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Astronomy Group, Department of Physics, University of Warwick
PMC SCIENCE MANAGEMENT
WORK PACKAGE DESCRIPTIONS
OPERATIONS
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
Other Detection Methods
PSM WP 112 400
22
Eclipse Timing Variations in Eclipsing Binaries
PSM WP 112 420
23
Phase Variations in Pulsating Stars
PSM WP 112 430
24
Multi-Planet Systems
PSM WP 112 500
25
Photometric Detection of Circumbinary Planets
PSM WP 112 510
26
Planets in Trojan Orbits
PSM WP 112 520
27
Exomoons and Binary Planets
PSM WP 112 530
28
Other Multiple Systems
PSM WP 112 540
29
PSM WPDs
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Transit Time Variations and Transit Duration Variations (TTV / TDV)
PSM WP 112 600
30
TTV / TDV Detection
PSM WP 112 610
31
TTV / TDV Modelling
PSM WP 112 620
32
Specification of Procedures to Rank Planet Candidates
PSM WP 113 000
33
Rank Planet Candidates
PSM WP 113 100
34
Specification for Space Based False Positive Identification Through Centroid Analysis
PSM WP 113 200
35
Astrophysical False Positives
PSM WP 113 300
36
Specification of Transit Fitting Tools
PSM WP 114 000
37
Specify Transit Curve Modelling Tools
PSM WP 114 100
38
Specify Tools for Accurate Orbital Period Determination
PSM WP 114 200
39
Rossiter-McLaughlin Modelling Tools
PSM WP 114 300
40
Development of PLATO Data Specific Science
PSM WP 115 000
41
Astrophysical Noise Sources and Their Impact on RV Determination
PSM WP 115 100
42
Improved Planetary System Characterisation
PSM WP 115 200
43
Planet-Star Interactions
PSM WP 115 300
44
Transits of Close-in Objects
PSM WP 115 400
45
Non-Transiting Planets via REBs
PSM WP 115 500
47
Development of PLATO Interpretation Specific Science
PSM WP 116 000
48
Compositions & Formation of Gas & Ice Giants
PSM WP 116 100
49
PSM WPDs
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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
Stability and Resonances in Multi-Planet Systems
PSM WP 116 620
67
PSM WPDs
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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
Limb Darkening
PSM WP 122 400
86
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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
Mode Physics
PSM WP 126 000
104
PSM WPDs
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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
Project Office Assistant
PSM WP 130 100
123
PSM WPDs
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Catalogues Analysis
PSM WP 131 000
124
Gaia Catalogues Analysis
PSM WP 131 100
125
PLATO-Gaia Simulations
PSM WP 131 150
126
Other Large Catalogues Analysis
PSM WP 131 200
127
Photometric and Astrometric Catalogues
PSM WP 131 210
128
M-Dwarfs
PSM WP 131 220
129
M-Dwarfs as Planet Hosts
PSM WP 131 221
130
Stellar Activity
PSM WP 131 230
131
Binary Systems
PSM WP 131 240
132
Known and Candidate Exoplanets
PSM WP 131 260
133
Single Target Additional Data
PSM WP 131 300
134
High Resolution and Deep Imaging
PSM WP 131 310
135
Spectroscopic Data
PSM WP 131 320
136
Preparatory Observations
PSM WP 131 330
137
K2 Data
PSM WP 131 400
138
TESS Data
PSM WP 131 500
139
Contaminant Analysis
PSM WP 131 600
140
Contaminant Analysis From Other Catalogues
PSM WP 131 630
141
Field and Target Selection
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PSM WP 132 000
142
Field Selection
PSM WP 132 100
143
Target Selection and Prioritisation
PSM WP 132 200
144
PLATO Field Contaminants
PSM WP 132 300
145
False Alarm Probability
PSM WP 132 320
146
Interface to Other PSM WPs and PDC
PSM WP 133 000
147
Interface to Other PSM WPs
PSM WP 133 100
148
Interface to PDC
PSM WP 133 200
149
Interface Gaia-PLATO
PSM WP 133 300
150
Interface to PLATO CCD Image Simulator
PSM WP 133 400
151
Interface to TOU
PSM WP 133 500
152
Coordination of PLATO Follow-Up Observations
PSM WP 140 000
153
Strategy and Operation Preparation
PSM WP 141 000
154
Target Distribution Requirements
PSM WP 141 100
155
Aids for Optimizing Photometric and Spectroscopic Measurements
PSM WP 141 200
156
Information Transfer
PSM WP 141 300
157
Planet Yield Determination
PSM WP 141 400
158
Radial Velocity Follow-up
PSM WP 142 000
159
Radial Velocity Computation and Global Analysis Tools
PSM WP 142 100
160
PSM WPDs
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First Radial Velocity Screening [≥ 10 m/s]
PSM WP 142 200
161
Intermediate Precision Radial Velocity Follow-Up [3-5 m/s]
PSM WP 142 300
162
Very High-Precision RV Measurements [≤ 1 m/s]
PSM WP 142 400
163
Infrared Radial-Velocity Measurements
PSM WP 142 500
164
Time Critical Photometry
PSM WP 143 000
165
Photometry Specific Tools
PSM WP 142 100
166
Photometric Follow-Up with Small Telescopes
PSM WP 143 200
167
Standard Photometric Observations
PSM WP 143 300
168
Very High Precision Photometric Observations
PSM WP 143 400
169
High Angular Resolution Imaging
PSM WP 144 000
170
Imaging Analysis Tools
PSM WP 144 100
171
Single-Epoch Seeing-Limited Imaging
PSM WP 144 200
172
Reconnaissance High Resolution Imaging
PSM WP 144 33
173
High Contrast Imaging
PSM WP 144 400
174
Candidate Classification
PSM WP 144 500
175
Additional Exoplanet Follow-Up
PSM WP 145 000
176
Transmission Spectroscopy Follow-Up
PSM WP 145 100
177
Secondary Eclipse and Phase-Variation Spectroscopy
PSM WP 145 200
178
Developing Techniques for Atmosphere Characterization
PSM WP 145 300
179
PSM WPDs
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Rossiter-McLaughlin Observations
PSM WP 145 400
180
Additional Long Term Follow-Up (RV and Transit Timing)
PSM WP 145 500
181
Spectroscopy
PSM WP 146 000
182
Activity Indicators and Doppler Information on Active Stars
PSM WP 146 100
183
Tools for Spectral Classification
PSM WP 146 200
184
Infrared Spectroscopy
PSM WP 146 300
185
Spectropolarimetric Follow-Up
PSM WP 146 400
186
Performance Assessment & FU Efficiency
PSM WP 147 000
187
Interfaces to Other PSM WPs and PDC
PSM WP 148 000
188
Complementary Science
PSM WP 160 000
189
PSM WPDs
OPERATIONS
PSM Coordination
Leader: Don Pollacco
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PSM WP 100 000
Operations phase
01/2024 — 03/2030
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
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:
06/2024: Mission Commissioning Results Review (MCRR)
03/2030: Final reports and improved specifications, updated PDC input catalogue data to PDC
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
OPERATIONS
PSM Project Office
Leader: David J. A. Brown
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PSM WP 101 000
Operations phase
Institution: University of Warwick (UK)
Key Personnel: D. J. A. Brown
Objectives:
Support coordination of the PSM activities.
Tasks:
1. Organization of PSM meetings, teleconferences, etc.
2. Organization of workshop with scientific community
3. Editing of PSM documentation
Input:
Organization request from PSM
Dependencies:
Close interactions foreseen with WP 100 000 and WP 103 000
Output:
1. Organization of meetings, teleconferences, etc.
2. Documentation
Deliverables:
Documentation of the PSM activities
Milestones:
06/2024: Mission Commissioning Results Review (MCRR)
03/2030: Final PSM reports in operation phase
Risks:
Acceptable risk
Ref.: PLATO-UWA-PSMWPD-002
01/2024 — 03/2030
PSM WPDs
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PSM Coordination Team
Leader: Don Pollacco
Rev.: 5
Operations phase
PSM WP 103 000
01/2024 — 03/2030
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 PSM during the operation phases by regular telephone conferences and
meetings
2. Coordinate the update on science specifications and priorities between each PSM task needed to
achieve the science goals
3. Agree on the updates on science specifications to be implemented in the PDC
4. Review the implementation of PSM specifications and input at the PDC
Input:
Activities and reports from PSM task coordinators; documentation of results obtained; report on implementations
in PDC.
Dependencies:
Close interactions foreseen with 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:
06/2024: Mission Commissioning Results Review (MCRR)
Risks:
Late delivery of any of the outputs from the PSM will impact on the work of the PDC
PSM WPDs
OPERATIONS
Exoplanet Science Coordination
Leader: Don Pollacco
Operations phase
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PSM WP 110 000
01/2024 — 03/2030
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco
Objectives:
Coordination of exoplanet work packages for input to PDC.
Tasks:
1.
2.
3.
4.
Liaise with work package coordinators over progress in meeting their objectives
Liaise and respond to the PMC Science Management Coordinator over project requirements
Attend meetings (etc.) as required
Provide updated scientific specification for both algorithm & tools
Input:
1.
2.
3.
4.
PLATO Red Book
Scientific literature
Implemented algorithms by the PDC
Scientific validation and updated specifications of the algorithms by all Exoplanet Science WP’s
Dependencies:
All sub-packages
Output:
1. Successful review of exoplanet work packages and recommendations as input to PDC on a yearly
timescale.
2. Scientific validation and updated specifications of the algorithms
Deliverables:
Reports from each work packages listing recommendations for performance evaluation and improvements
during operations phase.
Milestones:
06/2026: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Late delivery of any of the outputs from these work packages will impact on the work of the PDC.
PSM WPDs
OPERATIONS
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Coordination of Tools for Lightcurve Filtering
Leader: Antonino F. Lanza
Rev.: 5
PSM WP 111 000
Operations phase
01/2024 — 03/2030
Institution: INAF-Catania (Italy)
Key Personnel: A. F. Lanza; S. Aigrain (Oxford); F. Faedi (Warwick)
Objectives:
Coordination of the activities of the work packages from WP 111 100 to WP 111 200.
Tasks:
1. Coordination of the validation work that consists in checking that the procedures to estimate and correct
the impact of residual instrumental noise and intrinsic stellar noise on PLATO light curves are fully
adapted and work properly with real PLATO data;
2. Coordination of the work for deriving new specifications of procedures, algorithms, and theoretical
models, if necessary;
3. Coordination of the work to reduce the impact of the noise on PLATO data of the planet host stars, in
particular for targets that need a specific treatment;
4. Coordination of the theoretical work based on PLATO light curves, seismic data, and follow up
observations to learn more about intrinsic stellar noise. This requires to coordinate the flux of information
towards and from other WPs external to 111 000. This ought to lead to further improvements in the
physical description of stars and to a third generation of stellar models. This will further improve the
accuracy of the derived stellar and planetary characteristics;
5. Organization of working and review meetings gathering the leaders of the WPs
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red book
Current PLATO performance estimation
PLATO light curves
Dependencies:
Input from and output from WPs 112 000, 114 000, and 117 000, PLATO End-to-End Simulator
Output:
Understanding of stellar noise on PLATO photometry and its impact on transit detection and modelling in
collaboration with WP 112 000 and 114 000; 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:
02/2024-12/2024: Improvements of the procedures, algorithms, and theoretical models after testing with real
PLATO data
01/2025-07/2025: Theoretical developments to improve the physical description of stellar noise based on our
improved knowledge of stellar physics and PLATO data
08/2025-03/2030: Delivery of the third generation of validated models and procedures related to the
characterization of the intrinsic noise of the host stars and of the residual instrumental noise
in general.
Meetings with the WP 111 XXX leaders twice a year
Risks:
Acceptable risks of delay for delivering the third generation of methods to account for intrinsic and residual
instrumental noise, scaling relationships, and theoretical models related to them
PSM WPDs
OPERATIONS
Specification of Tools for Lightcurve Filtering
Leader: Suzanne Aigrain
Operations phase
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PSM WP 111 100
01/2024 — 03/2030
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. Test of light curve
filtering algorithms with PLATO-DR1 data, and algorithms optimization. Interaction with the Science
Coordinator and PDC.
Tasks:
1. Continued evaluation of scientific literature
2. Testing algorithms for different types of variability using PLATO-DR1 data
3. Algorithm optimization using PLATO photometry
Input:
1. Scientific literature
2. PLATO Red book
3. PLATO DR1 data
Dependencies:
WP 111 100: Instrumental systematics reduction
Output:
Understanding and removal of stellar noise on PLATO transit photometry
Deliverables:
Report on status and tests of algorithms.
Milestones:
Optimal de-trending algorithms for stellar intrinsic variability. Understanding and mitigation of stellar variability on
levels only accessible with PLATO exceptional photometric precision, observation cadence and length.
09/2024: Assessment of algorithms performance, interaction with the Science Coordinator and PDC
01/2025: Analysis on DR1 data to assess Statistical analysis of transit detection in variability dominated
lightcurves
2027 – 2030: Algorithms maintenance/updating using new knowledge on PLATO data.
Risks:
If variability is not properly understood detectability of small planets will only be possible around the quietest stars,
and more transits will be required for detection.
PSM WPDs
OPERATIONS
Specification of Tools for Detecting and Filtering
Residual Instrumental Noise
Leader: Don Pollacco
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
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PSM WP 111 200
01/2024 — 03/2030
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.
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.
Input:
1.
2.
3.
4.
5.
Scientific literature
PLATO Red book
Current PLATO performance estimation
CoRoT and Kepler datasets
Data release 1 (PLATO)
Dependencies:
Exchange of information and coordination with WP 112 000 and WP 114 000
Output:
Mitigation of the effects of residual instrumental noise on PLATO photometry. For example residuals correlation
with colour, magnitude, time scales of observation. Test for the optimal de-trending technique.
Deliverables:
Optimized tools for the filtering of instrumental noise especially relevant for small planets, circumbinary planets
etc.
Milestones:
Test algorithms for filtering residual noise using PLATO first data release. Work closely with WP 112 000 and
WP 114 000 to improve and characterize PLATO noise pattern:
09/2024: Test algorithms performance with first PLATO-DR1 data.
09/2024: Preliminary reports to the Science Coordinator and PDC
12/2024: Fine tuning/optimization of operation-stage algorithms. Exchange/interaction with WP 112 000 and WP
114 000 for optimization.
2027 – 2030: Algorithms maintenance/updating using new knowledge on PLATO data.
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
OPERATIONS
Specification of Planet Detection Tools
Leader: Juan Cabrera
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
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PSM WP 112 000
01/2024 — 03/2030
Institution: DLR (Germany)
Key Personnel: J. Cabrera; NN (DLR)
Objectives:
Coordination and scientific validation of the work of the sub-work packages related to improvements and
updates of the planet detection 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
updates of the algorithms and requirements based on real PLATO data.
Tasks:
1. Liaise with sub-work package leaders
2. Liaise with Exoplanet coordinator
3. Responsible for reports and updated algorithms from sub-work packages
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book
PLATO performance
PLATO data
Dependencies:
Close interactions foreseen with the WP 111 000; 113 000; 114 000 and sub-WP
Output:
Planet detection updated algorithms and strategies
Deliverables:
Reports from sub-work packages and scientific specifications and updated tools
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
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
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
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Transit Detection Tools
Leader: Juan Cabrera
Rev.: 5
PSM WP 112 100
Operations phase
01/2024 — 03/2030
Institution: DLR (Germany)
Key Personnel: J. Cabrera; NN (DLR); S. Aigrain (Oxford); R. Alonso (IAC); A. Bonomo (INAF-Torino);
L. Carone (Leuven); S. Carpano (ESTEC/ESA); P. Eigmüller (DLR); A. Ofir (Weizmann); M. Pätzold (Köln);
Objectives:
Scientifically review the actual performance of the transit detection algorithms with real data. Make sure that the
expected performances are achieved. Provide updates of the algorithms and specifications.
Tasks:
1. Verify that the algorithms perform as expected with real data from the satellite
2. Suggest improvements based on the results of the analysis of the first pointings
3. Provide updates
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book
PLATO performance
PLATO data
Dependencies:
WP 110 000, WP 116 000, WP 160 000,WP 112 000, PLATO End-to-End Simulator
Output:
Report on the activities done. Provide improvements and updates.
Deliverables:
Report and updates on scientific specifications of algorithms
Milestones:
05/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process. Update
scientific specifications according to prior validation results in phase with PDC implementation cycle.
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
OPERATIONS
Detection of Single and Unusual Transit Events
Leader: Don Pollacco
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 21/190
PSM WP 112 200
01/2024 — 03/2030
Institution: University of Warwick (UK)
Key Personnel: D. Pollacco; F. Faedi (Warwick); J. Cabrera (DLR); A. Erikson (DLR)
Objectives:
Realistic detection probabilities and statistics from single and / or unusual transit events
Test / optimization of de-trending techniques. Analysis of real post-de-trended PLATO light curves is crucial for
individual-transit detection; PLATO’s real levels of residual noise (or variability) could prevent detection of
individual, shallow signals. Test detection of unusual light curve morphology, including transits, using Correlation
Plots. Estimate real detection probability of singular events for a range of observation timespans, expected
orbital periods, and host spectral types, accounting for PLATO’s residual noise level.
Tasks:
1. Assessment of detection algorithms’ performance using PLATO first release data.
2. Algorithm optimization for PLATO photometry.
3. Determination of real statistic of detection reliability for single and / or unusual events.
Input:
1. Scientific literature
2. PLATO Red book
3. PLATO DR1 data
Dependencies:
Exchange of information and coordination with WP 111 000, WP 114 000; PLATO End-to-End Simulator
Output:
Realistic estimate of ability and efficiency of individual transit detection. Optimized solutions for PLATO data
sets.
Deliverables:
Report on status and scientific tests of algorithms.
Milestones:
09/2024: Assessment of algorithm performance and interaction with the Science Coordinator and PDC
06/2025: First statistical analysis using first data release assessing realistic detection limits fro individual transits.
12/2026: Algorithms improvements for individual transit detection on long timescale, Earth analogues,
circumbinary planets.
2027 – 2030: Algorithms maintenance/updating using new knowledge on PLATO data.
Risks:
Ability and efficiency of transit detection will be impaired without an optimized solution for PLATO data sets.
PSM WPDs
OPERATIONS
Other Detection Methods
Leader: Roberto Silvotti
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 22/190
PSM WP 112 400
01/2024 — 03/2030
Institution: INAF-Torino (Italy)
Key Personnel: R. Silvotti; V. Nascimbeni (INAF-Padova); S. Dreizler (Göttingen); S. Schuh (MPSSR);
M. Burleigh (Leicester); Sz. Csizmadia (DLR); F.V. Hessman (Göttingen)
Objectives:
To use PLATO photometry to detect planets 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 within WP 160.
3. Monitoring of data products
4. Tuning of analysis tools.
5. Arrange of follow-up observations.
Input:
1. Light curve processing
2. Stellar parameters
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 within WP 160.
Output:
Confirmed performance of data reduction with feedback for PDC.
Definition of follow-up observations.
Deliverables:
Reports for Science Coordinator and PDC.
Milestones:
06/2025: Performance assessment report
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
2026: Observing plan for follow-up observations
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Low risk
PSM WPDs
OPERATIONS
Eclipse Timing Variations in Eclipsing Binaries
Leader: Stefan Dreizler, Sonja Schuh
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 23/190
PSM WP 112 420
01/2024 — 03/2030
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. Monitoring of data products
2. Tuning of analysis tools.
3. Arrange follow-up observations.
Input:
1. Light curve processing
2. Stellar parameters
Dependencies:
Coordination with WP 112 500 (Multi-planet Systems), WP 367 400 (Circumbinary Planet Parameters).
Output:
1. Confirmed performance of data reduction with feedback for PDC.
2. Fine tuning of algorithms with feedback for PDC.
3. Definition of follow-up observations.
Deliverables:
Reports for Science Coordinator and PDC.
Milestones:
06/2025: Performance assessment report
2026: Observing plan for follow-up observations
Scientific validation of implementation at PDC will be performed as part of the PDC review process. Update
scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Low risk
PSM WPDs
OPERATIONS
Phase Variations in Pulsating Stars
Leader: Roberto Silvotti
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 24/190
PSM WP 112 430
01/2024 — 03/2030
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). Extend PLATO discovery space to relatively
unexplored types of stars.
Tasks:
1. Perform scientific validation of the algorithms assessed during the Development phase, including false
positives.
2. Fine-tuning of algorithms and analysis tools on real Plato data.
3. Monitoring of data products.
4. Define and perform the needed follow-up observations.
5. Write relevant documents/reports.
Input:
1. Light curve processing
2. Stellar parameters
Dependencies:
Coordination with relevant sub-WPs within WP 160.
Output:
1. Confirmed performance of data reduction with feedback for PDC.
2. Fine tuning of algorithms with feedback for PDC.
3. Definition of follow-up observations.
Deliverables:
Reports
Milestones:
06/2025: Performance assessment report
2026: Observing plan for follow-up observations
Scientific validation of implementation at PDC will be performed as part of the PDC review process. Update
scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Low risk
PSM WPDs
OPERATIONS
Multi-Planet Systems
Leader: Silvano Desidera
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 25/190
PSM WP 112 500
Operations phase
01/2024 — 03/2030
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 Development Phase documentation
3. PLATO data
Dependencies:
Coordination with WP 112 400 needed
Output:
1. Reports on detectability of planets in multiple systems with PLATO
2. Detection algorithms for photometric detections of multi-planet systems
Deliverables:
Interim Report, Final Report, Requirements for PDC (detection algorithms)
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Reduced scientific impact of mission.
PSM WPDs
OPERATIONS
Photometric Detection of Circumbinary Planets
Leader: Hans J. Deeg
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 26/190
PSM WP 112 510
01/2024 — 03/2030
Institution: IAC (Spain)
Key Personnel: H.J. Deeg; 1 postdoc
Objectives:
1. Detection/characterization of circumbinary planets, from PLATO photometric data, towards a
maximisation in the numbers and variety of circumbinary planets detected.
2. Optimization of PLATO mission design and of protocols for observing or data-handling towards a
maximum science return of this WP
3. Optimization of existing or newly developed detection methods.
Tasks:
1. Scientific validation of detection algorithms for circumbinary planets (using real PLATO data)
2. Identification of updates on algorithms for photometric identification of circumbinary planets
3. Analysis and scientific interpretation of PLATO data of circumbinary planets (including e.g. dynamical
modelling)
4. Provide inputs for follow-up observations
Input:
1. Scientific literature
2. PLATO Development Phase documentation
3. PLATO data
Dependencies:
1. Specification of PLATO mission parameters,
2. Performance and data format.
Output:
Review of published knowledge. Detection algorithms, Development of theory (as required) to fully exploit
PLATO data in this area
Deliverables:
1. Reports on validation of detection algorithms and upgrades of detection algorithms to be implemented
2. Planetary parameters
3. Input for follow-up observations
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Unknown abundance of circumbinary planets does not permit that their discovery will be guaranteed.
PSM WPDs
OPERATIONS
Planets in Trojan Orbits
Leader: Francesco Marzari
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 27/190
PSM WP 112 520
Operations phase
01/2024 — 03/2030
Institution: University of Padova (Italy)
Key Personnel: F. Marzari; G. Picogna (INAF-Padova)
Objectives:
Detection of Trojan planets (either co-orbital companions of planets or in binary systems) using PLATO.
Tasks:
1. Scientific validation of detection algorithms for planets in Trojan orbits (using real PLATO data)
2. Identification of updates on algorithms for photometric identification of planets in Trojan orbits in their
various configurations
3. Analysis and scientific interpretation of PLATO data of planets in Trojan orbits (including e.g. dynamical
modelling)
4. Provide inputs for follow-up observations
Input:
1. Scientific literature
2. PLATO Development Phase documentation
3. PLATO data
Dependencies:
Detectability of Trojan planets using timing techniques considered in WP 112 400
Output:
Review of published knowledge. Detection algorithms, Development of theory (as required) to fully exploit
PLATO data in this area, Scientific papers
Deliverables:
1. Reports on validation of detection algorithms and upgrades of the specifications of detection algorithms
to be implemented
2. Planetary parameters
3. Input for follow-up observations
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Unknown abundance of Trojan planets does not permit that their discovery will be guaranteed.
PSM WPDs
OPERATIONS
Exomoons and Binary Planets
Leader: Gyula Szabo
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 28/190
PSM WP 112 530
01/2024 — 03/2030
Institution: Konkoly Observatory (Hungary)
Key Personnel: G. Szabo; A. E. Simon (Konkoly)
Objectives:
The main task of this WP in the operations phase is to improve and validate the tools developed in the
development phase that will enable us to identify binary exoplanets and moons orbiting extrasolar planets
directly in the raw photometric data. These algorithms will be applied to all transiting planets and candidates
identified by PLATO.
Tasks:
1. Scientific validation of detection algorithms for exomoons and binary (using real PLATO data)
2. Identification of updates on algorithms for photometric identification of exomoons and binary planets in
their various configurations
3. Analysis and scientific interpretation of PLATO data on exomoons and binary planets (positive
detections, upper limits, including e.g. dynamical modelling)
4. Provide inputs for follow-up observations
Input:
1. Scientific literature
2. PLATO Development Phase documentation
3. PLATO data
Dependencies:
Interface with WP 112 400 for the detection of exomoons using timing
Output:
Review of published knowledge. Detection algorithms, Development of theory (as required) to fully exploit
PLATO data in this area, Scientific papers
Deliverables:
1. Reports on validation of detection algorithms and upgrades of detection algorithms to be implemented
2. Planetary parameters
3. Input for follow-up observations
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Unknown abundance of exomoons and binary planets does not permit that their discovery will be guaranteed.
PSM WPDs
OPERATIONS
Other Multiple Systems
Leader: Silvano Desidera
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 29/190
PSM WP 112 540
Operations phase
01/2024 — 03/2030
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. Scientific validation of detection algorithms for planets in multiple systems (using real PLATO data)
2. Identification of updates on algorithms for photometric identification of multi-planet systems in their
various configurations
3. Analysis and scientific interpretation of PLATO data of planets in multiple systems (including e.g.
dynamical modelling)
4. Provide inputs for follow-up observations
Input:
1. Scientific literature
2. PLATO Development Phase documentation
3. PLATO data
Dependencies:
Coordination with WP 112 400 on synergy between photometric and timing methods to detect multi-planet
systems
Output:
Review of published knowledge. Detection algorithms, Development of theory (as required) to fully exploit
PLATO data in this area, Scientific papers
Deliverables:
1. Reports on validation of detection algorithms and upgrades of detection algorithms to be implemented
2. Planetary parameters
3. Input for follow-up observations
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Reduced scientific impact of mission.
PSM WPDs
OPERATIONS
Transit Time Variations and Transit Duration
Variations (TTV / TDV)
Leader: Valerio Nascimbeni
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 30/190
PSM WP 112 600
01/2024 — 03/2030
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 scientific validation
of the algorithms defined by the sub-WPs during the Development phase, and of ongoing updates to the
algorithms based on real PLATO data. 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.
2.
3.
4.
5.
6.
Light curve processing
Stellar parameters
PLATO red book
PLATO specifications
PLATO light curves
Kepler, CoRoT, K2, TESS 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)
Output:
1. Refined algorithms with feedback for PDC.
2. Definition of follow-up observations.
Deliverables:
1. Observing plan for follow-up observations.
2. Reports/documents for PDC.
Milestones:
06/2025: Performance assessment report
2026: Observing plan for follow-up observations
Scientific validation of implementation at PDC will be performed as part of the PDC review process. Update
scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
TTV analysis could not be enough to derive a unique orbital solution on some systems, or can be too much
computationally intensive; follow-up in those cases will be much more demanding.
PSM WPDs
OPERATIONS
TTV / TDV Detection
Leader: Valerio Nascimbeni
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 31/190
PSM WP 112 610
Operations phase
01/2024 — 03/2030
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 the scientific validation of the algorithms assessed during the Development phase.
Fine-tune the above-mentioned algorithms analysing the output from real PLATO data.
Define the needed follow-up observations.
Write relevant documents/reports.
Input:
1.
2.
3.
4.
5.
6.
Light curve processing
Stellar parameters
PLATO red book
PLATO specifications
PLATO light curves
Kepler, CoRoT, K2, TESS 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).
Output:
1. Refined detection algorithms with feedback for PDC.
2. Definition of follow-up observations.
Deliverables:
1. Observing plan for follow-up observations.
1. Reports/documents for PDC.
Milestones:
06/2025: Performance assessment report
2026: Observing plan for follow-up observations
Scientific validation of implementation at PDC will be performed as part of the PDC review process. Update
scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
TTV analysis could not be enough to derive a unique orbital solution on some systems; follow-up in those cases
will be much more demanding.
PSM WPDs
OPERATIONS
TTV / TDV Modelling
Leader: Rosemary Mardling
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 32/190
PSM WP 112 620
Operations phase
01/2024 — 03/2030
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, ranked planet candidates from WP 113 000.
Output:
1. TBD
Deliverables:
1. TBD
Milestones:
06/2025: Performance assessment report
2026: Observing plan for follow-up observations
Scientific validation of implementation at PDC will be performed as part of the PDC review process. Update
scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
TBD
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 33/190
Specification of Procedures to Rank Planet
Candidates
Leader: Magali Deleuil
Rev.: 5
Operations phase
PSM WP 113 000
01/2024 — 03/2030
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 algorithms
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.
2.
3.
4.
Scientific literature
PLATO Red book
Current PLATO performance estimation
Real PLATO data
Dependencies:
WP 113 work packages
Output:
Procedure for full ranking of candidates for follow-up observations
Deliverables:
Reports from each work packages listing recommendations for implementation within PDC
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
None
PSM WPDs
OPERATIONS
Rank Planet Candidates
Leader: Andrew Collier Cameron
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 34/190
PSM WP 113 100
01/2024 — 03/2030
Institution: St Andrews University (UK)
Key Personnel: A. Collier Cameron
Objectives:
Improve 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. Produce ranked lists of candidates as a function of planet mass, determined from the results from light
curve modelling and centroid fitting during operations phase.
3. Select top-ranked targets for false-positive screening prior to ground-based radial-velocity follow-up.
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red book
Current PLATO performance estimation
PLATO data
Dependencies:
Other WP 113 work packages, WP 112
Output:
Report ranked lists of new candidates to work package leader.
Deliverables:
Reports and ranked lists of targets for ongoing RV follow-up.
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
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
OPERATIONS
Specification for Space Based False Positive
Identification Through Centroid Analysis
Leader: Magali Deleuil
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 35/190
PSM WP 113 200
01/2024 — 03/2030
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 light curve measuring methods
3. Development and test of algorithms for centroiding light curves and mimic rejection
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red book
Current PLATO performance estimation
PLATO data
Dependencies:
Other WP 113 work packages, WP 111, WP 112, WP 114
Output:
Updates of criteria and specifications of algorithms for centroid filtering.
Deliverables:
Report and algorithms
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
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
OPERATIONS
Astrophysical False Positives
Leader: Andrew Collier Cameron
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 36/190
PSM WP 113 300
01/2024 — 03/2030
Institution: St Andrews University (UK)
Key Personnel: A. Collier Cameron
Objectives:
To identify astrophysical phenomena mimicking planetary transits in PLATO data. Feedback properties of false
positives that escape detection to improve identification procedures.
Tasks:
1. Continued review of the scientific literature.
2. Critically examine likely and unlikely astrophysical false positives identified in PLATO data including
grazing and blended stellar binaries and blended transiting gas-giant systems.
3. Apply mitigation procedures combining astrometric and photometric catalogue data with light curve
modelling, to allow the most efficient identification of these objects with the minimal use of ground based
telescope time.
4. Analyse properties of false positives that escape early detection to improve discrimination.
Input:
1. Scientific literature
2. PLATO Red book
3. Current PLATO performance estimation
Dependencies:
Other WP 113 work packages, WP 112, WP 113
Output:
Improved procedure and algorithm for efficient mimic detection and mitigation based on actual PLATO data and
ground-based follow-up results.
Deliverables:
Reports and algorithms
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
This WP directly affects the efficiency of the ground based follow up project and that of confirming planets.
PSM WPDs
OPERATIONS
Specification of Transit Fitting Tools
Leader: Szilard Csizmadia
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 37/190
PSM WP 114 000
01/2024 — 03/2030
Institution: DLR (Germany)
Key Personnel: Sz. Csizmadia; N.N. (DLR); A. Bonomo (INAF-Torino); M Gillon (Liège)
Objectives:
Analysis of the PLATO transit light curves with the PLATO Eclipse Fitting Tool PEFT, while pursuing its
development and making it available to the PLATO community.
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.
7.
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.
Continuous reviewing of the literature for improvement of PEFT.
Liaise with Exoplanet Coordinator and PMC Science Management Coordinator as required.
Transit light curves analysis, independent or global (i.e. using all available data and priors).
Responsible for delivery of PEFT results to the PLATO community.
Responsible for the continuous improvement of PEFT and delivery to the PDC.
Input:
1.
2.
3.
4.
PLATO data
Follow-up data
External data
Scientific literature
Dependencies:
WP 114 work packages
Output:
PEFT Eclipse Fitting Tool for global modelling/analysis for PLATO data.
Reports with posterior distributions for the planetary systems parameters.
Deliverables:
Reports giving algorithms + models description and listing recommendations for implementation within PDC.
PEFT prototype.
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Low quality planetary parameters due to inadequate codes, or inappropriate application.
PSM WPDs
OPERATIONS
Specify Transit Curve Modelling Tools
Leader: Szilard Csizmadia
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 38/190
PSM WP 114 100
01/2024 — 03/2030
Institution: DLR (Germany)
Key Personnel: Sz. Csizmadia; N.N. (DLR); A. Bonomo (INAF-Torino); M Gillon (Liège)
Objectives:
Evaluate transit parameters and their uncertainties from PLATO data; provide up-to-date software environment
for transit modelling.
Tasks:
1.
2.
3.
4.
5.
Validation of the derived parameters and their uncertainties
Update algorithms based on the experience of the real PLATO data
Continuous scientific literature review to implement new developments
Check performance and quality
Coordination of the team work of this WP
Input:
1.
2.
3.
4.
5.
Scientific literature
PLATO Red book
Current PLATO performance estimation
PLATO specifications
Plato data
Dependencies:
Close interaction foreseen with the relevant tasks within WP 110, 113, 114.
Output:
Transit fitting algorithms and their optimized areas of applicability.
Deliverables:
Report on the activities done. Algorithms.
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
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
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 39/190
Specify Tools for Accurate Orbital Period
Determination
Leader: Magali Deleuil
Rev.: 5
Operations phase
PSM WP 114 200
01/2024 — 03/2030
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.
6.
7.
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.
Update scientific specifications based on real PLATO data
Scientifically validate implementation of the algorithms by the PDC
Input:
1.
2.
3.
4.
5.
Scientific literature
PLATO Red book
Current PLATO performance estimation
PLATO data
Commonly available codes within the PLATO community or freely available
Dependencies:
Other WP 114 work packages, WP 111, WP 112, WP 113
Output:
Ability to produce accurate ephemeris for single and multiple systems.
Deliverables:
Report and updates of algorithms
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Non-optimized orbital solutions will lead to inaccurate ephemeris. This will make the follow-up radial velocity
observations inefficient.
PSM WPDs
OPERATIONS
Rossiter-McLaughlin Modelling Tools
Leader: Guillaume Hébrard
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 40/190
PSM WP 114 300
01/2024 — 03/2030
Institution: IAP/OHP (France)
Key Personnel: G. Hébrard; F. Bouchy (LAM-CNRS); A. Collier Cameron (St Andrews); M. Gillon (Liège);
A. Lecavelier (IAP); A. Santerne (Porto/CAUP); A. Triaud (Toronto)
Objectives:
Improvements of models and algorithms for Rossiter-McLaughlin analysis
Tasks:
1. Improve the algorithms and tools to compute the Rossiter-McLaughlin (RM) effect from the experience
of actual data, in classical way from radial velocity measurements and tomographic way from spectral
line profile variation analysis.
2. Apply the differential RM (as a function of wavelength) for atmosphere characterization. Improve the
tools for the analysis.
Input:
1. Planets 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
Dependencies:
WP 142 XXX, WP 145 400, WP 145 100, WP 144 XXX, WP 114 000
Output:
1. Fitting tools included in the PLATO Eclipse Fitting Tool
2. Systems parameters
Deliverables:
Report and updates of algorithms
Milestones:
06/2025: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Update scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Low risk
PSM WPDs
OPERATIONS
Development of PLATO Data Specific Science
Leader: Don Pollacco
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 41/190
PSM WP 115 000
01/2024 — 03/2030
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 115 work packages
Output:
Continued review of current state of knowledge and identification of important areas for future progress
Deliverables:
Developments to understand aspects of PLATO data
Milestones:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
OPERATIONS
Astrophysical Noise Sources and Their Impact on RV
Determination
Leader: Chris Watson
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 42/190
PSM WP 115 100
01/2024 — 03/2030
Institution: Queens University Belfast (UK)
Key Personnel: C. Watson
Objectives:
Monitoring the performance of astrophysical noise mitigation techniques and procedures, and utilizing feedback
during the operation phase to maintain and improve aids where required. Act in responsive mode to additional
developments or issues identified by observers to improve functionality and ensure mission efficiency. Provide
general user support throughout operation phase.
Tasks:
1.
2.
3.
4.
To maintain and oversee the application of astrophysical noise mitigation aids.
To extend functionality according to observer feedback received during operations.
Ensure software documents and procedures are updated where applicable.
To respond actively to user needs, including adapting/improving noise mitigation aids in reaction to any
changing needs or special circumstances likely to arise.
5. Identify further areas requiring 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.
3. PLATO astrophysical noise mitigation aids/procedures and documents.
Dependencies:
Exchange of information with all RV follow-up packages, WP 140.
Output:
Continued development and support of astrophysical mitigation aids, ensuring efficient use of facilities and
ability to adapt reactively to any changing requirements identified during the operational phase.
Deliverables:
Noise mitigation aid procedures, software and manuals maintained and updated as required.
Continued assessment appraisals of the efficiency of noise reduction algorithm/strategies.
Milestones:
09/2027: Review of mitigation aids and procedures from first year of operation.
03/2030: Delivery of final report on WP activity
Risks:
Reduced ground-based follow-up efficiency leading to increased pressures on ground-based facilities & overall
reduction in the scientific impact of PLATO. Inability to respond to changing requirements/priorities likely to arise
as identified during the operational phase, further compromising PLATO science return.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 43/190
Improved Planetary System Characterisation
Leader: Alessandro Sozzetti
Rev.: 5
Operations phase
PSM WP 115 200
01/2024 — 03/2030
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
operations phase, (simulated) data from other sources will be combined with simulated and actual PLATO data
demonstrating expected system improvements. Where applicable, observing programs will be proposed to
advance the synergetic effort during PLATO mission operations.
Tasks:
1. Continued review of the scientific opportunities presented by and of instrumentation at current and future
facilities
2. Use of simulated and actual publicly available data to define comparison metrics describing the
advantages and improvements on planetary systems characterization from combined datasets
3. Optimization of the algorithms 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.
2.
3.
4.
Scientific literature
Simulated/actual data from ground-based and space-borne facilities devoted to exoplanet detection
PLATO Red Book
Simulated and actual PLATO data on specific targets of interest
Dependencies:
Other WP 115 work packages, WP 112, WP 113, WP 114
Output:
Scientific results on the synergy between PLATO and other planet-hunting facilities (based on combinations of
simulated and actual datasets). Optimized algorithms demonstrating areas of applicability as a function of
systems’ architecture and datasets combination. Where applicable, additional observational data on PLATO
targets of interest during mission operations.
Deliverables:
Detailed report with global review of published knowledge and 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.
Milestones:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of the mission, unavailability of complementary datasets.
PSM WPDs
OPERATIONS
Planet-Star Interactions
Leader: Stéphane Mathis
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 44/190
PSM WP 115 300
01/2024 — 03/2030
Institution: CEA (France)
Key Personnel: S. Mathis; I. Pagano (INAF-Catania); F. Remus (Paris/CEA/DSM); A.-S. Brun (CEA-CNRS);
G. Scandariato (INAF-Catania)
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. Coordination of the validation work that consists in checking that the modelling of star-planet interaction
effects that we achieved during the development phase is fully adapted and runs properly with the data
provided by PLATO.
2. Coordination of the work for building new specifications for modelling if necessary.
3. Coordination of the work on PLATO data for planetary system properties.
4. Coordination of the theoretical work based on PLATO data to learn more about planetary system
properties. This will give further improvements in the physical description of star-planet interactions and
contribute to the understanding of planetary system evolution.
Input:
PLATO data and scientific literature.
Dependencies:
Input and output from PDC (WP 370) and PSM.
Output:
Development of theory and numerical codes (as required) to fully exploit PLATO data in this area.
Deliverables:
Scientific publications, numerical codes and algorithms.
Milestones:
01/2024-12/2024: Improvements of the modelling procedure after tests with PLATO data. Modelling of starplanet interactions for first sets of PLATO data for detected planetary systems.
01/2025-12/2027: Theoretical developments to improve the description of physical processes in planetary
systems as required.
2028+: Contribution to the delivery of a new generation of star-planet interaction models.
Risks:
Reduced scientific impact of the mission.
PSM WPDs
OPERATIONS
Transits of Close-in Objects
Leader: Carole Haswell
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 45/190
PSM WP 115 400
01/2024 — 03/2030
Institution: The Open University
Key Personnel: C Haswell
Objectives:
Analyse and interpret PLATO outputs relating to extremely close-in planets and sub-planetary bodies, i.e. those
with orbital periods of about 1.5 days or less. Perform wavelength-resolved follow-up observations to determine
composition of the mass lost from these bodies using techniques from DEV phase. Compare the results with
models of planetary bulk compositions and analyses of previously known mass-losing exoplanets (e.g. WASP12b and KIC 1255b). Thus inform models for planetary system formation and evolution in the context of
Galactic chemical evolution.
Tasks:
1.
2.
3.
4.
Search PLATO outputs, prioritising hosts and candidate hosts identified in DEV phase.
Produce catalogue of confirmed close-in objects.
Prioritise targets for follow-up observations
Perform radial velocity follow-up of selected objects not covered by PLATO programmatic follow-up RV
to determine masses
5. Perform transmission spectroscopy and/or multicolour photometry to determine gas and dust
composition in priority targets.
6. Collect information on other planets in the systems studied.
7. Liaise with WP 116 200 to produce models of individual disintegrating rocky planets and to generate
information on the impact of Galactic chemical evolution on planet composition (using stellar ages).
Input:
1.
2.
3.
4.
5.
Relevant scientific literature.
PLATO data products
Strategies and software for identifying small close-in orbiting bodies.
Tested observational techniques for determining the composition of mass-losing bodies.
Catalogue produced in DEV phase of known and candidate hosts of mass-losing bodies amongst
PLATO targets.
Dependencies:
1. Inputs 3,4,5 will be generated in development phase of this WP.
2. Interaction with WP 116 200
3. PLATO data products
4. Availability of suitable ground-based facilities
Output:
1. Insights into planetary system formation and evolution throughout the history of the Galaxy.
2. Detailed knowledge of the composition of individual rocky planets, some of which are likely to be cores
of evaporated hot Jupiters
3. Detailed knowledge of the composition of sub-planetary bodies orbiting stars of various spectral types
and ages.
4. Masses of selected close-in planetary bodies.
5. Catalogue of close-in objects (planetary and sub-planetary) orbiting nearby bright stars.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 46/190
Deliverables:
1. Scientific papers reporting studies of individual systems, the catalogue, and implications for the Galactic
history of planet formation.
2. 2026: Progress Report
3. 2030: Delivery of final report on activity.
Milestones:
06/2026: Delivery of interim reports
12/2030: Delivery of final report on activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Non-Transiting Planets via REBs
Leader: David Barrado
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 47/190
PSM WP 115 500
01/2024 — 03/2030
Institution: Centro de Astrobiología, INTA-CSIC (Spain)
Key Personnel: D. Barrado; H. Bouy (CAB, INTA-CSIC); N. Huélamo (CAB, INTA-CSIC); M. MoralesCalderón (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. Detection of new non-transiting exoplanets.
2. Ground-based observations of the detected planet candidates (with detected transits) to look for the presence
of blended (contaminating) background/foreground sources. The presence of these sources dilutes the transit
dip, contaminating the determination of the planet properties. Also, for the subsequent (expensive) radial
velocity follow-up it would be necessary to have high-resolution images to avoid contaminating the spectra
with additional blended sources. Feedback on task #1.
Input:
Task 1 - Light curves with or without detected transits.
Task 2 - List of targets with planet candidates.
Dependencies:
Task 1 - 111 000, 112 100, 112 300, 112 400, 114 000, 116 000, 121 000, 123 000, 125 000, 131 000.
Task 2 - 112 000, 113 000, 114 000, 131 100, 143 000.
Output:
Task 1 - Non-transiting exoplanets, masses. Orbital and physical characterization of the surrounding objects
Task 2 - High-resolution images of the candidates and determination of the probability for a given planet host
candidate to have a blended (undetected companion).
Computation of the probability of having non-detected visual contaminants. Effect on the estimated planetary
parameters.
Deliverables:
Task 1 - Catalogue with system information: mass, physical separation, orbital inclination, and eccentricity.
Task 2 - Priority of the observed candidates to be followed-up by radial velocity analysis according to their
probability of having blended undetected sources that could contaminate the radial velocity signal. Correction
factor fort he light curves with nearby companions.
Progress reports
Milestones:
09/2024 Test with PLATO DR1 data.
2027 - 2030 Final catalogue
Task 2 - 1 year after the delivery of the planet candidates.
Risks:
The success depends on telescope time assignations
PSM WPDs
OPERATIONS
Development of PLATO Interpretation Specific
Science
Leader: Heike Rauer
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 48/190
PSM WP 116 000
01/2024 — 03/2030
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 116 work packages
Output:
Continued review of current state of knowledge and identification of important areas for future progress.
Deliverables:
Reports from each sub-work package
Milestones:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
OPERATIONS
Compositions & Formation of Gas & Ice Giants
Leader: Tristan Guillot
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 49/190
PSM WP 116 100
01/2024 — 03/2030
Institution: OCA/CNRS (France)
Key Personnel: T. Guillot; M. Havel (OCA)
Objectives:
Analyse PLATO data/ discoveries in terms of the structure and composition of gas and ice giants Infer
consequences for their formation and for planetary formation models in general.
Tasks:
1. Software developed in the development phase enabling a routine, homogeneous calculation of the
evolution of exoplanets (gas to ice giants) to be discovered by PLATO
2. Analyse data in a statistical way
3. Link planet evolution/structure/composition with up-to-date formation scenarios.
Input:
1. PLATO data
2. Stellar & planet evolution codes developed in the development phase
Dependencies:
WP 110, PLATO End-to-End Simulator
Output:
Analysis of PLATO data.
Deliverables:
Scientific analysis of PLATO discoveries (planet compositions, validation of formation models)
Milestones:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 50/190
The Mass-Radius Relationship for Terrestrial Planets
Leader: Frank Sohl
Rev.: 5
PSM WP 116 200
Operations phase
01/2024 — 03/2030
Institution: DLR (Germany)
Key Personnel: F. Sohl; N.N. (DLR)
Objectives:
Use PLATO photometry and ground-based radial velocity observations to study structural and compositional
models of solid exoplanet interiors based on improved 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
3. Science development needed to fully exploit PLATO data
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book
PLATO observational data
Commonly available codes within the PLATO community or freely available
Dependencies:
WP 110
Output:
1. Ongoing review of published knowledge.
2. Development of theory (as required) to fully exploit PLATO data in this area.
Deliverables:
Report
Milestones:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of the mission.
PSM WPDs
OPERATIONS
Planetary Formation and Orbital Evolution
Leader: Richard Nelson
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 51/190
PSM WP 116 300
01/2024 — 03/2030
Institution: Queen Mary, University of London (UK)
Key Personnel: R. Nelson; O. Gressel (NBI); W. Kley (Tuebingen); A. Johansen (Lund); Y. Alibert (Bern);
A. Morbidelli (OCA); M. Davies (Lund); M. Wyatt (IoA, Cambridge); C. Mordasini (Bern)
Objectives:
Provide on-going theoretical research in planet formation and orbital evolution for interpretation on in-coming
results. Update simulation codes, and examine formation and evolution scenarios for individual systems
discovered by PLATO. Develop statistical comparison between PLATO data and theoretical models as mission
proceeds.
Tasks:
1.
2.
3.
4.
5.
Continuously review relevant scientific literature
Undertake theoretical research to improve input physics to models
Update simulation software to maintain up-to-date input physics
Maintain library of simulation outputs based on most recent theoretical developments
Simulate formation and orbital evolution scenarios for individual systems discovered by PLATO to
provide interpretation of key discoveries
Input:
1. Relevant scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics
Dependencies:
Close interactions foreseen with all sub-packages 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 and orbital evolution
2. Synthetic planet populations generated using state-of-the-art theoretical models
3. Formation and evolution scenarios for PLATO discoveries and associated scientific publications,
applying to individual PLATO systems and to statistical comparisons between data and theoretical
model outputs.
Deliverables:
1. State of the art software tools for planet formation and orbital evolution simulations – capable of rapid
turnaround in event of significant discoveries by PLATO
2. Fully maintained library of simulated planetary systems for comparison with new discoveries, and for
statistical comparison with exoplanet data sets
3. 2028: Progress report
4. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Protoplanetary Disc Models
Leader: Oliver Gressel
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 52/190
PSM WP 116 310
01/2024 — 03/2030
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-to-date
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 and theoretical developments
2. PLATO data and discoveries
3. Observations of protoplanetary discs 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 dynamics and 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:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks: Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Disc-Planet Interactions
Leader: Wilhelm Kley
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 53/190
PSM WP 116 320
01/2024 — 03/2030
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:
Provide on-going theoretical research in planet-disc interaction and subsequent orbital and mass evolution for
interpretation of incoming PLATO data. Update simulation codes and incorporate the latest disc models, and
examine formation scenarios for individual systems discovered by PLATO.
Tasks:
1. Continued review of the scientific literature in this area
2. Theoretical research to improve understanding of relevant physics
3. Update simulation software to maintain up-to-date input physics and disc models
4. Maintain library of simulation outputs based on most recent theoretical developments
5. Simulate formation and evolution scenarios for individual systems discovered by PLATO to provide
interpretation of key discoveries
Input:
1. Scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics
Dependencies:
Close interactions foreseen with all sub-packages within WP 116
Output:
1. New theoretical insights into physical mechanisms of planet migration in discs and mass growth of planets
2. Increased knowledge about the long-term evolution of planets and planetary systems during disc phase
3. Formation and evolution scenarios for PLATO discoveries and associated scientific publications
4. Publication of obtained results in peer-reviewed journals
Deliverables:
1. State of the art software tools for planet formation and orbital evolution simulations
2. Prescriptions for mass growth and migration of planets for input in planet formation simulations
3. 2028: Progress report
4. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks: Reduced scientific impact of the mission.
PSM WPDs
OPERATIONS
The Assembly of Planetary Systems
Leader: Yann Alibert & Anders Johansen
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 54/190
PSM WP 116 330
01/2024 — 03/2030
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:
Provide on-going theoretical research in planet formation for interpretation of in-coming results. Update
simulation codes, and examine formation scenarios for individual systems discovered by PLATO.
Tasks:
1.
2.
3.
4.
Continuously review relevant scientific literature
Take into account results of other WPs (and literature) regarding key processes
Update planet formation software to maintain up-to-date input physics
Simulate formation scenarios for individual systems discovered by PLATO to provide interpretation of
key discoveries
Input:
1. Relevant scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics
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. Formation scenarios for key PLATO discoveries
4. Associated publications
Deliverables:
1. State of the art planet formation tools. Ability to rapid reaction in event of significant discoveries by
PLATO
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
The Post-Formation Long-Term Dynamical Evolution
of Planetary Systems
Leader: Alessandro Morbidelli
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 55/190
PSM WP 116 340
01/2024 — 03/2030
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:
Provide on-going theoretical research in long-term evolution of planetary systems for interpretation of in-coming
results. Develop statistical comparison between PLATO data and predictions from theoretical models as mission
proceeds.
Tasks:
1. Continuously review relevant scientific literature
2. Maintain library of outputs from long-term evolution simulations
3. Simulate formation and long-term evolution scenarios to explain the origin of individual systems
discovered by PLATO to provide interpretation of key discoveries
4. Comparing predictions from theoretical models with discoveries from PLATO
Input:
1.
2.
3.
4.
Relevant scientific literature and theoretical developments
PLATO data and discoveries
PLATO performance characteristics
Planetary systems issued from WP 116 320 & 330
Dependencies:
Close interactions foreseen with all sub-packages within WP 116
Output:
1. New theoretical insights into mechanisms leading to planet instabilities
2. New theoretical insights into long-term evolution of planetary systems following their instability and their
settling into a new stable configuration, and effects of tides for short period systems
3. Synthetic planet populations generated using state-of-the-art theoretical models
4. Formation and evolution scenarios for PLATO discoveries and associated scientific publications
5. Statistical comparisons between data and theoretical model outputs.
Deliverables:
1. Fully maintained library of simulated planetary systems for comparison with new discoveries, and for
statistical comparison with exoplanet data sets
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks: Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Planet Formation and Evolution in Binary Systems
Leader: Richard Nelson
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 56/190
PSM WP 116 350
01/2024 — 03/2030
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: On-going development of models of planet formation and evolution in binary systems, including
both circumbinary planets and planetary systems with external binary companions. Models will consider all
phases of planetary formation, and the long-term evolution after disc dispersal to explain incoming PLATO
data.
Tasks:
1. Review of relevant scientific literature
2. Code development to allow simulations of planet formation in binary systems to be computed
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
5. Modelling of key systems observed by PLATO to provide formation and evolution history
6. Critical analysis of models in the light of on-going PLATO discoveries.
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red book
PLATO data and discoveries
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.
Comparison between PLATO data and simulation results
Deliverables:
Synthetic planet populations for comparison with in-coming data
Interim report on scientific activity
Final report on scientific activity
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Influence of Birth Environment on the Formation and
Evolution of Planetary Systems
Leader: Melvyn Davies
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 57/190
PSM WP 116 360
01/2024 — 03/2030
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:
Provide on-going theoretical research into the effects of stellar birth environments on planetary systems.
Update modelling and examine formation scenarios/encounter histories for individual systems discovered by
PLATO.
Tasks:
1.
2.
3.
4.
Continuously review relevant scientific literature
Update simulation software to maintain up-to-date input physics
Maintain library of simulation outputs based on most recent theoretical developments
Simulate formation scenarios for individual systems discovered by PLATO to provide
interpretation of key discoveries
1.
2.
3.
Relevant scientific literature and theoretical developments
PLATO data and discoveries
PLATO performance characteristics
Input:
Dependencies:
Close interactions foreseen with all sub-subpackages within WP 116 300 particularly with WP 116 330 and WP
116 340.
Output:
1.
2.
3.
New theoretical insights into processes affecting protoplanetary discs and planetary systems in
clusters.
Models of the effects of encounters on planetary populations.
Encounter history scenarios for PLATO discoveries and associated scientific publications.
Deliverables:
Fully maintained library of encounter histories and final configurations for planetary systems for a variety of birth
environments.
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Post-Main Sequence Evolution of Planetary Systems
Leader: Mark Wyatt
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 58/190
PSM WP 116 370
01/2024 — 03/2030
Institution: University of Cambridge (UK)
Key Personnel: M. Wyatt; D. Veras (Warwick); E. Villaver (UAM); M. Davies (Lund); A. Mustill (Lund);
C. Migaszewski (NCU); A. Bonsor (Bristol)
Objectives:
Provide ongoing theoretical research into the evolution of planetary systems as the stars evolve into the postmain sequence phase to aid interpretation of incoming PLATO results. Examine past evolutionary scenarios for
individual detected systems. Develop population models that build on the main sequence planet population also
characterised by PLATO.
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 PLATO observations of post-main sequence planetary systems to interpret these within
the context of the main sequence progenitor and its evolution
Input:
1. Scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics
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 observations of individual post-main sequence planetary systems with PLATO
4. Simulations of PLATO observations of the population of post-main sequence stars
Deliverables:
1. 2028: Interim report on scientific activity
2. 2030: Final report on scientific activity
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Statistical Comparison Between Theory and PLATO
Data
Leader: Christoph Mordasini
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 59/190
PSM WP 116 380
01/2024 — 03/2030
Institution: University of Bern (Switzerland)
Key Personnel: C. Mordasini; Y. Alibert (Bern); A. Johansen (Lund); M. Davies (Lund); R. Church (Lund);
R. Alexander (Leicester); E. Lopez (IoA, Cambridge); C. Migaszewski (NCU); A. Mustill (Lund); S. Nayakshin
(Leicester); R. Nelson (QMUL)
Objectives:
Statistical comparison of theoretical predictions, such as synthetic planetary systems, and in-coming PLATO
data. Identification of theoretical descriptions in the formation and evolution models that are in (dis)agreement
with the observational data. Feedback into the theoretical models.
Tasks:
1. Continuously review relevant scientific literature
2. Update statistical comparison software to adapt to new theoretical developments and observational
results, potentially also from additional observational techniques/surveys
3. Maintain and update library of simulation outputs based on most recent theoretical models
4. Use of statistical methods to perform comparison between models and in-coming PLATO data regarding
radius, distance, eccentricity, mass, inclination, multiplicity, composition etc. distributions
5. Investigation of the statistical impact of: time (temporal evolution), stellar properties like mass and
metallicity, stellar binarity, formation environment etc. and associated correlations
6. Derivation of quantitative and qualitative statistical constraints for theoretical descriptions in models
Input:
1. Relevant scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics for usage as synthetic observational bias
4. New outputs of 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, WP 116 360 (input)
Output:
1. Preliminary assessment of the theoretical description by comparison with PLATO data, constraints for
theoretical models.
2. Ongoing review of published knowledge
3. Updated and adapted software tools for statistical comparisons
4.
Updated library and online analysis interface
Deliverables:
1. Updated statistical comparison tools
2. Statistical key quantities encapsulated in statistical indicators (e.g. KS tests and correlation coefficients)
3. Constraints and feedback for theoretical models
4. 2028: Progress report
5. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 60/190
Atmospheres of PLATO Planets
Leader: John Lee Grenfell
Rev.: 5
Operations phase
PSM WP 116 400
01/2024 — 03/2030
Institution: DLR (Germany)
Key Personnel: J. L. Grenfell; H. Rauer (DLR, Germany); F. Selsis (Bordeaux, CNRS)
Objectives:
Examination of current exoplanet model atmospheres especially 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. Continued 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:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
OPERATIONS
PLATO Habitable Zone Planets
Leader: Manuel Güdel / Helmut Lammer
Development phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 61/190
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
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 62/190
The Environments of PLATO Habitable Zone Planets
Leader: Helmut Lammer
Rev.: 5
Operations phase
PSM WP 116 510
01/2024 — 03/2030
Institution: Space Research Institute, Austrian Academy of Sciences (Austria)
Key Personnel: H. Lammer; 2 co-workers (SRI, AAS)
Objectives:
Evaluation and characterization of environmental (stellar and planetary) conditions for habitable zone planets
discovered with PLATO, including follow-up observations.
Tasks:
1. Science development and code applications needed to fully exploit PLATO data
2. Scientific publications
Input:
1. Scientific literature
2. PLATO performance
3. Studies and data related to follow-up observations of PLATO planets
Dependencies:
WP 110
Output:
1. Ongoing review of published knowledge.
2. Development of theory (as required) to fully exploit PLATO data in this area.
Deliverables:
Report
Milestones:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
OPERATIONS
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-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 63/190
PSM WP 116 520
04/2016 — 12/2023
PSM WPDs
OPERATIONS
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-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 64/190
PSM WP 116 530
04/2016 — 12/2023
PSM WPDs
OPERATIONS
Dynamical Interactions in Multi-Planet Systems
Leader: Jacques Laskar
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 65/190
PSM WP 116 600
Operations phase
01/2024 — 03/2030
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: J. Laskar; A. Correia (Aveiro); G. Boué (IMCCE); A. Fienga (OCA)
Objectives:
Provide on-going theoretical research in orbital and rotational dynamics of multi-planet systems for interpretation
on in-coming results. Examine the global dynamics in the vicinity of individual systems discovered by PLATO.
Use dynamical constraints to characterise the multi-planet PLATO systems.
Tasks:
1. Continuously review relevant scientific literature
2. Maintain and improve software tools for the dynamical analysis of PLATO systems.
3. Perform global dynamical analysis of multi-planet systems discovered by PLATO to provide
interpretation of key discoveries.
4. Perform stability analysis for both orbital and rotational evolution for multi-planet PLATO systems.
Input:
1.
2.
3.
4.
Relevant scientific literature and theoretical developments
PLATO data and discoveries
PLATO performance characteristics
Data from WP 112, WP 113, WP 114.
Dependencies:
Close interactions foreseen with all sub-packages 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 in presence or not of dissipation.
2. New insights on the role of resonances in multi-planet systems.
3. Climate long-term stability analysis of PLATO planets in the habitable zone.
4. Stability analysis for PLATO discoveries and associated scientific publications.
Deliverables:
1. Software tools for the analysis of PLATO data with dynamical constraints.
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Long-Term Dynamical Evolution of Planetary
Systems
Leader: Jacques Laskar
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 66/190
PSM WP 116 610
01/2024 — 03/2030
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: J. Laskar
Objectives:
Provide on-going theoretical research in long-term evolution of planetary systems. Provide long-term stability
analysis for all systems discovered by PLATO with specific analysis on selected systems.
Tasks:
1.
2.
3.
4.
Continuously review relevant scientific literature
Maintain software tools for a fast analysis of long-term stability of multi-planet systems.
Analyse the long-term evolution of all PLATO systems using the fast analysis tools.
Provide in-depth analysis on the long-term behaviour for selected systems.
Input:
1. Relevant scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics
4. Earth based Follow up data on PLATO systems.
Dependencies:
Close interactions foreseen with all sub-packages within WP 112, WP 113, WP 114, WP 115, and WP 116
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. Estimate of the long term-stability for all PLATO system.
4. Detailed analysis of long-term evolution for selected PLATO systems.
Deliverables:
1. Database of estimates of long-term stability for PLATO systems.
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Stability and Resonances in Multi-Planet Systems
Leader: Jacques Laskar
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 67/190
PSM WP 116 620
01/2024 — 03/2030
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: J. Laskar
Objectives:
Provide on-going theoretical research in dynamical studies of resonant planetary systems. Provide global
stability analysis for a selection of systems discovered by PLATO with specific analysis on resonant systems.
Tasks:
1.
2.
3.
4.
Continuously review relevant scientific literature
Maintain software tools for a fast analysis of global dynamics of multi-planet systems.
Analyse the global dynamics of selected PLATO systems, using input from WP 116 610.
Provide in-depth analysis on the global dynamics for resonant or close to resonant systems.
Input:
1. Relevant scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics
4. Earth based Follow up data on PLATO systems.
Dependencies:
Close interactions foreseen with all sub-packages within WP 112, WP 113, WP 114, WP 115, WP 116, and
especially WP 116 610.
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. Estimate of the global dynamics for a selection of PLATO system.
4. Detailed analysis the global dynamics for the resonant PLATO systems.
Deliverables:
1. Database of global dynamics for a selection of PLATO systems.
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Tidal Dissipation and Evolution of Multi-Planet
Systems
Leader: Alexandre C. M. Correia
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 68/190
PSM WP 116 630
01/2024 — 03/2030
Institution: University of Aveiro (Portugal)
Key Personnel: A. Correia
Objectives:
Provide on-going theoretical research in tidal dissipation and evolution of planets in multiple systems. Research
equilibrium configurations for interpretation on in-coming results. Update simulation codes, and examine
evolution scenarios for individual systems discovered by PLATO. Derive constraints for the formation process
and internal structures of the planets based on the observed equilibrium final configurations.
Tasks:
1. Continuously review relevant scientific literature
2. Update tidal evolution software to maintain up-to-date input physics
3. Run evolution scenarios for individual systems discovered by PLATO to provide interpretation of key
discoveries and derive constraints for the formation process and internal structures of the planets.
Input:
1. Scientific literature and theoretical developments
2. PLATO observational data and discoveries
3. Orbital architectures and internal structures issued from WP 116
Dependencies:
Close interactions foreseen with all sub-packages within WP 116, and WP 114 200, WP 115 200, WP 115 300.
Output:
1. New theoretical insights into tidal evolution and equilibrium configurations of multi-planet systems
2. Evolutionary scenarios for PLATO discoveries and associated scientific publications
3. Better characterization of PLATO planetary systems
4. Additional constraints for the formation processes and internal structures of the planets
Deliverables:
1. State of the art software tools for planet tidal evolution simulations – capable of rapid turnaround in
event of significant discoveries by PLATO
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Rotational Evolution of Planets in Multiple Systems
Leader: Gwenaël Boué
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 69/190
PSM WP 116 640
01/2024 — 03/2030
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: G. Boué
Objectives:
Provide on-going theoretical research in rotational evolution of planetary systems. Examine orbital forcing on the
climate of newly discovered planets, especially for those in the Habitable zone. Build a statistical sample of
rotational dynamics based on the PLATO population as the mission proceeds.
Tasks:
1. Continuously review relevant scientific literature
2. Improve and upgrade the library based on enhanced theoretical models and PLATO discoveries
3. Simulate rotation evolutions for individual systems discovered by PLATO to provide habitability
constraints and/or to highlight key dynamical behaviours
Input:
1. Relevant scientific literature and theoretical developments
2. PLATO data and discoveries
3. Earth based Follow up data on PLATO systems
Dependencies:
Close interactions foreseen with all sub-packages within WP 116
Output:
1. New theoretical insights into rotational evolution in multiple systems
2. Habitability constraints for individual PLATO systems based on their long term rotation
3. Statistical distribution of spin-axis behaviours in planetary systems
Deliverables:
1. Fully maintained catalogue of spin-axis dynamical characteristics of the PLATO population for
subsequent analysis of their climate and/or atmospheric evolution
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Planetary Ephemerides of PLATO Systems
Leader: Agnes Fienga
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 70/190
PSM WP 116 650
01/2024 — 03/2030
Institution: Observatoire de la Côte d’Azur (France)
Key Personnel: A. Fienga
Objectives:
Develop a planetary ephemerides database for a selection of PLATO multi-planet systems.
Tasks:
1. Continuously review relevant scientific literature
2. Maintain software tools for a fast elaboration of planetary ephemerides including follow up data.
3. Elaborate planetary ephemerides for a selection of PLATO systems.
Input:
1. Relevant scientific literature and theoretical developments
2. PLATO data and discoveries
3. PLATO performance characteristics
4. Earth based Follow up data on PLATO systems.
Dependencies:
Close interactions foreseen with sub-packages within WP 112, WP 113, WP 114, WP 115, WP 116
Output:
1. New theoretical insights for a fast elaboration of planetary ephemerides for a large number of systems.
2. Elaboration of a database for ephemerides of a selection of PLATO planetary systems including follow
up data.
3. Ongoing review of published knowledge
Deliverables:
1. Database of ephemerides for a selection of PLATO systems.
2. 2028: Progress report
3. 2030: Final report on activities
Milestones:
06/2028: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission
PSM WPDs
OPERATIONS
Specifications for Interface to Other PSM WPs and
PDC
Leader: Nuno Santos
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 71/190
PSM WP 117 000
01/2024 — 03/2030
Institution: CAUP (Portugal)
Key Personnel: N. Santos; D. Pollacco (Warwick)
Objectives:
Control if data flow from other work packages (in particular stellar and follow-up) is being done in the most
efficient way.
Tasks:
1. Continued review of scientific literature.
2. Follow the data flow scheme and verify if the best strategy is being used, or revise/refine the procedures.
Input:
1.
2.
3.
4.
5.
Scientific literature
PLATO Red Book
PLATO current performance
Reports from development phase
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 results
Deliverables:
Report
Milestones:
09/2027: Delivery of interim reports
03/2030: Delivery of final report on WP activity
Risks:
Low risk
PSM WPDs
OPERATIONS
Stellar Science Coordination
Leader: Marie-Jo Goupil
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 72/190
PSM WP 120 000
01/2024 — 03/2030
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. Coordination of the validation work that consists in checking that the procedures to derive stellar
characteristics (mass, radius, age, rotation period, stellar activity model etc.) that we specified during the
development phase are fully adapted and run properly with the data provided by PLATO
2. Coordination of the work for deriving new specifications of procedures and algorithms if necessary
3. Coordination of the work (seismology and stellar modelling) on PLATO data of the stars of the core
program
4. Coordination of the theoretical work based on PLATO seismic data to learn more about stars. This
ought to lead to further improvements in the physical description of stars and to a third generation of
stellar models. This will then provide an improved accuracy for the derived stellar characteristics.
5. Organization of working and review meetings gathering the leaders of the WPs
6. Delivery updated scientific specification for both algorithm and tools
7. Review scientific validation
Input:
1. Scientific specifications from the sub-packages
2. Scientific validation and update on the algorithms by the Stellar Science sub-packages
Dependencies:
1. Input from and output from PDC (WP 370) and PSM (WP 100, WP 130, WP 160); PLATO End-to-End
Simulator.
2. Input by all Stellar Science sub-packages
Output:
1. Scientific validation of stellar models
2. Updates on specifications of algorithms and tools
Deliverables:
Reports, algorithms and tools
Milestones:
06/2025: End of the first scientific validation of algorithms and tools with real PLATO data.
03/2029: Validated algorithms and updated stellar models (third generation) and procedure.
Risks:
Acceptable risks of delay for delivering third generation of stellar models
PSM WPDs
OPERATIONS
Stellar Models
Leader: Marc-Antoine Dupret
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 73/190
PSM WP 121 000
Operations phase
01/2024 — 03/2030
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 low
mass stars from the PMS to the subgiant phase.
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 PLATO data.
Input:
1. Existing stellar model grids and evolutionary codes, including those obtained in the previous phase
2. Existing 2D/3D hydro codes; results from hydro-simulations (to be completed)
3. First seismic constraints from PLATO data
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
3. First PLATO seismic constraints from WP 124 000
Output:
Grids of second-generation stellar models, evolutionary tracks and oscillation frequencies.
Deliverables:
Updated validated stellar model grids, evolutionary tracks and oscillation frequencies, with full documentation.
Milestones:
03/2024: Grids of third generation of models.
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
Risks: Minimal risks
PSM WPDs
OPERATIONS
1D Stellar Models
Leader: Yveline Lebreton
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 74/190
PSM WP 121 100
Operations phase
01/2024 — 03/2030
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: Validate and refine grids of high-quality stellar models and associated frequencies.
Tasks:
1. Use PLATO data to test and validate stellar models grids of very low mass to intermediate mass
stars covering evolutionary stages from pre main sequence to subgiant stages. These comparisons
are expected to further call for revisions in the physical processes already implemented in the codes
and for new processes to be considered.
2. Implement in stellar evolution codes the amendments and deeper improvements in the physics that
will be provided by WP 121 200, WP 121 300, WP 121 400 and WP 122 000, WP 123 200, WP 127
100
3. Recalculate improved grids of models from very low mass to intermediate mass stars covering
evolutionary stages from pre main sequence to subgiant stages.
4. Provide the oscillation spectra associated to these models and computed by different oscillation
codes.
5. Perform a new iteration of comparison of improved grids with PLATO data.
Input:
1.
2.
3.
4.
Existing stellar evolutionary codes appropriate to calculate MS and subgiant branch stellar models.
Existing stellar oscillation codes.
Model atmospheres to be used as boundary conditions (from WP 122 000).
Improved formulations for heat, chemical element and angular momentum transport and other physical
processes from WP 121 200, WP 121 300, WP 121 400, WP 127 100 as well as other external inputs
(microscopic physics: equation of state, opacities, nuclear reaction rates; macroscopic processes: mass
loss etc.)
Dependencies: WP 121 200, WP 121 300, WP 121 400 and WP 122 000, WP 123 200, WP 127 100. Output
from and input to PDC.
Output:
Grids of stellar models, evolutionary tracks and oscillation frequencies.
Deliverables:
Stellar model grids, evolutionary tracks and oscillation frequencies, with full documentation.
Milestones:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
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
OPERATIONS
Very Low Mass Stellar Models
Leader: Santi Cassisi
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 75/190
PSM WP 121 110
Operations phase
01/2024 — 03/2030
Institution: INAF- Astronomical Observatory 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 subgiant phase.
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:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
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
OPERATIONS
Low Mass Stellar Models
Leader: Josefina Montalban
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 76/190
PSM WP 121 120
01/2024 — 03/2030
Institution: University of Padova (Italy)
Key Personnel: J. Montalban; Y. Lebreton (Paris, GEPI); J. P. Marques (IAS-Orsay); A. Palacios
(Montpellier); P. Eggenberger (Geneva); A. Noels (Liège); P. Ventura (INAF-Rome); S. Cassisi (INAF-Teramo)
Objectives:
Validate and refine grids of high quality 1D stellar models for low/intermediate mass main sequence (MS) and
subgiant stars.
Tasks:
1. Keeping updating the physical description of low/intermediate mass stellar models in dedicated
evolutionary codes
2. Use PLATO data to test the physics included in theoretical stellar models, and define the improvements
to be included in new generation of models
3. Implement in the stellar evolution codes the improvements in the physics that will be provided by WP
121 200, 121 300, 121 500 and 122 000
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:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
Risks: None
PSM WPDs
OPERATIONS
Theoretical Oscillation Frequencies
Leader: Juan Carlos Suárez
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 77/190
PSM WP 121 130
Operations phase
01/2024 — 03/2030
Institution: Universidad de Granada (Spain)
Key Personnel: J.C. Suárez; A. García Hernández (Porto); J.R. Rodón (IAA-CSIC)
Objectives:
Support the automatic pipeline tasks related with the theoretical oscillation frequencies. Improve or design new
algorithms to obtain theoretical oscillation frequencies from PLATO observational evidences. Calculate the
theoretical oscillation frequencies of the third generation stellar models if any.
Tasks:
1. Correct any possible incidence during the pipeline execution related with the theoretical oscillation
frequencies grid.
2. Implement new algorithms or improve those in the pipeline following the possible new discoveries of
PLATO data related with the theoretical oscillation calculations.
3. When the third generations of stellar models are obtained, to calculate the corresponding theoretical
oscillation frequencies.
Input:
1. Models from the grid obtained in the WP121 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:
Improvements of the specifications of procedures and algorithms
Deliverables:
A complete set of frequencies for every model of the grids.
Milestones:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
Risks: Acceptable risks of delay interpreting unexpected observations coming from PLATO.
PSM WPDs
OPERATIONS
Transport Processes
Leader: Ana Palacios
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 78/190
PSM WP 121 200
Operations phase
01/2024 — 03/2030
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,
improved or developed to this end.
Tasks:
1.
2.
Follow up on the results obtained in models including transports processes
Proposition of new formulations/implementations if required
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:
Updates on transport processes modelling (theoretical formalisms and introduction in stellar evolution codes)
Deliverables:
Reports and grids of third generation stellar evolution models
Milestones:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
Risks: Acceptable risks
PSM WPDs
OPERATIONS
PMS Evolution
Leader: Joao Pedro Marques
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 79/190
PSM WP 121 300
Operations phase
01/2024 — 03/2030
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: Delivery of upgraded stellar models of PMS stars.
Tasks:
1. Verification that the procedures to derive stellar characteristics of PMS objects (mass, radius, age,
rotation period, stellar activity model etc.) that was specified during the development phase are fully
adapted and run properly with the data provided by PLATO.
2. Derivation of new specifications of procedures and algorithms if necessary.
3. Participation in the work (seismology and stellar modelling) on PLATO data of PMS stars.
4. Participation in the theoretical work based on PLATO seismic data to learn more about PMS stars, to
improve their physical description through stellar models with the goal of obtaining higher accuracy in
the derived stellar characteristics.
5. Impact of PMS evolution on MS structure and evolution and consequently on the age of stars of the core
program
Input:
Existing stellar evolutionary codes.
Dependencies:
Input from and output to PSM WP 121 200 – WP 121 400 – WP 121 500.
Output:
1. Validated procedures.
2. Updated specifications of procedures and algorithms.
Deliverables: Grids of PMS models.
Milestones:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
Risks: Acceptable risks of delay for delivering third generation of stellar models.
PSM WPDs
OPERATIONS
2D / 3D Stellar Evolution Models
Leader: Michel Rieutord
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 80/190
PSM WP 121 400
01/2024 — 03/2030
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 parameters 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
oscillations codes, which already exist and will just need slight adaptations, out of which the most precise stellar
parameters can be drawn. After launch we foresee that the main weakness of evolution code will be the
treatment of turbulent transport and the atmosphere. Manpower will thus be devoted to the improvement of
these features in the models.
Tasks:
1. Adapt 2D evolutionary codes with more refined models of turbulent transport and modelling of the
atmosphere, and compare with data
2. Adapt the associated oscillation codes that are able to use the 2D evolutionary models to invert data
3. Organize the scientific community to make an efficient use of the new tools
Input:
Existing codes
Dependencies:
WP 122, WP 121 100
Output:
Models of stars at any rotation rate including state-of-the-art models of transport processes and programs that
are able to invert asteroseismic data for 2D models
Deliverables:
At each milestone a numerical code will be delivered, with its associated oscillation code and documentation
Milestones:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
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
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 81/190
Evolution of Stars in Multiple Systems
Leader: Stéphane Mathis
Rev.: 5
Operations phase
PSM WP 121 500
01/2024 — 03/2030
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 (KU Leuven)
Objectives: Coordination of the modelling of the evolution of stars in multiple systems for PLATO stellar
science.
Tasks:
1. Coordination of the validation work that consists in checking that the modelling of stellar and planetary
companions effects (impact on stellar oscillations, orbital and spin evolution, internal transport of angular
momentum in each host star) that we achieved during the development phase is fully adapted and runs
properly with the data provided by PLATO.
2. Coordination of the work for building new specifications for modelling if necessary.
3. Coordination of the work (stellar and seismic modelling) on PLATO data for stars in multiple systems.
4. Coordination of the theoretical work based on PLATO seismic data to learn more about stars in multiple
systems. This will give further improvements in the physical description of stars and contribute to the
building of a third generation of stellar models. This will then provide an improved accuracy for the
derived stellar characteristics.
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), Planets-star
interactions (WP 115 300), Model of rotational evolution and gyrochronology (WP 123 300), Multiple
stars (128230).
Dependencies:
WP 115 300, WP 121 100, WP 121 200, WP 121 300, WP 121 400, WP 123 300, WP 128 230.
Output:
New specifications for modelling.
Deliverables:
Reports and models.
Milestones:
03/2024: Grids of third generation of models
03/2029: Validated algorithms and updated stellar models (third generation) and procedures.
Risks: Acceptable risks of delay for delivering a third generation of stellar models.
PSM WPDs
OPERATIONS
Non-Seismic Diagnostics and Model Atmospheres
Leader: Thierry Morel
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 82/190
PSM WP 122 000
01/2024 — 03/2030
Institution: University of Liège (Belgium)
Key Personnel: T. Morel
Objectives: Coordination of the activities of the work packages WP 122 100 to WP 122 500.
Tasks
1. Coordination of the work involving the stellar parameter determination of the PLATO targets based on
ground-based and Gaia data, as well as the modelling of their atmosphere.
2. Coordination of the validation work to ensure that the procedures to derive the stellar characteristics
(temperature, radius, chemical composition, etc.) that were specified during the development phase are
adapted to the PLATO data and provide results fully compliant with the scientific requirements of the
mission.
3. Further validating the adequacy of the procedures implemented for the determination of the stellar
parameters by comparing with the results provided by the theoretical modelling of the PLATO seismic
data.
4. Identifying procedures that need to be optimised and implementing new specifications of procedures and
algorithms, if necessary. Improving the 1D/3D modelling of the stellar atmospheres based on what is
learnt from the PLATO data and eventually provide a third-generation grid of model atmospheres and
limb-darkening coefficients that will be used to further improve the accuracy of the derived stellar
characteristics.
5. Ensure close coordination and efficient data exchange with other relevant WPs outside WP 122 000
(listed in Dependencies section below).
6. 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,
WP 131 000, and WP 140 000)
Output:
Validation of procedures, optimised scientific specifications
Deliverables:
Reports
Milestones:
06/2025: Improvements of the procedures and algorithms after extensive tests with PLATO data.
06/2026: Theoretical developments to improve the physical description of stellar atmospheres.
06/2029: Delivery of a second-generation grid of validated model atmospheres and limb-darkening coefficients,
as well as procedures to obtain non-seismic stellar parameters as input for seismic analysis.
Risks: Acceptable risks of delay for delivering third-generation grid of model atmospheres and limb-darkening
coefficients
PSM WPDs
OPERATIONS
1D Model Atmospheres
Leader: Bertrand Plez
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 83/190
PSM WP 122 100
Operations phase
01/2024 — 03/2030
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:
Keep model atmosphere grids updated for PLATO targets analysis. Use PLATO data to improve models.
Tasks:
1.
2.
3.
4.
Use PLATO observations to validate atmosphere models.
Improve the description of dust formation, and non-homogeneity of dust distribution.
Use 3D models to improve the description of the coupling of the atmosphere and interior of FGKM stars.
Improve the 1D model atmospheres covering the parameter space of FGKM stars observed with
PLATO.
5. Maintain the database that contains the output of the theoretical calculations (e.g., 1D model
atmospheres and associated model fluxes).
Input:
Spectroscopic and spectrophotometric observations of reference stars. Astrometry from Gaia. PLATO data.
Improved molecular and atomic line lists. Grids of 3D models.
Dependencies:
Other WP 122 000 sub-packages, WP 121 000, WP 123 000, WP 127 000, WP 131 000, and WP 140 000
Output:
Grid of updated 1D atmosphere models.
Deliverables:
1. Detailed report on accomplished work and reasons for the choices that were made.
2. Full grid of model atmospheres for FGKM stars in 1D.
Milestones:
06/2025: Improvements of the procedures and algorithms after extensive tests with PLATO data.
06/2026: Theoretical developments to improve the physical description of stellar atmospheres.
06/2029: Delivery of a second-generation grid of validated model atmospheres and limb-darkening coefficients,
as well as procedures to obtain non-seismic stellar parameters as input for seismic analysis.
Risks: None
PSM WPDs
OPERATIONS
3D Model Atmospheres
Leader: Martin Asplund
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 84/190
PSM WP 122 200
Operations phase
01/2024 — 03/2030
Institution: Australian National University (Australia)
Key Personnel: M. Asplund; F. Allard (Lyon); L. Bigot (Nice); A. Chiavassa (Nice); R. Collet (Canberra);
D. Homeier (Lyon); Z. Magic (MPA); F. Thévenin (Nice) ; R. Trampedach (Boulder)
Objectives:
Improve 3D hydrodynamical stellar model atmospheres of late-type stars.
Tasks: Improve existing grid of 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) based on observations obtained with PLATO and other facilities, as well as improved input physics.
Input:
Existing models computed during development phase
Dependencies:
Other WP 122 000 sub-packages, WP 121 000, WP 123 000, and WP 127 000
Output:
Improved 3D stellar atmosphere grid
Deliverables:
Reports and updated atmosphere models
Milestones:
06/2025: Improvements of the procedures and algorithms after extensive tests with PLATO data.
06/2026: Theoretical developments to improve the physical description of stellar atmospheres.
06/2029: Delivery of a second-generation grid of validated model atmospheres and limb-darkening coefficients,
as well as procedures to obtain non-seismic stellar parameters as input for seismic analysis.
Risks:
None. All the mentioned key personnel have the needed expertise.
PSM WPDs
OPERATIONS
Fundamental Stellar Parameters
Leader: Carlos Allende Prieto
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 85/190
PSM WP 122 300
01/2024 — 03/2030
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 (INAF-Torino)
Objectives:
Validate and improve the procedures to determine the stellar parameters of FGKM stars and provide grids of
model fluxes for them. Update the stellar parameters based on new external data (e.g., from ground-based
multi-object spectrographs) and follow-up observations of PLATO targets.
Tasks:
1. Ensure that the grids of model fluxes and procedures to determine the stellar parameters are suited for
the analysis of PLATO data and meet the scientific requirements.
2. Examine the effect of incorporating seismic information from PLATO observations (e.g., surface gravity)
on the stellar parameters.
3. Maintain the database that contains the outputs from theoretical calculations (e.g., model fluxes for
FGKM stars).
4. Continuously update the database, designed for seismic use, that contains the parameters of the FGKM
stars based on new external data and incoming observations
Input:
External databases and follow-up data, seismic parameters, 1D and 3D model atmospheres for FGKM stars.
Dependencies:
Other WP 122 000 sub-packages, WP 125 000, WP 131 000, and WP 140 000
Output:
Improved grids of model fluxes for FGKM stars. Updated quality assurance for parameters. Updates for
parameters of FGKM stars based on external and PLATO data.
Deliverables:
Improved grids of model fluxes.
Milestones:
06/2025: Improvements of the procedures and algorithms after extensive tests with PLATO data.
06/2026: Theoretical developments to improve the physical description of stellar atmospheres.
06/2029: Delivery of a second-generation grid of validated model atmospheres and limb-darkening coefficients,
as well as procedures to obtain non-seismic stellar parameters as input for seismic analysis.
Risks: None
PSM WPDs
OPERATIONS
Limb Darkening
Leader: Antonio Claret
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 86/190
PSM WP 122 400
Operations phase
01/2024 — 03/2030
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: Improve knowledge of the limb-darkening distribution of host stars. Identify and quantify the
sources of uncertainties in the limb-darkening coefficients. Validate the computed limb-darkening coefficients
based on PLATO data.
Tasks:
1. Computation/tests of limb- and gravity-darkening coefficients.
2. Refine the computation of limb-darkening coefficients for several atmosphere models. The calculations
will be performed for the photometric system of PLATO, as well as for the most commonly used
passbands (uvbyUBVRIJHK, Sloan, etc.) by adopting least-squares and flux conservation methods.
Concerning the effects of tidal/rotational distortions, we plan to compute gravity-darkening coefficients,
(lambda), using the same models of stellar atmospheres as in the case of limb-darkening.
3. Ensure that the grids computed are suited for the analysis of the PLATO data and meet the scientific
requirements.
Input:
Grids of atmosphere (specific intensities)
Dependencies:
WP 110 000, other WP 122 000 sub-packages
Output:
Grids of limb and gravity-darkening coefficients. Improved numerical methods.
Deliverables:
Reports. Distribution of the grids of limb and gravity-darkening coefficients.
Milestones:
12/2025: Numerical tests using the available specific intensities for late-type stars. Evaluation of the
confrontation between the empirical data from PLATO and the theoretical calculations.
12/2029: Theoretical improvements in the numerical methods adopted to describe the intensity distribution of
stellar configurations based on our acquired knowledge of stellar physics.
Risks: Acceptable risks of delay for delivering a new generation of atmosphere models
PSM WPDs
OPERATIONS
Interstellar Extinction
Leader: Douglas Marshall
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 87/190
PSM WP 122 500
Operations phase
01/2024 — 03/2030
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. Perform validation on derived extinction values
2. Evaluate uncertainties on extinction estimates
3. Refine algorithms based on results from 1 and 2 above
Input:
Gaia reddening, ground-based spectroscopic data
Dependencies:
Other WP 122 000 sub-packages, WP 131 000, and WP 140 000
Output:
Extinction maps. Extinction for each source.
Deliverables:
Validation report of the software module
Milestones:
12/2024: Assign extinction to each star (from GAIA)
12/2027: Explore other extinction estimates
12/2029: Validation of the extinction estimates for individual stars
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Stellar Activity and Rotation
Leader: Antonino Francesco Lanza
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 88/190
PSM WP 123 000
01/2024 — 03/2030
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: Coordination of the works of the work packages from WP 123 100 to WP 123 600.
Tasks:
1. Coordination of the validation work that consists in checking that the procedures to derive stellar rotational
and magnetic activity characteristics (rotation rate, amplitude and sign of differential rotation, short- and
long-term cycles of activity, surface convective patterns, models for dynamo action and differential
rotation, models for angular momentum evolution) be those specified during the development phase and
are fully adapted and run properly with the data provided by PLATO.
2. Coordination of the work for deriving new specifications of procedures, algorithms, and theoretical models, if
necessary.
3. Coordination of the work (rotation and magnetic activity studies) on PLATO data of the stars of the core
program.
4. Coordination of the theoretical work based on PLATO light curves, seismic data, and follow up observations
to learn more about activity and rotation of the stars. This requires to coordinate the flux of information
towards and from other WPs external to 123 000. This ought to lead to further improvements in the
physical description of stars and to a third generation of stellar models. It will further improve the accuracy
of the derived stellar characteristics.
5. Organization of working and review meetings gathering the leaders of the WPs.
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:
Input from and output towards PDC (WP 373 000) and PSM (WP 122 000, WP 124 000, WP 125 000, WP 127
000 also for interaction with WPs external to 120 000).
Output:
Updated scientific specifications of algorithms, procedures, and models
Deliverables:
Reports and models
Milestones:
06/2025: Improvements of the procedures, algorithms, and theoretical models of atmosphere after testing with
PLATO data; Rotational and stellar activity modeling on first sets of PLATO data; checking of the scaling
relationship relating activity and convection to global stellar parameters with PLATO data.
06/2026: Theoretical developments to improve the physical description of models of atmosphere.
06/2029: Delivery of the third generation of validated models of atmosphere and procedures related to the nonseismic characterization of host stars.
Risks: Acceptable risks of delay for delivering the third generation of rotational and activity parameters, scaling
relationships, and theoretical models related to them.
PSM WPDs
OPERATIONS
Spot Models
Leader: Benoit Mosser
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 89/190
PSM WP 123 100
Operations phase
01/2024 — 03/2030
Institution: Observatoire de Paris (France)
Key Personnel: B. Mosser; N. Meunier (Grenoble); A.-M. Lagrange (Grenoble); A. Palacios (Montpellier); N.
Krivova (Göttingen); S. Solanki (Göttingen); A. S. Bonomo (INAF-Torino); Y. Unruh (Imperial College London);
L. Bigot (Nice); D. Mourard (Nice); N. Nardetto (Nice); D. Salabert (CEA); M. Schuessler (MPSSR); O.
Kochukhov (Uppsala); H. Schunker (MPSSR); R. Cameron (MPSSR), D. Barrado (CSIC-INTA)
Objectives:
Measurement of the spot distribution, in close relation with the stellar activity and rotation measurement
Tasks:
1. Validation work that consists in checking that the procedures to derive stellar rotational and magnetic
activity characteristics (rotation rate, amplitude and sign of differential rotation, short and long-term
cycles of activity, surface convective patterns, models for dynamo action and differential rotation,
models for angular momentum evolution) be that specified during the development phase and are fully
adapted and run properly with the data provided by PLATO.
2. Deriving new specifications of procedures, algorithms, and theoretical models, if necessary
3. Further improvements in the physical description of stars and to a third generation of stellar models. It
will further improve the accuracy of the derived stellar characteristics.
4. Delivering, spots models, rotation rates, differential rotations rates, spot lifetimes
Input:
Stellar atmosphere models from Stellar Science WP 122 000, WP 122 300, CoRoT or Kepler data, synthetic
data, stellar characteristics (effective temperature, gravity, chemical composition, rotation period, chromospheric
indexes, asteroseismic age); solar activity measurements
Dependencies:
Models of different contributions from WP Stellar Science/Stellar Activity
Output :
Updated scientific specifications of algorithms and procedures and models
Deliverables:
Reports and models
Milestones:
06/2025: Improvements of the procedures, algorithms, and theoretical models of atmosphere after testing with
PLATO data; Rotational and stellar activity modeling on first sets of PLATO data; checking of the scaling
relationship relating activity and convection to global stellar parameters with PLATO data.
06/2026: Theoretical developments to improve the physical description of models of atmosphere.
06/2029: Delivery of the third generation of validated models of atmosphere and procedures related to the nonseismic characterization of host stars.
Risks:
Acceptable risks of delay for delivering the third generation of rotational and activity parameters, scaling
relationships, and theoretical models related to them
PSM WPDs
OPERATIONS
Surface Convection (1D & 3D)
Leader: Friedrich Kupka
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 90/190
PSM WP 123 200
01/2024 — 03/2030
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: Construction and analysis of 1D & 3D models of stellar granulation and surface convection.
Tasks:
1. Production of simulations of stellar surface convection for early runs of PLATO
2. Development of further improved models for the computation of the theoretical contribution of
granulation to observed intensity and its signature in power spectra as required for the third generation
of validated third generation stellar models.
3. Use of PLATO data of the stars oft he core program to probe the completeness of the physics of the
granulation simulations
4. Improving the theoretical models and simulations in response to the results from available PLATO data
Input:
Models of granulation developed for use with PLATO data.
Dependencies:
This WP is part of the WP 123 000.
Output:
Updated models
Deliverables:
Reports and models
Milestones:
12/2022: Development of the new generation of models and simulations of stellar granulation in response to
early results from PLATO data
12/2023: Making the new models available in time for the development of the third generation of validated
models and procedures related to the characterization of host stars
Risks:
Acceptable risks
PSM WPDs
OPERATIONS
Models of Rotational Evolution and Gyrochronology
Leader: Marc Pinsonneault
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 91/190
PSM WP 123 300
01/2024 — 03/2030
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. Empirically constrain distinct rotation-age relationships appropriate for both unevolved and evolved low
mass stars using PLATO data and quantify their uncertainties.
2. Explore observational selection effects in the detectability of rotation and the impact of blends and
binary companions.
3. Explore mixing as a diagnostic of angular momentum transport.
4. 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
Deliverables:
Reports and updated stellar models
Milestones:
12/2024: Test our procedures for inferring rotation-mass-age relationships against actual PLATO data. Work
with groups studying rotation periods to understand selection effects in rotation measurements.
12/2025: Produce calibrated rotation-age estimates from PLATO data.
12/2029: Develop next-generation models including rotation; this includes seismic constraints from PLATO data
and rotation physics results from other PLATO subgroups.
Meetings with the WP 123 XXX leaders twice a year.
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 92/190
Dynamos and Differential Rotation
Leader: A.S. Brun
Rev.: 5
Operation phase
PSM WP 123 400
01/2024 - 03/2030
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:
In collaboration with WP 120 000
• Coordination of theoretical and modelling effort of stellar rotation proxy for solar-like stars
• Coordination of theoretical and modelling effort of stellar dynamo and magnetic activity proxies
• Multi-D numerical simulations of convection, rotation, turbulence & magnetism of solar like stars
• Benchmark of 3-D MHD models of a selection of Plato targeted stars
• Code maintenance and development
• Regular reports on WP progress, participation to PSM meetings
Input:
• Seismic inversion of internal rotation profile (WP 125)
• Extent of convective envelope (WP 126), 1-D stellar state (WP 121 100) for 3-D models
• Proxies of magnetic activity (WP 125)
Dependencies:
WP 120 000, and sub-WPs
Output:
(WP 121, 124, 127)
• Impact of magnetism, convection and rotation on light curves as a function of spectral type
• Version 1.0 of scaling laws of differential rotation and activity levels as a function of spectral type
• Realistic 3-D Simulations of some PLATO targeted stars
• Turbulent convective spectra for waves excitation
• Updates on specifications of algorithms and tools
Deliverables:
Spectra (turbulent and of gravity modes) and 2-D and 3-D models of target star, regime diagrams,
Regular reports of advancement of WP, regular meeting with PSM WP and sub-WP leaders
Milestones:
2025: Specific models of targeted stars.
2026: Interpretation of stellar data collected on convection, rotation and magnetism.
2028: Detailed multi-dimensional MHD model of some PLATO target stars.
Risks: Lack of precision of inverted convection extent, differential rotation profiles and magnetic activity
PSM WPDs
OPERATIONS
Tools to Measure Rotational Modulation
Leader: Sergio Messina
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 93/190
PSM WP 123 500
01/2024 — 03/2030
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. Validate that methods and algorithms needed for the detection and the analysis of the rotational modulation of
the flux we specified in the development phase run properly on the PLATO data.
2. Validate that the methods and algorithms needed for exploiting the information from activity models we
specified in the development phase run properly on the PLATO data.
3. Derive the stellar rotation period, estimate of the surface differential rotation, spot lifetimes.
4. Validate that the procedures to use spectroscopic rotation measurements to improve and check results work
properly.
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:
1. Output for WP 123 300 and WP 123 400
2. Input from WP 123 100
Output:
Updated scientific specifications of procedures and algorithms
Deliverables:
Reports and algorithms
Milestones:
12/2024: Improvements of procedures and algorithms for period detection and of check with spectroscopic data;
12/2025: Improvements of procedures and algorithms for activity modeling;
12/2028: Deliver of catalogue of rotation period, differential rotation, and photometric activity parameters.
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
OPERATIONS
Stellar Rotation from Transits
Leader: Adriana Valio
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 94/190
PSM WP 123 600
01/2024 — 03/2030
Institution: CRAAM, Mackenzie University (Brazil)
Key Personnel: A. Valio
Objectives:
1. Determine the rotation period of a planet-hosting star through the detection of spots on the stellar surface
during a planetary transit. The period will be determined by following the spots position through time during
consecutive transits. 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. From the average rotation period of the star, or if the rotation period at
different latitudes from multiple transiting planets is known, then assuming a solar like differential rotation
profile, or another given one, the differential rotation profile of the star may be determined.
Tasks:
1. Check that the spot detection algorithm works properly with PLATO data, by identifying intensity variations in
the transit light curves due to spots;
2. Verify that the spot modelling is appropriate, that is, define the acceptable interval for the values of the spots
characteristics such as position (latitude and longitude), relative intensity, and size;
3. Improve the identification of the same spot on successive transits in order to determine the stellar rotation
period with more precision;
4. Test the computer codes in the determination of the stellar differential rotation for systems with multiple
transiting planets at different stellar latitudes.
Input:
Computer codes to detect and model the spots; Model data; CoRoT and Kepler light curves.
Dependencies:
Transit light curves; planet/companion orbital parameters (such as period and inclination angle), stellar
parameters (mass, radius, effective temperature)
Output:
1. Updated scientific specifications of procedures and algorithms
2. Improved models
Deliverables: Reports and algorithms
Milestones:
06/2025: Improvements of the procedures, algorithms, and theoretical models of atmosphere after testing with
PLATO data; Rotational and stellar activity modeling on first sets of PLATO data; checking of the scaling
relationship relating activity and convection to global stellar parameters with PLATO data.
06/2026: Theoretical developments to improve the physical description of models of atmosphere.
06/2029: Delivery of the third generation of validated models of atmosphere and procedures related to the nonseismic characterization of host stars.
Risks: Low, since this technique has already been proven to be effective with CoRoT and Kepler data.
PSM WPDs
OPERATIONS
Seismic Diagnostics
Leader: Margarida Cunha
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 95/190
PSM WP 124 000
Operations phase
01/2024 — 03/2030
Institution: Universidade do Porto, CAUP (Portugal)
Key Personnel: M. Cunha; I. Roxburgh (QMUL); D. Reese (Birmingham); S. Deheuvels (OMP, IRAP)
Objectives:
Coordination of the work to be carried out by WP 124 100, WP 124 200, and WP 124 300.
Tasks:
1. Coordinate the validation of the seismic diagnostic tools developed and implemented during the
development phase, with the data acquired by PLATO.
2. Coordinate any updates of the algorithms concerning the forward, inverse, and glitch-related
approaches of stellar parameter estimation that may be found necessary as a result of the inferences
made on PLATO data.
3. Organization of work meetings and conference calls involving WP 124 100, WP 124 200, and WP 124
300.
Input:
PLATO data and ground-based non-seismic complementary data; procedures developed in WPs 124 100 to 124
300.
Dependencies:
Input from and output to WPs 124 100 to 124 300 and WP 120 000
Output:
Updated scientific specifications of procedures
Deliverables:
Reports and algorithms
Milestones:
06/2025: End of validation and adjustment of the forward and inverse algorithms.
06/2027: Delivery of new forward and inverse procedures for seismic inference of stellar properties,
incorporating the information learned from the analysis of PLATO data.
Risks: Acceptable risks. The end of validation and adjustment can be slightly delayed depending on whether
the data acquired by PLATO correspond to what was expected in the preparatory work
PSM WPDs
OPERATIONS
Forward Approaches
Leader: Ian Roxburgh
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 96/190
PSM WP 124 100
Operations phase
01/2024 — 03/2030
Institution: Queen Mary University of London (UK)
Key Personnel: I. Roxburgh; S. Vorontsov (QMUL); M. Cunha (Porto); M. Bazot (Porto)
Objectives:
Validate the adopted forward procedures used in the determination of the mass, radius, age, and other
properties of planet-host stars using PLATO data, and further develop/adapt these procedures as necessary.
Tasks
1. Validate the forward procedures developed and implemented prior to launch, with the data acquired by
PLATO.
2. Develop further / adapt the forward procedures to incorporate the findings resulting from the analysis of
PLATO data.
3. Update the algorithms concerning the forward procedures according to the conclusions of point 2.
Input:
Procedures developed and implemented prior to launch; PLATO data
Dependencies:
Input from and output to WP 124 000
Output:
Updated scientific specifications of procedures and algorithms
Deliverables:
Reports and algorithms
Milestones:
06/2025: End of validation and adjustment of the forward algorithms.
06/2027: Delivery of new forward procedures for seismic inference of stellar properties, incorporating the
information learned from the analysis of PLATO data.
Risks:
Acceptable: The end of validation and adjustment can be slightly delayed depending on whether the data
acquired by PLATO correspond to what was expected in the preparatory work
PSM WPDs
OPERATIONS
Inverse Techniques
Leader: Daniel Reese
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 97/190
PSM WP 124 200
Operations phase
01/2024 — 03/2030
Institution: University of Birmingham (UK)
Key Personnel: D. Reese; G. Buldgen (Liège); I. Roxburgh (QMUL); S. Deheuvels (OMP, IRAP)
Objectives:
Insure quality of inversion output from the PDC, and propose improvements as needed.
Tasks:
1. Validate inversion procedure(s) implemented by the PDC and insure quality of associated output.
2. Propose corrections/improvements as needed.
Input:
Inversion procedure(s) implemented in the PDC
Dependencies:
Input from and output to WP 124 000
Output:
Updated scientific specifications of procedures
Deliverables:
Reports and algorithms
Milestones:
06/2025: End of validation and adjustment of the inverse algorithms.
06/2027: Delivery of new inverse procedures for seismic inference of stellar properties, incorporating the
information learned from the analysis of PLATO data.
Risks: Acceptable risks. The end of validation and adjustment can be slightly delayed depending on whether
the data acquired by PLATO correspond to what was expected in the preparatory work.
PSM WPDs
OPERATIONS
Acoustic Glitches
Leader: Sébastien Deheuvels
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 98/190
PSM WP 124 300
Operations phase
01/2024 — 03/2030
Institution: Observatoire Midi-Pyrénées, IRAP (France)
Key Personnel: S. Deheuvels; M. Monteiro (CAUP); M. Cunha (Porto); J. Ballot (IRAP); D. Reese
(Birmingham)
Objectives: To validate the procedures established in the development phase on PLATO targets and to update
and improve them if necessary.
Tasks:
1. Validate the procedures selected to fulfil tasks 1, 2, and 3 of the development phase on PLATO data.
2. Propose and implement improvements to these procedures.
3. Use the estimates of the extension of convective cores from the PLATO targets to search for potential
relations between the core extension and stellar parameters such as the mass or the metallicity. Such
relations could then be included in 1D stellar models to reach a better precision on stellar ages.
Input:
Procedures established during the development phase and implemented by the PDC. PLATO data.
Dependencies:
Input from and output to WP 124 000
Output:
Updated description of procedures to be applied and potential relations involving the convective core extension.
Deliverables:
1. Reports on the tests with PLATO data and updated algorithms
2. Relations between convective core extensions and stellar parameters
Milestones:
06/2025: End of validation and adjustment of new algorithms.
06/2027: Delivery of new procedures for seismic inference of stellar properties, incorporating the information
learned from the analysis of PLATO data.
Risks: Acceptable: The end of validation and adjustment can be slightly delayed depending on whether the
data acquired by PLATO correspond to what was expected in the preparatory work
PSM WPDs
OPERATIONS
Determination of Stellar Parameters
Leader: Jørgen Christensen-Dalsgaard
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 99/190
PSM WP 125 000
01/2024 — 03/2030
Institution: Aarhus University (Denmark)
Key Personnel: J. Christensen-Dalsgaard; Hans Kjeldsen (Aarhus); B. Chaplin (Birmingham)
Objectives: Supervise the application in the PDC of procedures that deliver masses, radii, ages, and chemical
composition of planet host stars with the precision required by the exoplanet WPs, and with full statistical
characterization in terms of Probability Density Functions. 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 122 00 to ensure that optimal modelling tools are used for determination of
'classical' parameters under WP 125 200.
Tasks:
1.
2.
3.
4.
Coordination of the work done by WP 125 100 to 125 400
Make sure that the quality of the outputs from WP 125 100 to 125 400 match the specified requirements
Ensure that updates are made in the procedures based on the properties of actual PLATO data
Develop and apply procedures for utilizing the asteroseismic insights obtained through the analysis of
PLATO data to improve the determination of stellar parameters.
Input:
Procedures, results and documentation from WP 125 100 to WP 125 400
Dependencies:
Input from WP 121 000, WP 122 000, WP 123 000, WP 124 000
Output:
Continued verification of optimized procedures to determine accurate masses, radii, ages, chemical composition
as well as statistical characterization that satisfy the exoplanet specifications, with full documentation of the
procedures
Deliverables:
Reports on the operations of the procedures to determine accurate masses, radii, ages, chemical composition
as well as uncertainties that satisfy the exoplanet specifications, with documentation of the need for updates.
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: Minimal
PSM WPDs
OPERATIONS
Scaling Laws
Leader: Andrea Miglio
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 100/190
PSM WP 125 100
Operations phase
01/2024 — 03/2030
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. Validate the scaling relations by using new generations of stellar models and oscillation frequencies
delivered by WP 121 100,
2. Update the calibration of the scaling relations using targets with available independent mass/radius
estimates (detached eclipsing binaries, stars in clusters, nearby stars with precise interferometric and
astrometric constraints)
Input:
1.
2.
3.
4.
Grids of stellar models (from WP 121 100),
Predictions of mode amplitudes (from WP 126 100)
Average seismic parameters (from WP 372 100)
Non-seismic information on the targets (from WP 122 000).
Dependencies:
Input from WP 121 100, 122 000, and WP 126 100
Output:
Updated, optimized and validated procedures to determine accurate masses, radii, ages, as well as
uncertainties that satisfy the exoplanet specifications
Deliverables:
Optimized and validated procedures to determine accurate masses, radii, ages as well as uncertainties that
satisfy the exoplanet specifications, with full documentation
Milestones:
12/2024: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms and update stellar models and procedure
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Improve scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks: Minimal risks
PSM WPDs
OPERATIONS
Incorporating Classical Parameters
Leader: Sofia Feltzing
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 101/190
PSM WP 125 200
01/2024 — 03/2030
Institution: Lund Observatory, Lund University (Sweden)
Key Personnel: S. Feltzing
Objectives: Improve and validate the procedures developed during the development phase 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 parallaxes, from the Gaia observations, expected to be available when PLATO is
launched. The analysis will make use of standard stellar model atmospheres, in collaboration with other WPs. A
full statistical analysis and proper error propagation must be ensured.
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:
From WP 122 000, WP 121 000
Dependencies:
Input from WP 122 000, WP 121 000
Output:
Work with WP 122 000 and WP 121 000 to produce the relevant data for the mission. Undertake additional
ground based follow-up observations (if this was found necessary during the development phase).
Deliverables:
Algorithm part devised to include the non-seismic data in the algorithms that will deliver mass, age and other
characteristics of host stars, including full documentation.
Milestones:
12/2024: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms and update stellar models and procedure
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Improve scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Acceptable. The efficiency of including the non-seismic information in the algorithms to determine the
characteristics of host stars depends on the quality of the non-seismic data available during this phase.
PSM WPDs
OPERATIONS
Seismic Parameters
Leader: Christoffer Karoff
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 102/190
PSM WP 125 300
Operations phase
01/2024 — 03/2030
Institution: Aarhus University (Denmark)
Key Personnel: C. Karoff
Objectives:
Based on procedures from WP 125 100 and WP 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:
Interface between WP 125 000 and other WP such as seismic observables, including individual frequencies
(WP 124 000), and models (WP 121 000)
Input:
Procedures from WP 125 100 and WP 125 200
Dependencies:
This WP is part of WP 125 000
Output:
Updated scientific specifications of procedures and algorithms, including full documentation.
Milestones:
12/2024: Improvements of the procedures after tests with PLATO data. Delivery of first generation of optimized
procedures.
07/2025: Detailed tests of the benefit of including individual frequencies. Analysis of systematic errors in the
inferred stellar parameters.
12/2028: Delivery of second generation of optimized procedures.
Risks:
Acceptable risk
PSM WPDs
OPERATIONS
Open Clusters
Leader: Sarbani Basu
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 103/190
PSM WP 125 400
Operations phase
01/2024 — 03/2030
Institution: Yale University (USA)
Key Personnel: S. Basu
Objectives:
Based on procedures from WP 125 100 and WP 125 200, and using input from WP 125 300, validate the
procedures put in place 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 included for full statistical analysis, allowing determination of error properties of the inferred
quantities to be tested.
Tasks:
1. Validation that the pipeline involved in determining the basic properties of cluster stars from seismic and
non-seismic data works with PLATO data.
2. Determining if new algorithms will be needed, and if so implement them.
3. Determine cluster properties from the properties of the cluster members.
Input:
Procedures from WP 125 100 and WP 125 200
Dependencies:
Input from WP 125 100, WP 125 200 and WP 125 300
Output:
Validated code. Better statistical analyses.
Deliverables:
Improved codes. Initial results
Milestones:
12/2024: Improvements of the procedures and algorithms after tests with PLATO data; Determining tentative
cluster properties with first sets of PLATO data.
07/2025: Improve estimated based on parallel developments in the physical description of stellar models.
12/2028: Delivery of validated models of the clusters.
Risks:
Acceptable risks of delivering the final cluster properties if stellar models are improved significantly in the
meantime.
PSM WPDs
OPERATIONS
Mode Physics
Leader: Kevin Belkacem
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 104/190
PSM WP 126 000
Operations phase
01/2024 — 03/2030
Institution: LESIA, Observatoire de Paris (France)
Key Personnel: K. Belkacem; F. Baudin (IAS)
Objectives:
The mode physics sub-working groups will be designed to converge toward realistic determination of mode
amplitudes and line-widths. The objectives are to provide realistic stellar light-curves, for internal use in 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.
Coordination of the works of the work packages WP 126 100 to WP 126 400.
Tasks:
1. Coordination of the validation work that consists in checking that the procedures to derive mode
amplitudes and line-width that we specified during the development phase are fully adapted and run
properly with the data provided by PLATO
2. Coordination of the validation work that consists in checking that the procedures to correct mode
frequencies from surface and magnetic effects are fully adapted and run properly with the data provided
by PLATO
3. Improvements of the methods to correct mode frequencies from surface and magnetic effects.
Input:
PLATO data
Dependencies:
Input from and output from PLATO End-to-End Simulator and PSM (WP 126 100 to WP 126 400)
Output :
Updated scientific specifications of procedures and algorithms
Deliverables:
Reports and algorithms
Milestones:
06/2025: Improvements of the procedures and algorithms after tests with PLATO data
03/2029: Delivery of third generation of procedures and algorithms, validated using PLATO data
Risks:
Acceptable risks of delay
PSM WPDs
OPERATIONS
Mode Amplitude and Near-Surface Effects on Mode
Parameters
Leader: R. Samadi
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 105/190
PSM WP 126 100
01/2024 — 03/2030
Institution: LESIA, Observatoire de Paris (France)
Key Personnel: R. Samadi; K. Belkacem (LESIA, Paris); H.-G. Ludwig (Heidelberg); L. Bigot (Nice); E. Caffau
(GEPI, Paris)
Objectives:
1. Comparison between amplitudes of solar-type oscillations measured by PLATO and those derived from
the models developed during the development phase;
2. Improvements of the modelling of the mode amplitudes;
3. Test modelling of the near-surface effects using PLATO observations;
4. Improvements of the modelling of the near-surface effects
Tasks:
1. Extend the grid of models computed during the development phase;
2. Comparison of the preliminary releases of PLATO seismic data with models developed during the
development phase;
3. Interpretation of the observed differences and improvement of the models;
4. Compute mode frequencies (using the first generation of PLATO stellar models) and apply the near surface models developed during the implementation phase;
5. Interpretation of the observed differences and improvement of the modelling of the near-surface effects.
Input:
Seismic data: mode frequencies, mode line-widths and mode heights (WP 370)
Dependencies:
PDC (WP 370)
Output:
Second generation of models of mode driving and near surface effects.
Deliverables:
Full grid of stellar models of mode driving and near surface effects. Reports of WP activity.
Milestones:
12/2026: Extend of the grid of models and preliminary comparison with the first releases of PLATO data
12/2027: Comparison between consolidated PLATO observations and model predictions
07/2028: Model improvements
Risks: acceptable risks
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 106/190
Mode Line-Width
Leader: Marc-Antoine Dupret
Rev.: 5
PSM WP 126 200
Operations phase
01/2024 — 03/2030
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. Computation of mode-linewidths with the new code obtained in the development phase, over the grid of
stellar models computed in WP 121 000
2. Validation of the previous mode line-width modelling using first PLATO data
3. Improvement of time-dependent convection models
4. New line-widths computations
Input:
-
Non-radial non-adiabatic oscillation code MAD
3D simulations of convection (WP 122 100 and WP 123 200)
Grid of stellar models computed in WP 121 000
First PLATO data
Dependencies:
WP 126 000, WP 122 100, WP 123 200 and WP 121 000
Output:
Second generation grid of mode line-widths and time-dependent convection model
Deliverables:
Validated mode line-width model.
Milestones:
12/2024: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms and update stellar models and procedure
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Improve scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks: Minimal risk
PSM WPDs
OPERATIONS
Intensity-Velocity Relation
Leader: Günter Houdek
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 107/190
PSM WP 126 300
01/2024 — 03/2030
Institution: Aarhus University (Denmark)
Key Personnel: G. Houdek
Objectives:
Coordination of the work packages WP 126 300.
Tasks:
1. Coordination of the workload consisting of testing procedures for computing stellar models and nonadiabatic pulsation eigenfunctions for the data sets provided by PLATO.
2. Coordination of the work for deriving specifications of new procedures and algorithms for seismic
diagnoses as required for processing the PLATO data.
3. Coordination of the work (stellar and pulsation modelling, asteroseismic diagnoses) of data collected
from PLATO host stars.
Input:
PLATO data.
Dependencies:
Input and output from PDC (WP 370) and PSM (WP 100, WP130, WP160); PLATO End-to-End Simulator.
Output:
Updated scientific specifications of the procedures and algorithms for modelling and describing pulsation
properties.
Deliverables:
Report and procedures.
Milestones:
12/2024: Improvements of the procedures and algorithms after tests with PLATO data seismology and stellar
modeling on first sets of PLATO data
07/2025: Theoretical developments to improve the physical description of stellar models based on our improved
knowledge of stellar physics
12/2028: Delivery of third generation of validated models and procedures related to the characterization of host
stars
Risks:
rd
Acceptable risks of delay for delivering improved (3 generation) stellar models.
PSM WPDs
OPERATIONS
Seismology of Magnetic Activity
Leader: Laurent Gizon
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 108/190
PSM WP 126 400
01/2024 — 03/2030
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, using a code that computes the interaction of seismic waves with surface magnetic activity (starspots and
active regions). Application of 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. Maintain 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.
2. Maintenance of development system
3. Characterization and parameterization of magnetic effects on oscillations
4. Application of methods to clean frequencies from magnetic effects
5. Application of methods to infer the magnetic field from stellar-cycle variations in mode frequencies
Note: These methods will preferentially be applied to Sun-like stars hosting planets.
Input:
1. Scientific literature
2. MHD pulsation code from development phase
3. PLATO seismic analyses of Sun-like stars with planets
4.
Dependencies:
WP 126 000, WP 123 000, WP 123 100, WP 123 400, WP 372 220
Output:
Completion of tasks 1 to 5
Deliverables:
Reports, operational development system, operational MHD pulsation code, methods to correct mode
frequencies and infer stellar magnetic activity levels
Milestones:
06/2025: Improvements of the procedures and algorithms after tests with PLATO data.
03/2029: Delivery of third generation of procedures and algorithms, validated using PLATO data
Risks: Acceptable risks
PSM WPDs
OPERATIONS
Seismic Constraints From Aging Stars
Leader: Benoît Mosser
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 109/190
PSM WP 127 000
Operations phase
01/2024 — 03/2030
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:
Validation of red giant models and of the seismic tools designed to derive masses, radius evolutionary state and
chemical composition required by the WP dedicated to exoplanets around red giant stars.
Validation of stellar evolution models for constraining the properties of main-sequence stars according to the
observation of more evolved stars.
Coordination with the activities under WP 121 (stellar models), WP 123 (stellar activity), WP 122 (non-seismic
diagnostics).
Tasks:
1. Coordination of the work done by WP 127 100-300, WP 121, WP 122, WP 128
2. Use PLATO data to define the improvements in the physics to be included in evolutionary stellar models
3. Test that the quality of the outputs from WP 127 100-300, 121, and 122 match the specified
requirements
4. Establish procedures for utilizing the asteroseismic insights obtained through the analysis of PLATO
data to improve the determination of stellar parameters.
Input:
PLATO data
Dependencies:
From WP 127 100-300, WP 122, 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:
06/2025: End of first scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation validated algorithms and updated procedures.
Risks:
Minimal risks, owing to the experience gained with precursors (CoRoT, Kepler)
PSM WPDs
OPERATIONS
Stellar Models of Evolved Stars
Leader: Paolo Ventura
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 110/190
PSM WP 127 100
01/2024 — 03/2030
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:
Validate and refine grids of high quality 1D stellar models for low/intermediate mass in the phases of red giant
branch (RGB) and core He-burning (He-B). The initial set of stellar parameters and the precision will be updated
if required by the exoplanet transit detection in the framework of PLATO.
Tasks:
1. Keeping updating the physical description of low/intermediate mass stellar models in dedicated
evolutionary code
2. Use PLATO data to test the physics included in theoretical stellar models, and define the improvements
to be included in new generation of models
3. Implement in the stellar evolution code the improvements in the physics that will be provided by WP 121
200, 121 300, 121 500 and 122 000.
4. If necessary, extension of the physical parameter domain considered in the first release of the grid.
Input:
1. Relevant data concerning some physical inputs: Equation of State, conductive opacity, nuclear reaction
rates; boundary conditions from atmosphere models (WP 122 000)
2. Evolutionary code and numerical tools for extracting the structural and evolutionary properties of the
various stellar models.
3. Inputs from current works on standard and non-standard transport processes.
4.
Dependencies:
WP 127 and WP 121
Output:
Improved and validated grids of 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:
12/2024: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms and update stellar models and procedure
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Improve scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks:
Acceptable risks for the delay in the implementation of the algorithms for transport processes
PSM WPDs
OPERATIONS
Seismic Diagnostics for Evolved Stars
Leader: Andrea Miglio
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 111/190
PSM WP 127 200
01/2024 — 03/2030
Institution: University of Birmingham (UK)
Key Personnel: A. Miglio; S. Deheuvels (OMP, IRAP); M.-A. Dupret (Liège); P. Eggenberger (Geneva);
V. Silva Aguirre (Aarhus); J. Montalban (INAF-Padova)
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.
Tasks:
1. Compute adiabatic oscillation frequencies as updated/improved models are provided by WP 127 100
2. Check that the procedures to derive stellar characteristics (mass, radius, age) are fully adapted to the
data provided by PLATO
Input:
Grids of stellar models (from WP 127 100), seismic average parameters and oscillation frequencies from WP
372 100 and WP 372 250, non-seismic constraints from WP 130.
Dependencies:
Input from WP 127 100, WP 372 100, WP 372 250, WP 130 000
Output:
Updated, 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:
12/2024: Finish first scientific validation of algorithms and tools with real PLATO data
Until 2030: Continue validation of algorithms and update stellar models and procedure
Scientific validation of implementation at PDC will be performed as part of the PDC review process.
Improve scientific specifications according to prior validation results in phase with PDC implementation cycle.
Risks: Minimal risks
PSM WPDs
OPERATIONS
Constraints on Main-Sequence Stars
Leader: Josefina Montalban
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 112/190
PSM WP 127 300
Operations phase
01/2024 — 03/2030
Institution: University of Padova (Italy)
Key Personnel J. Montalban; A. Miglio (Birmingham); S. Deheuvels (OMP, IRAP); M.-A. Dupret (Liège);
P. Eggenberger (Geneva); V. Silva Aguirre (Aarhus); L. Girardi (INAF-Padova); A. Bressan (INAF-Padova);
Y. Lebreton (GEPI, Paris); S. Cassisi (INAF-Teramo); A. Palacios (Montpellier)
Objectives: Deriving constraints on main-sequence stars hosting planets from the comprehensive study of the
observations of stellar populations including all evolutionary stages
Tasks:
1. Use adiabatic oscillation frequencies as updated/improved models are provided by WP 127 100
2. Check seismic diagnostic tools all along stellar evolution
3. Check that the procedures to derive stellar characteristics (mass, radius, age) are fully adapted to the
data provided by PLATO
Input:
Oscillation frequencies of stellar models (from WP 127 200), seismic average parameters and oscillation
frequencies from WP 372 100 and WP 372 250, non-seismic constraints from WP 130.
Dependencies:
Input from WP 127 100, WP 372 100, WP 372 250, WP 130 000
Output:
Updated, 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:
06/2025: End of first scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation validated algorithms and updated procedures.
Risks: Minimal risks
PSM WPDs
OPERATIONS
Power Spectrum Fitting Tools
Leader: Bill Chaplin
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 113/190
PSM WP 128 000
01/2024 — 03/2030
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:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 000 is part of the Stellar Science work package
Output:
Updates to the recommended procedures
Deliverables:
Updates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: None
PSM WPDs
OPERATIONS
Average Seismic Parameters
Leader: Rafael A. García
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 114/190
PSM WP 128 100
Operations phase
01/2024 — 03/2030
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 solar-like
oscillators
Tasks:
1.
Validation of procedures from results on early PLATO data
2.
Review of necessary or desirable updates to the procedures
3.
Development and full specifications for any updates needed to the procedures
Input:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 100 is part of the Stellar Science work package
Output:
Any necessary updates to the recommended procedures
Deliverables:
Updates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data
03/2029: Third generation of validated algorithms and updated procedures
Risks: none
PSM WPDs
OPERATIONS
Mode Fitting Tools
Leader: Bill Chaplin
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 115/190
PSM WP 128 200
Operations phase
01/2024 — 03/2030
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 peak-bagging,
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:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 200 is part of the Stellar Science work package.
Output:
Any necessary updates to the recommended procedures
Deliverables:
Updates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: none
PSM WPDs
OPERATIONS
Solar-Like Stars
Leader: Bill Chaplin
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 116/190
PSM WP 128 210
Operations phase
01/2024 — 03/2030
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. Validation of procedures from results on early PLATO data
2. Review of necessary or desirable updates to the procedures
3. Development and full specifications for any updates needed to the procedures
Input:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 210 is part of the Stellar Science work package
Output:
Any necessary updates to the recommended procedures
Deliverables:
Updates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: none
PSM WPDs
OPERATIONS
Solar-Like Stars with Planets
Leader: Tiago Campante
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 117/190
PSM WP 128 220
Operations phase
01/2024 — 03/2030
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. Validation of procedures from results on early PLATO data
2. Review of necessary or desirable updates to the procedures
3. Development and full specifications for any updates needed to the procedures
Input:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 220 is part of the Stellar Science work package
Output:
Any necessary updates to the recommended procedures
Deliverables:
Updates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: None
PSM WPDs
OPERATIONS
Multiple Stars
Leader: Guy Davies
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 118/190
PSM WP 128 230
Operations phase
01/2024 — 03/2030
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. Validation of procedures from results on early PLATO data
2. Review of necessary or desirable updates to the procedures
3. Development and full specifications for any updates needed to the procedures
Input:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 230 is part of the Stellar Science work package
Output:
Any necessary updates to the recommended procedures
Deliverables:
Updates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: None
PSM WPDs
OPERATIONS
Ensemble Fit
Leader: Jerôme Ballot
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 119/190
PSM WP 128 240
Operations phase
01/2024 — 03/2030
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. Validation of procedures from results on early PLATO data
2. Review of necessary or desirable updates to the procedures
3. Development and full specifications for any updates needed to the procedures
Input:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 240 is part of the Stellar Science work package
Output:
Any necessary updates to the recommended procedures
Deliverables:
Updates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: None
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 120/190
Fitting Tools for Evolved Stars
Leader: Saskia Hekker
Rev.: 5
Operations phase
PSM WP 128 250
01/2024 — 03/2030
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. Validation of procedures from results on early PLATO data
2. Review of necessary or desirable updates to the procedures
3. Define and test full specifications for any updates needed to the procedures
Input:
Results on real PLATO data from application of procedures in the PDC
Dependencies:
WP 128 250 is part of the Stellar Science work package
Output:
Any necessary updates to the recommended procedures
Deliverables:
pdates and reports on operation of procedures on real PLATO data
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data.
03/2029: Third generation of validated algorithms and updated procedures.
Risks: None
PSM WPDs
OPERATIONS
Interfaces
Leader: Frédéric Baudin
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 121/190
PSM WP 129 000
Operations phase
01/2024 — 03/2030
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 activities of the WP 120.
Tasks:
1. Ensure updates to the tools and algorithms are properly validated and transmitted to PDC
2. Interface for outreach activities of WP 120: fulfilling demands of general PLATO outreach activities and
proposing outreach material based on WP 120 activities
Input:
Updated models, prototyped algorithms and tools from WP 120 XXX (to be transmitted to PDC), potential
outreach material
Dependencies:
None
Output:
Validated updated specifications to be transmitted to PDC, outreach material ready to be included in PLATO
general outreach activities
Deliverables:
Reports and proposed validations of updated algorithms and tools
Milestones:
06/2025: End of scientific validation of algorithms and tools with real PLATO data
03/2029: Third generation of validated algorithms and updated procedures
Risks: None
PSM WPDs
OPERATIONS
Target / Field Characterization and Selection
Leader: Giampaolo Piotto
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 122/190
PSM WP 130 000
01/2024 — 03/2030
Institution: Università di Padova (Italy)
Key Personnel: G. Piotto; 1 postdoc
Objectives:
Coordinate all the WPs to deliver the PLATO input catalogue with all relevant parameters for each target.
Tasks:
1. Refinement of first field PIC content
2. Refinement of all PLATO fields coordinates
3. Refinement of the criteria for identification, selection and prioritization of the all field targets and
corresponding parameters, also on the basis of the actual PLATO collected data and experience
4. Provide the criteria for contaminant list and properties selection
5. Provide target false alarm probability
Input:
All catalogues/parameters gathered by WP 131 000 and WP 132 000
Dependencies:
Output of WP 131 000, 132 000
Output:
Final list of targets/parameters of the PLATO input catalogue
Deliverables:
Final catalogue of PLATO targets
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
None
PSM WPDs
OPERATIONS
Project Office Assistant
Leader: Valentina Granata
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 123/190
PSM WP 130 100
01/2024 — 03/2030
Institution: Università di Padova (Italy)
Key Personnel: V. Granata
Objectives:
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 meeting 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:
Preparation of all PIC Documents
Deliverables:
Meeting / teleconference minutes, WP Documents
Milestones:
L+6m: Preparation of documents for refined PIC for the first PLATO field
L+96m: Preparation of documents for validation of the PIC for all PLATO fields (in due time for the delivery of
PIC to SOC)
Risks:
None
PSM WPDs
OPERATIONS
Catalogues Analysis
Leader: Valerio Nascimbeni
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 124/190
PSM WP 131 000
Operations phase
01/2024 — 03/2030
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. The task
continues during the operational phase because of the need of updating the PIC content following the schedule
of Gaia releases and the scheduling of PLATO observations beyond the first run.
Tasks:
1. Update the list of parameters to be collected (in particular using the intermediate Gaia releases)
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:
Updated 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+6m: Updated criteria for the characterization of the first PLATO field and preliminary criteria for the other
fields
L+96m: Updated 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
OPERATIONS
Gaia Catalogue Analysis
Leader: Alessandro Sozzetti
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 125/190
PSM WP 131 100
01/2024 — 03/2030
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 with WP 133 200 for the purpose of continuously refining and finalizing the set of data
products requirements ahead of the publication of the Gaia 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 refined assessments of nearby dwarf targets based on the new Gaia early release catalogue.
Detailed parameterization of potential targets criteria for PIC
Milestones:
L-End-to-end: Further refinements to parameterization of potential PLATO targets criteria based on Gaia final
catalogue release, if applicable.
Risks:
Unavailability of the necessary catalogue parameters from Gaia astrometry, photometry and spectroscopy at
the level of early data releases and final catalogue - MINIMAL
PSM WPDs
OPERATIONS
PLATO-Gaia Simulations
Leader: Holger Voss
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 126/190
PSM WP 131 150
01/2024 — 03/2030
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 final Gaia catalogue, b) to simulate PLATO targets
from Gaia catalogues, and c) to become a tool to refine the selection of PLATO target fields.
Tasks:
1. Update transformations from Gaia photometry to PLATO photometry for the sources in the Gaia
catalogue based on the knowledge about the PLATO instrument after launch and during the operations.
2. Implement error models in GOG according to the final Gaia catalogue
3. Provide tools to evaluate the contribution of faint Gaia sources to the background level of the pixel
4. Update GOG to become a simulations tool provider for WP 131 110, WP 131 120, WP 131 130 and WP
131 140 in operations phase.
5. Compile additional data (ground based or space based) that may be needed to provide simulations for
PLATO.
Input:
Gaia final catalogue: astrometric, photometric and spectroscopic data
Gaia DPAC GOG tool for simulation
PLATO instrument characterisation (passband, sensitivity, QE and pixel sizes in particular) kept updated
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:
2024: Updated error model from the Gaia final release (astrometry, photometry, spectroscopy, stellar
parameters) and possible extensions of Gaia mission.
2025 - Updated GOG to simulate PLATO output data based on PLATO real observations in early operational
phases (commissioning).
Risks: None
PSM WPDs
OPERATIONS
Other Large Catalogues Analysis
Leader: Ricardo Claudi
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 127/190
PSM WP 131 200
01/2024 — 03/2030
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 specify 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:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
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
PSM WPDs
OPERATIONS
Photometric and Astrometric Catalogues
Leader: Valerio Nascimbeni
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 128/190
PSM WP 131 210
Operations phase
01/2024 — 03/2030
Institution: INAF-OAPD (Italy)
Key Personnel: V Nascimbeni; G. Piotto (Padova); S. Ortolani (Padova); 1 postdoc
Objectives:
Optimal extraction of the stellar parameters for the candidate targets in the PLATO Stellar Samples 1, 2, 3, 5
within the PLATO fields selected by WP 132 200, from the analysis of photometric and astrometric catalogues
Tasks:
1. Use the classification technique(s) chosen during the Definition Phase to determine stellar parameters
within the selected PLATO fields
2. Include photometric/astrometric data coming from new surveys which will have become available, and
re-assess the reliability (completeness and contamination level) of the output data
3. Implement software tools to provide a single, homogeneous final database of stellar parameters to WP
132 300 and WP 132 400. Cross-check targets from Gaia (WP 131 100)
Input:
1. Existing and forthcoming photometric/astrometric catalogues
2. PLATO fields selected by WP 132 200
Dependencies:
Selected PLATO fields from WP 132 000
Output:
Database of stellar parameters with reliability diagnostics for candidate targets within PLATO Stellar Samples
1, 2, 3, 5.
Deliverables:
Document with the assessment of the reliability of the extracted stellar parameters, along with a detailed
description of the technique(s) and tools used to derive stellar classification
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Available data could not be sufficient to extract the candidate list for all the Stellar Sample with the required
level of reliability. In particular, the Stellar Sample 5 (mV<11) is the most critical one. The opportunity of a
dedicated ground-based survey would be considered
PSM WPDs
OPERATIONS
M-Dwarfs
Leader: Loredana Prisinzano
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 129/190
PSM WP 131 220
Operations phase
01/2024 — 03/2030
Institution: INAF - Osservatorio Astronomico di Palermo (Italy)
Key Personnel: L. Prisinzano; L. Affer (INAF-Palermo); G. Micela (INAF-Palermo)
Objectives:
Extraction of the M-dwarf targets to be observed in the second PLATO long-duration field and in the step &
stare fields by using the latest release of the Gaia catalogue
Tasks:
1. Use of the latest available release of the Gaia catalogue to check both the luminosity class and the
spectral type of M-dwarf targets selected during the development phase
2. Provide a single, homogeneous final catalogue of M-dwarfs to be observed by PLATO
Input:
1. Output catalogue from the WP 131 220 development phase
2. PLATO fields selected by WP 132 200
3. Most recent Gaia release.
Dependencies:
Selected PLATO fields from WP 132 200
Output:
Catalogue of M-dwarf candidate targets to be used for the PLATO Stellar Sample 4 in the second PLATO longduration field and for the step & stare fields
Deliverables:
Report with description and discussion of the criteria used to classify the candidates for the PLATO Stellar
Sample 4, based on the latest Gaia catalogue
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Available data could be contaminated by reddened early type stars and/or giants and/or pre-main sequence
objects in case of time delay in the release of the Gaia results.
PSM WPDs
OPERATIONS
M-Dwarfs as Planet Hosts
Leader: Peter Wheatley
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 130/190
PSM WP 131 221
01/2024 — 03/2030
Institution: University of Warwick (UK)
Key Personnel: P. Wheatley
Objectives:
Apply models of the P4 sample of M-dwarfs developed during the implementation phase to plan for P4 sample
during the step-and-stare phase of the mission. The P4 targets are faint, but provide the primary opportunity to
discover habitable planets during the step-and-stare phase (because habitable planets around M-dwarfs will
have short orbital periods). This work package addresses issues of targeting, analysis and follow up that are
unique to the P4 sample, due to the faintness, red spectrum and variability characteristics of the host stars. The
P4 sample detectable against jitter noise will be simulated for each of the step and stare fields, in order to
determine the numbers and magnitude distributions of faint targets, the likely planet catch, and to ensure that
adequate and appropriate follow-up resources are allocated to the confirmation of this small-planet sample
(with priority given to 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 P4 sample in each step and stare field, accounting for M-dwarf spectra and jitter noise.
3. Simulations of likely planet catch and magnitude distribution of M-star planet hosts.
4. Assessment of P4 variability characteristics.
5. Feedback on P4 selection criteria from WP 131 220.
6. Analysis of follow-up resources needed to confirm terrestrial planets around M-star sample.
Input:
Scientific Literature; P4 simulations developed during implementation phase; criteria for P4 target selection
from WP 131 220.
Dependencies:
P4 simulations developed during implementation phase; criteria for P4 target selection from WP 131 220.
Output:
An understanding of the P4 M-dwarf sample in the step and stare fields, including the impact of stellar activity
and variability; feedback on target selection criteria from 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:
06/2023: Delivery of final report on activity
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
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
OPERATIONS
Stellar Activity
Leader: Isabella Pagano
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 131/190
PSM WP 131 230
Operations phase
01/2024 — 03/2030
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 and update the catalogue
with new data from the literature
Tasks:
1. Extraction of data on stellar activity from the literature according to what defined during the definition
phase
2. Acquisition and reduction of new data on activity level for the targets not already characterized
3. Production of the catalogue to be ingested by the PDC
4. 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:
1. A catalogue of data useful to assess the activity level of the PLATO candidate targets
2. Updated release of the catalogue after its first release
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Acceptable risk
PSM WPDs
OPERATIONS
Binary Systems
Leader: Silvano Desidera
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 132/190
PSM WP 131 240
Operations phase
01/2024 — 03/2030
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 on individual targets from WP 131 000
Dependencies:
Input from WP 132 000, interface with WP 350 000 and WP 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:
L+96m: identify required information for PLATO Step & Stare fields
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)
PSM WPDs
OPERATIONS
Known and Candidate Exoplanets
Leader: Serena Benatti
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 133/190
PSM WP 131 260
01/2024 — 03/2030
Institution: INAF-Osservatorio Astronomico 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
- PLATO Planets candidate
Dependencies:
None
Output:
Catalogue of known and candidate planets
Deliverables:
- Software Tools
- Reports
- Catalogue
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
Risks:
Minimal
PSM WPDs
OPERATIONS
Single Target Additional Data
Leader: Isabelle Boisse
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 134/190
PSM WP 131 300
01/2024 — 03/2030
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 WP
2. Validate regular updates of the catalogue
Tasks:
Gather the outputs from WP 131 310, WP 131 320, WP 131 330
1. Update the catalogue of stellar parameters derived from spectroscopic or imaging data analysis
2. Check compliance of the catalogue with the specifications
3. Validate 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+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Minimal risks
PSM WPDs
OPERATIONS
High Resolution and Deep Imaging
Leader: Arthur Vigan
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 135/190
PSM WP 131 310
Operations phase
01/2024 — 03/2030
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: A. Vigan; I. Boisse (LAM); F. Bouchy (IAP/OHP); M. Deleuil (LAM)
Objectives:
1. Update the imaging catalogue for individual stars
2. Validate the updates
Tasks:
1. Check results from new HR imaging observations that might be of interest for PLATO and prepare
updates of the catalogue
2. Check compliance of the updates with the specifications
3. Validate regular updates
Input:
Catalogues from various observatory archives and/or scientific publications
Dependencies:
WP 131 300
Output:
Catalogue of stars observed by imaging facility with their characteristics (observatory, instrument, resolution,
wavelength range, etc.) and the derived parameters, including those of close contaminants to be provided to
WP 131 000
Deliverables:
Catalogue of stars observed by imaging facility with their characteristics (observatory, instrument, resolution,
wavelength range, etc.) and the derived parameters, including those of close contaminants
Milestones:
Post launch: Continuing refinements of the catalogues
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Spectroscopic Data
Leader: Isabelle Boisse
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 136/190
PSM WP 131 320
Operations phase
01/2024 — 03/2030
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: I. Boisse
Objectives:
1. Update the spectroscopic catalogue for individual stars
2. Validate the update
Tasks:
1. Gather new spectra from ground-based facilities archives
2. Update the 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 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:
Post launch Continuing refinements of the catalogues
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Preparatory Observations
Leader: Klaus G. Strassmeier
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 137/190
PSM WP 131 330
01/2024 — 03/2030
Institution: AIP (Germany)
Key Personnel: K.G. Strassmeier, T. Granzer (AIP); J. Bartus (Konkoly); E. Depagne (AIP); I. Di Varano
(AIP); G. Bihain (AIP); N.N.
Objectives:
Provide a stellar-variability survey for the PLATO short–pointing fields
Tasks:
1. Carry out a time-series photometric survey for the short-cadence PLATO fields.
2. Apply either a smaller cadence compared to the long-duration fields or cover only the central PLATO
field of view (e.g. the field with all cameras) but aim for two proposed fields per year. tbd
Input:
Need to know the exact location of the fields
Dependencies:
WP 132 000
Output:
A time-series of 200 CCD pointings of the full 2,300-sqrd PLATO FOV per 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: (as for the long-duration fields)
1. Provide seasonal-long light curves of all targets between 8th-17th magnitude within the short-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. 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). It will allow a statistical separation of dwarfs from giants and a crude
separation of early-type from late-type stars.
Milestones:
2024: Start of survey in the northern hemisphere.
2028: Start of survey in the southern hemisphere.
Risks:
None.
PSM WPDs
OPERATIONS
K2 Data
Leader: Magali Deleuil
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 138/190
PSM WP 131 400
Operations phase
01/2024 — 03/2030
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: M. Deleuil; I. Boisse (LAM); F. Bouchy (IAP/OHP); A. Vigan (LAM); Don Pollacco (Warwick)
Objectives:
1. Update the catalogue for individual stars and planets observed with K2
2. Validate the update
Tasks:
1. Check for new results from publications of K2 observations and update accordingly the catalogue for
individual stars and planets observed
2. Check compliance of the updates with the specifications
3. Validate regular updates
Input:
Catalogues from NASA archives and/or scientific publications
Dependencies:
WP 131 000
Output:
Updates of the 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:
Updates of the 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:
Post launch: deliver refinements of the catalogue
Risks:
No risks identified
PSM WPDs
OPERATIONS
TESS Data
Leader: Magali Deleuil
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 139/190
PSM WP 131 500
Operations phase
01/2024 — 03/2030
Institution: Laboratoire d’Astrophysique de Marseille (France)
Key Personnel: M. Deleuil; I. Boisse (LAM); F. Bouchy (IAP/OHP); A. Vigan (LAM); Don Pollacco (Warwick)
Objectives:
1. Update the catalogue for individual stars and planets observed by TESS
2. Validate the updates
Tasks:
1. Check for new results from publications of TESS and update accordingly the catalogue for individual
stars and planets
2. Check compliance of updates with the specifications
3. Validate regular updates
Input:
Catalogues from NASA archives and/or scientific publications
Dependencies:
WP 131 000
Output:
Update of the 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:
Updates of the 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:
Post launch: deliver refinements of the catalogues
Risks:
No risks identified
PSM WPDs
OPERATIONS
Contaminant Analysis
Leader: Ulrich Kolb
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 140/190
PSM WP 131 600
Operations phase
01/2024 — 03/2030
Institution: The Open University (UK)
Key Personnel: U. Kolb
Objectives:
Explore contaminant information of PLATO targets in new surveys (LSST)
Tasks:
Only WP 131 630 is envisaged to contribute in this phase. The Coordination and management of the package.
Input:
WP 131 630
Dependencies:
None
Output:
Enhanced assessment of contaminant information in Gaia and other pertinent catalogues.
Deliverables:
Assimilate information in contaminant modeller
Milestones:
WP 131 630 milestones
Risks:
None
PSM WPDs
OPERATIONS
Contaminant Analysis From Other Catalogues
Leader: Valerio Nascimbeni
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 141/190
PSM WP 131 630
01/2024 — 03/2030
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni; S. Hodgkin (IoA); U. Kolb (OU)
Objectives:
Define algorithms to supply contaminant information from new pertinent surveys (LSST)
Tasks:
1. Develop procedure for contaminant extraction from respective catalogues
2. Provide calibrator for contaminant modeller
Input:
Dependencies:
WP 132 300
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 new surveys (LSST)
Milestones:
Driven by LSST timetable.
Risks:
Acceptable risk.
Rev.: 5
PSM WPDs
OPERATIONS
Field and Target Selection
Leader: Ricardo Claudi
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 142/190
PSM WP 132 000
01/2024 — 03/2030
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, other than the first
2. Select criteria for PLATO targets and deliver them
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 criteria and prioritisation
Deliverables:
PIC and PLATO fields
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Field Selection
Leader: Sergio Ortolani
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 143/190
PSM WP 132 100
Operations phase
01/2024 — 03/2030
Institution: Università di Padova (Italy)
Key Personnel: S. Ortolani; G. Piotto (Padova); V. Nascimbeni (INAF-Padova); C. Afonso
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:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Acceptable risk
PSM WPDs
OPERATIONS
Target Selection and Prioritisation
Leader: Valentina Granata
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 144/190
PSM WP 132 200
01/2024 — 03/2030
Institution: Università di Padova (Italy)
Key Personnel: V. Granata
Objectives:
Deliver all relevant criteria and parameters for each target 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 target parameters into PIC
and for target criteria for selection from extended PLATO catalogue
4. Select criteria for PLATO targets and deliver them
5. Estimate completeness/contamination of the selected targets
6. Provide stellar parameters criteria for selection
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 list of criteria for all targets/parameters for the PLATO input catalogue
Deliverables:
Final criteria and prioritisation of all PLATO targets
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Depends on Gaia output; in case of delay or failure from Gaia the catalogue will rely on available
photometric/astrometric catalogues, including some current ongoing wide field surveys.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 145/190
PLATO Field Contaminants
Leader: Ulrich Kolb
Rev.: 5
Operations phase
PSM WP 132 300
01/2024 — 03/2030
Institution: The Open University (UK)
Key Personnel: U. Kolb
Objectives:
Rolling improvement of false positive estimate algorithm in view of new survey output (such as LSST) and
emerging PLATO data.
Tasks:
Coordination and management of the package.
Input:
WP 131 600, WP 113 000, WP 111 000
Dependencies:
A close liaison with WP 113 000 and WP 111 000 and relevant sub-WPs is required
Output:
Improved false positive probability tool for catalogue sources, to generate improved contaminant information for
each source.
Deliverables:
Improved code to obtain contaminant assessment on a source-by-source basis
Milestones: Rolling programme
Risks:
Minimal risks
PSM WPDs
OPERATIONS
False Alarm Probability
Leader: Alexandre Santerne
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 146/190
PSM WP 132 320
Operations phase
01/2024 — 03/2030
Institution: University of Porto
Key Personnel: A. Santerne; U. Kolb (OU)
Objectives:
Improve calculation of individual false positive probabilities, taking into account both observed contaminant
properties and theoretical models of the physical nature of contaminants.
Tasks:
1. Assimilate new catalogue information
2. Assimilate new model information
3. Update PLATO-PASTIS code
Input:
WP 131 600, WP 113 000, WP 111 000
Dependencies:
None
Output:
Improved algorithm for calculating the false positive probability prior to the availability of PLATO data.
Deliverables:
Improved code
Milestones:
Rolling programme, driven by analysis of completed PLATO fields.
Risks:
None.
PSM WPDs
OPERATIONS
Interface to Other PSM WPs and PDC
Leader: Silvano. Desidera
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 147/190
PSM WP 133 000
Operations phase
01/2024 — 03/2030
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 WPs
Tasks:
Coordinate WP 133 100, WP 133 200, WP 133 300, WP 133 400 and WP 133 500 work
Input:
Development Phase documentation
Dependencies:
Output of the WP 133 100, WP 133 200, WP 133 300, WP 133 400 and WP 133 500
Output:
Interface documentation
Deliverables:
Reports
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Acceptable risk
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 148/190
Interface to Other PSM WPs
Leader: Silvano Desidera
Rev.: 5
Operations phase
PSM WP 133 100
01/2024 — 03/2030
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 WPs
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:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Interface problems, efficiency losses
PSM WPDs
OPERATIONS
Interface to PDC
Leader: Valentina Granata
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 149/190
PSM WP 133 200
Operations phase
01/2024 — 03/2030
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:
Launch: Management of IRD / ICD
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Interface Gaia-PLATO
Leader: Nicholas Walton
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 150/190
PSM WP 133 300
Operations phase
01/2024 — 03/2030
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:
12/2028: Final delivery of interface document to WP 130.
Milestones:
06/2025: Proposal for selection of the step and stare PLATO fields
03/2026: Final catalogue of the second PLATO field
09/2027: Preliminary catalogues for the step and stare PLATO fields
09/2028: Refined catalogues for the step and stare PLATO fields
Risks:
This WP will comply with the PSM RMP.
PSM WPDs
OPERATIONS
Interface to PLATO CCD Image Simulator
Leader: Luca Borsato
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 151/190
PSM WP 133 400
01/2024 — 03/2030
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 (updates of the Simulator due to variations of the PLATO specs 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:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Interface problems, misinterpretation of the simulations and expected photometric quality
PSM WPDs
OPERATIONS
Interface to TOU
Leader: Riccardo Claudi
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 152/190
PSM WP 133 500
Operations phase
01/2024 — 03/2030
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 performance and calibration WP
Input:
Telescope Optical Unit (TOU) Calibration
Dependencies:
Performances of TOU
Output:
Refinement on Limit for target parameters
Deliverables:
Reports
Milestones:
L+6m: Refined PIC for the first PLATO field
L+96m: Validation of the PIC for all PLATO fields (in due time for the delivery of PIC to SOC)
L+96m Continuous refinement of PIC for all fields, building up on PLATO experience and accounting for the
performance changes
Risks:
Minimal Risk
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 153/190
Coordination of PLATO Follow-Up Observations
Leader: Stéphane Udry
Rev.: 5
Operations phase
PSM WP 140 000
01/2024 — 03/2030
Institution: Geneva University (Switzerland)
Key Personnel: S. Udry (Geneva); NN (Geneva)
Objectives:
Coordination of the follow-up observations of PLATO transit candidates.
Tasks:
1. Control that WP activities are progressing according to strategy and planning; facilitate horizontal
transfer of information; etc.
2. 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 performances)
Dependencies:
WP 100 000, WP 110 000, WP 120 000, WP 130 000, WP 14X XX0, WP 160 000.
Output:
WP’s coordination
Deliverables:
Report synthesizing the FU-activities at the end of each phase
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Shortage of observing facilities that would lower the follow-up efficiency and thus the scientific return of the
mission.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 154/190
Strategy and Operation Preparation
Leader: Don Pollacco
Rev.: 5
Operations phase
PSM WP 141 000
01/2024 — 03/2030
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 monitor aids to be used by observers for efficient assessment of observation quality. 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 tools to be used by observing assessing an observations 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:
01/2025: Critical examination of FU strategy
03/2025: Start of FU observations for first PLATO field
03/2028: Start of FU observations for second PLATO field
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
OPERATIONS
Target Distribution Requirements
Leader: Ignasi Ribas
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 155/190
PSM WP 141 100
Operations phase
01/2024 — 03/2030
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. GarcíaPiquer (ICE); J. Guàrdia (ICE); J. Sanz (ICE)
Objectives:
To monitor the application, efficiency and performance of the target distribution methodology to ensure optimal
PLATO target follow-up during operational phase. To reassess and report on the target distribution strategy, and
reactively implement any necessary procedural changes or improvement in response to feedback from
observers and/or facilities.
Tasks:
1. To maintain and oversee user support and effective target distribution to ground-based facilities –
thereby ensuring optimum efficiency.
2. To respond to observer/facility feedback during the operational phase (particularly during the early
phase in year 1), readjusting distribution methodology accordingly.
3. To monitor follow-up facility efficiencies during the operational phase, rerouting target distribution to
facilities taking into account any changing circumstances where appropriate.
Input:
1.
2.
3.
4.
Scientific literature.
PLATO Red book and current PLATO performance estimation.
Current follow-up facility performance and software manuals.
Current Target Distribution procedures and manuals.
Dependencies:
Exchange of information and coordination with all WP 140 packages and WP 115 100.
Output:
Continued adaptation, improvement and monitoring of Target Distribution to follow-up efficiencies. Appraisal of
Target Distribution performance, ensuring continued effectiveness and ability to respond to changing facilities
and capabilities.
Deliverables:
Reports on efficiency of current distribution techniques and updated procedures/software defining methodology
of object distribution in response to feedback during operational phase. Updated report on facility requirements
and efficiencies, including observational aids.
Milestones:
01/2025: Critical examination of FU strategy
03/2025: Start of FU observations for first PLATO field
03/2028: Start of FU observations for second PLATO field
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
OPERATIONS
Aids for Optimizing Photometric and Spectroscopic
Measurements
Leader: Josep Colomé
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 156/190
PSM WP 141 200
01/2024 — 03/2030
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. GarcíaPiquer (ICE); J. Guàrdia (ICE); J. Sanz (ICE)
Objectives:
Monitoring the performance of the PLATO observation aid set and to use feedback during the operational phase
to further develop them as required by observers.
Tasks:
1. To maintain the PLATO Observational aid set during the operational phase.
2. To respond to observers and facility requests to extend functionality.
3. Review performance of the PLATO observational aid set as reported by observers and facility operators.
Input:
1.
2.
3.
4.
Scientific literature and instrumentation manuals.
Current PLATO Observational Aid documentation
PLATO Red book and current PLATO performance estimation.
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:
Continued use of PLATO Observation aids that will enable the observer to make best use of telescope time and
assess the quality of the data obtained.
Deliverables:
Aids maintained and documentation kept up to date.
Milestones:
01/2026: Review of PLATO Observational aids performance after first year of operation.
Annual mini-reports on activity thereafter
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
OPERATIONS
Information Transfer
Leader: Francesc Vilardell
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 157/190
PSM WP 141 300
Operations phase
01/2024 — 03/2030
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. GarcíaPiquer (ICE); J. Guàrdia (ICE); J. Sanz (ICE)
Objectives:
Monitor the performance of the PLATO Observer Interface and feedback to ancillary database during the
operational phase. Develop this as required by observers and as experiences dictate.
Tasks:
1. To maintain the PLATO Observer Interface aid set during the operational phase
2. To respond to observers and facility requests to extend functionality
3. Review performance of the PLATO Observer Interface aid set as reported by observers and facility
operators
Input:
1.
2.
3.
4.
Scientific literature and instrumentation manuals
Current PLATO Observer Interface documentation
PLATO Red book and current PLATO performance estimation.
Current follow-up facility performance descriptions and software manual
Dependencies:
Exchange of information and coordination with all WP 140 packages along with the Ancillary Database WP 312
500.
Output:
Continued use and enhancement of the PLATO Observer Interface that will enable observers to make best use
of telescope time and assess the quality of the data obtained
Deliverables:
Observer Interface maintained and documentation kept up to date.
Milestones:
01/2026: Review of PLATO Observational aids performance after first year of operation.
Annual mini-reports on activity thereafter
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
OPERATIONS
Planet Yield Determination
Leader: Yann Alibert
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 158/190
PSM WP 141 400
Operations phase
01/2024 — 03/2030
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. Taking into account the first PLATO results:
2. Update the estimate the number of transiting planets detected by PLATO and for which a RV
characterization is possible.
3. Update the estimate the corresponding observation time required for the planet characterization, for
each category of telescope
4. Update the estimate of the rate of false positives
5. Update the estimate of the corresponding observation time required to discard the false positives
Input:
Selected stellar field
Dependencies:
WP 140 000 and all of its sub-packages
Output:
1. Yield of planets per bin of mass and separation
2. Percentage of false positives of the different types
Deliverables:
Estimate of the telescope time required for planet confirmation and for discarding false positives
Milestones:
01/2025: Critical examination of FU strategy
03/2025: Start of FU observations for first PLATO field
03/2028: Start of FU observations for second PLATO field
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Radial Velocity Follow-Up
Leader: François Bouchy
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 159/190
PSM WP 142 000
01/2024 — 03/2030
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:
Perform and coordinate the ground-based radial-velocity measurements of PLATO transit candidates.
Tasks:
1. Coordinate the different teams linked to a RV instrument
2. Collect radial velocity data
3. Perform RV analysis
Input:
Ranked transiting candidates from the core science program detected by PLATO
Dependencies:
WP 140 000, WP 141 000, WP 146 000, WP 113 000
Output:
RV Follow-up of PLATO transiting candidates
Deliverables:
Radial velocity to the ancillary database, nature of the candidates
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Acceptable risks
PSM WPDs
OPERATIONS
Radial Velocity Computation and Global Analysis
Tools
Leader: Damien Ségransan
Operations phase
Institution: Geneva University (Switzerland)
Key Personnel: D. Ségransan; F. Bouchy (LAM); C. Lovis (Geneva)
Objectives:
Perform and coordinate the activities of Radial Velocity computation and analysis
Tasks:
Software testing, maintenance and algorithm upgrade, implementation.
Input:
RV data from the different facilities used in the RV follow-up
Dependencies:
WP 140 000, WP 142 000, WP 146 000, WP 114 000
Output:
Radial velocity Analysis
Deliverables:
Reports, updates on algorithms and tools
Milestones:
06/2024: Scientific validation of algorithms and tools
Until 2030: Improvements on the algorithms and tools when needed
Risks:
Acceptable risks
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 160/190
PSM WP 142 100
01/2024 — 03/2030
PSM WPDs
OPERATIONS
First Radial Velocity Screening [≥ 10 m/s]
Leader: Eike W. Guenther
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 161/190
PSM WP 142 200
01/2024 — 03/2030
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:
Perform and coordinate the activities of the first radial velocity screening of PLATO transit candidates to remove
binaries and blends from candidate list, so that high-accuracy RV-measurements focus only on key targets.
Perform and coordinate the activities of mass measurement of brown dwarfs, massive giant planets and hotJupiters.
Tasks:
1.
2.
3.
4.
5.
Get telescope time
Prepare the scheduling and optimize the target’s observation strategy
Collect and analysis of radial velocity data
Update the status of candidates (binary, blend, brown-dwarf, massive giant planet, no variation, etc.)
If needed trig the candidate’s observation to the most appropriate RV instrument.
Input:
List of ranked PLATO candidates.
Dependencies:
WP 140 000, WP 141 000, WP 142 000, WP 146 000, WP 113 000
Output:
After removing the false-positives, “good” candidates will then be send to the repository of candidates suitable
for higher-precision RV-measurements.
Deliverables:
Improved list of candidates, RVs, and mass of brown dwarfs, massive giant planets and hot-Jupiters.
Milestones:
12/2024: Start of FU observations for first PLATO field
Until 2030: Screening of candidates list
Risks:
Limited number of telescope facilities to carry out the follow-up observations.
PSM WPDs
OPERATIONS
Intermediate Precision Radial Velocity Follow-Up
[3-5 m/s]
Leader: Claire Moutou
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 162/190
PSM WP 142 300
Operations phase
01/2024 — 03/2030
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:
Perform and coordinate the ground-based radial-velocity observations using spectrographs of intermediate
precision [3-5 m/s] on the ranked transiting candidate list
Tasks:
1.
2.
3.
4.
Select targets from initial list and update as Operation progress
Get telescope time on facilities achieving the needed precision
Prepare the scheduling and optimize the observation strategy
Collect and analyse spectra and RV data
Input:
Ranked transiting candidates detected by PLATO
Dependencies:
WP 113 000, WP 142 000, WP 115 000, WP 140 000, WP 144 100, WP 146 000
Output:
1. List of observations made
2. Radial Velocities and orbital solutions
3. Spectra/RV Data and preliminary analysis
Deliverables:
Radial velocity data to the ancillary data base, combined fits and false-positive analysis
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Continuous availability of spectrographs with moderate RV precision up to 2025
PSM WPDs
OPERATIONS
Very High-Precision RV Measurements [≤ 1 m/s]
Leader: Francesco Pepe
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 163/190
PSM WP 142 400
Operations phase
01/2024 — 03/2030
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:
Perform and coordinate the activities of very high-precision radial-velocity measurements of PLATO transit
candidates around quiet stars
Tasks:
1.
2.
3.
4.
Select targets from initial list and update as Operation progress
Get telescope time on high precision facilities
Prepare the scheduling and optimize the observation strategy
Collect and analyse spectra and RV data
Input:
Ranked transiting candidates detected by PLATO
Dependencies:
WP 113 000, WP 142 000, WP 115 000, WP 140 000, WP 144 100, WP 146 000
Output:
1. List of observations made
2. Radial Velocities and orbital solutions
3. Spectra/RV Data and preliminary analysis
Deliverables:
Radial velocity data to the ancillary data base, combined fits and false-positive analysis
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Continuous availability of spectrographs with high RV precision up to 2025
PSM WPDs
OPERATIONS
Infrared Radial-Velocity Measurements
Leader: Thierry Forveille
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 164/190
PSM WP 142 500
Operations phase
01/2024 — 03/2030
Institution: IPAG (France)
Key Personnel: T. Forveille; P. Figueira (Porto); X. Bonfils (IPAG); X. Delfosse (IPAG); N. Santos (Porto);
P. J. Amado (IAA); E. Guenther (TLS)
Objectives:
Prepare and coordinate the activities of ground-based radial-velocity measurements of PLATO transit candidates
using infrared spectrographs.
Tasks:
1. Follow strategy developed during development phase and apply for telescope time
2. Prepare scheduling and optimize the observation strategy
3. Collect data and perform analysis
Input:
1. PLATO transit candidates
2. The properties of their host stars (mass, luminosity, activity, spectral type, etc.)
Dependencies:
WP 140 000, WP 141 000, WP 113 000, WP 144 100, WP 115 200
Output:
1. Identification of planets and false positives
2. Mass of PLATO planets (that are best measured in the IR)
Deliverables:
Report (for mid-term and final reviews), RVs and spectra
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Existing infrared spectrographs are not optimized for RVs (but have already reach 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 the operations phase.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 165/190
Time Critical Photometry
Leader: Roi Alonso
Rev.: 5
Operations phase
PSM WP 143 000
01/2024 — 03/2030
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: R. Alonso; H.J. Deeg (IAC); E. Pallé (IAC); M. Montalto (CAUP)
Objectives:
To coordinate and lead the ground-based time critical photometric follow-up observations of PLATO transit
candidates
Tasks:
1. Coordinate applications for telescope time on the photometric facilities identified in the development
phase
2. Liaise with other WPs, notably WP 144 000 and WP 142 000
3. Coordinate preparation of observing runs with optimized observing strategy: on/off images, time
series photometry, additional colour information to add constraints for validation of difficult cases.
4. Coordinate collection, analysis and interpretation of time critical photometric data, and reports
5. Update status of candidates based on photometric results
Input:
Ranked transit candidates identified in PLATO data
Meetings with PLATO Follow-Up Management Team
Dependencies:
Information exchange with other WP’s, especially WP 144 000 and WP 142 000
Output:
Optical and/or NIR time critical photometric data of transiting candidates and confirmed systems
Deliverables:
1. Photometric data to ancillary database
2. Conclusions as to candidates’ false-positive and/or colour constraints for validation of difficult cases
Milestones:
07/2024: Critical examination of FU strategy
01/2025: Start of FU observations for first PLATO field
01/2028: Start of FU observations for second PLATO field
Risks:
Uncertainty as to which ground-based facilities will be available from 2024.
PSM WPDs
OPERATIONS
Photometry Specific Tools
Leader: H.J. Deeg
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 166/190
PSM WP 143 100
01/2024 — 03/2030
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: H. J. Deeg
Objectives:
Assure that contributing facilities have state-of-the-art data analysis techniques for photometric follow-up, and
provide the contributing observing facilities with a homogeneous set of analysis tools.
Tasks:
Software implementation and upgrades
Input:
• Scientific literature
• Feedback from observers
Dependencies:
Information exchange with other WP’s, especially WP 143 200, WP 143 300, WP 143 400
Output:
Methods to improve efficiency of existing photometric algorithms
Deliverables:
Improved pipelines, documentation.
Milestones:
07/2024: Critical examination of FU tools
Risks: None; ample experience from prior follow-up programs (for CoRoT, Kepler) is present
PSM WPDs
OPERATIONS
Photometric Follow-Up with Small Telescopes
Leader: G. Wuchterl
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 167/190
PSM WP 143 200
01/2024 — 03/2030
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.
2.
3.
4.
Link with registered facilities to PLATO Follow-Up
Coordinate execution of follow-up observations requested and defined in WP 143 000.
Assure required precision is met.
Report results to WP 143 000
Input:
• Candidates to be followed-up by small telescopes
Dependencies:
Information exchange with other WPs, especially WP 143 000, WP 143 100, WP 143 300, WP 143 400
Output:
Results of observations.
Deliverables:
Updates on documentation
Milestones:
Risks:
Uncertainty as to which ground-based facilities will be available from 2024.
PSM WPDs
OPERATIONS
Standard Photometric Observations
Leader: R. Alonso
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 168/190
PSM WP 143 300
01/2024 — 03/2030
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.
2.
3.
4.
Link with registered facilities to PLATO Follow-Up
Coordinate execution of follow-up observations requested and defined in WP 143 000.
Assure required precision is met.
Report results to WP 143 000
Input:
• Candidates to be followed-up by moderate-sized telescopes
Dependencies:
Information exchange with other WPs, especially WP 143 000, WP 143 100, WP 143 200, WP 143 400
Output:
Results of observations.
Deliverables:
Reports on observations, statistics.
Milestones:
Risks:
Uncertainty as to which ground-based facilities will be available from 2024.
PSM WPDs
OPERATIONS
Very High Precision Photometric Observations
Leader: E. Pallé
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 169/190
PSM WP 143 400
01/2024 — 03/2030
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.
2.
3.
4.
5.
Link with registered facilities to PLATO follow-up
Coordinate time allocations at required facilities
Coordinate execution of follow-up observations requested and defined in WP 143 000.
Assure required precision is met.
Report results to WP 143 000
Input:
• Candidates to be followed-up by big telescopes and/or space telescopes.
Dependencies:
Information exchange with other WPs, especially WP 143 000, WP 143 100, WP 143 200, WP 143 300
Output:
Results of observations.
Deliverables:
Reports on observations, observing logs, photometric time series, statistics.
Milestones:
Assure observations of all high priority targets in need of high-precision follow-up
Risks:
Uncertainty as to which suitable facilities will be available from 2024.
PSM WPDs
OPERATIONS
High Angular Resolution Imaging
Leader: Silvano Desidera
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 170/190
PSM WP 144 000
Operations phase
01/2024 — 03/2030
Institution: INAF – Osservatorio Astronomico di Padova (Italy)
Key Personnel: S. Desidera; V. Nascimbeni (Padova); M. Janson (Stockholm); D. Mesa (INAF-Padova);
M. Bonavita (Edinburgh); A. Vigan (LAM); V. D’Orazi (INAF-Padova)
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, WP 144 500, 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 130 000) have been properly taken into account
4. Monitor the amounts of required observing time with respect to expectations
5. Coordinate applications for telescope time on the facilities identified in the development phase
6. Coordinate preparation of observing runs to optimize observing strategy for imaging transit candidates
on different spatial scales, and to potentially characterize confirmed planetary systems through AO
imaging
7. Coordinate collection, analysis and interpretation of these data
Input:
1. Ranked transit candidates and confirmed planetary systems identified in PLATO data
2. Contaminants and companions identified by other WPs (130 000, 140 000)
3. Results of simulation on contamination probability
Dependencies:
Other follow-up WPs, WP 350 000, WP 130 000, WP 131 6xx, WP 131 3xx
Output:
Follow-up strategy
Data to WP 350 000
Third light dilution (for transit parameter determination) to WP 132 3xx
Deliverables:
Identification of potential contaminants and companions around PLATO candidates, imaging data
Milestones:
L+3m: Critical examination of high contrast imaging FU strategy
L+6m: Start of high angular resolution imaging FU observations for first PLATO field
L+3y: Start of high angular resolution imaging FU observations for second PLATO field
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. Uncertainty as to which observing facilities will be available from 2024.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 171/190
Imaging Analysis Tools
Leader: Arthur Vigan
Rev.: 5
Operations phase
PSM WP 144 100
01/2024 — 03/2030
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
Tasks:
Update tools to be exploited in the analysis of high-angular resolution observations
Input:
1. Results of high-angular resolution imaging (WP 144 200, 144 300, 144 400)
2. New analysis procedures from the literature
Dependencies:
Coordination with WP 143 000 for the analysis of seeing-limited observations
Output:
Analysis procedures and tools
Deliverables:
Report on analysis procedures and tools to be adopted in high angular resolution imaging follow-up
Milestones:
L+3m: Critical examination of high contrast imaging FU data analysis procedures
Until 02/2030: improvements of tools when needed
Risks:
Non-optimal use of allocated imaging follow-up observing time.
PSM WPDs
OPERATIONS
Single-Epoch Seeing-Limited Imaging
Leader: Valerio Nascimbeni
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 172/190
PSM WP 144 200
01/2024 — 03/2030
Institution: INAF-OAPD (Italy)
Key Personnel: V. Nascimbeni; R. Alonso (IAC); G. Piotto (Padova); S. Desidera (INAF-Padova)
Objectives:
Acquire and analyse seeing-limited observations (wide field, individual objects, guide images from spectroscopic
observations), to contribute to the elimination of false positives.
Tasks:
1.
2.
3.
4.
Applications for telescope time on the facilities identified in the development phase
Preparation of observing runs to optimise observing strategy for imaging transit candidates
Collection, analysis and interpretation of these data
Coordinate with WP 142 000 and WP 145 000 the use of guide images from spectroscopic observations
Input:
Ranked transit candidates and confirmed planetary systems identified in PLATO data
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:
Data to WP 350 000
Deliverables:
Imaging data to ancillary database (WP 350 000).
Identification of potential contaminants and companions
Milestones:
L+3m: Critical examination of seeing-limited imaging FU strategy
L+6m: Start of seeing-limited imaging FU observations for first PLATO field
L+3y: Start of seeing-limited imaging FU observations for second PLATO field
Risks:
Uncertainty as to which observing facilities will be available from 2024
PSM WPDs
OPERATIONS
Reconnaissance High Resolution Imaging
Leader: Markus Janson
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 173/190
PSM WP 144 300
Operations phase
01/2024 — 03/2030
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:
Acquire and analyse high angular resolution reconnaissance observations (lucky imaging, speckle imaging, AO
on medium-class telescopes), to contribute to the elimination of false positives.
Tasks:
1. Applications for telescope time on the facilities identified in the development phase
2. Preparation of observing runs to optimise observing strategy for imaging transit candidates
3. Collection, analysis and interpretation of these data
Input:
Ranked transit candidates and confirmed planetary systems identified in PLATO data
Dependencies:
Information exchange with other WPs
Output:
Data to WP 350 000
Deliverables:
Imaging data to ancillary database (WP 350 000).
Identification of potential contaminants and companions
Milestones:
L+3m: Critical examination of reconnaissance high resolution imaging FU strategy
L+6m: Start of reconnaissance high resolution imaging FU observations for first PLATO field
L+3y: Start of reconnaissance high resolution imaging FU observations for second PLATO field
Risks:
Uncertainty as to which observing facilities will be available from 2024
PSM WPDs
OPERATIONS
High Contrast Imaging
Leader: Dino Mesa
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 174/190
PSM WP 144 400
Operations phase
01/2024 — 03/2030
Institution: INAF (Osservatorio Astronomico di Padova)
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:
Acquire and analyse high-quality AO imaging and sparse aperture masking and space-based imaging, to
contribute to the elimination of false positives.
Tasks:
1.
Coordinate applications for telescope time on the facilities identified in the development phase
2.
Coordinate preparation of observing runs to optimize observing strategy for imaging transit candidates
3.
Coordinate collection, analysis and interpretation of these data
Input:
Ranked transit candidates and confirmed planetary systems identified in PLATO data
Dependencies:
Information exchange with other WPs
Output:
Data to WP 350 000
Deliverables:
Imaging data to ancillary database (WP 350 000).
Identification of potential contaminants and companions
Milestones:
L+3m: Critical examination of high contrast imaging FU strategy
L+6m: Start of high contrast imaging FU observations for first PLATO field
L+3y: Start of high contrast imaging FU observations for second PLATO field
Risks:
Uncertainty as to which observing facilities will be available from 2024
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 175/190
Candidate Classification
Leader: M. Bonavita
Rev.: 5
Operations phase
PSM WP 144 500
01/2024 — 03/2030
Institution: Edinburgh (UK)
Key Personnel: M. Bonavita, A. Vigan, S. Desidera, M. Janson, D. Mesa, R. Claudi, V. D’Orazi
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. Apply procedures to identify the nature of candidates close to PLATO targets found by WP 144 000
(physical companions vs. field objects)
2. Apply procedures for characterization of stellar companions of PLATO targets
3. Apply procedures for characterization of substellar companions in wide orbits around PLATO targets
4. Evaluate need of additional observations
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 2.0 follow-up WPs
Output:
Data to WP 350 000
Deliverables:
Data to be provided to the Ancillary Database (WP 350 000)
Milestones:
L+3m: Critical examination of the adopted strategy
L+1y: Start of analysis for first PLATO field
L+4y: Start of analysis for second PLATO field
Risks:
Incomplete evaluation of the environment of planets identified by PLATO in terms of stellar companions and
substellar companions in wide orbits
PSM WPDs
OPERATIONS
Additional Exoplanet Follow-Up
Leader: Xavier Bonfils
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 176/190
PSM WP 145 000
01/2024 — 03/2030
Institution: IPAG (France)
Key Personnel: X. Bonfils
Objectives:
Perform 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. Rank PLATO planets regarding their characterization potential
2. Get telescope on facilities identified during development phase
3. Coordinate the different teams linked to the follow-up characterization
Input:
1. Established planets detected by PLATO and their basic characteristics (mass, radius, period)
2. Physical characteristics of their host stars (mass, radius, luminosity, photometric variability, etc.)
Dependencies:
WP 110 000, WP 113 000, WP 115 000, WP 116 000, WP 130 000, WP 140 000, WP 141 000, WP 142 000,
WP 146 000; Information exchange with WP 114 000
Output:
1. Transmission, emission and reflective spectra of PLATO planets
2. Physical properties of PLATO planets: planetary structure, T-P profile of atmospheres, etc.
3. Chemical composition: abundance of atomic and molecular species
4. Orbital parameters (and in particular the orbit obliquities) and additional planet detections
Deliverables:
Data base
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
1. Expected performances may vary according to available facilities and method developments
2. Risk spread on numerous facility and a wide range of methods
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 177/190
Transmission Spectroscopy Follow-Up
Leader: David Ehrenreich
Rev.: 5
Operations phase
PSM WP 145 100
01/2024 — 03/2030
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. Rank the confirmed PLATO planets with a merit function relative to their atmospheric characterisation
potential with transmission spectroscopy.
2. Dispatch the confirmed PLATO planets among the different and best-suited characterisation facilities
identified during the development phase.
3. Collect and centralise information about characterisation programs proposed to different telescopes.
Input:
1.
2.
Report, tables & plots produced during the development phase.
Observed PLATO planets/stars properties.
Dependencies:
WP 113 000, WP 116 400, WP 116 500, WP 122 300, WP 123 000, WP 131 000.
Output:
Ranking, recommendations, and science cases to optimise the requests for telescope time.
Deliverables:
Ranking list and reports
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
WP relies on other facilities with their own intrinsic risks
PSM WPDs
OPERATIONS
Secondary Eclipse and Phase-Variation
Spectroscopy
Leader: Roi Alonso
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 178/190
PSM WP 145 200
01/2024 — 03/2030
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.
Tasks:
1.
2.
3.
4.
5.
Apply tools to estimate strength of spectral signatures for PLATO planets
Rank PLATO planets according to strategy defined during development phase
Get telescope time on facilities identified during development phase
Get data
Perform analysis
Input:
1.
2.
Planets discovered and confirmed by PLATO
The physical properties of their host stars
Dependencies:
WP 113 000, WP 116 400, WP 116 500, WP 122 300, WP 123 000, WP 131 000; Information exchange with
WP 114 000
Output:
1. Raw data
2. Reduced data (extracted and calibrated observations)
3. Product of analysis (occultation spectra, heat re-distribution factors, day/night temperature contrast,
reconstructed surface thermal maps)
Deliverables:
Data base
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
WP relies on other facilities with their own intrinsic risks
PSM WPDs
OPERATIONS
Developing Techniques for Atmosphere
Characterization
Leader: Xavier Bonfils
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 179/190
PSM WP 145 300
01/2024 — 03/2030
Institution: IPAG (France)
Key Personnel: X. Bonfils
Objectives:
Developing techniques that have matured for characterization will be used in a similar way as for Transmission
spectroscopy (WP 145 100) and Occultation/Phase spectroscopy (WP 145 200)
Tasks:
1.
2.
3.
4.
5.
Apply tools to estimate strength of spectral signatures for PLATO planets
Rank PLATO planets according to strategy defined during development phase
Get telescope time on facilities identified during development phase
Get data.
Perform analysis
Input:
1. Established planets from PLATO
2. Stellar properties of PLATO planet hosts
Dependencies:
WP 140 000, WP 146 000
Output:
1. Raw & reduced data
2. Product of analysis (transmission spectra, physical properties, chemical abundances, etc.)
Deliverables:
Data base
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 180/190
Rossiter-McLaughlin Observations
Leader: Guillaume Hébrard
Rev.: 5
Operations phase
PSM WP 145 400
01/2024 — 03/2030
Institution: IAP/OHP (France)
Key Personnel: G. Hébrard; F. Bouchy (LAM); A. Collier Cameron (St Andrews); M. Gillon (Liège);
A. Lecavelier (IAP); A. Santerne (CAUP); A. Triaud (Toronto)
Objectives:
Perform and coordinate the activities of radial-velocity measurements of the Rossiter-McLaughlin effect
Tasks:
1. Evaluate if planetary candidates may benefit from RM measurements to establish their planetary
nature. Evaluate feasibility of RM measurement for PLATO planets.
2. Get telescope time on adapted facilities
3. Prepare the scheduling and optimize the observation strategy
4. Collect and analyse RV data
Input:
1.
2.
Planets candidates detected by PLATO
Stellar properties of PLATO planet hosts
Dependencies:
WP 140 000, WP 142 XXX, WP 145 100, WP 146 000, WP 114 XXX
Output:
1. Planet characterization
2. Measure of the obliquity between stellar rotation axis and the orbital planet
Deliverables:
Data base
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Additional Long Term Follow-Up
(RV and Transit Timing)
Leader: François Bouchy
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 181/190
PSM WP 145 500
01/2024 — 03/2030
Institution: LAM (France)
Key Personnel: F. Bouchy; X. Bonfils (IPAG); S. Udry (Geneva); I. Skillen (IAC); G. Piotto (Padova)
Objectives:
Perform and coordinate the activities of long-term radial velocity and transiting timing follow-up observations of
selected PLATO exoplanets for search for additional planets in these systems.
Tasks:
1. Following strategy developed during development phase, apply for telescope time.
2. Prepare the scheduling and optimize the observation strategy
3. Collect and analyse data
Input:
1.
2.
Established PLATO exoplanets
Stellar properties of PLATO exoplanets host star
Dependencies:
WP 140 000, WP 142 000, WP 143 000, WP 146 000, WP 112 600, WP 112 420, WP 112 520
Output:
1. Detection of additional planets in the PLATO exoplanetary systems
2. Refined orbital characterization of known PLATO exoplanets
Deliverables:
Reports
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Acceptable risks
PSM WPDs
OPERATIONS
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 182/190
PSM WP 146 000
Spectroscopy
Leader: Artie P. Hatzes
Ref.: PLATO-UWA-PSMWPD-002
Operations phase
01/2024 — 03/2030
Institution: Thüringer Landessternwarte Tautenburg (Germany)
Key Personnel: A. P. Hatzes; L. Buchhave (NBI); I. Boisse (LAM); C. Lovis (Geneva); N. Santos (Porto);
E. W. Guenther (TLS), P. Petit (OMP); S. Sousa (CAUP); D. Gandolfi (ZAH)
Objectives:
To acquire spectra of PLATO objects to be used by WP to determine basic stellar parameters. These will be
used to exclude poor candidates (giants) and to make rapidly a list of priority 1-planet candidates for further
follow-up by precise stellar radial velocity measurements. To correct the radial velocity measurement for activity
jitter in active stars. Prepare and coordinate the activities of spectropolarimetric follow-up in the planetary
systems found by PLATO.
Tasks:
1.
2.
3.
4.
5.
Coordinate subpackages
Identify suitable telescope resources and prepare observing proposals
Data reduction
Determine basic stellar parameters of PLATO Objects of Interest (POI).
Determine activity level of POIs
Input:
PLATO Objects of Interest (POI)
Dependencies:
WP 140 000, WP 141 000,WP 141 200, WP 142 000, WP 142 100, WP 142 300. WP 142 400, WP 142 600,
WP 144 000, WP 144 200, WP 146 000, WP 147 000
Output:
1. First order stellar parameters of POIs
2. Activity level of POIs
Deliverables:
1. Preliminary stellar parameters
2. Spectral Data to other WP
3. Web-based dissemination of results to PLATO community
Milestones:
12/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
Risks:
Acceptable risks.
PSM WPDs
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 183/190
Activity Indicators and Doppler Information on Active
Stars
Leader: Christophe Lovis
PSM WP 146 100
Operations 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:
Correct RV measurements for activity.
Input:
PLATO Targets of Interests that are active
Dependencies:
WP 140 000, WP 142 300, WP 142 400, WP 142 500, WP 142 600, WP 146 000
Output:
1. Corrected RVs
2. Confirmed planets around active stars
Deliverables:
Documents and algorithms
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Acceptable risk
Rev.: 5
01/2024 — 03/2030
PSM WPDs
OPERATIONS
Tools for Spectral Classification
Leader: Lars Buchhave
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 184/190
PSM WP 146 200
01/2024 — 03/2030
Institution: Niels Bohr Institute (Denmark)
Key Personnel: L. Buchhave; A. Hatzes (TLS); E. W. Guenther (TLS); S. Sousa (CAUP)
Objectives:
Obtain preliminary spectral types of PLATO targets
Tasks:
1. Preparing observing proposals
2. Acquiring and reducing observations
3. First spectral analysis of spectra acquired of PLATO Targets
Input:
Spectral observations (low and high resolution) of PLATO Targets
Dependencies:
WP 142 300, WP 142 400, WP 142 500, WP 142 600, WP 146 000
Output:
1. Basic Stellar parameters (Teff, gravity, chemical composition)
2. Priority 1 PLATO planet candidates for radial velocity measurements
Deliverables:
1. Preliminary stellar parameters
2. Priority 1 Planet candidates
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Acceptable risks
Rev.: 5
PSM WPDs
OPERATIONS
Infrared Spectroscopy
Leader: Pedro Figueira
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 185/190
PSM WP 146 300
Operations phase
01/2024 — 03/2030
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:
1.
2.
3.
4.
Proposal preparation
Acquisition of data
IR analysis of data
Application IR activity indicators to acquired spectra of PLATO targets
Input:
Infrared spectra of PLATO targets
Dependencies:
WP 140 000, WP 142 300, WP 142 400, WP 142 500, WP 142 600, WP 146 000
Output:
1. Activity level of stars
2. Improved RV measurements of PLATO targets that are active
3. Planet confirmation
Deliverables:
IR analysis of PLATO targets of interest.
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Minimal risks
Rev.: 5
PSM WPDs
OPERATIONS
Spectropolarimetric Follow-Up
Leader: Pascal Petit
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 186/190
PSM WP 146 400
01/2024 — 03/2030
Institution: OMP (France)
Key Personnel: P. Petit; T. Böhm (OMP), J. Morin (Göttingen); R. Farès (INAF-Catania); S. Berdyugina
(Freiburg); O. Kochukhov (Uppsala)
Objectives:
Coordinate the spectropolarimetric follow-up of the planetary systems found by PLATO. Prepare the observing
proposals required to achieve the spectropolarimetric follow-up, check the data quality, run a systematic
extraction of Zeeman signatures through multi-line techniques, model the stellar magnetic geometries using
tomographic modelling. Provide the PDC with final data and associated model outputs.
Tasks:
1. Prepare observing proposals to achieve the monitoring of all selected targets.
2. Evaluate the data quality and adjust the observing strategy accordingly.
3. Run a systematic extraction of Zeeman signatures using multi-line techniques. Extract broadband
polarization.
4. Reconstruct the magnetic field topology of central stars, using tomographic modelling of the polarized
signatures in spectral lines.
5. Transmit final outputs of the spectropolarimetric follow-up to PDC (reduced polarized spectra, crosscorrelation profiles, magnetic topologies).
Input:
Spectropolarimetric data
Dependencies:
WP 140 000, WP 142 600, WP 144 100, WP 144 200, WP 145 000, WP 146 000
Output:
Analysis of Zeeman signatures
Deliverables:
Reports
Milestones:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Performances Assessment & FU Efficiency
Leader: Stéphane Udry
Institution: Geneva University (Switzerland)
Key Personnel:
Objectives:
Tasks:
Input:
Dependencies:
Output:
Deliverables:
Milestones:
Risks:
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 187/190
PSM WP 147 000
01/2024 — 03/2030
PSM WPDs
OPERATIONS
Interfaces to Other SPM WPs and PDC
Leader: Stéphane Udry
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 188/190
PSM WP 148 000
Operations phase
01/2024 — 03/2030
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. Interfaces to the PDC.
Tasks:
1. Maintenance of interface to other Science WPs
2. 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:
06/2024: Critical examination of FU strategy
12/2024: Start of FU observations for first PLATO field
12/2027: Start of FU observations for second PLATO field
Risks:
Minimal risks
PSM WPDs
OPERATIONS
Complementary Science
Leader: Conny Aerts
Operations phase
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 189/190
PSM WP 160 000
01/2024 — 03/2030
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 PLATO core science the knowledge of
primarily age, mass and chemistry of planet hosting stars has to be significantly improved, which
requires substantial updates on models of stellar structure and evolution.
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. Coordinate and supervise the Complementary Science work packages.
2. Organization of regular teleconferences, and face-to-face meetings of the thematic sub-teams.
3. Coordinate activities with the instrument team, PDC and among the PSM tasks and investigate
implications of project developments 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. Stimulate and support information exchange and collaboration within the PLATO community through
dedicated workshops
2. Specifications and data input to PDC,
3. PR activities
Deliverables:
Milestones:
Risks:
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
OPERATIONS
Ref.: PLATO-UWA-PSMWPD-002
Issue: 2
st
Date: September 1 2015
Page: 190/190
PMC SCIENCE MANAGEMENT
WORK PACKAGE DESCRIPTIONS
OPERATIONS
END
Rev.: 5