Personnel: Y. Alibert; S. Udry (Geneva); F. Bouchy (LAM); X. Dumusque (CfA)
Objectives:
Estimate of the PLATO global follow effort
Tasks:
1.
Estimate the number of transiting planets detected by PLATO and for which a RV characterization is
possible.
2.
Estimate the corresponding observation time required for the planet characterization, for each category
of telescope
3.
Estimate the rate of false positives
4.
Estimate the corresponding observation time required to discard the false positives
Input:
Selected stellar field
Dependencies:
WP 140 000
Output:
1.
Yield of planets per bin of mass and separation
2.
Percentage of false positives of the different types
Deliverables:
Reports
Milestones:
07/2018: First global follow-up effort estimation
03/2020: Preliminary agreement with major available observing facilities
Risks:
Acceptable risk
PSM WPDs
DEVELOPMENT
Radial Velocity Follow-up
Leader: François Bouchy
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 169/200
PSM WP 142 000
04/2016 — 12/2023
Institution: LAM (France)
Key Personnel: F. Bouchy; C. Moutou (LAM); S. Udry (Geneva); E. W. Guenther (TLS); D. Ségransan
(Geneva); T. Forveille (IPAG); F. Pepe (Geneva)
Objectives:
Prepare and coordinate the activities of ground-based radial-velocity measurements of PLATO transit
candidates to establish the nature of the transit events and to characterize the mass of the companion of the
core science program from earth-like planets to brown-dwarfs.
Tasks:
1.
Identify and list all the existing and in-development RV facilities that will be in operation during the
PLATO mission (2024-2030) with a significant amount of available time, competent teams and efficient data
reduction systems. Facilities will be ranked not as function of the telescope diameter but as a function of the RV
uncertainties effectively obtained for a solar-type star of magnitude mv=11 in a 1h exposure. The uncertainty
should include photon-noise and instrumental systematic error.
2.
Prepare a list of benchmark observations to qualify the participating facilities.
3.
If existing and in-development facilities are estimated to be not sufficient, define the strategy to build new
facilities or/and upgrade existing ones.
Input:
Estimation numbers of transiting candidates + estimated rate of false-positives
Dependencies:
WP 140 000, WP 141 000, WP 146 000, WP 113 000
Output:
List of RV facilities ranked as function of their precision, available time and their associated teams
Deliverables:
Reports about the radial velocity facilities and performances.
Milestones:
07/2017: Identification of RV facilities
07/2018: Definition of benchmark observations
03/2019: Preliminary agreement with major available observing facilities
07/2019: Organization of the benchmark observations
Risks:
Radial Velocity Follow-up will be key to the success of PLATO. An insufficient capacity in RV Follow-up
observations will result in a low return in planet detection.
PSM WPDs
DEVELOPMENT
Radial Velocity Computation and Global Analysis
Tools
Leader: Damien Ségransan
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 170/200
PSM WP 142 100
04/2016 — 12/2023
Institution: Geneva University (Switzerland)
Key Personnel: D. Ségransan; F. Bouchy (LAM); C. Lovis (Geneva)
Objectives:
Prepare and coordinate the activities of radial-velocity computations and global analysis tools to search for and
characterize planetary systems
Tasks:
1.
Definition of requirements for the deliverables of RV facilities
2.
Definition of requirements for tools to compute the RV of stars of different types with different physical
properties (e.g. high rotation), and in various environments (e.g. binaries).
3.
Definition of requirements to calibrate the RV offset between different RV instruments.
4.
Define tools allowing the combination of data of different nature (astrometric, photometric, spectroscopic)
to optimize RV follow-up observations.
Input:
PLATO Stellar population properties
Dependencies:
WP 140 000, WP 142 000, WP 146 000
Output:
Software tools and web pages services
Deliverables:
Reports on algorithms and specification. Reports on tests performed.
Milestones:
07/2017: Specifications and requirements for tools and algorithms
07/2019: Test and scientific validation of these tools.
Risks:
Acceptable risks
PSM WPDs
DEVELOPMENT
First Radial Velocity Screening [≥ 10 m/s]
Leader: Eike W. Guenther
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 171/200
PSM WP 142 200
04/2016 — 12/2023
Institution: Thüringer Landessternwarte Tautenburg (Germany)
Key Personnel: E. W. Guenther; C. Moutou (LAM); G. Hébrard (IAP/OHP); A. Hatzes (TLS); A. Niedzielski
(NCU); L. Buchhave (NBI); C. Aerts (Leuven)
Objectives:
Prepare and coordinate the activities of the first radial velocity screening at low precision and the mass
determination of hot-Jupiters and brown-dwarfs for PLATO with RV facilities like ES@TLS (2m), FIES@NOT
(2.5m), HERMES@Mercator (1.2m), and CAFE@CalarAlto (2.2m)
Tasks:
1.
Define an efficient screening strategy using low-precision RV measurements (10-30 m/s) in order to
optimize the RV-follow-up observations.
2.
Define the appropriate criteria to stop, or to continue RV-measurements.
3.
Define and develop tools to estimate from these first low-precision RV-measurements to the expected
RV-accuracy that will be obtained with instruments of higher precision in order to optimize the follow-up strategy.
4.
Define the optimum strategy in order to distinguish giant planets from brown dwarfs and binaries with the
minimum number of RV-measurements.
Input:
1.
Estimated numbers of candidates.
2.
Estimated rate of false-positives.
3.
List of available telescope facilities that are available for the project.
Dependencies:
WP 140 000, WP 141 000, WP 146 000
Output:
1.
Inventory of low-precision spectrographs available for the project.
2.
Expected amount of observing-time required to carry out the observations.
3.
Expected amount of time and manpower to carry out the observations and reduce the data.
4.
Estimate number of candidates that require further RV-observations at higher precision.
Deliverables:
Reports and algorithms to carry out screening. Estimate of time required after a candidate has been identified
until screening is finished.
Milestones:
07/2017: Specifications and requirements for tools and algorithms
07/2019: Test and scientific validation of these tools.
Risks:
Small number of telescope facilities to carry out the follow-up observations will limit the number of detected
planets.
PSM WPDs
DEVELOPMENT
Intermediate Precision Radial Velocity Follow-Up
[3-5 m/s]
Leader: Claire Moutou
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 172/200
PSM WP 142 300
04/2016 — 12/2023
Institution: LAM (France)
Key Personnel: C. Moutou; R. Diaz (Geneva); A. Santerne (CAUP); G. Hébrard (IAP/OHP); D. Naef (Geneva);
X. Bonfils (IPAG); A. Niedzielski (NCU)
Objectives:
Prepare and coordinate the activities of ground-based radial-velocity measurements of PLATO transit
candidates using spectrographs of intermediate precision (3 – 5 m/s) like SOPHIE@OHP (1.9m),
CORALIE@Euler (1.2m), FEROS@ESO (2.2m), and Neo-Narval@TBL (2m)
Tasks:
1.
Specify the needs of follow-up observations with intermediate precision (3-5 m/s): number of targets,
strategy, time estimate, analysis
2.
Assess the status, performance and availability of telescope and instruments in this range of precision
3.
Contribute to collect radial velocity data of moderate-precision instruments (pre-launch) on PLATO
potential targets
Input:
1.
Yields for transiting candidates and false positives
2.
The properties of their host stars (mass, luminosity, activity, spectral type, etc.)
Dependencies:
WP 140 000, WP 141 000, WP 142000, WP 146 000
Output:
Inventory of moderate precision spectrographs, and their expected performance in term of identification of false
positives/planet confirmation and mass measurement
Deliverables:
Progress reports
Milestones:
07/2017: Specifications and requirements for tools and algorithms
07/2019: Test and scientific validation of these tools.
Risks:
Small number of telescope facilities to carry out the follow-up observations will limit the number of detected
planets.
PSM WPDs
DEVELOPMENT
Very High-Precision RV Measurements [≤ 1 m/s]
Leader: Francesco Pepe
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 173/200
PSM WP 142 400
04/2016 — 12/2023
Institution: Geneva University (Switzerland)
Key Personnel: F. Pepe; S. Udry (Geneva); C. Lovis (Geneva); D. Ségransan (Geneva); F. Bouchy (LAM); A.
Hatzes (TLS); G. Piotto (Padova); A. Sozzetti (INAF-Torino); R. Claudi (INAF-OPAD); N. Santos (Porto)
Objectives:
Prepare and coordinate the activities of high-precision radial-velocity measurements of PLATO candidates
around quiet stars to measure the mass of Earth and super-Earth like planets with spectrographs like
HARPS@ESO (3.6m), HARPS-N@TNG (3.6m), and ESPRESSO@ESO (8.2m)
Tasks:
1.
Define the best strategy of very high-precision RV follow-up (≤1 m/s) to measure the mass of Earth and
super-Earths out to the habitable zone of quiet stars.
2.
Define the appropriate criteria to stop, or to continue very high-precision RV-measurements.
3.
Specify the needs for follow-up observations with very high precision
4.
Assess the status, performance and availability of telescope and instruments
5.
Define and develop tools to select most appropriate quiet stars with a transiting companion in the
domain of telluric planet
Input:
1.
Estimate number of candidates (and their characteristics) and false positives.
2.
The properties of their host stars (mass, luminosity, activity, spectral type, etc.)
3.
List of facilities available for the project.
Dependencies:
WP 140 000, WP 141 000, WP 146 000
Output:
1.
Inventory of very high-precision spectrographs, and their expected performance for RV measurements,
and expected contribution from these spectrographs in term of mass measurement.
2.
Expected amount of observing-time required to carry out the observations.
3.
Expected amount of time and manpower to carry out the observations and to reduce the data.
Deliverables:
Reports for mid-term and final reviews
Milestones:
07/2017: Specifications and requirements for tools and algorithms
07/2019: Test and scientific validation of these tools.
Risks:
Small number of telescope facilities to carry out the follow-up observations will limit the number of detected
planets.
PSM WPDs
DEVELOPMENT
Infrared Radial-Velocity Measurements
Leader: Thierry Forveille
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 174/200
PSM WP 142 500
04/2016 — 12/2023
Institution: IPAG (France)
Key Personnel: T. Forveille; P. Figueira (Porto); X. Bonfils (IPAG); X. Delfosse (IPAG); N. Santos (Porto);
J. Amado (IAA); E. Guenther (TLS)
P.
Objectives:
Prepare and coordinate the activities of ground-based radial-velocity measurements of PLATO transit
candidates using infra-red spectrographs like SPIROU@CFHT (3.6m), CARMENES@CalarAlto (3.5m),
CRIRES@ESO (8.2m), NAHUAL@GTC (10m), and GIANO@TNG (3.6m)
Tasks:
1.
Establish which type of stars are best observed with IR spectrograph: M dwarfs (brighter in the IR),
active stars (which systematic error are lower in the IR), …
2.
Assess the status, performance and availability of telescope and instruments
3.
Define the best use and strategy of IR spectrograph for the RV follow-up screening and mass
determination
Input:
1.
Yields for transiting candidates and false positives
2.
The properties of their host stars (mass, luminosity, activity, spectral type, etc.)
Dependencies:
WP 140 000, WP 141 000, WP 146 000, WP 113 000
Output:
1.
Inventory of IR spectrograph, and their expected performance for RV measurements
2.
Expected contribution from IR spectrograph in term of identification of false positives/planet confirmation
and mass measurement
Deliverables:
Reports (for mid-term and final reviews)
Milestones:
03/2019: Preliminary agreement with major available observing facilities
07/2021: Specify the Expected contribution from IR spectrograph in term of identification of false positives/planet
confirmation
Risks:
Existing infrared spectrographs are not optimized for RVs (but have already reached a precision of few m/s on
short time scales). Numerous infrared spectrographs optimized for radial velocity are in development. Their
precision will be assessed during development phase.
PSM WPDs
DEVELOPMENT
Time Critical Photometry
Leader: Roi Alonso
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 175/200
PSM WP 143 000
04/2016 — 12/2023
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: R. Alonso; H.J. Deeg (IAC); E. Pallé (IAC); M. Montalto (CAUP)
Objectives:
Identify and assess false positive transit detections in PLATO photometry caused by stellar blends. Define
suitable optical and NIR photometric time critical follow-up strategies. Estimate required resources.
Tasks:
1.
Coordinate generation of simulations to predict the expected numbers of false positives in different
blend scenarios in the PLATO fields. Evaluate/calibrate with Kepler, K2 and TESS results.
2.
Estimate expected demand of observational resources.
3.
Assemble and organize group of observers.
4.
Organize and execute benchmark observations to assess the performances of each facility.
5.
Define efficient and effective strategies for time critical follow-up photometry.
Input:
1.
2.
3.
4.
5.
6.
Scientific literature
PLATO Red Book
Information on facilities registered to PLATO follow-up
Updated PLATO characteristics and performance estimation
Images and lightcurves from the PLATO End-to-End Simulator
TESS and CHEOPS results
Dependencies: Information exchange with other WPs, especially WP 140 000, WP 141 000, WP 141300,
WP141400, WP 142 000, WP 144 000, WP 146 000, WP 115 200, WP 112 000, WP 114 000.
Output:
A quantitative understanding of the expected frequency of blending in PLATO photometry, detailed strategies of
how to identify and assess false positive transit detections using time critical photometric techniques,
identification of suitable observatories and facilities for follow-up observations
Deliverables:
Reports on simulations of predicted frequency of false positive detections, optimal observing strategies and of
suitable ground-based facilities. Prevision of demand of time critical photometry observations. Guidelines for
observing, data analysis, and documentation of follow-up observations.
Milestones:
31/12/2017: Evaluation of ground based photometry follow-up facilities available to PLATO
31/12/2018: Quantitative estimates of expected frequency and spatial scales of blending
31/12/2019: Establish detailed photometric methodologies, and reduction software
31/12/2020: Establish follow-up observing teams
31/12/2021: On-sky end-to-end evaluation of these techniques
31/12/2023: Final version of methodology
Risks: Miss estimation of estimated required resources (e.g. due to inaccurate inputs)
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 176/200
Photometry Specific Tools
Leader: H. J. Deeg
Rev.: 5
Development phase
PSM WP 143 100
04/2016 — 12/2023
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: H. J. Deeg
Objectives:
Provide the different teams contributing to time critical photometric follow-up with guidelines and software tools
for a uniform analysis and reporting of data.
Tasks:
1.
Perform an exhaustive comparison of existing photometric methods (aperture photometry, PSF
photometry, image subtraction, etc.)
2.
Select the photometric methods best suited for PLATO follow-up
3.
Implement, document, and distribute the tools to contributing observing facilities.
4.
Receive feedback from contributing observing facilities.
Input:
1.
Existing algorithms, methods from follow-up of prior photometric space missions
2.
New developments from scientific literature
3.
Information on facilities registered to PLATO Follow-up
Dependencies: Information exchange with other WPs, especially WP 143 000, WP 143 200, WP 143 300, WP
143 400
Output:
Comparison of different photometric methods. Implementation of selected ones with adaptations specific to
PLATO follow-up.
Deliverables:
Documentation and algorithms for photometric follow-up observations. Reports on different photometric
methods.
Milestones:
31/12/2019: Implement selected photometric methodologies, and reduction software
31/12/2021: On-sky end-to-end evaluation of these techniques
31/12/2023: Final version of methodology and algorithms
Risks: None; ample experience from prior follow-up programs (for CoRoT, Kepler) is present
PSM WPDs
DEVELOPMENT
Photometric Follow-Up with Small Telescopes
Leader: G. Wuchterl
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 177/200
PSM WP 143 200
04/2016 — 12/2023
Institution: Thüringer Landessternwarte Tautenburg (Germany)
Key Personnel: G. Wuchterl
Objectives:
Coordinate the follow-up activities that are feasible with small (diameter < 0.9 m) telescopes.
Tasks:
1.
Link with registered facilities to PLATO Follow-Up
2.
Coordinate execution of benchmark observations requested and defined in WP 143 000.
3.
Assure required precision is met.
Input:
•
Benchmark observations details from WP 143 000
•
Information of facilities registered to PLATO Follow-up
•
Dependencies:
Information exchange with other WPs, especially WP 143 000, WP 143 100, WP 143 300, WP 143 400
Output:
Results of benchmark observations.
Deliverables:
Results of benchmark observations. Documentation for interested participants.
Milestones:
12/2019: List of interested participants and observing facilities.
12/2021: On-sky end-to-end benchmark observations
Risks:
None
PSM WPDs
DEVELOPMENT
Standard Photometric Observations
Leader: R. Alonso
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 178/200
PSM WP 143 300
04/2016 — 12/2023
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: R. Alonso
Objectives:
Coordinate the time critical photometric follow-up activities that are feasible with moderate (0.9 m < diameter <=
2.0 m) telescopes.
Tasks:
1.
Link with registered facilities to PLATO Follow-Up
2.
Coordinate execution of benchmark observations requested and defined in WP 143 000.
3.
Assure required precision is met.
Input:
•
Benchmark observations details from WP 143 000
•
Information of facilities registered to PLATO Follow-up
•
Dependencies:
Information exchange with other WPs, especially WP 143 000, WP 143 100, WP 143 200, WP 143 400
Output:
Results of benchmark observations.
Deliverables:
Results of benchmark observations. Documentation for interested participants.
Milestones:
12/2021: On-sky end-to-end benchmark observations
Risks:
None
PSM WPDs
DEVELOPMENT
Very High Precision Photometric Observations
Leader: E. Pallé
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 179/200
PSM WP 143 400
04/2016 — 12/2023
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: E. Pallé
Objectives:
Lead and coordinate the time critical photometric follow-up activities requiring big (mirror diameter > 2.0 m)
ground-based and/or space telescopes.
Tasks:
1.
Link with registered facilities for PLATO follow-up
2.
Coordinate execution of benchmark observations requested and defined in WP 143 000.
3.
Conduct test to assure that required precision is met.
Input:
•
Benchmark observations details from WP 143 000
•
Information of facilities registered to PLATO Follow-up
•
Dependencies:
Information exchange with other WPs, especially WP 143 000, WP 143 100, WP 143 200, WP 143 300
Output:
Results of benchmark observations.
Deliverables:
Results of benchmark observations. Documentation for interested participants.
Milestones:
12/2021: On-sky end-to-end benchmark observations
Risks:
None
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 180/200
High Angular Resolution Imaging
Leader: Silvano Desidera
Rev.: 5
Development phase
PSM WP 144 000
04/2016 — 12/2023
Institution: INAF – Osservatorio Astronomico di Padova (Italy)
Key Personnel: S. Desidera; V. Nascimbeni (Padova); M. Janson (Stockholm); D. Mesa (INAF-Padova);
Bonavita (Edinburgh); A. Vigan (LAM); V. D’Orazi (INAF-Padova)
M.
Objectives:
To coordinate and lead work packages which will identify and assess false positive transit detections in PLATO
photometry caused by stellar blends. Define optical and infrared imaging follow-up strategies on a range of
spatial scales from seeing-limited to high-quality AO imaging to space-based imaging, to contribute to the
elimination of false positives. Define and assess AO imaging strategies for potential characterization of planetary
systems detected by PLATO.
Tasks:
1.
Coordinate WP 144 100; WP 144 200; WP 144 300, WP 144 400, and WP 144 500, and control that WP
activities are progressing according to planning; facilitate horizontal transfer of information; etc.
2.
Exchange of information with other follow-up WPs for coordination of the follow-up strategy
3.
Ensure that existing literature and archive data (WP 130000) have been properly taken into account
4.
Quantification of amounts of observing time required for imaging follow-up for PLATO core science
5.
Collect list of participating facilities/teams to the various components of high-angular resolution follow-up
observations
Input:
Activities of sub-WPs, results of simulations of contaminants and false alarms (WP 131 6xx)
Dependencies:
Other follow-up WPs, WP 350 000, WP 130 000, WP 131 6xx, WP 132 3xx
Output:
Follow-up strategy
Data to WP 350 000
Third light dilution (for transit parameter determination) to WP 132 3xx
Deliverables:
Report on imaging follow-up plan and list of suitable observing facilities
Milestones:
L-3yr: Evaluation of ground based imaging follow-up facilities available to PLATO
L-3yr: Determination of the amount of observing time required for imaging follow-up
L-2yr: Establish follow-up science teams
L-1yr: Preliminary imaging follow-up plan
L: Final version of imaging follow-up plan
Risks:
If false positive transit detections due to diluted eclipses, or even due to diluted transits of giant planets, are not
identified with a high level of completeness, then undetected false positives will lead to ambiguous small-planet
detections
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
st
Date: September 1 2015
Page: 181/200
Imaging Analysis Tools
Leader: Arthur Vigan
Rev.: 5
Development phase
PSM WP 144 100
04/2016 — 12/2023
Institution: LAM (France)
Key Personnel: A. Vigan; V. Nascimbeni (Padova); R. Alonso (IAC); M. Janson (Stockholm); D. Mesa (INAFPadova)
Objectives:
Prepare and coordinate the activities related to the definition and development of the high-angular resolution
imaging analysis tools, to ensure best quality and homogeneity in the analysis of follow-up images from the
participating facilities
Tasks:
1.
2.
3.
4.
Definition of requirement of tools to be exploited in the analysis of high-angular resolution observations
Collection of available tools in the literature and in WP144000 team.
Critical evaluation of tools adopted by participating facilities/teams (e.g. instrument pipelines)
Development of dedicated tools optimized for PLATO follow-up requirements
Input:
1.
Available analysis procedures from the literature and participating facilities
2.
List of facilities participating to the imaging follow-up
Dependencies:
Coordination with WP 143 000 for the analysis of seeing-limited observations. List of facilities from WP 144 000
Output:
Analysis procedures and tools
Deliverables:
Reports on analysis procedures to be adopted.
Milestones:
L-3yr: Definition of requirements for high-angular resolution imaging analysis tools
L-1yr: Implementation of procedures/tools
L-6m: Validation of the proposed procedures/tools
L: Final version of methodology
Risks:
Non-optimal use of allocated imaging follow-up observing time
PSM WPDs
DEVELOPMENT
Single-Epoch Seeing-Limited Imaging
Leader: V. Nascimbeni
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 182/200
PSM WP 144 200
04/2016 — 12/2023
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni; R. Alonso (IAC); G. Piotto (Padova); S. Desidera (INAF-Padova)
Objectives:
Define optical and infrared imaging follow-up strategies for single-epoch seeing-limited observations (wide field,
individual objects, guide images from spectroscopic observations), to contribute to the elimination of false
positives.
Tasks:
1.
Evaluate the scientific literature, with special reference to the experience gained by the CoRoT, Kepler,
K2, CHEOPS, and TESS projects in this context
2.
Coordinate definition of efficient and effective strategies of follow-up single-epoch seeing-limited imaging
observations
3.
Coordinate identification of observatories suited to making these follow-up observations
4.
Coordinate with WP 142 000 and WP 145 000 the use of guide images from spectroscopic observations
Input:
1.
Scientific literature
2.
PLATO documentation
3.
Manuals and web sites of potential ground-based follow-up facilities
Dependencies:
Interface with WP 142 000 - 145 000 about the use of guide images from spectroscopic observations, synergy
with WP 143 000 about the use of seeing-limited images.
Output:
Reports and documents
Deliverables:
Document with specification of information to be provided to the Ancillary Database (WP 350 000)
Milestones:
L-3yr: Evaluation of ground based imaging follow-up facilities available to PLATO
L-2yr: Establish detailed imaging methodologies, and analysis software
L-2yr: Establish follow-up science teams
L-1yr: On-sky end-to-end evaluation of these techniques
L: Final version of methodology
Risks:
If false positive transit detections due to diluted eclipses, or even due to diluted transits of giant planets, are not
identified with a high level of completeness, then undetected false positives will lead to ambiguous small-planet
detections
PSM WPDs
DEVELOPMENT
Reconnaissance High Resolution Imaging
Leader: Markus Janson
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 183/200
PSM WP 144 300
04/2016 — 12/2023
Institution: University of Stockholm (Sweden)
Key Personnel: M. Janson; A. Brandeker (Stockholm); S. Desidera (INAF-Padova); D. Barrado (CAB, INTACSIC); H. Bouy (CAB, INTA-CSIC); N. Huélamo (CAB, INTA-CSIC); M. Morales-Calderon (CAB, INTA-CSIC); J.
Lillo-Box (CAB, INTA-CSIC)
\
Objectives:
Define
optical and infrared imaging follow-up strategies for high angular resolution reconnaissance observations
\
(lucky imaging, speckle imaging, AO on medium-class telescopes), to contribute to the elimination of false
positives. Define and assess AO imaging strategies for potential characterization of planetary systems detected
by PLATO.
Tasks:
1.
Evaluate the scientific literature, with special reference to the experience gained by the CoRoT, Kepler,
Kepler2, CHEOPS and TESS projects in this context
2.
Coordinate definition of efficient and effective strategies of follow-up reconnaissance imaging observing
3.
Coordinate identification of observatories suited to making these follow-up observations
Input:
1.
Scientific literature
2.
PLATO documentation
3.
Manuals and web sites of potential ground-based follow-up facilities
Dependencies:
Information exchange with other WPs
Output:
Reports and documents
Deliverables:
Document with specification of information to be provided to the Ancillary Database (WP 350 000)
Milestones:
L-3yr: Evaluation of follow-up facilities available to PLATO for high angular resolution reconnaissance
observations (lucky imaging, speckle imaging, AO on medium-class telescopes)
L-2yr: Establish detailed methodologies and analysis software
L-2yr: Establish follow-up science teams
L-1yr: On-sky end-to-end evaluation of these techniques
L: Final version of methodology
Risks:
If false positive transit detections due to diluted eclipses, or even due to diluted transits of giant planets, are not
identified with a high level of completeness, then undetected false positives will lead to ambiguous small-planet
detections
PSM WPDs
DEVELOPMENT
High Contrast Imaging
Leader: Dino Mesa
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 184/200
PSM WP 144 400
04/2016 — 12/2023
Institution: INAF - Osservatorio Astronomico di Padova (Italy)
Key Personnel: D. Mesa; S. Desidera (INAF-Padova); M. Janson (Stockholm); A. Vigan (LAM); M. Bonavita
(Edinburgh); R. Claudi (INAF-OAPD); V. D’Orazi (INAF-Padova)
Objectives:
Define optical and infrared follow-up strategies for high-quality AO imaging, sparse-aperture masking, and
space-based imaging, to contribute to the elimination of false positives. Define and assess AO imaging
strategies for potential characterization of planetary systems detected by PLATO.
Tasks:
1.
Evaluate the scientific literature, with special reference to the experience gained by the CoRoT, Kepler,
Kepler2, CHEOPS and TESS projects in this context
2.
Definition of efficient and effective strategies of follow-up AO imaging observing
3.
Identification of observatories suited to making these follow-up observations
Input:
1.
Scientific literature
2.
PLATO documentation
3.
Manuals and web sites of potential ground-based follow-up facilities
Dependencies:
Information exchange with other WPs
Output:
Reports and documents
Deliverables:
Document with specification of information to be provided to the Ancillary Database (WP 350 000)
Milestones:
L-3yr: Evaluation of ground based high-contrast imaging follow-up facilities available to PLATO (AO on 8m class
telescopes and beyond)
L-2yr: Establish detailed methodologies for high-contrast imaging, and analysis software
L-2yr: Establish follow-up science teams
L-1yr: On-sky end-to-end evaluation of these techniques
L: Final version of methodology
Risks:
If false positive transit detections due to diluted eclipses, or even due to diluted transits of giant planets, are not
identified with a high level of completeness, then undetected false positives will lead to ambiguous small-planet
detections
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
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Date: September 1 2015
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Candidate Classification
Leader: M. Bonavita
Rev.: 5
Development phase
PSM WP 144 500
04/2016 — 12/2023
Institution: Edinburgh (UK)
Key Personnel: M. Bonavita; A. Vigan (LAM); S. Desidera (INAF-Padova); M. Janson (Stockholm); R. Claudi
(INAF-OAPD); V. D’Orazi (INAF-Padova)
Objectives:
Identify the nature of the candidates close to PLATO targets (physical companions vs. field objects) down to
substellar objects for a better understanding of the environment of PLATO targets and the architecture of the
planetary systems discovered with PLATO
Tasks:
1.
Develop procedure to identify the nature of candidates close to PLATO targets found by WP 144 000
(physical companions vs. field objects)
2.
Develop procedure for characterization of stellar companions of PLATO targets
3.
Develop procedure for characterization of substellar companions in wide orbits around PLATO targets
Input:
Candidates close to PLATO targets from WPs 144 100, 144 200, 144 300, 144 400
Results of simulations with contamination/companions probabilities (WP 130 000)
Dependencies:
Interface with WP 130 000, WP 350 000, and with other PLATO follow-up WPs
Output:
Reports and documents
Deliverables:
Document with definition of the adopted procedures for the classification of objects close to PLATO targets and
the characterization of the companions.
Data to be provided to the Ancillary Database (WP 350 000)
Milestones:
L-2yr: Establish procedures for candidate classification and characterization
L-2yr: Establish dedicated team
L: Final version of methodology
Risks:
Incomplete evaluation of the environment of planets identified by PLATO in terms of stellar companions and
substellar companions in wide orbits
PSM WPDs
DEVELOPMENT
Additional Exoplanet Follow-Up
Leader: Xavier Bonfils
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 186/200
PSM WP 145 000
04/2016 — 12/2023
Institution: IPAG (France)
Key Personnel: X. Bonfils; R. Alonso (IAC); F. Bouchy (LAM); D. Ehrenreich (Geneva); G. Hébrard
(IAP/OHP); A. Lecavelier (IAP); S. Udry (Geneva); H. Rauer (DLR); F. Selsis (Bordeaux, CNRS); A. Bonomo
(INAF-Torino); P. Wheatley (Warwick); I. Snellen (Leiden); A. Santerne (CAUP); A. Triaud (Toronto);
I.
Skillen (IAC); G. Piotto (Padova)
Objectives:
Prepare and coordinate follow-up observations to increase the scientific return on the mission. The
characterization of PLATO planets takes place after their planetary nature has been established (from PLATO
light curves plus ground based photometry and RV follow-up). It aims at measuring their physical properties
and their chemical composition. It will also measure complementary orbital parameters, such as orbit
obliquities, and possibly detect additional planets.
Tasks:
1.
Identify and list existing and in-development methods that can provide additional characterization for
the planetary systems detected.
2.
Match methods with existing and foreseen facilities. Estimate the demand on telescope time. Define
a strategy to rank targets regarding planet characterization.
3.
Define strategy for observations and for rapid response soon after PLATO planets are detected.
Define recommendation requirements for the community.
Input:
1.
Estimation of the planet population expected to be detected by PLATO, with their basic physical
properties (mass, radius, period)
2.
The physical properties of their host stars (distance, mass, radius, luminosity, etc.)
Dependencies:
WP 110 000 (WP 113 000, WP 115 000, WP 116 000), WP 130 000, WP 141 000, WP 142 000;
Information exchange with WP 114 000
Output:
1.
List of facilities
2.
Physical properties: planetary structure, T-P profile of atmospheres, orbital obliquities …
3.
Chemical composition: abundance of atomic and molecular species
Deliverables:
Doc: Method inventory.
Doc: Requirements for the recommendations issued to the community for the observations
Milestones:
03/2017: Preliminary agreement with major available observing facilities
12/2019: Define observing strategy regarding planet characterization
Risks:
Expected performances may vary according to available facilities and method developments. But risks are
also spread on various methods and a wide range of facilities. Also, this WP comes only other WPs
completed the detection of PLATO planets, and therefore as a second priority.
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
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Date: September 1 2015
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Transmission Spectroscopy Follow-up
Leader: David Ehrenreich
Rev.: 5
Development phase
PSM WP 145 100
04/2016 — 12/2023
Institution: University of Geneva (Switzerland)
Key Personnel: D. Ehrenreich; X. Bonfils (IPAG); A. Lecavelier (IAP); H. Rauer (DLR); F. Selsis (Bordeaux,
CNRS); P. Wheatley (Warwick)
Objectives:
This WP aims at optimising the scientific return of PLATO by assessing the atmospheric characterisation
potential of discovered planets with transmission spectroscopy. For each planet in the PLATO sample, it will
guide observers to the more adapted ground- or space-based facilities that could be used to detect
atmospheric markers relevant in both different wavelength domains and different spectral resolutions.
Tasks:
1.
Establish which atmospheric signatures are the more relevant markers used to characterise PLATO
planets with transmission spectroscopy in different spectral domains (task divided in two sub-WPs).
2.
Survey the existing and foreseen facilities contemporary to PLATO (JWST, WSO-UV, VLT, GTC, EELT, etc.) suitable for transmission spectroscopy observations in different domains (X, UV, visible, IR, and
beyond) and estimate how much telescope time would be needed to detect the identified atmospheric markers
(task divided in 6 sub-WPs, organized by spectral domains and instruments).
Input:
1.
"Bulk" properties of PLATO planets from adapted population synthesis models.
2.
Atmospheric properties of PLATO planets from atmospheric models.
3. Properties of the PLATO stellar sample (spectral types, fluxes, spectra, limb darkening coefficients).
Dependencies:
WP 113 000, WP 116 400, WP 116 500, WP 122 300, WP 123 000, WP 131 000, WP 140 000, WP 146 000.
Output:
1.
List of available facilities
2.
Atmospheric signatures which are relevant markers used to characterise PLATO planets with
transmission spectroscopy
Deliverables:
Report synthesizing the characterization potential for the instruments considered.
Milestones:
03/2017: Preliminary agreement with major available observing facilities
12/2019: Define observing strategy
Risks:
Expected performances may vary according to available facilities and method developments. But risks are also
spread on various methods and a wide range of facilities. Also, this WP comes only after other WPs completed
the detection of PLATO planets, and therefore as a second priority.
PSM WPDs
DEVELOPMENT
Secondary Eclipse and Phase-Variation
Spectroscopy
Leader: Roi Alonso
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 188/200
PSM WP 145 200
04/2016 — 12/2023
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: R. Alonso; A. Bonomo (INAF-Torino); D. Ehrenreich (Geneva); M. Gillon (Liège); I. Snellen
(Leiden)
Objectives:
Prepare and coordinate the activities of secondary eclipse and phase-variation studies on PLATO discovered
planets. Extending the wavelength detection of the light coming from the planets allows a deeper
understanding of the atmospheric dynamics and composition. For each planet in the PLATO sample, it will
guide observers to the more adapted ground- or space-based facilities.
Tasks:
1.
2.
Define and develop tools to compute the emission and reflective spectra for different types of planets.
Define and develop tools to estimate the strength of occultation and phase signatures for specific
atomic and molecular species for different types of planets
3.
Determine the degree of characterization achievable for different types of planets. Compare the
advantages of occultation and phase-variation methods
4.
Make the inventory of existing and foreseen facilities that are contemporary to PLATO and suitable for
both occultation and phase-variation spectroscopy observations.
5.
Estimate the amount of telescope time required for the characterization of PLATO planets. Define a
merit function or a strategy to prioritize the targets.
6.
Define requirements to coordinate the target repartition with the community
Input:
1.
2.
Simulated planet population expected for PLATO (mass, radius, orbital period)
The physical properties of their host stars (distance, mass, radius, luminosity, etc.)
Dependencies:
WP 113 000, WP 116 400, WP 116 500, WP 122 300, WP 123 000, WP 131 000, WP 140 000, WP 146 000.
Information exchange with WP 114 xxx
Output:
1.
List of facilities.
2.
Expected measurable physical properties of the PLATO planets. (Tables & plots).
3.
Strategy to prioritize the targets.
Deliverables:
Reports for mid-term and final reviews.
Milestones:
03/2017: Preliminary agreement with major available observing facilities
07/2019: Definition of observing strategy
Risks:
Expected performances may vary according to available facilities and method developments. But risks are also
spread on various methods and a wide range of facilities. Also, this WP comes only after other WPs completed
the detection of PLATO planets, and therefore as a second priority.
PSM WPDs
DEVELOPMENT
Developing Techniques for Atmosphere
Characterization
Leader: Xavier Bonfils
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 189/200
PSM WP 145 300
04/2016 — 12/2023
Institution: IPAG (France)
Key Personnel: X. Bonfils
Objectives:
Watch new technical developments of potential interest for the characterization of PLATO planets. Many
techniques to characterize planets have not yet reached maturity or are not yet sensitive enough for
exoplanetary science, but might be for PLATO planets.
Tasks:
1.
Watch the technical developments of high-angular resolution techniques for the characterization of
PLATO planets (closure phase interferometry, aperture masking, adaptive optics, nulling…)
2.
Watch the technical developments of precise astrometry (VLT/Gravity, ESA/THEIA, etc.) for possible
addition to GAIA data.
3.
Watch for yet different techniques
Input:
Literature
Dependencies:
WP 145 XXX
Output:
Optimum technical approach for planet characterization
Deliverables:
Report
Milestones:
07/2017: Overview on technical developments of interest
12/2019: Final report
Risks:
Acceptable risk
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
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Date: September 1 2015
Page: 190/200
Rossiter-McLaughlin Observations
Leader: Guillaume Hébrard
Rev.: 5
Development phase
PSM WP 145 400
04/2016 — 12/2023
Institution: IAP/OHP (France)
Key Personnel: G. Hébrard; F. Bouchy (LAM); A. Collier Cameron (St Andrews); M. Gillon (Liège);
Lecavelier (IAP); A. Santerne (CAUP); A. Triaud (Toronto)
A.
Objectives:
Prepare and coordinate the activities of radial-velocity measurements of the Rossiter-McLaughlin effect
Tasks:
1.
Define and develop tools to compute the Rossiter-McLaughlin (RM) effect, in classical way and
tomographic way.
2.
Assess which planetary candidates may benefit from RM measurements to establish their planetary
nature. Define in which configuration the RM amplitude is larger than the Keplerian amplitude.
3.
Evaluate the need to account for RM when transmission spectroscopy is performed at high spectral
resolution.
4.
Prepare for the organization and coordination of the observations of the RM curves for the PLATO
transiting planet candidates
Input:
1.
Estimation of the planet population detected by PLATO, with their basic physical properties (mass and
radius)
2.
3.
The physical properties of their host stars, in particular their project rotational velocity v*sini
Dependencies:
WP 142 XXX, WP 145 100, WP 114 XXX
Output:
Estimation of the needed ground-based telescopes facilities and observing time
Deliverables:
1.
Algorithms to model the Rossiter-McLaughlin effect
2.
Tools to fit data to the model
Milestones:
07/2017: Specifications and requirements for tools and algorithms
07/2019: Test and scientific validation of these tools.
Risks:
This WP comes only after other WPs completed the detection of PLATO planets, and therefore as a second
priority with acceptable risks
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
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Date: September 1 2015
Page: 191/200
Additional Long Term Follow-Up
(RV and Transit Timing)
Leader: François Bouchy
Rev.: 5
Development phase
PSM WP 145 500
04/2016 — 12/2023
Institution: LAM (France)
Key Personnel: F. Bouchy; X. Bonfils (IPAG); S. Udry (Geneva); I. Skillen (IAC); G. Piotto (Padova)
Objectives:
Prepare and coordinate the activities of long-term radial velocity and transit timing follow-up for the search for
additional planets in the planetary systems found by PLATO. Evaluate the benefits of long-term radial velocity
follow-up for long-period planets unseen in the PLATO light curves. Evaluate the benefits of long-term groundbased photometric follow-up for transit timing variation of planets found by PLATO.
Tasks:
1.
Assess the benefit of additional radial velocities (RVs) and transit timing (TTs) to detect more planets
and how these complementary detections would compare with the population of planets detected by PLATO
2.
Evaluate the need of complementary RVs and TTs to refine the orbital elements after the planets have
been established
3.
Evaluate the observational effort (with WP 143 000 and WP 142 000)
Input:
1.
Estimation of the planet population detected by PLATO, with their basic physical properties (mass,
radius, period)
2.
The physical properties of their host stars
Dependencies:
WP 140 000, WP 143 000, WP 142 000, WP 112 600, WP 112 420, WP 112 520
Output:
Estimation of the needed ground-based telescopes facilities and observing time
Deliverables:
Assessment and evaluation reports
Milestones:
03/2017: Mid-term review
12/2019: Final review
Risks:
Same as RV follow-up (WP 142 XXX) and ground-based photometric follow-up (WP 143 XXX)
PSM WPDs
DEVELOPMENT
Spectroscopy
Leader: Artie P. Hatzes
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 192/200
PSM WP 146 000
Development phase
04/2016 — 12/2023
Institution: Thüringer Landessternwarte Tautenburg (Germany)
Key Personnel: A. P. Hatzes; L. Buchhave (NBI); I. Boisse (LAM); C. Lovis (Geneva); N. Santos (Porto);
W. Guenther (TLS), P. Petit (OMP); S. Sousa (CAUP); D. Gandolfi (ZAH)
E.
Objectives:
st
Coordination of sub-work packages related to the 1 order spectroscopic analysis of PLATO Objects of Interest
(POI). To define this, this package will provide a rapid first estimation of stellar parameters, which can be used to
screen out unsuitable stars (e.g. giant stars). Activity indicators will be defined and used to estimate the influence
of stellar noise on the radial velocity determination and to plan observing strategies.
Tasks:
Coordinate the work of sub-WPs, and ensure that tasks are completed, and milestones met.
Input:
1.
Define activity indicators to be estimated from spectra. Develop strategies to improve the RV
measurements in the visible using spectra of active stars (WP 144 100).
st
2.
Define tools for the 1 order estimate (on site) of the spectral type from spectral observations obtained
during the follow-up (e.g. removal of giant stars from the priority list).
Dependencies:
WP 140 000, WP 141 000, WP 142 000, WP 142 200, WP 142 300, WP 142 600. WP 144 100, WP 144 200,
WP 146 000, WP 147 000
Output:
1.
Inventory of low-precision spectrographs available for the project.
2.
Expected amount of observing-time required to carry out the observations.
3.
Expected amount of time and manpower to carry out the observations and reduce the data.
4.
Estimate number of candidates that require further RV-observations at higher precision.
Deliverables:
Reports and algorithms to carry out screening. Estimate of time required after a candidate has been identified
until screening is finished.
Milestones:
12/2016: Scientific specification of tools
12/2017: Tests with synthetic/real data
12/2018: Implementation of scheme
Risks:
Minimal risks in development phase
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
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Date: September 1 2015
Page: 193/200
Activity Indicators and Doppler Information on Active
Stars
Leader: Christophe Lovis
PSM WP 146 100
Development phase
Institution: Geneva University (Switzerland)
Key Personnel: C. Lovis; I. Boisse (LAM), E. W. Guenther (TLS), A. Hatzes (TLS)
Objectives:
To develop strategies to improve the radial velocity (RV) measurement of active stars.
Tasks:
1.
Define activity indicators to be estimated from spectra.
2.
Develop tools for corrections to RV
Input:
Spectra of active stars
Dependencies:
WP 142 300, WP 142 400, WP 142 500, WP 142 600
Output:
Algorithms for correcting radial velocities for activity
Deliverables:
Documents and algorithms
Milestones:
07/2013: Scientific specification of tools
01/2016: Tests with synthetic/real data
11/2018: Implementation of scheme
Risks:
Minimal risks
Rev.: 5
04/2016 — 12/2023
PSM WPDs
DEVELOPMENT
Tools for Spectral Classification
Leader: Lars Buchhave
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 194/200
PSM WP 146 200
04/2016 — 12/2023
Institution: Niels Bohr Institute (Denmark)
Key Personnel: L. Buchhave; A. Hatzes (TLS); E. W. Guenther (TLS); S. Sousa (CAUP)
Objectives:
st
Define Tools for the 1 order estimate (on site) of the spectral type of the star that will be obtained from follow-up
observations.
Tasks:
Specify pipeline for obtaining spectral parameters
Input:
Synthetic and real stellar spectra at various resolutions
Dependencies:
WP 142 300, WP 142 400, WP 142 500, WP 142 600
Output:
Basic Stellar parameters
Deliverables:
Pipeline for efficient spectral typing
Interface for distributing information
Documents and Algorithms
Milestones:
07/2017: Scientific specification of tools
01/2020: Tests with synthetic/real data
11/2022: Implementation of scheme
Risks:
Acceptable risks
PSM WPDs
DEVELOPMENT
Infrared Spectroscopy
Leader: Pedro Figueira
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
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Date: September 1 2015
Page: 195/200
PSM WP 146 300
04/2016 — 12/2023
Institution: University of Porto (Portugal)
Key Personnel: P. Figueira; N. Santos (Porto); E. W. Guenther (TLS); P. Figueira (Porto)
Objectives:
Define Tools for radial velocity measurements in the Infrared
Tasks:
Define activity indicators for the infrared
Input:
1.
Infrared spectra of active stars
2.
Model atmospheres
Dependencies:
WP 142 300, WP 142 400, WP 142 500, WP 142 600
Output:
Specifications of tools and algorithms
Deliverables:
IR diagnostics
Milestones:
07/2017: Scientific specification of tools
01/2020: Tests with synthetic/real data
11/2022: Implementation of scheme
Risks:
Acceptable risks
Rev.: 5
PSM WPDs
DEVELOPMENT
Spectropolarimetric Follow-Up
Leader: Pascal Petit
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 196/200
PSM WP 146 400
04/2016 — 12/2023
Institution: OMP (France)
Key Personnel: P. Petit; T. Böhm (OMP), J. Morin (Göttingen); R. Farès (INAF-Catania); S. Berdyugina
(Freiburg); O. Kochukhov (Uppsala)
Objectives:
Prepare and coordinate the activities of spectropolarimetric follow-up in the planetary systems found by PLATO.
Evaluate the benefits of spectropolarimetry in the filtering of the activity jitter, in the study of star-planet
interaction, and in the detection of light reflected by the planet. Propose the development of visible or NIR
spectropolarimetric facilities required by follow-up of PLATO targets.
Tasks:
1.
Estimate the benefit of spectropolarimetric observations to improve the filtering of activity jitter.
2.
Evaluate the potential of spectropolarimetric observations to study the stellar imprint of the star-planet
interaction (magnetospheric interaction or tidal coupling)
3.
Assess the capabilities of spectropolarimetry in the detection and characterization of polarized light
reflected by the surface of exoplanets.
4.
Identify a sub-sample of PLATO targets on which to concentrate the spectropolarimetric follow-up and, if
needed, propose the development of visible and/or NIR spectropolarimetric facilities to complement available
instruments.
5.
Prepare for the organization and coordination of the observations
Input:
1.
Estimation of the planet population detected by PLATO, with their basic orbital parameters (semi-major
axis, eccentricity) and their physical properties (mass, radius)
2.
The physical properties of their host stars (including rotation and activity)
Dependencies:
WP 140 000, WP 142 600, WP 144 100, WP 144 200, WP 145 000, WP 146 000
Output:
Assessment study on the benefits of spectropolarimetry
Deliverables:
Assessment study
Milestones:
07/2017: Scientific specification of tools
01/2020: Tests with synthetic/real data
11/2022: Implementation of scheme
Risks:
Acceptable risks
PSM WPDs
DEVELOPMENT
Performances Assessment & FU Efficiency
Leader: Stéphane Udry
Institution: Geneva University (Switzerland)
Key Personnel:
Objectives:
Tasks:
Input:
Dependencies:
Output:
Deliverables:
Milestones:
Risks:
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 197/200
PSM WP 147 000
04/2016 — 12/2023
PSM WPDs
DEVELOPMENT
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
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Date: September 1 2015
Page: 198/200
Interfaces to Other PSM WPs and PDC
Leader: Stéphane Udry
Rev.: 5
PSM WP 148 000
Development phase
04/2016 — 12/2023
Institution: Geneva University (Switzerland)
Key Personnel: S. Udry; NN (Geneva)
Objectives:
1.
Coordinate efficient passage of information between the FU activities and other work packages, primarily
in the stellar area and light curve analysis, in order to meet the aims of the mission. We expect that this will be an
iterative process.
2.
Definition of the interfaces to the PDC.
Tasks:
1.
2.
3.
4.
Definition and Maintenance of interface to Exoplanet Science
Definition and Maintenance of interface to Stellar Science
Definition and Maintenance of interface to Complementary Science
Definition and Maintenance of interface to PDC
Input:
Input by other Follow-Up WPs and interfaces within other science tasks and the PDC
Dependencies:
WP 140 000, WP 142 000, WP 143 000, WP 144 000, WP 145 000, WP 117 000, WP 128 000, WP 133 100,
PDC
Output:
Output to other Follow-Up WPs and interfaces within other science tasks and the PDC
Deliverables:
Reports
Milestones:
07/2019: Fist definition and documentation of interface structures
07/2021: Review and update of Interface strategy
Risks:
Acceptable risk
PSM WPDs
DEVELOPMENT
Complementary Science
Leader: Conny Aerts
Development phase
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 199/200
PSM WP 160 000
04/2016 — 12/2023
Institution: University of Leuven (Belgium)
Key Personnel: C. Aerts
Objectives:
1.
The first goal of WP160 is to support the core science of PLATO, which is to detect exoplanets,
understand planets and planetary systems. To achieve this goal the knowledge of age, mass and chemistry of
planet hosting stars has to be improved, which requires substantial updates on models of stellar structure and
evolution. However, to reliably test the new codes for modelling stellar structure and evolution also stars outside
the astrophysical parameter space defined by the core science have to be considered, in particular stars
assembled in clusters and associations. Inadequate approximations of astrophysical processes can best be
identified with stars where such effects dominate, which frequently happen for stars not subject to core science.
Such stars will help to significantly improve our understanding of how stars (planet hosting or not) are working.
The virtue of the large field of view of PLATO allows obtaining highest accuracy photometry for asteroseismic
analyses also for such stars in the context of complementary science. Obviously complementary science will be
relevant well beyond of PLATO and for astrophysics in general. An immediate goal of this WP is to provide input
to the PDC and instrument operation on how to optimize the complementary science capability of PLATO.
2.
The second goal of WP 160 is to provide the community with any PLATO data not related to stellar
science, which may be called the “additional science” aspect of WP 160, and to provide feedback to the
instrument team, PDC and PSM concerning requirements of the community.
Tasks:
1.
Implement, coordinate and supervise the Complementary Science work packages.
2.
Organization of regular teleconferences, and face-to-face meetings of the thematic sub-teams.
3.
Investigate interfaces with the instrument team, PDC and among the PSM tasks and implications for
complementary science.
Input:
1.
Requirements of the complementary science community,
2.
Performance characteristics of the PLATO instrument,
3.
Specifications from the PDC
Dependencies:
All activities of WP 160 000 and sub-WPs are not mission-critical.
Output:
1.
Concepts for improving models, based on complementary science observations and activities
2.
Specifications and data input to PDC,
3.
PR activities
Deliverables:
Document on the potential for PLATO on complementary science and structured in sub-work packages.
Specifications for PDC and instrument operation to include needs for the complementary science programme.
Milestones:
2019: Complementary Science Conference
Risk:
None. The science community has expressed great interest in participating to complementary science as is
demonstrated in the 160 – sub-work packages. Funding will be searched at the level of institutional and national
science funds.
PSM WPDs
DEVELOPMENT
PMC SCIENCE MANAGEMENT
WORK PACKAGE DESCRIPTIONS
DEVELOPMENT
END
Ref.: PLATO-UWA-PSMWPD-001
Issue: 2
Rev.: 5
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Date: September 1 2015
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