PSM WPDs
POST-OPERATIONS
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Astronomy Group, Department of Physics, University of Warwick
PMC SCIENCE MANAGEMENT
WORK PACKAGE DESCRIPTIONS
POST-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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
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Table of Contents
PSM Coordination
PSM WP 100 000
10
PSM Project Office
PSM WP 101 000
11
PSM Coordination Team
PSM WP 103 000
12
Exoplanet Science Coordination
PSM WP 110 000
13
Coordination of Tools for Lightcurve Filtering
PSM WP 111 000
14
Specification of Planet Detection Tools
PSM WP 112 000
15
Transit Detection Tools
PSM WP 112 100
16
Other Detection Methods
PSM WP 112 400
17
Eclipse Timing Variations in Eclipsing Binaries
PSM WP 112 420
18
Phase Variations in Pulsating Stars
PSM WP 112 430
19
Multi-Planet Systems
PSM WP 112 500
20
Photometric Detection of Circumbinary Planets
PSM WP 112 510
21
Planets in Trojan Orbits
PSM WP 112 520
22
Exomoons and Binary Planets
PSM WP 112 530
23
Other Multiple Systems
PSM WP 112 540
24
Transit Time Variations and Transit Duration Variations (TTV / TDV)
PSM WP 112 600
25
TTV / TDV Detection
PSM WP 112 610
26
TTV / TDV Modelling
PSM WP 112 620
27
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Specification of Procedures to Rank Planet Candidates
PSM WP 113 000
28
Specification for Space Based False Positive Identification Through Centroid Analysis
PSM WP 113 200
29
Specification of Transit Fitting Tools
PSM WP 114 000
30
Specify Transit Curve Modelling Tools
PSM WP 114 100
31
Specify Tools for Accurate Orbital Period Determination
PSM WP 114 200
32
Rossiter-McLaughlin Modelling Tools
PSM WP 114 300
33
Development of PLATO Data Specific Science
PSM WP 115 000
34
Astrophysical Noise Sources and Their Impact on RV Determination
PSM WP 115 100
35
Improved Planetary System Characterisation
PSM WP 115 200
36
Planet-Star Interactions
PSM WP 115 300
37
Signatures of Close-in Planets
PSM WP 115 400
38
Non-Transiting Planets via REBs
PSM WP 115 500
39
Development of PLATO Interpretation Specific Science
PSM WP 116 000
40
Compositions & Formation of Gas & Ice Giants
PSM WP 116 100
41
The Mass-Radius Relationship for Terrestrial Planets
PSM WP 116 200
42
Planetary Formation and Orbital Evolution
PSM WP 116 300
43
Protoplanetary Disc Models
PSM WP 116 310
44
Disc-Planet Interactions
PSM WP 116 320
45
The Assembly of Planetary Systems
PSM WP 116 330
46
PSM WPDs
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The Post-Formation Long-Term Dynamical Evolution of Planetary Systems
PSM WP 116 340
47
Planet Formation and Evolution in Binary Systems
PSM WP 116 350
48
Influence of Birth Environment on the Formation and Evolution of Planetary Systems
PSM WP 116 360
49
Post-Main Sequence Evolution of Planetary Systems
PSM WP 116 370
50
Statistical Comparison Between Theory and PLATO Data
PSM WP 116 380
51
Atmospheres of PLATO Terrestrial Planets
PSM WP 116 400
52
Dynamical Interactions in Multi-Planet Systems
PSM WP 116 600
53
Long-Term Dynamical Evolution of Planetary Systems
PSM WP 116 610
54
Stability and Resonances in Multi-Planet Systems
PSM WP 116 620
55
Tidal Dissipation and Evolution of Multi-Planet Systems
PSM WP 116 630
56
Rotational Evolution of Planets in Multiple Systems
PSM WP 116 640
57
Planetary Ephemerides of PLATO Systems
PSM WP 116 650
58
Specifications for Interface to Other PSM WPs and PDC
PSM WP 117 000
59
Stellar Science Coordination
PSM WP 120 000
60
Stellar Models
PSM WP 121 000
61
1D Stellar Models
PSM WP 121 100
62
Very Low-Mass Stellar Models
PSM WP 121 110
63
Low Mass Stellar Models
PSM WP 121 120
64
PSM WPDs
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Theoretical Oscillation Frequencies
PSM WP 121 130
65
Transport Processes
PSM WP 121 200
66
PMS Evolution
PSM WP 121 300
67
2D / 3D Stellar Evolution Models
PSM WP 121 400
68
Evolution of Stars in Multiple Systems
PSM WP 121 500
69
Non-Seismic Diagnostics and Model Atmospheres
PSM WP 122 000
70
1D Model Atmospheres
PSM WP 122 100
71
3D Model Atmospheres
PSM WP 122 200
72
Fundamental Stellar Parameters
PSM WP 122 300
73
Limb Darkening
PSM WP 122 400
74
Interstellar Extinction
PSM WP 122 500
75
Stellar Activity and Rotation
PSM WP 123 000
76
Spot Models
PSM WP 123 100
77
Surface Convection (1D & 3D)
PSM WP 123 200
78
Models of Rotational Evolution and Gyrochronology
PSM WP 123 300
79
Dynamos and Differential Rotation
PSM WP 123 400
80
Tools to Measure Rotational Modulation
PSM WP 123 500
81
Stellar Rotation from Transits
PSM WP 123 600
82
Seismic Diagnostics
PSM WP 124 000
83
PSM WPDs
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Forward Approaches
PSM WP 124 100
84
Inverse Techniques
PSM WP 124 200
85
Acoustic Glitches
PSM WP 124 300
86
Determination of Stellar Parameters
PSM WP 125 000
87
Scaling Laws
PSM WP 125 100
88
Incorporating Classical Parameters
PSM WP 125 200
89
Seismic Parameters
PSM WP 125 300
90
Open Clusters
PSM WP 125 400
91
Mode Physics
PSM WP 126 000
92
Mode Amplitude and Near-Surface Effects on Mode Parameters
PSM WP 126 100
93
Mode Line-Width
PSM WP 126 200
94
Intensity-Velocity Relation
PSM WP 126 300
95
Seismology of Magnetic Activity
PSM WP 126 400
96
Seismic Constraints From Aging Stars
PSM WP 127 000
97
Stellar Models of Evolved Stars
PSM WP 127 100
98
Seismic Diagnostics for Evolved Stars
PSM WP 127 200
99
Constraints on Main-Sequence Stars
PSM WP 127 300
100
Power Spectrum Fitting Tools
PSM WP 128 000
101
PSM WPDs
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Average Seismic Parameters
PSM WP 128 100
102
Mode Fitting Tools
PSM WP 128 200
103
Solar-Like Stars
PSM WP 128 210
104
Solar-Like Stars with Planets
PSM WP 128 220
105
Multiple Stars
PSM WP 128 230
106
Ensemble Fit
PSM WP 128 240
107
Fitting Tools for Evolved Stars
PSM WP 128 250
108
Interfaces
PSM WP 129 000
109
Target / Field Characterization and Selection
PSM WP 130 000
110
Project Office Assistant
PSM WP 130 100
111
Interface to Other PSM WPs and PDC
PSM WP 133 000
112
Interface to Other PSM WPs
PSM WP 133 100
113
Interface to PDC
PSM WP 133 200
114
Coordination of PLATO Follow-Up Observations
PSM WP 140 000
115
Strategy and Operation Preparation
PSM WP 141 000
116
Target Distribution Requirements
PSM WP 141 100
117
Aids for Optimizing Photometric and Spectroscopic Measurements
PSM WP 141 200
118
Information Transfer
PSM WP 141 300
119
Planet Yield Determination
PSM WP 141 400
120
PSM WPDs
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Radial Velocity Follow-up
PSM WP 142 000
121
Radial Velocity Computation and Global Analysis Tools
PSM WP 142 100
122
First Radial Velocity Screening [≥ 10 m/s]
PSM WP 142 200
123
Intermediate Precision Radial Velocity Follow-Up [3-5 m/s]
PSM WP 142 300
124
Very High-Precision RV Measurements [≤ 1 m/s]
PSM WP 142 400
125
Infrared Radial-Velocity Measurements
PSM WP 142 500
126
Time Critical Photometry
PSM WP 143 000
127
Photometry Specific Tools
PSM WP 143 100
128
Photometric Follow-Up with Small Telescopes
PSM WP 143 200
129
Standard Photometric Observations
PSM WP 143 300
130
Very High Precision Photometric Observations
PSM WP 143 400
131
High Angular Resolution Imaging
PSM WP 144 000
132
Imaging Analysis Tools
PSM WP 144 100
133
Single-Epoch Seeing-Limited Imaging
PSM WP 144 200
134
Reconnaissance High Resolution Imaging
PSM WP 144 300
135
High Contrast Imaging
PSM WP 144 400
136
Candidate Classification
PSM WP 144 500
137
Additional Exoplanet Follow-Up
PSM WP 145 000
138
PSM WPDs
POST-OPERATIONS
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Transmission Spectroscopy Follow-Up
PSM WP 145 100
139
Secondary Eclipse and Phase-Variation Spectroscopy
PSM WP 145 200
140
Developing Techniques for Atmosphere Characterization
PSM WP 145 300
141
Rossiter-McLaughlin Observations
PSM WP 145 400
142
Additional Long Term Follow-Up (RV and Transit Timing)
PSM WP 145 500
143
Spectroscopy
PSM WP 146 000
144
Activity Indicators and Doppler Information on Active Stars
PSM WP 146 100
145
Tools for Spectral Classification
PSM WP 146 200
146
Infrared Spectroscopy
PSM WP 146 300
147
Spectropolarimetric Follow-Up
PSM WP 146 400
148
Performance Assessment & FU Efficiency
PSM WP 147 000
149
Interfaces to Other PSM WPs and PDC
PSM WP 148 000
150
Complementary Science
PSM WP 160 000
151
PSM WPDs
POST-OPERATIONS
PSM Coordination
Leader: Don Pollacco
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PSM WP 100 000
Post-operations phase
04/2030 — 03/2033
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:
Activities and reports from PSM task coordinators; 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:
03/2033: Final reports and improved specifications, final 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
POST-OPERATIONS
PSM Project Office
Leader: David J. A. Brown
Post-operations phase
Key Personnel: D. J. A. Brown
Objectives:
Support coordination of the PSM activities.
Tasks:
1.
Organization of PSM meetings, teleconferences
2.
Organization of workshop with scientific community
3.
Editorial of PSM documentation
Input:
Organization request from PSM
Dependencies:
Close interactions foreseen with WP 100 000 and WP 103 000.
Output:
Organization of meetings, teleconferences; documentation
Milestones:
03/2033: Final PSM reports in post-operation phase
Risks:
Acceptable risk
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PSM WP 101 000
Institution: University of Warwick (UK)
Deliverables:
Documentation of the PSM activities
Ref.: PLATO-UWA-PSMWPD-003
04/2030 — 03/2033
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
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PSM Coordination Team
Leader: Don Pollacco
Rev.: 5
Post-operations phase
PSM WP 103 000
04/2030 — 03/2033
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 post-operation phases by regular telephone conferences
and meetings
2.
Coordinate the final update on science
3.
Agree on the final 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:
03/2033: Final reports and improved specifications, final updated PDC input catalogue data to PDC
Risks:
Late delivery of any of the outputs from the PSM will impact on the work of the PDC
PSM WPDs
POST-OPERATIONS
Exoplanet Science Coordination
Leader: Don Pollacco
Post-operations phase
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PSM WP 110 000
04/2030 — 03/2033
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 final scientific specification for both algorithm & tools
Input:
1.
PLATO Red Book
2.
Scientific literature
3.
Input from sub work packages
Dependencies:
All WP 110 work packages
Output:
Successful review of existing exoplanet work packages and recommendations as input to PDC on a yearly
timescale.
Deliverables:
Reports from each work packages listing recommendations for performance evaluation and improvements at
end of operations phase.
Milestones:
Until 2033: 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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
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Coordination of Tools for Lightcurve Filtering
Leader: Antonino F. Lanza
Rev.: 5
Post-operations phase
PSM WP 111 000
04/2030 — 03/2033
Institution: INAF-Catania (Italy)
Key Personnel: A. F. Lanza; S. Aigrain (Oxford); F. Faedi (Warwick)
Objectives:
Coordination of the works of the work packages WP 111 100 to WP 111 200.
Tasks:
1.
Coordination of the work for deriving new specifications of procedures, algorithms, and theoretical
models for the final treatment of the residual instrumental noise and the intrinsic stellar noise, if necessary;
2.
Coordination of the final work concerning both kinds of noise on PLATO data of the planet hosting stars;
3.
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 stellar noise and the residual instrumental noise. This will provide a finally improved accuracy for
the derived stellar and planetary characteristics and final products of the mission;
4.
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, the last one taking care of the communication
with the PDC.
Output:
1.
Final improvements of scientific specifications
2.
Reports on the activity
Deliverables:
1.
Reports on algorithms and specifications.
2.
Reports on tests performed as algorithms and their implementation evolve.
Milestones:
04/2030-03/2032: Final improvements of the procedures and algorithms, if necessary, for the last runs obtained
during the operation phase;
04/2032-03/2033: Final theoretical developments to improve the physical description of the intrinsic stellar
noise, including the scaling relationships with global stellar parameters, based on our improved knowledge of
stellar physics; delivery of the final products of our studies.
PSM WPDs
POST-OPERATIONS
Specification of Planet Detection Tools
Leader: Juan Cabrera
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
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PSM WP 112 000
04/2030 — 03/2033
Institution: DLR (Germany)
Key Personnel: J. Cabrera; NN (DLR)
Objectives:
Coordination of the work of the sub-work packages related to improvements and updates of the planet detection
methods concerning the analysis of the data during the post operations phase. 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 analysis of the final results, including the study of the complete data set, the
inclusion of the stellar characterization, follow-up observations. Coordination of the archive of the algorithms and
specifications used.
Tasks:
1.
2.
3.
4.
5.
Liaise with sub-work package leaders
Liaise with Exoplanet coordinator and PMC Science Management Coordinator as required
Responsible for reports and algorithms from sub-work packages
Analysis of the final results
Archive of the tools
Input:
1.
Scientific literature
2.
PLATO performance
3.
PLATO data (including follow-up results and stellar characterization)
Dependencies:
Close interactions foreseen with WP 111 000, 113 000, 114 000 and sub-WP
Output:
Planet detection updated algorithms and strategies for PDC and for archive
Deliverables:
Reports from sub-work packages and scientific specifications and updated tools for archive
Milestones:
Until 2033: 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
POST-OPERATIONS
Transit Detection Tools
Leader: Juan Cabrera
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
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PSM WP 112 100
04/2030 — 03/2033
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:
Compare the actual detection yield of the mission with the expectations. Consider the reanalysis of the runs if
needed. Incorporate the updated information from the stellar characterization and follow-up. Archive the tools
and specifications used.
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 archive tools and specifications
Input:
1.
Scientific literature
2.
PLATO performance
3.
PLATO data (including follow-up results and stellar characterization)
Dependencies:
Close interactions foreseen with WP 110 000, WP 116 000, WP 160 000, WP 112 000; PLATO End-to-End
Simulator.
Output:
1.
Report on the activities done. Statistical analysis
2.
Archive of tools and specifications
Deliverables:
Report and algorithms
Milestones:
Until 2033: 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
POST-OPERATIONS
Other Detection Methods
Leader: Roberto Silvotti
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
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PSM WP 112 400
04/2030 — 03/2033
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 160 000.
3. Monitoring of data products
4. Final tuning of analysis tools.
5. Coordination 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 160 000.
Output:
1.
Confirmed performance of data reduction with feedback for PDC.
2.
Follow-up observations
Deliverables:
Reports for Science Coordinator and PDC.
Milestones:
Until 2033: 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
POST-OPERATIONS
Eclipse Timing Variations in Eclipsing Binaries
Leader: Stefan Dreizler, Sonja Schuh
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
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PSM WP 112 420
04/2030 — 03/2033
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. Final tuning of analysis tools.
3. Perform 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.
Final level of data reduction with feedback for PDC.
2.
Follow-up observations
Deliverables:
Reports for Science Coordinator and PDC
Milestones:
Until 2033: 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
POST-OPERATIONS
Phase Variations in Pulsating Stars
Leader: Roberto Silvotti
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
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Date: September 1 2015
Page: 19/152
PSM WP 112 430
04/2030 — 03/2033
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. Continued scientific validation of the algorithms assessed during the Implementation Phase, including false
positives.
2. Continued 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 160 000.
Output:
1.
Continued assessment of performance of data reduction with feedback for PDC.
2.
Continued fine-tuning of algorithms with feedback for PDC.
3.
Assessment and continued definition of follow-up observations.
Deliverables:
Reports for Science Coordinator and PDC.
03/2031: Performance assessment report to Science Coordinator and PDC
03/2032: Assessment of follow up observations
03/2033: Final report to Science Coordinator and PDC
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Multi-Planet Systems
Leader: Silvano Desidera
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 20/152
PSM WP 112 500
04/2030 — 03/2033
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, scientific papers
Deliverables:
Interim Report, Final Report, Requirements for PDC (detection algorithms), scientific papers
Milestones:
Until 2033: 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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 21/152
Photometric Detection of Circumbinary Planets
Leader: Hans J. Deeg
Rev.: 5
Post-operations phase
PSM WP 112 510
04/2030 — 03/2033
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:
Specification of PLATO mission parameters, performance and data format.
Output:
1.
Review of published knowledge.
2.
Detection algorithms,
3.
Development of theory (as required) to fully exploit PLATO data in this area,
4.
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:
Until 2033: 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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 22/152
Planets in Trojan Orbits
Leader: Francesco Marzari
Rev.: 5
Post-operations phase
PSM WP 112 520
04/2030 — 03/2033
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:
1.
Review of published knowledge.
2.
Detection algorithms,
3.
Development of theory (as required) to fully exploit PLATO data in this area,
4.
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:
Until 2033: 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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 23/152
Exomoons and Binary Planets
Leader: Gyula Szabo
Rev.: 5
Post-operations phase
PSM WP 112 530
04/2030 — 03/2033
Institution: Konkoly Observatory (Hungary)
Key Personnel: G. Szabo; A. E. Simon (Konkoly)
Objectives:
The main task of this WP in the post-operation phase is to use the tools developed tools to identify binary
exoplanets and moons orbiting extrasolar planets directly in the raw photometrical 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:
1.
Review of published knowledge
2.
Detection algorithms
3.
Development of theory (as required) to fully exploit PLATO data in this area
4.
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:
Until 2033: 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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 24/152
Other Multiple Systems
Leader: Silvano Desidera
Rev.: 5
Post-operations phase
PSM WP 112 540
04/2030 — 03/2033
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:
1.
Review of published knowledge.
2.
Detection algorithms,
3.
Development of theory (as required) to fully exploit PLATO data in this area,
4.
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:
Until 2033: 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
POST-OPERATIONS
Transit Time Variations and Transit Duration
Variations (TTV / TDV)
Leader: Valerio Nascimbeni
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 25/152
PSM WP 112 600
04/2030 — 03/2033
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 improvements and
updates to methods and algorithms, and of analysis of the final results. Coordination of the archive of relevant
algorithms and methods. 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.
5.
6.
Liaise with sub-work package leaders
Liaise with Exoplanet coordinator and PLATO Science Coordinator as required
Liaise with leader of WP 112 000
Responsible for reports and algorithms from sub-work packages
Analysis of the final results
Archive of the tools
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.
Final level of data reduction with feedback for PDC.
2.
Follow-up observations
Deliverables:
1.
Observing plan for follow-up observations.
Reports/documents for PDC (algorithms).
Milestones:
Until 2033: 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:
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
POST-OPERATIONS
TTV / TDV Detection
Leader: Valerio Nascimbeni
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 26/152
PSM WP 112 610
04/2030 — 03/2033
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
substellar 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. Final fine-tuning of detection algorithms / tools.
2. Perform follow-up observations.
3. 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:
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.
Final level of data reduction with feedback for PDC.
2.
Follow-up observations
Deliverables:
1.
Observing plan for follow-up observations.
2.
Reports/documents for PDC (algorithms).
Milestones:
Until 2033: 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:
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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 27/152
TTV / TDV Modelling
Leader: Rosemary Mardling
Rev.: 5
Post-operations phase
PSM WP 112 620
04/2030 — 03/2033
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:
Observing plan for follow-up observations. Reports/documents for PDC (algorithms).
Milestones:
Until 2033: 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:
TBD
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 28/152
Specification of Procedures to Rank Planet
Candidates
Leader: Magali Deleuil
Rev.: 5
Post-operations phase
PSM WP 113 000
04/2030 — 03/2033
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. Scientific literature
2. PLATO Red book
3. Current PLATO performance estimation
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:
Until 2033: 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
POST-OPERATIONS
Specification for Space Based False Positive
Identification Through Centroid Analysis
Leader: Magali Deleuil
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 29/152
PSM WP 113 200
04/2030 — 03/2033
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. Scientific literature
2. PLATO Red book
3. Current PLATO performance estimation
Dependencies:
Other WP 113 work packages, WP 111, WP 112, WP 114
Output:
Development of criteria and algorithms for centroid filtering.
Deliverables:
Report and updated algorithms
Milestones:
Until 2033: 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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 30/152
Specification of Transit Fitting Tools
Leader: Szilard Csizmadia
Rev.: 5
Post-operations phase
PSM WP 114 000
04/2030 — 03/2033
Institution: DLR (Germany)
Key Personnel: Sz. Csizmadia; N.N. (DLR); A. Bonomo (INAF-Torino); M Gillon (Liège)
Objectives:
Optimal extraction of scientific results from PLATO data. Refinement of some results. Archiving of all results and
algorithms into a PEFT database. Global scientific inferences.
PEFT (PLATO Eclipse Fitting Tool) 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.
Continuous reviewing of the literature for improvement of PEFT.
Refinement of the results.
Global analysis of PEFT results.
Archiving of results and algorithms.
Coordination with WP 114 100 and WP 114 200.
Input:
1.
2.
3.
4.
PLATO data
Follow-up data
External data
Scientific literature
Dependencies:
WP 114 work packages
Output:
Posterior distributions for the planetary systems parameters available to the community via a PEFT database.
Algorithms.
Deliverables:
Reports and updated algorithms.
Milestones:
Until 2033: 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. Non-optimal scientific exploitation of PLATO data.
PSM WPDs
POST-OPERATIONS
Specify Transit Curve Modelling Tools
Leader: Szilard Csizmadia
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 31/152
PSM WP 114 100
04/2030 — 03/2033
Institution: DLR (Germany)
Key Personnel: Sz. Csizmadia; N.N. (DLR)
Objectives:
Refinement, consolidation and archiving the results, tools, algorithms and software used.
Tasks:
1.
2.
3.
4.
5.
Continue the review of scientific literature
Refine the algorithms and procedures
Consolidate the results
Active archiving of the procedures, algorithms and results
Team coordination of the task
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red book
Current PLATO performance estimation
PLATO specifications
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 and updated algorithms
Milestones:
Until 2033: 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
POST-OPERATIONS
Specify Tools for Accurate Orbital Period
Determination
Leader: Magali Deleuil
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 32/152
PSM WP 114 200
04/2030 — 03/2033
Institution: Laboratoire d'astrophysique de Marseille (France)
Key Personnel: M. Deleuil; A. Bonomo (INAF-Torino)
Objectives:
Specify period finding techniques and the generation of orbital ephemeris for single and multiple stars.
Tasks:
1.
2.
3.
4.
5.
Review of scientific literature
Evaluate the suitability of commonly used period determination techniques
Evaluate the suitability of commonly used methods of orbital ephemeris generation
Extension of the above (and evaluation) to binary and multiple star systems
Development and test of algorithms for above.
Input:
1. Scientific literature
2. PLATO Red book
3. Current PLATO performance estimation
4. Commonly available codes within the PLATO community or freely available
Dependencies:
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 updated algorithms
Milestones:
Until 2033: 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
POST-OPERATIONS
Rossiter-McLaughlin Modelling Tools
Leader: Guillaume Hébrard
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 33/152
PSM WP 114 300
04/2030 — 03/2033
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 updated algorithms
Milestones:
Until 2033: 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
POST-OPERATIONS
Development of PLATO Data Specific Science
Leader: Don Pollacco
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 34/152
PSM WP 115 000
04/2030 — 03/2033
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:
Reports from each sub-work package
Milestones:
Until 2033: 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
POST-OPERATIONS
Astrophysical Noise Sources and Their Impact on RV
Determination
Leader: Chris Watson
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 35/152
PSM WP 115 100
04/2030 — 03/2033
Institution: Queens University Belfast (UK)
Key Personnel: C. Watson
Objectives:
Extended user support for the application of astrophysical noise mitigation techniques for continued groundbased follow-up. Maintain documentation and quality control monitoring to sustain detection efficiencies during
the final phases of the PLATO follow-up campaign.
Tasks:
1.
To maintain user support for astrophysical noise mitigation aids.
2.
Undertake final adaptation of mitigation aids, with application to prior data where warranted.
3.
Final assessment of overall noise mitigation efficiency during PLATO mission.
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book.
Current estimation of PLATO performance and ground-based facility capabilities.
PLATO astrophysical noise mitigation aids/procedures and documents.
Dependencies:
Exchange of information with all RV follow-up packages, WP 140.
Output:
Final generation of noise mitigation algorithms and report on their efficiencies.
Deliverables:
Reports & updates of noise reduction algorithms and/or strategies for ground-based follow-up.
Milestones:
03/2031: Release of final generation of mitigation aids.
03/2033: Final report on activities and efficiency appraisal.
Risks:
RV follow-up for low-mass Earth-like planets (habitable) is likely to extend into the post-ops phase. Continued
quality control of, and user support for, astrophysical noise mitigation aids will be required to ensure maximizing
ground-based follow-up efficiency and the scientific impact of PLATO. Worst-case scenario would be a reduction
of low-mass planet detections.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 36/152
Improved Planetary System Characterisation
Leader: Alessandro Sozzetti
Rev.: 5
Post-operations phase
PSM WP 115 200
04/2030 — 03/2033
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 postoperations phase, (simulated) data from other sources will be combined with actual PLATO data demonstrating
expected system improvements. Where applicable, observing programs will be proposed and new data
gathered to advance the synergetic effort with final PLATO data for targets of interest.
Tasks:
1.
Continued review of the potential of current and future planet-hunting facilities/instrumentation
2.
Use of simulated and actual publicly available data to gauge the advantages and improvements on
planetary systems characterization from combined datasets
3.
Finalization 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). Finalized 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 science 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:
Until 2033: 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 the mission, unavailability of complementary datasets.
PSM WPDs
POST-OPERATIONS
Planet-Star Interactions
Leader: Stéphane Mathis
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 37/152
PSM WP 115 300
04/2030 — 03/2033
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 work that consists in checking that the modelling of star-planet interactions that we
achieved during the implementation and operation phases has allowed to give the best characterization as
possible of planetary systems observed 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:
1.
PLATO data
2.
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
04/2030-10/2030: Improvements of the modelling procedure for star-planet interactions if necessary after tests
with last PLATO run data.
10/2030-12/2031: Theoretical developments to improve the description of star-planet interactions.
2033: Contribution to the delivery of an updated new generation of validated models for star-planet interactions
and planetary system evolution.
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Transits of Close-in Objects
Leader: Carole Haswell
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 38/152
PSM WP 115 400
04/2030 — 03/2033
Institution: The Open University
Key Personnel: C Haswell
Objectives:
Use PLATO discoveries of close-in transiting bodies with compositional and mass information derived from
follow-up observations to reveal the mass-radius-composition relationship of rocky planets. Assess the effects
of Galactic chemical evolution on planetary system formation and evolution.
Tasks:
1. Review of the scientific literature in this area
2. Consolidate body of knowledge on size-mass-composition of mass-losing rocky bodies.
3. Place observational findings in the context of depth-dependent interior structure models of solid
exoplanets from WP 116 200
4. Interpret the planeticity of the systems containing mass-losing rocky bodies in the context of the
compositional information revealed by the mass loss.
5. Place findings in the context of Galactic chemical evolution using stellar ages.
Input:
1.
2.
3.
4.
5.
6.
Scientific literature
Size-mass-composition information on individual objects
Information on other planets in the systems studied from PLATO L2 data products and the literature.
Models from WP 116 200
Precise stellar ages of individual host stars from PLATO astroseismology
Latest detailed Galactic chemical evolution data to define the primordial make-up of individual planetary
systems
Dependencies:
1. Inputs 2,3, 4 and 5 will be generated during OPS phase of PLATO mission in a variety of WPs including
this one.
2. Interaction with WP 116 200
3. PLATO L1 and L2 data products
4. Availability of suitable ground-based facilities
Output:
Scientific papers reporting findings.
Deliverables:
Final Report.
Milestones:
Interim reports
01/2033: Final Report
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Non-Transiting Planets via REBs
Leader: David Barrado
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 39/152
PSM WP 115 500
04/2030 — 03/2033
Institution: Centro de Astrobiología, INTA-CSIC (Spain)
Key Personnel: D. Barrado; H. Bouy (CAB, INTA-CSIC); N. Huélamo (CAB, INTA-CSIC); M. Morales-Calderón
(CAB, INTA-CSIC); J. Lillo-Box (CAB, INTA-CSIC)
Objectives:
Detection of non-transiting planets via beaming and ellipsoidal effects in the light curve (REBs).
Tasks:
Task 1 - Processing of all out-of-transit region of the light-curves to look for the ellipsoidal and beaming effects,
both able to provide the mass of the surrounding planets for non-transiting systems.
Task 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-ups it would be necessary to have high-resolution images to avoid contaminating the
spectra with additional blended sources. Feedback on task #1.
Input
Light curves with or without detected transits.
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:
1. Orbital and physical characterization of the surrounding objects.
2. High-resolution images of the candidates and determination of the probability for a given planet host
candidate to have a blended (undetected companion).
3. 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 - Derived probabilities for each host candidate to have undetected blended sources contaminating the
PLATO light-curves. Final report.
Milestones:
04/2030-12/2031 Final catalogue
Risks:
Depends on telescope time assignations
PSM WPDs
POST-OPERATIONS
Development of PLATO Interpretation Specific
Science
Leader: Heike Rauer
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 40/152
PSM WP 116 000
04/2030 — 03/2033
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:
03/2032: Delivery of preliminary reports from sub-work packages
03/2033: Final reports from sub-work packages
Risks:
Reduced scientific impact of mission.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 41/152
Compositions & Formation of Gas & Ice Giants
Leader: Tristan Guillot
Rev.: 5
Post-operations phase
PSM WP 116 100
04/2030 — 03/2033
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.
Use 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:
1.
Analysis of PLATO data.
2.
Validation of formation models
Deliverables:
Scientific analysis of PLATO discoveries, validation of planet/star formation models
Milestones:
04/2031: Statistical analysis of PLATO data
03/2033: Validation of formation models from super-Earths to gas giants
Risks:
Reduced scientific impact of mission.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 42/152
The Mass-Radius Relationship for Terrestrial Planets
Leader: Frank Sohl
Rev.: 5
PSM WP 116 200
Post-operations phase
04/2030 — 03/2033
Institution: DLR (Germany)
Key Personnel: F. Sohl; N.N. (DLR)
Objectives:
Use PLATO photometry and ground-based radial velocity observations to refine 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:
This WP is part of PSM WP 116 000.
Output:
Ongoing review of published knowledge. Development of theory (as required) to fully exploit PLATO data in this
area.
Deliverables:
Report
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 43/152
Planetary Formation and Orbital Evolution
Leader: Richard Nelson
Rev.: 5
Post-operations phase
PSM WP 116 300
04/2030 — 03/2033
Institution: Queen Mary, University of London (UK)
Key Personnel: R. Nelson; O. Gressel (NBI); W. Kley (Tuebingen); A. Johansen (Lund); Y. Alibert (Bern);
Morbidelli (OCA); M. Davies (Lund); M. Wyatt (IoA, Cambridge); C. Mordasini (Bern)
A.
Objectives:
Provide on-going theoretical research in planet formation and orbital evolution for interpretation of the full
PLATO data set. Update simulation codes, 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
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,
6.
Undertake statistical comparison between PLATO data and outputs from theoretical models.
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book
PLATO observational data
Commonly available codes within the PLATO community or freely available
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
Deliverables:
1.
State of the art software tools for planet formation and orbital evolution simulations
2.
Fully maintained library of simulated planetary systems for comparison with new discoveries, and for
statistical comparison with exoplanet data sets
3.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Protoplanetary Disc Models
Leader: Oliver Gressel
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 44/152
PSM WP 116 310
04/2030 — 03/2033
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:
Undertake final development of codes for 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,
self-gravity, 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.
Developments will be based on critical analysis of results achieved during operations phase.
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.
2.
3.
4.
Scientific literature and theoretical developments
PLATO data and discoveries
Latest observations of protoplanetary discs from e.g. ALMA etc.
Critical assessment of the success of models to explain PLATO data set
Dependencies:
Close interaction foreseen with WP 116 320, WP 116 330, WP 116 350 and WP 116 360
Output:
Continued 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
Interim report on scientific activity
2033: Final report on scientific activity
Milestones:
03/2032: Delivery of interim reports
03/2033: Delivery of final report on activity
Risks: Reduced scientific impact of mission
PSM WPDs
POST-OPERATIONS
Disc-Planet Interactions
Leader: Wilhelm Kley
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 45/152
PSM WP 116 320
04/2030 — 03/2033
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 evolution and mass
growth for interpretation of the full PLATO data set. Update simulation codes, adapt 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
4.
Maintain library of simulation outputs based on most recent theoretical developments
5.
Simulate formation and evolution of individual systems discovered by PLATO to interpret key discoveries
Input:
1.
Scientific literature
2.
PLATO Red Book
3.
PLATO observational data
4.
Commonly available codes within the PLATO community or freely available
Dependencies:
Close interactions foreseen with all sub-packages within WP 116
Output:
1.
New theoretical insights into physical mechanisms of planet migration and mass growth in discs
2.
Increased knowledge about the long-term evolution of planets and planetary systems
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 disc-planet simulations
2.
Fully maintained library of simulated planetary systems for comparison with new discoveries
3.
Prescriptions for mass growth and migration for input into global planet formation simulation models
4.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 46/152
The Assembly of Planetary Systems
Leader: Yann Alibert & Anders Johansen
Rev.: 5
Post-operations phase
PSM WP 116 330
04/2030 — 03/2033
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 full PLATO data. Update simulation
codes, and examine formation scenarios for individual systems discovered by PLATO.
Tasks:
1.
Continued review of the scientific literature in this area
2.
Take into account results of other WPs (and literature) regarding key processes
3.
Simulate formation scenarios for individual systems discovered by PLATO to provide interpretation of
key discoveries
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book
PLATO observational data
Commonly available codes within the PLATO community or freely available
Dependencies:
Close interactions foreseen with the all subpackages within WP 116, in particular with WP 116 310, WP 116 320
(input), WP 116 340 and WP 116 380 (output)
Output:
1.
New theoretical insights into mechanisms of planet formation
2.
Synthetic planet populations generated using state-of-the-art theoretical models
3.
Formation scenarios for PLATO discoveries and associated scientific publications
Deliverables:
1.
State of the art software tools for planet formation simulations
2.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final report
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
The Post-Formation Long-Term Dynamical Evolution
of Planetary Systems
Leader: Alessandro Morbidelli
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 47/152
PSM WP 116 340
04/2030 — 03/2033
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 the full
PLATO data set. 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 processes in the long-term evolution of
planetary systems
3.
Maintain library of simulation outputs based on most recent theoretical developments
4.
Simulate formation and evolution scenarios to explain the origin of the systems discovered by PLATO
5.
Undertake statistical comparison between PLATO data and outputs from theoretical models.
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book
PLATO observational data
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.
Characterising the long-term evolution of planetary systems, from the instability phase to the final
settling into a new stable configuration. Influence of tides on 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
Deliverables:
1.
Fully maintained library of simulated planetary systems for comparison with new discoveries, and for
statistical comparison with exoplanet data sets
2.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks: Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Planetary Formation and Orbital Evolution
Leader: Richard Nelson
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 48/152
PSM WP 116 350
04/2030 — 03/2033
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:
Finalise development of models of planet formation and evolution in binary systems, including both circumbinary
planets and planetary systems with external binary companions. The models will consider all phases of
planetary formation, and the long-term evolution after disc dispersal. Make predictions to compare with the full
PLATO dataset on a statistical basis, and with reference to key individual discoveries.
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, …)
4.
Simulations that examine long-term dynamical evolution
5.
Modelling of key systems observed by PLATO to provide formation and evolution history
6.
Statistical comparison between model predictions and complete PLATO data set.
7.
Critical analysis of model fits in the light of PLATO discoveries
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red book
Full PLATO data set
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 complete PLATO data set and simulation results
Model fits for high profile systems discovered by PLATO
Deliverables:
Interim report on scientific activity
Final report on scientific activity
Milestones:
03/2032: Delivery of preliminary reports.
12/2032: Final report
Risks: Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 49/152
Influence of Birth Environment on the Formation and
Evolution of Planetary Systems
Leader: Melvyn Davies
Rev.: 5
Post-operations phase
PSM WP 116 360
04/2030 — 03/2033
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 theoretical research into the effects of stellar birth environments on planetary systems given the
planetary systems detected by PLATO. Assess the influence of birth environment on the total PLATO
population.
Tasks:
1.
Continued review of the scientific literature in this area.
2.
A reassessment in light of PLATO results of the effects of birth environments on planetary systems
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:
Close interactions foreseen with all sub-subpackages within WP 116 300 particularly with WP 116 330 and WP
116 340.
Output:
Ongoing review of published knowledge. Development of theory (as required) to fully exploit PLATO data in this
area. Library of simulations of planetary systems evolved under influence of environmental factors.
Deliverables:
Reports.
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final report
Risks:
Reduced scientific impact of mission
PSM WPDs
POST-OPERATIONS
Post-Main Sequence Evolution of Planetary Systems
Leader: Mark Wyatt
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 50/152
PSM WP 116 370
04/2030 — 03/2033
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 PLATO results. Examine 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:
Final report on scientific activity
Milestones:
03/2033: Delivery of final reports
Risks:
Reduced scientific impact of mission
PSM WPDs
POST-OPERATIONS
Statistical Comparison Between Theory and PLATO
Data
Leader: Christoph Mordasini
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 51/152
PSM WP 116 380
Post-operations phase
04/2030 — 03/2033
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:
Final comparison of extracted statistics of simulated planetary systems and full PLATO data
Tasks:
1.
Continued review of the scientific literature in this area
2.
Update comparison software to adapt to new observational results and theoretical developments
3.
Maintain and update library of simulation outputs based on most recent theoretical developments
4.
Usage of cutting edge statistical tools to compare PLATO data and theoretical models. In-depth analysis
of the statistical comparison of the predicted and observed radius, distance, eccentricity, mass, inclination,
multiplicity distributions etc. Derivation of statistical constraints on planetary internal structures from mass-radius
relation. Constraints for underlying properties of multi-planet systems.
5.
Final analysis 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 final statistical constraints for theoretical descriptions in formation and evolution models
Input:
1.
2.
3.
4.
5.
Scientific literature
PLATO observational data
PLATO performance characteristics for usage as synthetic observational bias
New output of theoretical models
Commonly available codes within the PLATO community or freely available
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). Constraints for the WP 116 100 and WP 116 200.
Output:
1.
Final assessment of the theoretical description by comparison with PLATO data
2.
Ongoing review of published knowledge
3.
Updated and adapted software tools for statistical comparison
4.
Online visualization and comparison tools for synthetic and actual population wide results, potentially via
a public online interactive web interface
Deliverables:
1.
Final statistical comparison tools and library
2.
Statistical key quantities encapsulated in statistical indicators (e.g. KS tests and correlation coefficients)
3.
Constraints and feedback for theoretical models
4.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final report
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 52/152
Atmospheres of PLATO Terrestrial Planets
Leader: John Lee Grenfell
Rev.: 5
Post-operations phase
PSM WP 116 400
04/2030 — 03/2033
Institution: DLR (Germany)
Key Personnel: J. L. Grenfell; H. Rauer (DLR); 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:
03/2032: Delivery of interim reports
03/2033: Delivery of final report on WP activity
Risks:
Reduced scientific impact of mission.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 53/152
Dynamical Interactions in Multi-Planet Systems
Leader: Jacques Laskar
Rev.: 5
Post-operations phase
PSM WP 116 600
04/2030 — 03/2033
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
of the full PLATO data set. Examine the global dynamics in the vicinity of individual systems discovered by
PLATO. Use dynamical constraints to characterise the multi-planet PLATO systems. Use the follow-up data to
improve the analyses of the Operation phase.
Tasks:
1.
Continuously review relevant scientific literature
2.
Maintain and improve software tools for the dynamical analysis of PLATO systems, including follow up
data.
3.
Perform global dynamical analysis of multi-planet systems discovered by PLATO to provide
interpretation of key discoveries, including follow up data.
4.
Perform stability analysis for both orbital and rotational evolution for multi-planet PLATO systems,
including follow up data.
Input:
1.
2.
3.
4.
Relevant scientific literature and theoretical developments
PLATO data and discoveries
PLATO systems follow-up data.
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.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Long-Term Dynamical Evolution of Planetary
Systems
Leader: Jacques Laskar
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 54/152
PSM WP 116 610
04/2030 — 03/2033
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, including follow up
data.
Tasks:
1.
2.
3.
data.
4.
5.
Continued review of the scientific literature in this area
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, including follow up
Provide in-depth analysis on the long-term behaviour for selected systems, including follow up data.
Statistical analysis of long-term stability 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 all sub-packages within WP 112, WP 113, WP 114, WP 115, 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, including follow up data.
4.
Detailed analysis of long-term evolution for selected PLATO systems and associated scientific
publications
Deliverables:
1.
Fully maintained database for long-term stability of PLATO systems.
2.
2033: Final report on activities
Milestones:
03/2032 Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Stability and Resonances in Multi-Planet Systems
Leader: Jacques Laskar
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 55/152
PSM WP 116 620
04/2030 — 03/2033
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, including follow up data with specific analysis
on resonant systems.
Tasks:
1.
Continuously review relevant scientific literature
2.
Maintain software tools for a fast analysis of global dynamics of multi-planet systems.
3.
Analyse the global dynamics of selected PLATO systems, using input from WP 116 610, including follow
up data
4.
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, including follow up data.
4.
Detailed analysis the global dynamics for the resonant PLATO systems and associated scientific
publications.
Deliverables:
1.
Fully maintained database for global dynamics for a selection of PLATO systems.
2.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Tidal Dissipation and Evolution of Multi-Planet
Systems
Leader: Alexandre C. M. Correia
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 56/152
PSM WP 116 630
04/2030 — 03/2033
Institution: University of Aveiro (Portugal)
Key Personnel: A. Correia
Objectives:
Continue to provide on-going theoretical research in tidal dissipation and evolution of planets in multiple
systems. Undertake a statistical analysis of the tidal evolution of multiple systems discovered by PLATO. Derive
constraints for the formation process and internal structures of the planets in general.
Tasks:
1.
Continuously review relevant scientific literature
2.
Theoretical research to improve the understanding of tidal dissipation and evolution in multi-planet
systems
3.
Maintain and improve software tools for the long-term tidal evolution of PLATO systems
4.
Undertake a statistical analysis of the tidal evolution of multiple systems discovered by PLATO
5.
Derive constraints for the formation process and internal structures of the planets in general
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
2.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of mission
PSM WPDs
POST-OPERATIONS
Rotational Evolution of Planets in Multiple Systems
Leader: Gwenaël Boué
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 57/152
PSM WP 116 640
04/2030 — 03/2033
Institution: IMCCE, Observatoire de Paris (France)
Key Personnel: G. Boué
Objectives:
Undertake a statistical analysis of planetary rotation in the full set of multiple systems discovered by PLATO.
Examine orbital forcing on climate of individual systems detected by PLATO to infer constraints on their
habitability.
Tasks:
1.
Continued review of the scientific literature in this area
2.
Theoretical research to improve understanding of the rotation motion in planetary systems
3.
Maintain the library of rotational dynamics of PLATO detected planets
4.
Simulate the long-term rotation of individual systems discovered by PLATO to provide constraints on
their habitability and/or to emphasize key dynamical behaviours
5.
Undertake statistical analysis of the rotation dynamics within the PLATO population
Input:
1.
2.
3.
4.
Scientific literature
PLATO Red Book
PLATO observational data
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 spin-orbit interaction and long term rotation motion in multiple systems
2.
Long-term rotational dynamics for PLATO discoveries and associated scientific publications
3.
Constraints on the climate evolution of the PLATO population detected in the habitable zone
Deliverables:
1.
Fully maintained library of rotation dynamics in planetary systems detected by PLATO
2.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Planetary Ephemerides of PLATO Systems
Leader: Agnes Fienga
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 58/152
PSM WP 116 650
04/2030 — 03/2033
Institution: Observatoire de la Côte d’Azur (France)
Key Personnel: A. Fienga
Objectives:
Develop a planetary ephemerides database for all PLATO multi-planet systems, including follow up data.
Tasks:
1.
Continued review of the scientific literature in this area
2.
Maintain software tools for a fast elaboration of planetary ephemerides including follow up data.
3.
Elaborate planetary ephemerides for all PLATO systems, including follow up data.
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 all PLATO planetary systems including follow up data.
3.
Ongoing review of published knowledge
Deliverables:
1.
Fully maintained database for the ephemerides of all PLATO multi planet systems.
2.
2033: Final report on activities
Milestones:
03/2032: Delivery of preliminary reports
03/2033: Final reports
Risks:
Reduced scientific impact of the mission.
PSM WPDs
POST-OPERATIONS
Specifications for Interface to Other PSM WPs and
PDC
Leader: Nuno Santos
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 59/152
PSM WP 117 000
04/2030 — 03/2033
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
Dependencies:
Stellar work packages WP 121/122/124/125/126/127/128
Output:
Report results
Deliverables:
Report
Milestones:
12/2031: Delivery of interim reports
03/2033: Delivery of final report on activity
Risks:
Low risk
PSM WPDs
POST-OPERATIONS
Stellar Science Coordination
Leader: Marie-Jo Goupil
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 60/152
PSM WP 120 000
04/2030 — 03/2033
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.) for the last PLATO runs
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 specification for both algorithm and tools
7. Review scientific validation
Input:
Updated stellar models and validated algorithms from sub-packages
Dependencies:
Input from and output from PDC (WP 350) and PSM (WP 100, WP 130, WP 160); PLATO End-to-End Simulator.
Output:
1.
Updated scientific specifications of both, tools and algorithms
2.
Updated stellar models
Deliverables:
Reports and updated specifications and stellar models
Milestones:
03/3030: Final validation of the third generation of models and procedures related to the characterization of stars
of the core program.
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Stellar Models
Leader: Marc-Antoine Dupret
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 61/152
PSM WP 121 000
Post-operations phase
04/2030 — 03/2033
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:
Validate and increase the accuracy of grids of stellar models and associated frequencies.
Tasks:
Coordination of works from work packages WP 121 100 to WP 121 500.
Use PLATO data to test and increase the accuracy of stellar models and associated frequencies computed in
the previous phases.
Input:
Grids of stellar models computed in the previous phases
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.
PLATO seismic constraints from WP 124 000
Output:
Grids of third generation stellar models, evolutionary tracks and oscillation frequencies.
Deliverables:
Updated validated stellar model grids, evolutionary tracks and oscillation frequencies, with full documentation.
Milestones:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects.
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
1D Stellar Models
Leader: Yveline Lebreton
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 62/152
PSM WP 121 100
Post-operations phase
04/2030 — 03/2033
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 previously refined stellar models grids of very low mass to
intermediate mass stars covering evolutionary stages from pre main sequence to subgiant stages.
2.
Implement in stellar evolution codes further improvements in the physics that will be provided by WP 121
200, WP 121 300, WP 121 400 and WP 122 000 (model atmospheres), WP 123 200 (surface convection), WP
127 100.
3.
Further refine the grids of models and provide the associated oscillation spectra.
4.
Perform a new iteration of comparison of improved grids with PLATO data.
Input:
1.
Existing stellar evolutionary codes appropriate to calculate MS and subgiant branch stellar models.
2.
Existing stellar oscillation codes.
3.
Model atmospheres to be used as boundary conditions (from WP 122 000).
4.
Improved formulations for heat, chemical element and angular momentum transport and other physical
processes from WP 121 200, WP 121 300, WP 121 400, WP 123 200, 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:
Grids of stellar models, evolutionary tracks and oscillation frequencies.
Deliverables:
Updated validated stellar model grids, evolutionary tracks and oscillation frequencies, with full documentation.
Milestones:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Very Low-Mass Stellar Models
Leader: Santi Cassisi
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 63/152
PSM WP 121 110
Post-operations phase
04/2030 — 03/2033
Institution: INAF - Astronomical Observatory of Teramo (Italy)
Key Personnel: S. Cassisi; M. Salaris (INAF-Teramo); A. Pietrinferni (INAF-Teramo)
Objectives:
Final validation of the stellar models for VLM stars.
Tasks:
1. Possible extensions of the stellar model grids; comparisons with alternative models provided by other
participating scientists
2. Detailed testing of the approaches used for accounting non-canonical processes in stellar model
computations, by means a careful comparison with PLATO data for specific stellar targets
3. On-demand computing of specific stellar models for selected PLATO targets
4. Documentation and publication of the stellar model grids
Input:
Existing model grids and PLATO data
Dependencies:
Input from and output from PDC (WP 370) and WP 121 100, WP 121 300, WP 122 400, WP 123 100
Output:
Updated Stellar Models
Deliverables:
Reports and updated stellar models
Milestones:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Low Mass Stellar Models
Leader: Josefina Montalban
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 64/152
PSM WP 121 120
04/2030 — 03/2033
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:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects
Risks: Acceptable risks
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 65/152
Theoretical Oscillation Frequencies
Leader: Juan Carlos Suárez
Rev.: 5
Post-operations phase
PSM WP 121 130
04/2030 — 03/2033
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. 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. When the third generations of stellar models are obtained, to calculate the corresponding theoretical
oscillation frequencies.
Input:
Existing model grids and PLATO data
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:
Updated stellar models
Deliverables:
Reports and updated stellar models
Milestones:
03/3030: Optimization of the theoretical stellar oscillation frequencies for selected PLATO objects; delivery of
new input to stellar evolution theory community based on PLATO key objects.
Risks:
Acceptable risks of delay interpreting unexpected observations coming from PLATO.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 66/152
Transport Processes
Leader: Ana Palacios
Rev.: 5
PSM WP 121 200
Post-operations phase
04/2030 — 03/2033
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.
Follow up on the results obtained in models including transports processes
2.
Proposition of new formulations/implementations if required
Input:
Existing stellar model grids and evolutionary codes (STAREVOL, GENEC, CESTAM).
Existing asteroseismic constraints
Dependencies:
Output to WP 121 100 – 1D stellar models, and WP 121 500
Output:
Updated stellar models
Deliverables:
Reports and updated stellar models
Milestones:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects
Risks: Acceptable risks
PSM WPDs
POST-OPERATIONS
PMS Evolution
Leader: Joao Pedro Marques
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 67/152
PSM WP 121 300
Post-operations phase
04/2030 — 03/2033
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 updated stellar models of PMS.
Tasks:
1. Validation work of the procedures to derive stellar characteristics of PMS objects (mass, radius, age, rotation
period, stellar activity model etc.) for the last PLATO runs.
2. Derivation of new specifications for 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
the physical description of stars using the latest generation of stellar models.
5. Impact of the improvements of the description of the PMS phase on MS models
Input:
Existing model grids and PLATO data.
Dependencies:
Input from and output to PSM WP 121 200 - WP 121 400 - WP 121.
Output:
1.
Updated scientific specifications of both tools and algorithms.
2.
Updated stellar models.
Deliverables:
Reports and updated stellar models and specifications
Milestones:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects
Risks: Acceptable risks.
PSM WPDs
POST-OPERATIONS
2D / 3D Stellar Evolution Models
Leader: Michel Rieutord
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 68/152
PSM WP 121 400
04/2030 — 03/2033
Institution: IRAP (France)
Key Personnel: M. Rieutord; B. Dintrans (IRAP); F. Lignières (IRAP); J. Ballot (IRAP); L. Jouve (IRAP)
Objectives:
The objectives of this last part will be to derive all the astrophysical consequences from the results obtained
during the previous years, concerning the planet and star formation etc.
Tasks:
Improvements of the physical description of the models based on what will be learned with PLATO on stars
Input:
Existing 2D/3D codes
Dependencies:
Existing codes
Output:
Updated 2D/3D codes
Deliverables:
Update 2D/3D codes and associated documentation
Milestones:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects
Risks:
Acceptable risks
PSM WPDs
POST-OPERATIONS
Evolution of Stars in Multiple Systems
Leader: Stéphane Mathis
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 69/152
PSM WP 121 500
04/2030 — 03/2033
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 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 implementation and operation phases has allowed to give the best
characterization as possible of multiple systems observed 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 multiple systems.
4. Coordination of the theoretical work based on all obtained PLATO seismic data to learn more about the
evolution of stars in multiple systems. This will give further improvements in the physical description of stars and
contribute to the building of a new generation of stellar models. This will then provide an improved accuracy for
the derived stellar characteristics.
5. Participation of review meetings gathering the leaders of PSM WPs.
Input:
Existing model grids and PLATO data.
Dependencies:
Input and output from PDC (WP 370) and PSM.
Output:
Updated stellar models.
Deliverables:
Reports and updated stellar models.
Milestones:
03/3030: Optimization of the stellar model grids for selected PLATO objects; delivery of new input to stellar
evolution theory community based on PLATO key objects
Risks: Minimal risks.
PSM WPDs
POST-OPERATIONS
Non-Seismic Diagnostics and Model Atmospheres
Leader: Thierry Morel
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 70/152
PSM WP 122 000
04/2030 — 03/2033
Institution: University of Liège (Belgium)
Key Personnel: T. Morel (Liège)
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 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 an updated, third-generation grid of model atmospheres and limbdarkening 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:
Existing model grids and PLATO data
Dependencies:
Input/output from and to PDC (WP 370 000) and PSM (WP 121 000, WP 123 000, WP 125 000, WP 127 000,
WP 131 000, and WP 140 000)
Output:
1.
Updated scientific specifications of both tools and algorithms
2.
Updated stellar models
Deliverables:
Reports and updated stellar models and specifications
Milestones:
03/3030: Theoretical developments to improve the physical description of stellar atmospheres.
03/3033: Delivery of updated, third-generation grid of validated model atmospheres and limb-darkening
coefficients, as well as procedures related to the non-seismic characterization of host stars.
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
1D Model Atmospheres
Leader: Bertrand Plez
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 71/152
PSM WP 122 100
04/2030 — 03/2033
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:
Provide final grids of model atmospheres for PLATO analysis.
Tasks:
1.
Compute the final 1D model atmosphere grid.
2.
Produce the final database that contains the output of the theoretical calculations (e.g., 1D model
atmospheres and associated model fluxes).
Input:
Observational and catalogue data from various facilities (ground-based spectrographs, Gaia, PLATO, etc.),
physical data (line lists)
Dependencies:
Other WP 122 000 sub-packages, WP 121 000, WP 123 000, WP 127 000, WP 131 000, and WP 140 000
Output:
Final grids of models and synthetic spectra.
Deliverables:
1.
Detailed report on accomplished work and reasons for the choices that were made.
2.
Final grid of model atmospheres for FGKM stars in 1D.
Milestones:
03/3030: Theoretical developments to improve the physical description of stellar atmospheres.
03/3033: Delivery of updated, third-generation grid of validated model atmospheres.
Risks:
PSM WPDs
POST-OPERATIONS
3D Model Atmospheres
Leader: Martin Asplund
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 72/152
PSM WP 122 200
04/2030 — 03/2033
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:
Complete computation of 3D hydrodynamical stellar model atmospheres.
Tasks:
Refine 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 previous phases
Dependencies:
Other WP 122 000 sub-packages, WP 121 000, WP 123 000, and WP 127 000
Output:
Final grid of 3D stellar atmospheres
Deliverables:
Reports and final atmosphere models
Milestones:
03/3030: Theoretical developments to improve the physical description of stellar atmospheres.
03/3033: Delivery of updated, third-generation grid of validated model atmospheres.
Risks: None. The key personnel have the needed expertise.
PSM WPDs
POST-OPERATIONS
Fundamental Stellar Parameters
Leader: Carlos Allende Prieto
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 73/152
PSM WP 122 300
04/2030 — 03/2033
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: C. Allende Prieto; A. Amarsi (ANU); M. Ammler-von-Eiff (MPSSR); P. Barklem (Uppsala);
M. Bergemann (MPIA); C. del Burgo (INAOE); L. Casagrande (ANU); L. Fossati (Argelander); J. I. González
Hernández (IAC); L. Koesterke (Texas); K. Lind (Uppsala); L. Mashonkina (Moscow); Y. Maqueo Chew (UNAM);
T. Merle (ULB); R. Monier (Meudon); D. Mourard (Nice); N. Nardetto (Nice); A. Sozzetti (Torino)
Objectives:
Complete the computation of grids of model fluxes for FGKM stars. Provide final stellar parameters for the
FGKM stars of interest observed by PLATO.
Tasks:
1.
2.
3.
4.
data.
Provide final grids of model fluxes.
Evaluate the uncertainties in the models.
Produce a final version of the database that contains the outputs of theoretical calculations.
Produce a final database that contains the parameters of the FGKM stars derived including non-seismic
Input:
External databases (Gaia, ground-based multi-object spectrographs, space spectrophotometry) and follow-up
PLATO data. 1D and 3D model atmospheres of FGKM stars.
Dependencies:
Other WP 122 000 sub-packages, WP 125 000, WP 131 000, and WP 140 000
Output:
Final grids of model fluxes for FGKM stars. Final values of the stellar parameters for the FGKM stars observed
by PLATO.
Deliverables:
Final grids of theoretical spectra. Documentation on uncertainties.
Milestones:
03/3030: Theoretical developments to improve the physical description of stellar atmospheres.
03/3033: Delivery of updated, third-generation grid of theoretical spectra.
Risks:
PSM WPDs
POST-OPERATIONS
Limb Darkening
Leader: Antonio Claret
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 74/152
PSM WP 122 400
Post-operations phase
04/2030 — 03/2033
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:
Identify and quantify the sources of uncertainties in the limb-darkening coefficients of the host stars.
Tasks:
Systematic comparison between theoretical limb-darkening coefficients and those obtained empirically by the
PLATO mission. As an additional task, we plan to investigate the influence of the coefficients of limb-darkening
on the absolute dimensions of the exoplanets.
Input:
PLATO data
Dependencies:
WP 110 000
Output:
Updated scientific specifications of the limb-darkening coefficients
Deliverables:
Reports and scientific specifications.
Milestones:
03/3030: Theoretical developments to improve the physical description of stellar atmospheres.
03/3033: Delivery of updated, third-generation grid of validated limb-darkening coefficients, as well as
procedures related to the non-seismic characterization of host stars
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
Interstellar Extinction
Leader: Douglas Marshall
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 75/152
PSM WP 122 500
04/2030 — 03/2033
Institution: Université Paris Diderot / CEA (France)
Key Personnel: D. Marshall; S. Sale (Oxford); J. Linsky (Colorado); R. Hanson (MPIA); K. Dobashi (Tokyo.);
J. Montillaud (Franche-Comté); E. Amores (Estadual de Feira de Santanta)
Objectives:
Provide values of anticipated extinction along different lines of sight. Ensure that interstellar extinction is handled
properly to enable precision estimates of stellar parameters.
Tasks:
1.
2.
3.
4.
Handle requests for extinction determination on reprocessed data
Perform validation on derived extinction values
Evaluate uncertainties on extinction estimates
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. Software module.
Deliverables:
Software test report, validation report
Milestones:
12/2027: Explore other extinction estimates
12/2029: Validation of the extinction estimates for individual stars
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
Stellar Activity and Rotation
Leader: Antonino Francesco Lanza
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 76/152
PSM WP 123 000
04/2030 — 03/2033
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 work of the work packages WP 123 100 to WP 123 600.
Tasks:
1. Coordination of the work to derive new specifications of procedures, algorithms, and theoretical models for
the final exploitation of PLATO data, if necessary;
2. Coordination of the final work (rotation and magnetic activity studies) on PLATO data of the stars of the core
program;
3. 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 finalize the delivery of the third generation of stellar models. It will then provide a finally improved
accuracy for the derived stellar characteristics and final products of the mission;
4. Organization of working and review meetings gathering the leaders of the WPs
Input:
PLATO data and existing models and procedures.
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 both, tools and algorithms.
Deliverables:
Reports and scientific specifications.
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary, for the last runs obtained during
the operation phase.
03/3033: Final theoretical developments to improve the physical description of stellar rotation and magnetic
activity, including the scaling relationships with global stellar parameters, based on our improved knowledge of
stellar physics; delivery of the final products of our studies.
Risks: Acceptable risks are foreseen.
PSM WPDs
POST-OPERATIONS
Spot Models
Leader: Benoît Mosser
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 77/152
PSM WP 123 100
Post-operations phase
04/2030 — 03/2033
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. Deriving improved and final observational results: spots models, rotation rates, differential rotations rates,
spot lifetimes
2. Deriving final observational results: spots models, rotation rates, differential rotations rates, spot lifetimes
3. Delivering theoretical improvements
4. Follow up observations
Input:
Implemented procedures
Dependencies:
Models of different contributions from WP Stellar Science/Stellar Activity
Output:
Updated scientific specifications of both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary, for the last runs obtained during
the operation phase.
03/3033: Final theoretical developments to improve the physical description of stellar rotation and magnetic
activity, including the scaling relationships with global stellar parameters, based on our improved knowledge of
stellar physics; delivery of the final products of our studies.
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Surface Convection (1D & 3D)
Leader: Friedrich Kupka
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 78/152
PSM WP 123 200
04/2030 — 03/2033
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. Simulations of stellar surface convection for the last PLATO runs
2. Possible revisions of the final generation of models and simulations of stellar granulation to optimize the
reliability of the procedures derived for the determination of stellar characteristics with the updated third
generation of stellar models based on the improvements in the model and simulation physics resulting
from earlier PLATO runs
Input:
Stellar models
Dependencies:
This WP is part of the WP 123 000.
Output:
Updated stellar models
Deliverables:
Reports and updated stellar models
Milestones:
07/2031: Theoretical developments to improve the 1D & 3D models of stellar granulation based on our
improved knowledge of stellar physics
12/2031: Delivery of these models to allow the production of the updated third generation of validated models
and procedures related to the characterization of host stars
Risks:
Acceptable risks
PSM WPDs
POST-OPERATIONS
Models of Rotational Evolution and Gyrochronology
Leader: Marc Pinsonneault
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 79/152
PSM WP 123 300
04/2030 — 03/2033
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.
Produce calibrated gyrochronology ages for PLATO targets.
2.
Explore mixing as a diagnostic of angular momentum transport.
3.
Test models of angular momentum evolution against internal and surface rotation diagnostics
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:
Age measurements for PLATO targets as a function of rotation, evolutionary state, mass, and composition;
calibrated stellar models including rotation and rotational mixing
Deliverables:
Ages and updated stellar models
Milestones:
12/2031: Explore consequences of next-generation models including rotation and refine age estimates.
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
Dynamos and Differential Rotation
Leader: A.S. Brun
Post-Operation phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 80/152
PSM WP 123 400
04/2030-03/2033
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:
•
•
proxies
•
•
Wrapping up coordination of theoretical and modelling effort of stellar rotation proxy for solar-like stars
Wrapping up coordination of theoretical and modelling effort of stellar dynamo and magnetic activity
Final code maintenance and development
Final reports on WP progress, participation to PSM meetings
Input:
•
Seismic inversion of internal rotation profile (WP 125 000)
•
Extent of convective envelope (WP 126 000), 1-D stellar state (WP 121 100) for 3-D models
•
Proxies of magnetic activity (WP 125 000)
Dependencies:
WP 120 000 and sub-WP 12x xxx
Output:
(WP 121 000, 124 000, 127 000)
•
Final scaling laws of differential rotation and activity levels as a function of spectral type
•
Final realistic 3-D Simulations of extended PLATO targeted stars
•
Final updates on specifications of algorithms and tools
Deliverables:
Data base of multi-D numerical simulations of convection, rotation, turbulence & magnetism of a selection of
PLATO targeted stars
Regular reports of advancement of WP, regular meeting with PSM WP and sub-WP leaders
Milestones:
12/2031: Version 2 of scaling laws (differential rotation, magnetic activity, convective power) to be implemented
in stellar evolution models
Regular reports of advancement of WP, regular meeting with PSM WP and sub-WP leaders
Risks: Lack of precision of inverted convection extent, differential rotation profiles and magnetic activity
PSM WPDs
POST-OPERATIONS
Tools to Measure Rotational Modulation
Leader: Sergio Messina
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 81/152
PSM WP 123 500
04/2030 — 03/2033
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. To 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. To 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. To validate the results obtained for the stellar rotation period, estimate of the surface differential rotation, spot
lifetimes;
4. To validate that the procedures to use spectroscopic rotation measurements to improve and check results
work properly;
Input:
Implemented methods and algorithms
Dependencies:
1. Output for WP 123 300 and WP 123 400
2. Input from WP 123 100
Output:
Updated scientific specifications of both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary, for the last runs obtained during
the operation phase;
03/3033: Final theoretical developments to improve the physical description of stellar rotation and magnetic
activity, including the scaling relationships with global stellar parameters, based on our improved knowledge of
stellar physics; delivery of the final products of our studies.
Risks:
Optical flux modulation dominated by star spot 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
POST-OPERATIONS
Stellar Rotation from Transits
Leader: Adriana Valio
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 82/152
PSM WP 123 600
04/2030 — 03/2033
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 the 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. If the average rotation period of the star is known, or the rotation
period at different latitudes from multiple transiting planets, then by assuming a solar like differential rotation
profile, or another given one, it may be possible to determine the differential rotation profile of the star.
Tasks:
1. Upgrade the spot detection algorithm to run with PLATO data;
2. Validate the spot modelling that infers its 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 and its differential rotation with more precision;
4. Advance the correlation laws between stellar rotation and stellar age.
Input:
Implemented procedures
Dependencies:
Transit light curves; planet/companion orbital parameters (such as period and inclination angle), stellar
parameters (mass, radius, effective temperature).
Output:
Updated scientific specifications of both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/2031: Improve the algorithm for spot detection and modelling for the last runs of PLATO data, if necessary.
03/2032: Further meliorate the theoretical models of stellar differential rotation profiles and how they relate to
stellar convection and magnetic dynamos.
03/2033: Deliver the third generation of validated models and procedures for spot characterization and stellar
rotation period at different latitudes of the star.
Risks: Acceptable risks
PSM WPDs
POST-OPERATIONS
Seismic Diagnostics
Leader: Margarida Cunha
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 83/152
PSM WP 124 000
04/2030 — 03/2033
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 work related to the further development of seismic diagnostic tools, if found necessary as
results of the analysis of PLATO last runs and improved analysis of PLATO best targets.
2.
Coordinate any necessary updates of the algorithms for forward, inverse, and glitch-related approaches
in accordance to the results of point 1.
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 WP 124 100 to 124
300.
Dependencies:
Input from and output to WPs 124 100 to 124 300 and from WP 120 000
Output:
Updated scientific specifications of both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/3030: Delivery of updated algorithms (if relevant) for forward and inverse procedures.
Risks: Minimal risk
PSM WPDs
POST-OPERATIONS
Forward Approaches
Leader: Ian Roxburgh
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 84/152
PSM WP 124 100
04/2030 — 03/2033
Institution: Queen Mary University of London (UK)
Key Personnel: I. Roxburgh; S. Vorontsov (QMUL); M. Cunha (Porto); M. Bazot (Porto)
Objectives:
Evaluate the need for, and implement further developments of the forward procedures used for the
determination of the mass, radius, age, and others properties of planet-host stars.
Tasks:
1.
Evaluate the need for further development of the forward procedures, based on the results of the
analysis of PLATO last runs, as well as on the results of detailed analysis of PLATO best targets.
2.
Develop/adapt forward procedures, in accordance to the results of the evaluation carried out in point 1.
3.
Implement any necessary updates to the algorithms for forward procedures, in accordance to the results
of point 2.
Input:
Implemented procedure; PLATO data
Dependencies:
Input from and output to WP 124 000
Output:
Updated scientific specifications of both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/3030: Delivery of updated algorithms (if relevant) for forward procedures.
Risks: Minimal risk
PSM WPDs
POST-OPERATIONS
Inverse Techniques
Leader: Daniel Reese
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 85/152
PSM WP 124 200
Post-operations phase
04/2030 — 03/2033
Institution: University of Birmingham (UK)
Key Personnel: D. Reese; G. Buldgen (Liège); I. Roxburgh (QMUL); S. Deheuvels (OMP, IRAP)
Objectives:
Insure quality of final inversion output from PDC
Tasks:
1.
Make further recommendations to improve inversion procedure(s), if found necessary as a result of the
analysis of the last PLATO runs.
2.
Validate any further modifications to inversion procedures, and associated output.
Input:
Implemented procedures
Dependencies:
Input from and output to WP 124 000
Output:
Updated scientific specifications of both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/3030: Delivery of updated algorithms (if relevant) for inverse procedures.
Risks: Minimal risk
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 86/152
Acoustic Glitches
Leader: Sébastien Deheuvels
Rev.: 5
PSM WP 124 300
Post-operations phase
04/2030 — 03/2033
Institution: Observatoire Midi-Pyrénées, IRAP (France)
Key Personnel: S. Deheuvels; M. Monteiro (CAUP); M. Cunha (Porto); J. Ballot (IRAP); D. Reese (Birmingham)
Objectives:
Evaluate the need for, and implement if needed further developments of the procedures implemented to extract
the properties of acoustic glitches.
Tasks:
1.
Propose improvements (if needed) to the procedures developed in the previous phases to estimate the
depths of acoustic glitches and the size of convective cores.
2.
Implement these improvements in the existing algorithms.
Input:
Procedures established during the development phase and updated in the operation phase. PLATO data
Dependencies:
Input from and output to WP 124 000
Output:
Updated description of procedures.
Deliverables:
Reports on the tests with PLATO data and updated algorithms.
Milestones:
03/3030: Delivery of updated algorithms (if relevant) for modelling acoustic glitches.
Risks: Minimal risk
PSM WPDs
POST-OPERATIONS
Determination of Stellar Parameters
Leader: Jørgen Christensen-Dalsgaard
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 87/152
PSM WP 125 000
04/2030 — 03/2033
Institution: Aarhus University (Denmark)
Key Personnel: J. Christensen-Dalsgaard; Hans Kjeldsen (Aarhus); B. Chaplin (Birmingham)
Objectives:
Review the application that has been made 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. Evaluate the need
for reanalysis of the whole PLATO data set in the light of the experience gained.
Tasks:
1. Coordination of the work done by WP 125 100 to 125 400
2. Make sure that the quality of the final outputs from WP 125 100 to 125 400 match the specified
requirements
3. Evaluate whether further updates are needed in the procedures based on the properties of actual PLATO
data
4. Evaluate whether further support observations are required for the full characterization of the PLATO targets
5. Review the asteroseismic insights obtained through the analysis of PLATO data on improvements to the
determination of stellar parameters.
Input:
Procedures, results and documentation from WP 125 100 to WP 125 400
Dependencies:
WP 125 000 is part of the Stellar Science work package, and depends on a large fraction of the results obtained
in the other sub-work-packages.
Output:
Final verification of optimized procedures to determine accurate masses, radii, ages, chemical composition, as
well as full statistical characterization in terms of Probability Density Functions, that satisfy the exoplanet
specifications, with full documentation of the procedures
Deliverables:
Final report on the operations of the procedures to determine accurate masses, radii, ages, chemical
composition as well as uncertainties that satisfy the exoplanet specifications, with full documentation of the
quality of the results.
Milestones:
03/3030: Detailed review of the operations of the procedures and algorithms as carried out throughout the
operations phase.
03/3033: Final evaluation and documentation of quality of the stellar parameters determined as a result of the
final re-analysis. Organization and documentation of the long-term archiving of the PLATO and associated data
and results
Risks: Minimal
PSM WPDs
POST-OPERATIONS
Scaling Laws
Leader: Andrea Miglio
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 88/152
PSM WP 125 100
Post-operations phase
04/2030 — 03/2033
Institution: University of Birmingham (UK)
Key Personnel: A. Miglio; K. Belkacem (LESIA, Paris); J. Montalban (INAF-Padova); B. Mosser (OBSPM);
I. W. Roxburgh (QMUL)
Objectives:
This WP must provide prescriptions to compute mass and radius based on scaling relations using combinations
of seismic and non-seismic pieces of information. It must also provide the uncertainties on the derived quantities
due to underlying simplifying assumptions.
Tasks:
1. Validation of the scaling relations by using third generation stellar models, oscillation frequencies, and mode
amplitudes delivered by WP 121 100 and 126 100,
2.
Update the calibration of the scaling relations using targets with available independent mass/radius
estimates (detached eclipsing binaries, stars in clusters, stars with precise and accurate 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 as well as uncertainties that satisfy the
exoplanet specifications, with full documentation
Milestones:
03/3030: Detailed review of the operations of the procedures and algorithms as carried out throughout the
operations phase.
03/3033: Final evaluation and documentation of quality of the stellar parameters determined as a result of the
final re-analysis. Organization and documentation of the long-term archiving of the PLATO and associated data
and results
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
Incorporating Classical Parameters
Leader: Sofia Feltzing
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 89/152
PSM WP 125 200
04/2030 — 03/2033
Institution: Lund Observatory, Lund University (Sweden)
Key Personnel: S. Feltzing
Objectives:
Review the results from the operations phase and work with the relevant teams to ensure that any updated
procedures are properly implemented.
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 and 121 000
Dependencies:
Input from WP 122 000 and 121 000
Output:
Work with WP 122 000 and WP 121 000 to produce the relevant data for the stellar part of the core program.
Deliverables:
Reports
Milestones:
03/3030: Detailed review of the operations of the procedures and algorithms as carried out throughout the
operations phase.
03/3033: Final evaluation and documentation of quality of the stellar parameters determined as a result of the
final re-analysis. Organization and documentation of the long-term archiving of the PLATO and associated data
and results
Risks: Acceptable risks.
PSM WPDs
POST-OPERATIONS
Seismic Parameters
Leader: Christoffer Karoff
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 90/152
PSM WP 125 300
04/2030 — 03/2033
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:
Implemented procedures
Dependencies:
Input from WP 125 100 and WP 125 200
Output:
Updated scientific specifications of both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/3030: Detailed review of the operations of the procedures and algorithms as carried out throughout the
operations phase.
03/3033: Final evaluation and documentation of quality of the stellar parameters determined as a result of the
final re-analysis. Organization and documentation of the long-term archiving of the PLATO and associated data
and results
Risks:
Acceptable risk
PSM WPDs
POST-OPERATIONS
Open Clusters
Leader: Sarbani Basu
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 91/152
PSM WP 125 400
Post-operations phase
04/2030 — 03/2033
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, use the developed
procedures to determine the properties of stars in open clusters. The fact that the stars are members of an open
cluster will be used to reduce the uncertainties in the inferred stellar properties, noting that internal consistency
amongst cluster stars may be particularly relevant for this. Auxiliary data from other work packages will be used.
A full statistical analysis will be carried out to determine the uncertainties in inferred properties. As a side benefit,
the results will be used to document how stellar models will need to be updated.
Tasks:
Run all data through the pipeline
Complete statistical analysis
Determine is existing stellar models are adequate
Create catalogue of cluster properties.
Input:
PLATO Data
Dependencies:
WP 125 100, WP 125 200 and WP 125 300 and codes created in earlier phases
Output:
Ages, and other properties of stars in clusters along with full statistical characterization in terms of Probability
Density Function.
Deliverables:
Reports
Milestones:
03/3030: Detailed review of the operations of the procedures and algorithms as carried out throughout the
operations phase.
03/3033: Final evaluation and documentation of quality of the stellar parameters determined as a result of the
final re-analysis. Organization and documentation of the long-term archiving of the PLATO and associated data
and results
Risks:
Acceptable Risks
PSM WPDs
POST-OPERATIONS
Mode Physics
Leader: Kevin Belkacem
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 92/152
PSM WP 126 000
Post-operations phase
04/2030 — 03/2033
Institution: LESIA, Observatoire de Paris (France)
Key Personnel: K. Belkacem; F. Baudin (IAS)
Objectives:
1.
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 including oscillations
as well as an estimation and modelling of sub-surface effects (e.g. turbulent pressure, granulation, magnetic
effects) on mode parameters for seismic studies. These developments will benefit from the CoRoT and KEPLER
legacy.
2.
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 both, tools and algorithms
Deliverables:
Reports and scientific specifications
Milestones:
03/3030: Delivery of updated third generation of procedures related to the characterization of host stars, if
necessary.
Risks: Acceptable risks of delay
PSM WPDs
POST-OPERATIONS
Mode Amplitude and Near-Surface Effects on Mode
Parameters Title
Leader: Réza Samadi
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 93/152
PSM WP 126 100
04/2030 — 03/2033
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.
Comparison of the final releases of PLATO seismic data with models developed during the operation
phase.
2.
Interpretation of the observed differences and improvement of the models.
3.
Compute mode frequencies (using the second generation of PLATO stellar models) and apply the near
-surface models developed during the operation phase.
4.
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 (WP370)
Output:
Third generation of models of mode driving and near-surface effects
Deliverables:
Milestones:
03/3030: Delivery of updated third generation of procedures related to the characterization of host stars, if
necessary.
Risks: none
PSM WPDs
POST-OPERATIONS
Mode Line-Width
Leader: Marc-Antoine Dupret
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 94/152
PSM WP 126 200
Post-operations phase
04/2030 — 03/2033
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.
Validation of the previous mode line-width modelling using available PLATO observations
2.
Improvement of time-dependent convection models
3.
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
PLATO data
Dependencies:
WP 126 000, WP 122 100, WP 123 200 and WP 121 000
Output:
Third generation grid of mode line-widths and time-dependent convection model
Deliverables:
Validated mode line-width model.
Milestones:
03/3030: Delivery of updated third generation of procedures related to the characterization of host stars, if
necessary.
Risks: Minimal risk
PSM WPDs
POST-OPERATIONS
Intensity-Velocity Relation
Leader: Günter Houdek
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 95/152
PSM WP 126 300
04/2030 — 03/2033
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 for
the core program.
Input:
PLATO data.
Dependencies:
Input and output from PDC (WP 370) and PSM (WP 100, WP 130, WP 160); PLATO End-to-End Simulator
Output:
1.
2.
Updated scientific specifications of both, tools and algorithms.
Updated stellar models.
Deliverables:
Reports, updated scientific specifications.
Milestones:
03/3030: Delivery of updated third generation of procedures related to the characterization of host stars, if
necessary.
Risks: Acceptable risks.
PSM WPDs
POST-OPERATIONS
Seismology of Magnetic Activity
Leader: Laurent Gizon
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 96/152
PSM WP 126 400
04/2030 — 03/2033
Institution: Max-Planck-Institut für Sonnensystemforschung (Germany)
Key Personnel: L. Gizon; A. Bhagatwala (Stanford); S. Hanasoge (Princeton); H. Schunker (MPSSR)
Objectives:
Continuation of Operations Phase activities, i.e. 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 optimized methods to clean frequencies from magnetic effects
5.
Application of optimized 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 operations phase 3. PLATO seismic analyses of Sun-like stars with planets
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:
03/3030: Delivery of updated third generation of procedures related to the characterization of host stars, if
necessary.
Risks: Acceptable risks.
PSM WPDs
POST-OPERATIONS
Seismic Constraints from Aging stars
Leader: Benoît Mosser
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 97/152
PSM WP 127 000
04/2030 — 03/2033
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:
1.
Validation of evolutionary stellar models of red giants
2.
Validation 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.
3.
Coordination with the activities under WP 121 (stellar models), WP 123 (stellar activity), WP 122 000
(non-seismic diagnostics).
4.
Validation of procedures providing constraints on MS physical process and update of the procedure if
necessary
Tasks:
1.
Coordination of the work done by WP 127 100, 127 200, 127 300, 122
2.
Use PLATO data to define the improvements in the physics to be included in red giant stellar models
physics.
3.
Test that the quality of the outputs from WP 127 100, 127 200, 127 200, and 122 match the specified
requirements
4.
Establish procedures for using the asteroseismic insights obtained through the analysis of PLATO data
to improve the determination of stellar parameters.
Input:
From WP 127 100-300, WP 122, WP 123, WP 124, WP 128 200
Dependencies:
With WP 121, WP 122, WP 124
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:
Optimized procedures to determine accurate masses, radii, evolutionary state, chemical composition, as well as
uncertainties that satisfy the exoplanet specifications, with full documentation.
Milestones:
03/3030: Delivery of updated third generation of validated models and procedures, if necessary.
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
Stellar Models of Evolved Stars
Leader: Paolo Ventura
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 98/152
PSM WP 127 100
04/2030 — 03/2033
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 the grid of high quality stellar models for low/intermediate mass in the phases of red giant branch (RGB)
and core He-burning (He-B).
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
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.
Dependencies:
WP 127 000 and WP 121 000
Output:
Grids of updated stellar models for low-mass red giant stars covering a large range of chemical composition and
with the required precision for oscillation computations. A documented user guide providing a detailed
description of the content of grids and of the physical description assumed in the model computation.
Deliverables:
Grids of stellar models for red giant evolutionary phase. Evolutionary tracks and internal structure files in a
standard format (FGONG) for oscillation computations.
Milestones:
03/3030: Delivery of updated third generation of validated models and procedures, if necessary.
Risks:
Acceptable risks for the delay in the implementation of the algorithms for transport processes
PSM WPDs
POST-OPERATIONS
Seismic Diagnostics for Evolved Stars
Leader: Andrea Miglio
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 99/152
PSM WP 127 200
04/2030 — 03/2033
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 XXX.
Dependencies:
Input from WP 127 100, WP 372 100, WP 372 250.
Output:
Optimised and validated procedures to determine accurate masses, radii, ages as well as uncertainties that
satisfy the exoplanet specifications.
Deliverables:
Reports and updated stellar models
Milestones:
03/3030: Delivery of updated third generation of validated models and procedures, if necessary.
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
Constraints on Main-Sequence Stars
Leader: Josefina Montalban
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 100/152
PSM WP 127 300
04/2030 — 03/2033
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:
Optimised and validated procedures to determine accurate masses, radii, ages as well as uncertainties that
satisfy the exoplanet specifications.
Deliverables:
Reports and updated stellar models
Milestones:
03/3030: Delivery of updated third generation of validated models and procedures, if necessary.
Risks: Minimal risks
PSM WPDs
POST-OPERATIONS
Power Spectrum Fitting Tools
Leader: Bill Chaplin
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 101/152
PSM WP 128 000
04/2030 — 03/2033
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:
Final updates to the recommended procedures
Deliverables:
Final updates and reports on operation of procedures on real PLATO data
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: none
PSM WPDs
POST-OPERATIONS
Average Seismic Parameters
Leader: Rafael A. García
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 102/152
PSM WP 128 100
04/2030 — 03/2033
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 for the final procedures
3. Development and full specifications for the final 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:
Final updates to the recommended procedures
Deliverables:
Final updates and reports on operation of procedures on real PLATO data
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: none
PSM WPDs
POST-OPERATIONS
Mode Fitting Tools
Leader: Bill Chaplin
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 103/152
PSM WP 128 200
Post-operations phase
04/2030 — 03/2033
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:
Final updates to the recommended procedures
Deliverables:
Final updates and reports on operation of procedures on real PLATO data
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: none
PSM WPDs
POST-OPERATIONS
Solar-Like Stars
Leader: Bill Chaplin
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 104/152
PSM WP 128 210
Post-operations phase
04/2030 — 03/2033
Institution: University of Birmingham (UOB)
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 for the final procedures
3.
Development and full specifications for the final 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:
Final updates to the recommended procedures
Deliverables:
Final updates and reports on operation of procedures on real PLATO data
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: none
PSM WPDs
POST-OPERATIONS
Solar-Like Stars with Planets
Leader: Tiago Campante
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 105/152
PSM WP 128 220
04/2030 — 03/2033
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 for the final procedures
3.
Development and full specifications for the final 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:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: None
PSM WPDs
POST-OPERATIONS
Multiple Stars
Leader: Guy Davies
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 106/152
PSM WP 128 230
Post-operations phase
04/2030 — 03/2033
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 for the final procedures
3.
Development and full specifications for the final 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:
Final updates to the recommended procedures
Deliverables:
Final updates and reports on operation of procedures on real PLATO data
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: None
PSM WPDs
POST-OPERATIONS
Ensemble Fit
Leader: Jerôme Ballot
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 107/152
PSM WP 128 240
Post-operations phase
04/2030 — 03/2033
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 for the final procedures
3.
Development and full specifications for the final 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:
Final updates to the recommended procedures
Deliverables:
Final updates and reports on operation of procedures on real PLATO data
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: None
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 108/152
Fitting Tools for Evolved Stars
Leader: Saskia Hekker
Rev.: 5
Operations phase
PSM WP 128 250
04/2030 — 03/2033
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:
Updates and reports on operation of procedures on real PLATO data
Milestones:
03/3030: Final improvements of the procedures and algorithms, if necessary.
Risks: None
PSM WPDs
POST-OPERATIONS
Interfaces
Leader: Frédéric Baudin
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 109/152
PSM WP 129 000
Post-Operations phase
04/2030 — 03/2033
Institution: Institut d’Astrophysique Spatiale (France)
Key Personnel: F. Baudin; C. Barban (Lesia)
Objectives:
Outreach activities related to activities of the WP 120.
Tasks:
Interface for outreach activities of WP 120: fulfilling demands of general PLATO outreach activities and
proposing outreach material based on WP 120 activities
Input:
Outreach material from WP 120
Dependencies:
Output:
Outreach material ready to be included in PLATO general outreach activities
Deliverables:
Milestones:
03/3033: Delivery of the last version of PLATO stellar results of the core program.
Risks:
PSM WPDs
POST-OPERATIONS
Target / Field Characterization and Selection
Leader: Giampaolo Piotto
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 110/152
PSM WP 130 000
Post-Operations phase
04/2030 — 03/2033
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.
2.
3.
4.
5.
Select PLATO fields
Define the list of parameters to be collected
Make sure the relevant information is searched for in all possible catalogues
Provide PIC and stellar parameters
Provide updated target and field characterization
Input:
All catalogues/parameters gathered by WP 131 000 and WP 132 000
Dependencies:
Output of WP 131 000, 132 000
Output:
Updated final list of targets/parameters of the PLATO input catalogue
Deliverables:
Updated final target/parameters specification of PIC
Milestones:
Until 04/2033: Continuing refinements of the selection criteria
Risks:
Depends on GAIA output; in case of delay or failure from GAIA the catalogue will rely on available
photometric/astrometric catalogues.
PSM WPDs
POST-OPERATIONS
Project Office Assistant
Leader: Valentina Granata
Post-Operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 111/152
PSM WP 130 100
04/2030 — 03/2033
Institution: Università di Padova (Italy)
Key Personnel: V. Granata
Objectives:
Management of WP 130.
Tasks:
1.
2.
3.
4.
5.
6.
7.
8.
Contribute to plan the activities of WP 130 team
Contribute to WP 130 team meeting organization
Contribute to monitoring of progresses and action items
WP 130 documentation management
Contribute to interface with the all WP 130 Leaders
Management of schedule
Participation to meeting
Participation to PSM teleconferences
Input:
•
•
•
•
•
PLATO Management Plan and PSM
PLATO Science Requirement Document
PDCR ESA review reports
All catalogues/parameters gathered by WP 131 000 and WP 132 000 and WP 133 000
Results from PLATO
Dependencies:
Output of WP 131 000, WP 132 000 and WP 133 000
Output:
Preparation of all Management Documentation
Deliverables:
Documents
Milestones:
Risks:
None
Rev.: 5
PSM WPDs
POST-OPERATIONS
Interface to Other PSM WPs and PDC
Leader: Silvano Desidera
Post-Operations phase
Institution: INAF- Astronomical Observatory of Padova (Italy)
Key Personnel: S. Desidera
Objectives:
The objective of this WP is to coordinate the activities of the Interface WP
Tasks:
Coordinate WP 133 100 and WP 133 200 work
Input:
Definition Phase documentation
Dependencies:
Output of the WP 133 100 and WP 133 200
Output:
Interface documentation
Deliverables:
Reports
Milestones:
Until 04/2033: Continuing refinements of the parameters criteria
Risks:
Acceptable risk
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 112/152
PSM WP 133 000
04/2030 — 03/2033
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 113/152
Interface to Other PSM WPs
Leader: Silvano Desidera
Rev.: 5
PSM WP 133 100
Post-Operations phase
04/2030 — 03/2033
Institution: INAF- Astronomical Observatory of 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 the PLATO
End-to-End Simulator.
Input:
Development Phase documentation
Dependencies:
Close interaction can be foreseen with WP 110 to 160
Output:
Update of collection of requirements from WP 110 000, WP 120 000, WP 140 000, and WP 160 000 for target
selection and target parameters criteria to be included in PIC
Deliverables:
Update of the requirement document for field and target parameters selection criteria
Milestones:
Until 04/2033: Continuing refinements of the selection criteria
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Interface to PDC
Leader: Valentina Granata
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 114/152
PSM WP 133 200
Post-Operations phase
04/2030 — 03/2033
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:
Management documents
Milestones:
Until 04/2033: Continuing refinements of the selection criteria
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 115/152
Coordination of PLATO Follow-Up Observations
Leader: Stéphane Udry
Rev.: 5
Post-operations phase
PSM WP 140 000
04/2030 — 03/2033
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 XXX, WP 160 000.
Output:
WP’s coordination
Deliverables:
Report synthesizing the Follow-Up activities at the end of the mission
Milestones:
Until 2033: Ongoing Follow-Up observations
Risks:
Shortage of observing facilities that would lower the follow-up efficiency and thus the scientific return of the
mission.
PSM WPDs
POST-OPERATIONS
Strategy and Operation Preparation
Leader: Don Pollacco
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 116/152
PSM WP 141 000
04/2030 — 03/2033
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:
Reports on algorithms and specifications. Reports on tests performed as algorithms and their implementation
evolve.
Milestones:
Until 2033: Updates on FU strategy when needed
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
POST-OPERATIONS
Target Distribution Requirements
Leader: Ignasi Ribas
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 117/152
PSM WP 141 100
04/2030 — 03/2033
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:
Extended support and monitoring of facility efficiencies/capabilities and the impact this has on established Target
Distribution procedures – undertaking alterations to standard methodology where required.
Tasks:
1.
To maintain and oversee user support and effective target distribution to ground-based facilities –
thereby ensuring optimum efficiency.
2.
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.
Output:
Maintenance ad adaptation of established Target Distribution procedures in light of changing facility capabilities
and observer feedback.
Deliverables:
1.
Continued user support to manage effective target distribution.
2.
Reports on distribution techniques and overall facility efficiencies.
Milestones:
Until 2033: Re-assessment of facility capabilities. Active adaptation of Target Distribution procedures.
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. This is especially
important to maintain during the latter phases of the mission when follow-up of Earth-like planets will still be in
progress.
PSM WPDs
POST-OPERATIONS
Aids for Optimizing Photometric and Spectroscopic
Measurements
Leader: Josep Colomé
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 118/152
PSM WP 141 200
04/2030 — 03/2033
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. Ground based observations will continue through this phase.
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:
06/2031: Review of PLATO Observational aids performance after operations phase and review of requirements
Post-Operation.
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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 119/152
Information Transfer
Leader: Francesc Vilardell
Rev.: 5
Post-operations phase
PSM WP 141 300
04/2030 — 03/2033
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:
Maintain the PLATO Observer Interface and feedback to ancillary database during the post operational phase.
Tasks:
To maintain the PLATO Observer Interface aid set during the operational phase
Input:
1.
Current PLATO Observer Interface documentation
2.
PLATO Red book and current PLATO performance estimation.
3.
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 maintenance 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:
Until 2033: Ongoing assessment and maintenance of the PLATO Observer Interface
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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 120/152
Planet Yield Determination
Leader: Yann Alibert
Rev.: 5
Post-operations phase
PSM WP 141 400
04/2030 — 03/2033
Institution: University of Bern (Switzerland)
Key Personnel: Y. Alibert; S. Udry (Geneva); F. Bouchy (LAM); X. Dumusque (CfA)
Objectives:
Estimate of PLATO global-up 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, WP 142 XXX
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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Radial Velocity Follow-Up
Leader: François Bouchy
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 121/152
PSM WP 142 000
04/2030 — 03/2033
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 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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Post-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:
1.
Software testing
2.
Maintenance and algorithm upgrade
3.
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:
Upgraded algorithms and tools
Milestones:
Until 2033: Ongoing Follow-Up observations, upgrades on algorithms when needed
Risks:
Acceptable risks
st
Date: September 1 2015
Page: 122/152
Radial Velocity Computation and Global Analysis
Tools
Leader: Damien Ségransan
Rev.: 5
PSM WP 142 100
04/2030 — 03/2033
PSM WPDs
POST-OPERATIONS
First Radial Velocity Screening [≥ 10 m/s]
Leader: Eike W. Guenther
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 123/152
PSM WP 142 200
04/2030 — 03/2033
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, 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 and uninteresting objects, “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:
Until 2033: Screening of candidates list will be carried out during the whole PLATO mission.
Risks:
Limited number of telescope facilities to carry out the follow-up observations.
PSM WPDs
POST-OPERATIONS
Intermediate Precision Radial Velocity Follow-Up
[3-5 m/s]
Leader: Claire Moutou
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 124/152
PSM WP 142 300
04/2030 — 03/2033
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 moderate
precision [3-5 m/s] on the ranked transiting candidate list
Tasks:
1.
2.
3.
4.
Select targets from initial list and update as operations 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:
1.
Radial velocity data to the ancillary data base
2.
Combined fits and false-positive analysis
Milestones:
Until 2033: Ongoing Follow-Up observations
Risks:
Continuous availability of spectrographs with moderate RV precision up to 2033
PSM WPDs
POST-OPERATIONS
Very High-Precision RV Measurements [≤ 1 m/s]
Leader: Francesco Pepe
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 125/152
PSM WP 142 400
04/2030 — 03/2033
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 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 operations 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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Infrared Radial-Velocity Measurements
Leader: Thierry Forveille
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 126/152
PSM WP 142 500
04/2030 — 03/2033
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 144 100, WP 113 000, 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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Time Critical Photometry
Leader: Roi Alonso
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 127/152
PSM WP 143 000
04/2030 — 03/2033
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.
phase
2.
3.
4.
5.
Coordinate post-mission applications for telescope time on the facilities identified in the development
Post-mission liaison with other WP’s, notably WP 144 000 and WP 142 000
Post-mission coordination of the various science teams involved in this follow-up activity
Coordinate collection, analysis and reporting of these data
Update status of candidates based on photometric results
Input:
Post-mission small-planet candidates of ambiguous nature but of high potential
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:
Until 2033: Ongoing Follow-Up observations
Risks:
Uncertainty as to which ground-based facilities will be available from 2024.
PSM WPDs
POST-OPERATIONS
Photometry Specific Tools
Leader: H. J. Deeg
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 128/152
PSM WP 143 100
04/2030 — 03/2033
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
POST-OPERATIONS
Photometric Follow-Up with Small Telescopes
Leader: G. Wuchterl
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 129/152
PSM WP 143 200
04/2030 — 03/2033
Institution: Thüringer Landessternwarte Tautenburg (Germany)
Key Personnel: G. Wuchterl
Objectives:
Coordinate the follow-up activities that are feasible with small (diameter < 0.9 m) telescopes.
Tasks:
1. Link with registered facilities to PLATO Follow-Up
2. Coordinate execution of follow-up observations requested and defined in WP 143 000.
3. Assure required precision is met.
4. 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:
None
PSM WPDs
POST-OPERATIONS
Standard Photometric Observations
Leader: R. Alonso
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 130/152
PSM WP 143 300
04/2030 — 03/2033
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 2030.
PSM WPDs
POST-OPERATIONS
Very High Precision Photometric Observations
Leader: E. Pallé
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 131/152
PSM WP 143 400
04/2030 — 03/2033
Institution: Instituto de Astrofísica de Canarias (Spain)
Key Personnel: E. Pallé
Objectives:
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 time critical high-precision follow-up
Risks:
Uncertainty as to which suitable facilities will be available from 2030.
PSM WPDs
POST-OPERATIONS
High Angular Resolution Imaging
Leader: Silvano Desidera
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 132/152
PSM WP 144 000
04/2030 — 03/2033
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.
Coordinate applications for telescope time on the facilities participating to follow-up
4.
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
5.
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 (130000, 140000)
3.
Results of simulation on contamination probability
Dependencies:
Other follow-up WPs, WP 350 000, WP 130 000, WP 131 6xx, WP 132 3xx
Output:
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:
On going high angular resolution imaging FU observations for PLATO fields
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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 133/152
Imaging Analysis Tools
Leader: Arthur Vigan
Rev.: 5
Post-operations phase
PSM WP 144 100
04/2030 — 03/2033
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:
1.
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 WP143 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:
Until 03/2033: improvements of tools when needed
Risks:
Non-optimal use of allocated imaging follow-up observing time
PSM WPDs
POST-OPERATIONS
Single-Epoch Seeing-Limited Imaging
Leader: V. Nascimbeni
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 134/152
PSM WP 144 200
Post-operations phase
04/2030 — 03/2033
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.
Applications for telescope time on the facilities participating to follow-up
2.
Preparation of observing runs to optimise observing strategy for imaging transit candidates
3.
Collection, analysis and interpretation of these data
4.
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:
On going high angular resolution imaging FU observations for PLATO fields
Risks:
Uncertainty as to which observing facilities will be available from 2024
PSM WPDs
POST-OPERATIONS
Reconnaissance High Resolution Imaging
Leader: Markus Janson
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 135/152
PSM WP 144 300
Post-operations phase
04/2030 — 03/2033
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 participating to follow-up
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:
On going high angular resolution imaging FU observations for PLATO fields
Risks:
Uncertainty as to which observing facilities will be available from 2024
PSM WPDs
POST-OPERATIONS
High Contrast Imaging
Leader: Dino Mesa
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 136/152
PSM WP 144 400
Post-operations phase
04/2030 — 03/2033
Institution: INAF - Osservatorio Astronomico di Padova (Italy)
Key Personnel: D. Mesa; S. Desidera (INAF-Padova); M. Janson (Stockholm); A. Vigan (LAM); M. Bonavita
(Edinburgh); R. Claudi (INAF-OAPD); V. D’Orazi (INAF-Padova)
Objectives:
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.
2.
3.
Coordinate applications for telescope time on the facilities participating to follow-up
Coordinate preparation of observing runs to optimize observing strategy for imaging transit candidates
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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 137/152
Candidate Classification
Leader: M. Bonavita
Rev.: 5
Post-operations phase
PSM WP 144 500
04/2030 — 03/2033
Institution: Edinburgh (UK)
Key Personnel: M. Bonavita; A. Vigan (LAM); S. Desidera (INAF-Padova); M. Janson (Stockholm); R. Claudi
(INAF-OAPD); V. D’Orazi (INAF-Padova)
Objectives:
Identify the nature of the candidates close to PLATO targets (physical companions vs. field objects) down to
substellar objects for a better understanding of the environment of PLATO targets and the architecture of the
planetary systems discovered with PLATO
Tasks:
1.
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
Input:
Candidates close to PLATO targets from WPs 144 100, 144 200, 144 300, 144 400
Results of simulations with contamination/companions probabilities (WP 130 000)
Dependencies:
Interface with WP 130 000, WP 350 000, and with other PLATO follow-up WPs
Output:
Data to WP 350 000
Deliverables:
Data to be provided to the Ancillary Database (WP 350 000)
Milestones:
On-going analysis for first PLATO fields.
Risks:
Incomplete evaluation of the environment of planets identified by PLATO in terms of stellar companions and
substellar companions in wide orbits
PSM WPDs
POST-OPERATIONS
Additional Exoplanet Follow-Up
Leader: Xavier Bonfils
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 138/152
PSM WP 145 000
04/2030 — 03/2033
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.)
3.
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:
Until 2033: Ongoing Follow-Up observations
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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 139/152
Transmission Spectroscopy Follow-Up
Leader: David Ehrenreich
Rev.: 5
Post-operations phase
PSM WP 145 100
04/2030 — 03/2033
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 centralize information about characterization 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:
Until 2033: Ongoing Follow-Up observations
Risks:
WP relies on other facilities with their own intrinsic risks
PSM WPDs
POST-OPERATIONS
Secondary Eclipse and Phase-Variation
Spectroscopy
Leader: Roi Alonso
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 140/152
PSM WP 145 200
04/2030 — 03/2033
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 (derive emission/reflection spectra, physical properties, chemical abundances...)
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:
Until 2033: Ongoing Follow-Up observations
Risks:
WP relies on other facilities with their own intrinsic risks
PSM WPDs
POST-OPERATIONS
Developing Techniques for Atmosphere
Characterization
Leader: Xavier Bonfils
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 141/152
PSM WP 145 300
04/2030 — 03/2033
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.
2.
Established planets from PLATO
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:
Reports
Milestones:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 142/152
Rossiter-McLaughlin Observations
Leader: Guillaume Hébrard
Rev.: 5
Post-operations phase
PSM WP 145 400
04/2030 — 03/2033
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.
Planets candidates detected by PLATO
2.
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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Additional Long Term Follow-Up
(RV and Transit Timing)
Leader: François Bouchy
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 143/152
PSM WP 145 500
04/2030 — 03/2033
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. Established PLATO exoplanets
2. 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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 144/152
PSM WP 146 000
Spectroscopy
Leader: Artie P. Hatzes
Ref.: PLATO-UWA-PSMWPD-003
Post-operations phase
04/2030 — 03/2033
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:
2033 Completion of Follow-up of PLATO objects of interest
Risks:
Acceptable risks.
PSM WPDs
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 145/152
Activity Indicators and Doppler Information on Active
Stars
Leader: Christophe Lovis
PSM WP 146 100
Post-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:
Corrected RVs
Confirmed planets around active stars
Deliverables:
Documents and algorithms
Milestones:
Until 2033: Ongoing Follow-Up observations
Risks:
Acceptable risks
Rev.: 5
04/2030 — 03/2033
PSM WPDs
POST-OPERATIONS
Tools for Spectral Classification
Leader: Lars Buchhave
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 146/152
PSM WP 146 200
04/2030 — 03/2033
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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
Rev.: 5
PSM WPDs
POST-OPERATIONS
Infrared Spectroscopy
Leader: Pedro Figueira
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 147/152
PSM WP 146 300
04/2030 — 03/2033
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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
Rev.: 5
PSM WPDs
POST-OPERATIONS
Spectropolarimetric follow-up
Leader: Pascal Petit
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 148/152
PSM WP 146 400
04/2030 — 03/2033
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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Performances Assessment & FU Efficiency
Leader: Stéphane Udry
Institution: Geneva University (Switzerland)
Key Personnel:
Objectives:
Tasks:
Input:
Dependencies:
Output:
Deliverables:
Milestones:
Risks:
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 149/152
PSM WP 147 000
04/2030 — 03/2033
PSM WPDs
POST-OPERATIONS
Interfaces to Other SPM WPs and PDC
Leader: Stéphane Udry
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 150/152
PSM WP 148 000
Post-operations phase
04/2030 — 03/2033
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:
Until 2033: Ongoing Follow-Up observations
Risks:
Minimal risks
PSM WPDs
POST-OPERATIONS
Complementary Science
Leader: Conny Aerts
Post-operations phase
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
Rev.: 5
st
Date: September 1 2015
Page: 151/152
PSM WP 160 000
04/2030 — 03/2033
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.
PR activities
Deliverables:
Milestones:
PMC Science Conferences
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
POST-OPERATIONS
Ref.: PLATO-UWA-PSMWPD-003
Issue: 2
st
Date: September 1 2015
Page: 152/152
PMC SCIENCE MANAGEMENT
WORK PACKAGE DESCRIPTIONS
POST-OPERATIONS
END
Rev.: 5