PLAnetary Transits and Oscillations of stars

Claude CATALAObservatoire de Paris, LESIA

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

Meeting of the Data Analysis SystemCambridge May 27&28, 2010

Status of the mission

PLATO was selected in Feb 2010 for a definition phase, togetherwith Solar Orbiter and Euclid

Definition phase:1. Phase A until June 20112. Down-selection in June 2011 : two missions out of three will remain3. Phase B1 until Dec. 2011

ESA will issue an AO for constituting a PLATO consortium in mid-June 2010

Answer to the AO expected around Sep. 15, 2010

The Data Analysis System andthe PLATO Data Centre: what is it?

MOC

SOC

PDCDat

a A

naly

sis

Syst

emL1:

validated lightcurvesvalidated centroid curves

L2:transit parametersseismic parametersetc

ancillary data:- input catalog- FU data- etc

consortium

ESA team

End-to-end Simulator

PLATO instrumentManagement

PA/QP

RAIV

PDC

Industrialstudies

Science Team

Systemteam

Science coordination

Input Catalogue

FU Coordination

Stellar Science

Exoplanet science

TOU

FPA/FEE

Fast DPU

ICU

Algorithms

Normal DPU

Payload

science activitiesOverall management

AEU

Prototype& FM AIV

PPLC PIPPLC five co-Pis

PPLC co-Is

OB Data ProcessingSystem

Cameras

Basic structure of Consortium: place of the PLATO data centre

development,implementation, andoperation of tools to fullyexploit the data fromPLATO and ancillary data

Goals of the meeting

1. Identify all tasks related to the PLATO Data Centre in themore general context of the Data Analysis System

2. Establish to first order the Work Breakdown Structure, anddistribution of responsibilities

3. Prepare the answer to the AO, for all issues related to PDC

4. Prepare Phase-A work

5. Discuss further steps: phase-B1, phase-C, etc.

Science Objectives of PLATOSearch for and characterization of transiting exoplanets, using

combination of ultra-high precision space photometry andgroundbased radial velocity follow-up observations:

1. Study of exoplanets of all kinds, including earth analogs, i.e.terrestrial planets in the habitable zone of solar-type stars

2. Provide full characterization of the planet host stars (radii,masses, ages) through seismic analysis and other data, fromwhich planet radii, masses and ages will be determined

3. Identification of transiting planets around brightest solar typestars, including in their habitable zone, which will becomeprivileged targets of future characterization work

4. Search for transiting planets around dM stars up to a fewtens of parsecs at various orbital periods and with all physicalsizes, in a significant fraction of the sky

5. Seismic studies of bright stars of all types

PLATO target samples> 20,000 bright (~ mV≤11)

cool dwarfs/subgiants (>F5V&IV):

exoplanet transits AND

seismic analysis of their host starsAND

ultra-high precision RV follow-up

noise < 2.7 10-5 in 1hr for 3 years

> 250,000 cool dwarfs/subgiants (~ mV≤13)

exoplanet transits + RV follow-up

>1,000 very bright (mV≤8)

cool dwarfs/subgiantsfor 3 years

>3,000 very bright (mV≤8)

cool dwarfs/subgiantsfor >5 months

exoplanets

around bright and nearby stars

Main focus of PLATO:Bright and nearbystars !!

PLATO…is watching you !

noise < 8.10-5 in 1hr for 3 years

> 5,000 (3 years) + 5,000 (5 months) nearby M-dwarfs (mV≤15-16) noise < 8. 10-4 in 1hr

Instrumental Concept

New design- 32 « normal » cameras : cadence 25 sec- 2 « fast » cameras : cadence 2.5 sec- pupil 120 mm- huge dynamical range: 4 ≤ mV ≤ 16 !!

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

FPA

356 mmS-FPL51

N-KzFS11 CaF2(Lithotec)

S-FPL53L-PHL1

KzFSN5

164.

6 m

m

optics

fully dioptric, 6 lenses

Orbit around L2 Lagrangian point, 6-year nominal lifetime

optical field37°

4 CCDs: 45102 18µm « normal » « fast »

focal planes

field increased bymore than 25% !

larger CCD than YB concept C --> wider field

Concept of overlapping line of sight4 groups of 8 cameras with offset lines of sight

baseline offset = 0.35 x field diameter (k=0.35)

8 8

8 8

16

16

16 16

2424

2424

32

Optimization of number of stars at given noise levelAND 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

Kepler PLATO

PLATO

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

Sky coverage

Expected noise level

jitter/PRNU

jitter/confusion + background

photon noise

photon noise dominant

noise calculated for 32 camerasno

ise

in 1

hr (

ppm

)

Performances of the long pointing phasesas a function of noise level

as a function of magnitude

noise of 800 ppm/√hr is reached down to- mag 15 (1 group)- mag 16 (4 groups)entirely dominated by background and jitter/confusion

search for habitable planetsaround M-dwarfs

111,3001158,4908

13.6

11.2

mV

3081,290

25,00011.6 - 12.7330,00080

1,3009.6 - 10.922,00027

nb of cool dwarfs &subgiants

mVnb of cool dwarfs &subgiants

noise level(ppm/√hr)

Kepler (100 deg2)PLATO (4360 deg2)

spec 20,000

spec 250,000

spec 1,000

Groundbased follow-up- Vigorous follow-up needed- Most important aspect = radial velocity monitoring

⇒ planet confirmation and mass measurement

Planet Distance(AU)

RV Amp.(m/s)

Jupiter 1 28.4Neptune 0.1 4.8Neptune 1 1.5SuperEarth 0.1 1.4SuperEarth 1 0.5Earth 1 0.1

- stellar intrinsic « noise »: oscillations, granulation, activity- need to apply proper averaging technique- time consuming- in practice limited to bright stars

PLATO

CoRoT - Kepler

telescope diameter neededto confirm earth-like planet

Scientific Impact Expected number of detected transiting planets by PLATO and Kepler:- each star has one and only one planet in each cell - planet is detected if a transit signal AND a radial velocity signal are measured- intrinsic stellar « noise » is taken into account

The lower right corner (telluric planets in the HZ), not covered by Kepler because of theoverwhelming difficulty of FU observations, will be explored by PLATO thanks to its

focus on bright stars

Data Processing System

4 full frameimages= 1.3 Gb/25 sec

4 frame transferimages= 660 Mb/2.5 sec

120,000 intensities12,000 centroids1,600+ imagettescadence 25 sec

400 intensities40 centroids40+ imagettescadence 2.5 sec

x 32

x 2

intensities + σ (2.5s, 50s, 600s)centroids + σ (2.5s, 50s, 600s)imagettes (2.5s, 25s)

pointing errors

MOC

SOC

PDCDat

a A

naly

sis

Syst

em

L1:validated lightcurvesvalidated centroid curves

L2:transit parametersseismic parametersetc

ancillary data:- input catalog- FU data- etc

PLATO Payload Consortium: Science activities and PDC

PLATO Instrument Manager

P. Bodin

MOC

SOC

Data Analysis System

PDCL. Gizon

Stellar Analysis SystemT. Appourchaux

data treatment AlgorithmsR. Samadi

main database & system architecture

R. Burston

Exoplanet Analysis System

N. WaltonEnd-to-end Simulator

W. Zima

Science coordination

H. Rauer

Input Catalogue

G. Piotto

FU Coordination

S. Udry

Stellar Science

M.J. Goupil

Exoplanet science

D. Pollacco

science activities

data treatment implementation

I. Pardowitz

PPLC PIPPLC five co-Pis

Data Analysis System

ancillary databasetbd

data accesscoordination

software for- production of L1- monitoring of onboardprocessing