PLATO PLAnetary Transits and Oscillations of stars - Isabella Pagano - INDICO @ INAF
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19 May 2021
PLATO
PLAnetary Transits and Oscillations of stars
Isabella Pagano
Resp. Scientifica partecipazione Italiana a PLATO
PLATO Co-PI
AUDIZIONI SCHEDE INAF
17-31 MAY 2021
The EP-RAT Roadmap
ESA EXOPLANET ROADMAP ADVISORY TEAM – Oct 2010
Time and difficulty
Time and difficulty
Rome, 5 Nov 2014
PLATO
PLAnetary Transits & Oscillations of Stars
• 3° M class mission in ESA’s Cosmic Vision 2015-2025 Programme
• Launch: end 2026 – Ariane 6 from Kourou
• Operation: 4.25 yr (+2) yrs
[satellite built with consumable for 8 yr]
Key Science Goals:
✓ Detection of terrestrial exoplanets in the habitable zone of
solar-type stars and characterization of their bulk properties needed to determine their habitability.
✓ Understanding of the formation, the architecture, and the evolution (ages) of planetary systems by
means of a full inventory of the physical properties of thousands of rocky, icy, and gaseous giant
planets.
Large diversity of planetary structure
Lacedelli et al. (2020, MNRAS 501, 4148)
ü Masses vary by a
factor of ~4
(with large errors)
ü Radii vary by a
factor of ~3
Mp
Planet diversity
• Planets of Earth mass and below remain to be
Earth 5.5 g/cm3 detected and characterized
GJ1214b 1.6 g/cm3
Mini gas planets
A biased view
Our knowledge on planet nature is limited to close-in planets so far.
All planets
Planets with P>80 days
Small planets with both Radius and Mass measured Illustration of PLATO science exoplanet target range in comparison to other missions (Rauer et al. in preparation)
The need for bright stars
Known planets from radial velocity and transit surveys
ü Why have so few targets been characterized?
ü Transit surveys targeted faint and distant stars
to maximize detection performance.
ü Radial velocity surveys need bright stars (≤11
mag) to keep telescope resources limited.
Lessons learned:
Future transit missions must target bright stars!
Large FoV concept
©PLATO @INAF
Searching for transits of Bright Stars
➔➔ large FoV!The Telescope Optical Units design concept
Single Telescope FoV ∼1200 sqdeg
One Camera Equivalent to a circle of ~38.7 deg diameter
✓ 24 Normal cameras
Telescopes
✓fully dioptric, 6 lenses
CCDs
✓ pupil 120 mm
FPAs & Test House
✓Dynam. range: ~8 ≤ mV ≤ 11 (13)
TOU+FPA integration
✓4 x CCD 4510×4510px per camera
Test House
✓Pixels size: 18 μm square
Test House
✓read-out cadence: 25 sec
FSS
✓Band: 500 – 1050 nm
©PLATO @INAF
OGSE+ MLI
✓2 Fast cameras
Transport Container
✓Bright stars (Payload Concept Instrument field of view is 2200 square degrees (vs 105 deg2 Kepler) ~2 billion pixels (2 000 Mpx vs 98 Mpx for Kepler) ~6 600 cm2 of sensitive area (2x Gaia)
The PLATO sky
T h e f in
al
w i l l b e o b s e r v in g s t
f ix e d ~ ra te g y
la u n c h 2 yrs b
a nd ca e fo
d u r in g n b e a d re
the m i a pted
Observing strategy s s io n .
• Baseline
2 long pointings of 2 years
• Alternative
3 years + 1 year step-and-stare phaseMethods and goals
PHOTOMETRY FROM SPACE SPECTROSCOPY FROM THE GROUND
Transit Method Asteroseismology Radial velocity method
→ Rp/R* → R* → Mp/M* sin i
→ Orbital inclination → M*
→ Orbit parameters → Stellar age
Mean Densities, Age Evolution of planets & planetary
systems, HabitabilityHow PLATO is organised
Steering About
Committee PLATO Mission 750
Consortium members
PM PI & co-PI
PS
PSWT PMC PMC Science
Board Team
MISSION Man
SATELLITE
PAYLOAD
LAUNCH PMC Man
Ground Segment
LAUNCHER
SOC Science Preparation
PLATO Data Center
MOCIl Team INAF (and associated)
ü INAF
• OA Catania Science, Payload
• OA Padova Science, Payload
• OA Brera Science, Payload
• IAPS Roma Science, Payload
• OAS Payload
• FGG Payload
• OA Palermo Science
• OA Torino Science • 114 people (95 INAF/ 19 associated)
• OA Capodimonte Science
• In the period 2021-2023
• OA Roma Science
• 15 FTE/yr INAF
• OAAB Science
• 4.5 FTE/yr associated
• OA Arcetri Science
• Distribution
ü UNIPD, UNIBO, UNIPI Science
• 40 è Payload
ü SSDC PDC • 72 è PSM
• 4 è PDC (SSDC)What we do for PLATO: PAYLOAD
TOUs
Cameras
System
Management
ICUPayload: Payload Team
CAMERAs TEAM Jose Lorenzo Alvarez
Payload Project Manager
OAS, IAPS, OACT, OAPD
F. Borsa
P. Battaglia G. Dinuzzi TBD
F. Calderone N. Auricchio
A. Meoli TBD
F. Sortino M. Munari TBD
R. Ragazzoni
Y. ZImmer
P. Apollonio
D. Dobrea
M. Fürmetz
G. TropeaOACT, OAPD, OAB
Telescope Optical Units Team
PROJECT SYSTEM ANALYSIS &
DESIGN PERFORMANCE AIV & GSE
OFFICE ENGINEERING
TOU Project Manager TOU Instrument Scientist TOU System Engineer Chief Optical Engineer Optical Engineer, Chief AIV Engineer
Straylight Analysis
Isabella Pagano Roberto Ragazzoni Valentina Viotto Demetrio Magrin §Matteo Munari Jacopo Farinato
INAF-OACT INAF-OAPD INAF-OAPD INAF-OAPD INAF-OACT INAF-OAPD
TOU Mechanical Structure TOU Mechanical Structure Mechanical Structure Optical Engineer,
Project Manager Scientist System Engineer Chief Mechanical Engineer Radiation analysis AIV Engineer
Virginie Cessa Willy Benz Timothy Bandy Daniele Piazza Mauro Ghigo Maria Bergomi
UBE INAF-OAPD
UBE UBE UBE INAF-OAB
F-TOU Filter Project TOU Product Assurance TOU Interface Engineer Mechanical Engineer Optical Engineer, AIV Engineer
Manager Manager Radiation analysis
Alexis Brandeker Simonetta Chinellato Maria Bergomi Timothy Bandy Francesco Borsa Gabriele Umbriaco
INAF-OAPD UBE INAF-OAPD
UST INAF-OAPD INAF-OAB
TOU Document TOU Project Office Visualization and Mechanical Engineer, AIV Engineer
Configuration Man Assistant Rendering Thermal Analysis
Flavia Calderone Flavia Calderone Marco Dima Stefano Basso Daniela Vassallo
INAF-OACT INAF-OAPD
INAF-OACT INAF-OAPD INAF-OAB
STM è
F-TOU Filters Product Thermal Engineer, Structural Tests Engineer
TOU Mechanical Structure Assurance Manager Thermal Analysis
Product Assurance TBD Sebastian Wolf Daniel Schaedeli
Manager UBE
UST UBE
Configuration Control and Mechanical Engineer,
Chief GSE Engineer
ction
Quality Control Structural Analysis
Serial Produ
Virginie Cessa Martin Rieder Luca Marafatto
INAF-OAPD
UBE UBE
ted
already star Optical Engineer, Optical
, 5 FS
Material Parts & Process Performance AIV support
1 PFM 2 5 FM
Timothy Bandy Demetrio Magrin Florian Hostettler
UBE UBE
INAF-OAPD
Optical Engineer, F-TOU
Filter Performance
Göran Olofsson
UST
ç EMOAA, IAPS, TNG
Payload: ICU Team
ç ICU EM#1Science Preparation
100 000
PSM
Coordination
D. Pollacco
110 000 120 000 130 000 140 000 160 000
Target / Field
Follow-up Complementary
Exoplanet Science Stellar Science Characterization
Coordination Science
D. Pollacco M.-J. Goupil and Selection
S. Udry C. Aerts
G. Piotto
RSN2
EXO-Arch EXO-Stars RSN3
EXO-Young RSN4
EXO-SPIPLATO Input Catalog
PLATO INPUT CATALOG
UNIPD, OAPD, OAPA, OACT e SSDC
The all sky PLATO Input Catalogue PLATO
AA/2021/40717 Data
CenterExoplanets Science preparation
110 000
Exoplanet Science
D. Pollacco
111 000 112 000 113 000 114 000 115 000 116 000 117 000
Coordination of Specification of Planet Candidate PLATO
Transit Fitting PLATO Data Interfaces to Other
Tools for Planet Detection Ranking Interpretation
Tools Specific Science PSM WPs & PDC
Lightcurve Filtering Tools Procedures Specific Science
J. Cabrera Sz. Csizmadia D. Pollacco N. Santos
I. Pagano M. Deleuil H. Rauer
111 100 112 100 113 100 114 100 115 100 116 100 117 100
Composition & Planet Host
Tools for Lightcurve Transit Detection Rank Planet Transit Curve Astrophysical Noise
Formation of Gas & Characterisation
Filtering Tools Candidates Modelling Tools Source
Ice Giants Requirements
S. Aigrain J. Cabrera A. Collier Cameron Sz. Csizmadia C. Watson Adibekyan
T. Guillot
111 200 112 200 113 200 114 200 115 200 116 200 117 200
Tools for Detecting Detection of Single False Positive Accurate Orbital Understanding
Planetary System Mass-radius
& Filtering Residual and Unusual Transit Identification Through Parameter planets through
Characterisation Terrestrial Planets
Instrumental Noise Events Centroid Analysis Determination their host stars
A. Sozzetti F. Sohl
D. Pollacco P. A. Strøm A. Santerne A. Santerne Van Eylen
112 300 113 300 114 300 115 300 116 300
Detection of
Astrophysical False Rossiter-McLaughlin Planet-Star Planetary Formation
Exoplanet Systems
Positives Modelling Tools Interactions and Orbital Evolution
via Reflected Light
A. Collier Cameron G. Hébrard S. Mathis R. Nelson
J.-M. Desert
112 400 115 400 116 400
Atmospheres of
Other Detection Transits of Close-In
PLATO Terrestrial
Methods Objects
Planets
R. Silvotti C. Haswell
J. L. Grenfell
112 500 115 500 116 500
PLATO Habitable
Multi-planet Non-Transiting
Zone Planets
Systems Planets via REBs
M. Güdel /
S. Desidera D. Barrado
H. Lammer
112 600 115 600 116 600
Transit Timing Composition and Dynamical
Variations / Transit Interior Evolution of Interactions in Multi-
Duration Variations Terrestrial Planets Planet Systems
V. Nascimbeni S. Werner J. Laskar
115 700
Planet Occurrence
Rates
V. Van EylenStellar Science Preparation
Follow-up Preparation
140 000
Follow-up
Coordination
S. Udry
141 000 142 000 143 000 144 000 145 000 146 000 147 000 148 000
Strategy and Higher Angular Perfomances
Time Critical Additional Exoplanet Interfaces to Other
Operation RV Follow-Up Resolution Spectroscopy Assessment and
Photometry Follow-Up PSM WPs and PDC
Preparation F. Bouchy Imaging A. Hatzes Follow-Up Efficiency
R. Alonso X. Bonfils S. Udry
D. Pollacco S. Desidera S. Udry
141 100 142 100 143 100 144 100 145 100 146 100
Radial Velocity Transmission Activity Indicators and
Target Distribution Photometry Specific Imaging Analysis
Computation and Spectroscopy Doppler Information
Requirements Tools Tools
Global Analysis Tools Follow-up on Active Stars
I. Ribas H. Deeg A. Vigan
D. Segransan D. Ehrenreich C. Lovis
141 200 142 200 143 200 144 200 145 200 146 200
Aids for Optimizing
Photometric Follow- Single-Epoch Secondary Eclipse
Photometric and First Radial Velocity Tools for Spectral
Up with Small Seeing-Limited and Phase Variation
Spectroscopic Screening [≥10 m/s] Classification
Telescopes Imaging Spectroscopy
Measurements E. Guenther L. Buchhave
G. Wuchterl V. Nascimbeni R. Alonso
J. Colomé
141 300 142 300 143 300 144 300 145 300 146 300
Intermediate Precision Standard Reconnaissance Developing Techniques
Information Infrared
Radial Velocity Follow- Photometric High Resolution for Atmosphere
Transfer Spectroscopy
Up [3-5 m/s] Observations Imaging Characterisation
F. Villardell P. Figueira
C. Moutou R. Alonso M. Janson X. Bonfils
141 400 142 400 143 400 144 400 145 400 146 400
Very High-Precision RV Very High Precision
Planet Yield High Contrast Rossiter-McLaughlin Spectropolarimetric
Measurements Photometric
Determination Imaging Effect Follow-up
[≤1 m/s] Observations
Y. Alibert D. Mesa G. Hébrard P. Petit
F. Pepe E. Palle
142 500 144 500 145 500
Infrared Radial Additional Long Term
Candidate
Velocity Follow-Up
Classification
Measurements (RV and Transit Timing)
M. Bonavita
T. Forveille F. BouchyComplementary Science
Programmazione
TOU è CDR going on
ICU è CDR ready to start
Critical Milestone è KOM July 2021Leadership
Steering About
Committee PLATO Mission 750
Consortium members
PM PI & co-PI
PSWT PMC PMC Science
12 members including: Board Team
I. Pagano, INAF
G. Piotto, UNIPD PI: H. Rauer, DLR
R. Ragazzoni, INAF Co-PI: I. Pagano, INAF Co-Is (TBD)
Co-PI: M. Mass-Hesse, INTA
PAYLOAD
20 members including:
Camera Team I. Pagano, INAF
L. Valenziano G. Piotto, UNIPD
F. Santoli
N. Gorius
D. BrienzaCHEOPS Isabella Pagano e Valerio Nascimbeni
S-class mission:
S is not for “Simple”
“Small” Budget Short time Several countries
milestone when
D A E B
I call issued Mar 2012
call answered Jun 2012
C ES
mission selected Nov 2012
H A mission adopted Feb 2014
instrument delivered Feb 2019
launch Dec 2019
• 4–5 years development
• total budget: ~105 M€ • 11 countries & ESA
time
• ESA: 50 M€ • ~30 institutions
Top Science was expected and is actually done!Il Satellite CHEOPS
From Europe to Kourou
Il Telescopio
Progetto ottico
Costruzione delle ottiche
Integrazione dello strumento
Test funzionamento e prestazioni
300 m m
Diametro dello specchio: 33 cm
Peso strumento: 60 kgIsabella Pagano Roberto Ragazzoni Giampaolo Piotto Valerio Nascimbeni Gaetano Scandariato Luca Borsato Giuseppe Leto Giovanni Bruno
INAF Catania INAF Padova Univ. Padova INAF Padova INAF Catania INAF Padova INAF Catania INAF Catania
Resp. Nazionale Instrument Scientist Membro dello Membro dello Membro dello Team Scientifico Team Scientifico Team Scientifico
Project Manager del del Telescopio Science Team Science Team Science Team
Telescopio Membro del Board
Membro del Board Vikash Singh Elisabetta Tommasi
Univ. Catania ASI
INAF Catania Resp. Accordo
Team Scientifico Scientifico
Mario Salatti
Daniela Sicilia ASI
Univ. Padova Project Manager
INAF Catania Contratto Industriale
Team Scientifico Steering Committee
Marco Dima Davide Greggio Luca Marafatto Valentina Viotto Demetrio Magrin Matteo Munari Jacopo Farinato Maria Bergomi Federico Biondi
INAF Padova INAF Padova INAF Padova INAF Padova INAF Padova INAF Catania INAF Padova INAF Padova INAF Padova
Rendering Progetto Ottico Progetto Ottico System Engineer del Progetto Ottico del Analisi Luce Diffusa Interfacce del AIV del Telescopio AIV del Telescopio
Telescopio Telescopio TelescopioThe Team
INAF
• OACT
• OAPD
• 28 people (23 INAF/ 5 associated)
• OAPA • In the period 2021-2023
• 5 FTE/yr INAF
• OATO
• 1.5 FTE/yr associated
• FGG
UNIPD
SSDC2012-2013 2013-2018
Improving
Ancillary radii
16% 6%
Characterising
atmospheres
Finding Improving 26%
transits radii
50% 50% Exploring new
planets Uncovering
29% new features
6%
Finding
transits
17%1 Some early science results 1) Measurement of the dayside temperature (3435±27 K) and true δ = 88 ± 4 ppm orbital obliquity (Ψ=85°±4°) of the hot-Jupiter WASP-189b (Lendl+ 2020) 2 2) Full reconstruction of the dynamical 3 architecture of a six-planet system locked in a chain of Laplace resonances (2:4:6:9:12), including mass and density measurements (Leleu+ 2021) 3) Discovery of an additional 2 R⊕ planet in a multiple system hosted by the bright star HD 108236 (Bonfanti+ 2021)
Some early science results 4
4) Characterization of a planetary system hosted by
a naked-eye star (Nu2 Lup), including the discovery
of a transiting, mildly-irradiated super-Earth
amenable of a detailed atmospheric 0 2 1
e 2
characterization (Delrez+ 2021, Nature Astronomy, u n
in press). m i dJ
t ill
a rgo
m b
r E
de
Un
4Criticità
• Ricercatori e ingegneri di altissimo profilo
• competenze maturate all'interno e all'esterno dell'ente.
• E' fondamentale trattenere all'interno queste competenze spesso difficili da reperire.
• Per mettere a frutto un giusto ritorno dell'investimento prodotto dalla nostra nazione nel progetto occorre
avere una generazione di ricercatori e ricercatrici pronti all'utilizzo dei dati della missione.
• Il campo esopianeti è molto attrattivo per i giovani a inizio di carriera.
• Occorre non farli scappare e essere capaci di attrarne da fuori.
• Per PLATO un aspetto che farà la differenza durante la fase operativa sarà la
capacità di partecipare da leader alla campagna ground based di follow-up, che è parte
intrinseca della missione.
• L'INAF parte in condizione di vantaggio grazie alla presenza di HARPS-N al TNG. Occorre che esso sia
disponibile a INAF quando PLATO sarà operative.Punti di forza • L’Italia è al top sui sistemi ottici per lo spazio: sinergia da rafforzare tra INAF e aziende • La comunità esoplanetologica italiana, che si è aggregata intorno al 2009 proprio grazie alla selezione di PLATO da parte di ESA per lo studio di fattibilità, e che ha proseguito insieme a crescere con l'opportunità giunta nel 2012 quanto la dirigenza INAF ha chiesto di valutare la proposta di installare HARPS-N al TNG, è oggi numerosa, rilevante a livello internazionale, piena di giovani promettenti, e coinvolta oltre che in PLATO in progetti di punta per lo studio degli esopianeti quali le missioni Cheops e Ariel, gli strumenti Espresso, SHARK-VIR e SHARK-NIR, spaziando dallo studio delle architetture e proprietà fisiche dei sistemi planetari (EXO-Arch), alla formazione ed evoluzione iniziale degli stessi (EXO-Young), alle atmosfere dei pianeti (EXO- Atm), alle caratteristiche dell'interazione stella-pianeta (EXO-SPI), allo studio delle proprietà stellari che servono a vincolare con precisione i parametri planetari (EXO-Stars). • Questa comunità è cresciuta grazie ai finanziamenti ricevuti dai Progetti Premiali WOW (PI. G. Micela) e FRONTIERA (PI I. Pagano) che sono stati gestiti in modo da includere e rafforzare il tema di ricerca e creare massa critica per incidere nell'ambito delle collaborazioni internazionali. • Altri finanziamenti sono stati ottenuti grazie a PRIN INAF, PRIN Universitari e bandi ASI più specificatamente mirati a focalizzare precisi temi di ricerca. • Assicurare continuità nei finanziamenti della ricerca di "oggi" per essere sempre più preparati a quella di "domani" è una delle criticità più rilevanti anche per PLATO.
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