PLATO 2.0PLATO 2.0PLAnetary Transits and Oscillations of starsPLAnetary Transits and Oscillations of stars

Selected as the 3rd class M mission for ESA Cosmic Vision programSelected as the 3rd class M mission for ESA Cosmic Vision programTo be launched in 2024

High precision space photometryHigh precision space photometry

High-precision photometry from space + radial velocity follow-up detection of exoplanetary transits→

Fourier analysis of the lightcurves power-spectrum→

→ asteroseismology → probe the internal structure + measure basic properties of stars

Kjeldsen et al. 2008

CoRoT-11b

Gandolfi et al., 2010

Some results from CoRoT & Kepler Some results from CoRoT & Kepler

CoRoT

Kepler

Large diversity of planetary systems Large diversity of planetary systems CoRoT confirmed exoplanets

Very successful CoRoT and Kepler missions dedicated to exoplanets detections and asteroseismology

New era for stellar physicsNew era for stellar physics CoRoT

Kepler

© NASA

© CNES

internal rotation of red giants

Goal of the PLATO 2.0 missionGoal of the PLATO 2.0 mission

Main goal of PLATO :Main goal of PLATO :

detect terrestrial exoplanets in the habitable zone of solar-type stars and characterise their bulk properties

CoRoT

Kepler

PLATO will be leading this effort by combining:

planet detection and radius determination from photometric transits,

determination of planet masses from ground-based radial velocity follow-up,

determination of accurate stellar masses, radii, and ages from asteroseismology,

identification of bright targets for atmospheric spectroscopy.

PLATO

Stellar modelling for asteroseismologyStellar modelling for asteroseismology

Oscillation spectra computed from stellar models guide the identification of modes.

The separations between modes allow to retrieve M and R provided that Teff is well known

→ need to combine high precision photometry and spectroscopy

→ need a grid of precise stellar models to interpret oscillation spectra

Chaplin & Miglio, 2013

PLATO shall give M within 2%

age within 10 %

Better accuracy required for host star!

PLATO and the PLATO and the LUPMLUPM

PLATO requiresPLATO requires

Confirmation of exoplanetary candidates by identification of false positives → understand and model the magnetic activity of host stars

Fundamental parameters of the host stars (Teff, gravity, chemical composition) → provide bona fide spectral analysis using state-of-the-art

model atmospheres and spectral synthesis

Precise masses, radii and ages of host stars → precise modelling of stellar structure and evolution with quantified errorbars

Characterization of the host stars (incident flux, stellar activity) and planetary environment → understand and model the magnetic activity of host stars

PLATO and the PLATO and the LUPMLUPM

PLATO requiresPLATO requires

Confirmation of exoplanetary candidates by identification of false positives → understand and model the magnetic activity of host stars

Fundamental parameters of the host stars (Teff, gravity, chemical composition) → provide bona fide spectral analysis using state-of-the-art

model atmospheres and spectral synthesis

Precise masses, radii and ages of host stars → precise modelling of stellar structure and evolution with quantified errorbars

Characterization of the host stars (incident flux, stellar activity) and planetary environment → understand and model the magnetic activity of host stars

Fully consistent with the actual research projects of several members of the AS team

LUPM in the PLATO ManagementLUPM in the PLATO Management

Payload Data CenterScience

Preparation Management

PLATO Mission Consortium (PMC)PMCLead

PMCBoard

ESA Study Team Science Advisory TeamMOC

SOC

LUPM implication

PSPM organizes the European and international community around the scientific preparation of the mission.

Level 2 products (L2) are science ready products to be put into the PLATO archive

LUPM in the PLATO ManagementLUPM in the PLATO Management

TransportprocessesA. Palacios

Work Package 120 000 Stellar Science

TransportprocessesA. Palacios

Work Package 120 000 Stellar Science

A. Palacios responsible WP 121200→

TransportprocessesA. Palacios

B. Plez responsible WP 122400→

Work Package 120 000 Stellar Science

A. Palacios responsible WP 121200→

TransportprocessesA. Palacios

B. Plez responsible WP 122400→

Direct implication in the WP 121 200 (O. Richard) WP 122100, WP 122200 (B. Plez)

Work Package 120 000 Stellar Science

A. Palacios responsible WP 121200→

Work Package 140 000Follow-up Coordination

Work Package 140 000Follow-up Coordination

Direct implication in the WP 144 400 (A. Lèbre, E. Josselin, J. Morin)

SummarySummary

PLATO 3rd M class mission of the ESA Cosmic Vision program to be launched in 2024→

To provide characterization of exoplanetary systems implies :

→ identification of stellar activity spots to remove false-positive transits → characterization of the host stars magnetism to understand habitability and planet evolution → grids of refined stellar evolution models to derive stellar masses, radii and ages → precise determination of the fundamental parameters of host stars via spectroscopy

6 researchers of the AS team actively working on these fields and already identified by the PLATO consortium

The PLATO mission is an opportunity for the LUPM to gain visibility on the core research activities of an important part of the AS team

FactsFacts : invited talk @ French community PLATO meeting (oct. 2014), 4 k€/yr expressed needs to the CNES for 2014-2018 period.

Level 2• The planetary transit candidates and their parameters with formal uncertainties.• The asteroseismic mode parameters with formal uncertainties.• The stellar rotation periods and stellar activity models inferred from activity-related periodicities in the light curves, with formal uncertainties.• The seismically-determined stellar masses and ages of stars, (and their formal errors), obtained from stellar model fits to the frequencies of oscillations• The list of confirmed planetary systems, which will be fully characterised by combining information from the planetary transits, the seismology of the planet-host stars, and the follow-up observations.

This represents the most important PLATO (the final and highest level PLATO science) deliverable.

The parameters of the confirmed planets will be the orbital parameters, planet size, mass, and age(from the seismology of central stars). Any additional characterisation of the properties of theplanetary systems from the long duration PLATO light curves (e.g., secondary transits) and fromspecific ground-based observations (e.g., planetary atmospheres, imaging, etc) will also be included.

Role of the PSPM (PLATO Science Preparation Management)

The PSPM is responsible for carrying out preparatory activities ensuring the scientific results of themission. It provides the PDC with the specifications and inputs required to implement optimisedmethods and tools for PLATO data exploitation.

the PSPM is responsible for the scientific specification of the required elements for carrying out the stellar physics part of the mission. Specifically as what concerns the detection of oscillation modes, stellar evolution models and the determination of fundamental stellar parameters.

The PSPM is also responsible for the target/field characterisation and thus the preparation of thePLATO input catalogue and the preparation of Target/Field selection.

• The PSPM is also responsible for the organisation, of the required (ground- and space-based) follow- up observations.

• The PSPM is responsible for the development and implementation of the End-to-End Simulator (PLATO Data Simulator).

• Finally the PSPM is also responsible for the preparation of the complementary science program.

Experts in the PSPM will provide updated stellar models to optimise the determination of stellar parameters. The CCD Simulator will make realistic simulated data available. The additional (complementary) science task in the PSPM includes experts from various scientific fields, but mainly on different aspects of stellar science not covered in the core program. These experts willhelp maximising the scientific return of the mission by expanding its science exploitation.

Role of the PSPM (PLATO Science Preparation Management)

PLATO et l equipe AS du LUPM'

Implication possible/envisageable

PLATO et l equipe AS du LUPM'

Implication possible/envisageable

PLATO et l equipe AS du LUPM'

PLATO et l equipe AS du LUPM'

Un appel à contribution devrait être à nouveau ouvert bientôt

Deux rdv intéressants :

Workshop PLATO à Marseille les octobre prochains

Plato 2.0 Science Workshop 3-5 décembre prochains, Catane (Italie)

adoption de la mission PLATO par le SPC en Feb. /Mars 2016

documents intermédiairesMars 2015, Octobre 2015, Novembre-Decembre 2015Le vrai travail commencera après 2017.Avant il s'agit seulement de la définition de la mission

Autres deadlines pour les WP