PLAnetary Transits and Oscillations of stars

http://www.oact.inaf.it/plato/PPLC/Home.html

PLATO Consortium kick-off meeting

Day 1: - plenary meeting- hosted by CNES (thank you!)- goal = browse all aspects of the mission- opportunity for each consortium participant to learn about the parts of the project

that he (she) doesn’t know

Messages to all speakers:Please respect your time allocation (includes discussion): very tight schedule today !!

Please send your presentation to Claude.Catala@obspm.fr AS SOON AS POSSIBLE

This evening: reception in Salle Cassini at Observatoire de Paris, starting at 19:30

Day 2: - splinter meetings at Observatoire de Paris: payload, PDC, PSPM- goal = organize the work of the three elements of the project- joint PDC + PSPM splinter in the morning

A few details on the meeting organization

Main objective: - detect and characterize exoplanets of all kinds around stars of all

types and all ages full statistical study of formation and evolution of

exoplanetary systems- including telluric planets in the habitable zone of their host stars

Three complementary techniques:- photometric transits : Rp/Rs (Rs known thanks to Gaia)

- groundbased follow-up in radial velocity : Mp/Ms

- seismic analysis of host-stars (stellar oscillations) : Rs, Ms, age

> measurement of radius and mass, hence of planet mean density

> measurement of age of host stars, hence of planetary systems

Tool:- ultra-high precision, long, uninterrupted, CCD photometric monitoring of very

large samples of bright stars: CoRoT - Kepler heritage

- bright stars: efficient groundbased follow-up and capability of seismic analysis

PLATO Science Objectives

monitor in ultra-high precision photometry

a very large number

of bright and very bright stars

The PLATO challenge

Instrumental Concept

- 32 « normal » cameras : cadence 25 sec- 2 « fast » cameras : cadence 2.5 sec, 2 colours- pupil 120 mm- dynamical range: 4 ≤ mV ≤ 16

optical field 37°

4 CCDs: 45102 18m « normal » « fast »

focal planes

fully dioptric, 6 lenses + 1 window

Very wide field + large collecting area :multi-instrument approach

optical design

On board data treatment: 1 DPU /2 cameras + 1 ICU Science ground segment

Orbit around L2 Lagrangian point, 6+2 year lifetime

Concept of overlapping line of sight

4 groups of 8 cameras with offset lines of sightoffset = 0.35 x field diameter

8 8

8 8

16

16

16 16

2424

2424

32

Optimization of number of stars at given noise level AND of number of stars at given magnitude

37°

50°

~ 50% of the sky !

0°

30°

60°

90°

120°

150°

180°

210°

240°

270°

300°

330°

0h2h4h6h8h10h12h14h16h18h20h22h

CoRoT CoRoT

KeplerPLATO

PLATO

1. two long pointings : 3 years or 2 years2. « step&stare » phase (1 or 2 years) : N fields 2-5 months each

Observation strategy and sky coverage

Expected noise level

shot noise + readout noise + background noise + jitter + digitization noise

27 ppm

80 ppm

800 ppm

fast cam

8 cam

16 cam24 cam 32 cam

jitter/confusion + background

photon noise

photon noise limited up to mV=11

Performances

as a function of noise level

as a function of magnitude

PLATO (4300 deg2) 20,000 deg2 KEPLER (100 deg2)

noise level

(ppm/√hr)

nb of cool dwarfs & subgiants

long monitoring

mV nb of cool dwarfs & subgiants

incl. step&stare

nb of cool dwarfs

& subgiants

mV

27 20,150 9.3 - 10.8 80,400 1,300 11.2

80 292,000 11.6 - 12.9 1,000,000 25,000 13.6

1,326 8 3,315 30 8

60,275 11 180,000 1,300 11

PLATO Mission Consortium- Study, develop and deliver instrument: cameras + DPS

- Study, develop and operate PLATO Data Centre

- Milestones:

Oct. 29, 2010: Answer to the ESA AO

Nov. 9 &10, 2010: PMC kick-off meeting

May 2011: Preliminary Instrument Requirement Review (PIRR)provide documentation by end of April on all aspects of the mission

Jun. 2011: M2 down-selection by SPC

Oct. 2011: Instrument Design Consolidation Review (IDCR)

Dec 2011: Official end of definition phase

Jun. 2012: Instrument Preliminary Design Review (PDR)

ESA project team

End-to-end Simulator

W. Zima

PLATO PayloadManagement

PIPM: P. Bodin

PDCPDPM: L. Gizon

Instrument System CoordinatorP. Levacher

Science Coordination

H. Rauer

Target/field Characterization

G. Piotto

FU Coordination

S. Udry

Stellar Science M.J. Goupil

Exoplanet scienceD. Pollacco

TOUR. Ragazzoni

Fast DPUG. Peter

Normal DPUPh. Plasson

PLATO Mission Consortium Science Preparation Management

AlgorithmsR. Samadi

Mission management

AEU S. Fredon

ICUR. Cosentino

Prototype& FM AIVP. Levacher

main / ancillary databasesystem architecture

R. Burston

exoplanet analysis System

N. Walton

data processing implementation

I. Pardowitz

stellar analysis systemT. Appourchaux

Input CatalogueP. Giommi

Data Centre

Normal TOUR. Ragazzoni

Fast TOUW. Benz

Project Manager

Project Scientist Science Team- 6 PMC members- 2 Legacy Scientists

PMC Board

ancillary database content management

M. Deleuil

data analysis support tools

L. Gizon

FPA/FEED. Walton/M. Mas

Hardware & boot softwareM. Mas

Application softwarePh. Plasson

PMC Lead

C. Catala

Camera ManagementD. Laubier

DPS ManagementB. Pontet

Payload

SOC

data processing algorithmsR. Samadi

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Additional programs

W. Weiss