O SATÉLITE PLATO: O

BRASIL NOVAMENTE NO

ESPAÇO

Eduardo Janot Pacheco

IAG, 14 de maio de 2014

Fresco painted 1509-1511 by Raphael (1483-1520) in theVatican (S tanza de lla S egnatura, Palazz i Pontifici)

ESA Cosmic Vision Programme (2015-2025)

L-Class missions: up to 109 Euros

M-class missions: up to a few 108

Euros

S-class missions: less than 50 x 106 Euros

4 themes:

Planets and Life

The Solar System

Fundamental Laws

The Universe

M missions 2011: launching 2017-2020

– Solar Orbiter: solar and heliospheric physics (NASA)– Euclid : universe's geometry

L mission 2012: launching in 2020

– JUICE (JUpiter ICe Moons Explorer)

S mission 2012:

– CHEOPS: ultra high precision photometry of small exoplanets with known mass è very precise radii

M mission 2014:

– PLATO (not selected in 2011)

(M missions) Not selected:

EchO (chemical composition of exoplanet atmospheres), LOFT (X-rays), Marco Polo (asteroid), STE-QUEST (Equivalence Principle)

Planetary Transits and Oscillations of stars (PLATO)

♦ 34 X 12 cm telescopes (~ 4 m diameter)

♦ 4 ccd per camera: total area of 0.9 m2

♦ ~ about 2250 deg2 per pointing (Kepler: 100deg2)

♦ relatively bright stars ( 4< V <8) è è easier to confirm extrasolar planets using follow-up RV measurements

♦at L2 (T and radiation stability)

Thales – Alenia Space concept

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 18µm

« 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

5

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

H. Rauer

Camera ManagementD. Laubier

DPS ManagementB. Pontet

Payload

SOC

data processing algorithmsR. Samadi

QuickTime™ et undécompresseur

sont requis pour vis ionner cette i mage.

Additional science W. Weiss

Q uic kTim e™ et und é co m pr es s eur

son t r e qui s po ur visio nne r ce tte im a ge.

6SAB, Sep 2011

300,000 dwarf and subgiant stars V< 8; Total of 105 stars for V< 11 photometric precision 3.4 10-5

2-3 years observations of same fields: to observe transits in 1 year orbits

PLATO GROUND SEGMENT

Science Operations Centre (SOC) - at the European Space Astronomy

Centre (ESAC), in Villanueva de la Cañada, Spain: light curve validation and

distribution

Mission Operations Centre (MOC) - at the European Space Operations

Centre (ESOC) in Darmstadt, Germany: - ground segment and operations

infrastructure for the flight operations and control.

(National) Science Data Centers, responsible for the pipeline processing

of the data leading to the final mission products (calibrated stellar light

curves)

Germany (DLR), Austria, Belgium, Brazil, Denmark, France,

Hungary, Italy, Portugal, Spain, Sweden, Switzerland, UK

PLATO main goals 1:

► detection of ~100 planets down to Earth- size in HZ

of solar-like stars

► determination of highly accurate stellar parameters

including masses and ages through seismological

analysis è è Mainly bright stars

► bulk properties (mass, radius, mean density, age) of

thousands of planets in a wide range of systems

Radii ± 2% Masses ± 4–10% Ages ± 10%

► detection of exomoons, planetary ring systems,

Trojan-planets, exo-comets, etc.

PLATO main goals 2:

► Place Solar System into context

► How do planets and planet systems evolve with age?

(constrain planet formation scenarios)

► How often are planetary systems co-planar, rather than

having been heated by more massive planets?

► How do planet properties and their frequencies correlate

with factors relevant for planet formation (e.g., stellar

metallicity, stellar type, orbital distance, disk properties)?

►Does the frequency of terrestrial planets depend on the

environment in which they formed?

Exoplanet Detection and Planet Parameters

• lightcurve filtering and transit detection planet candidates

• planet candidate ranking input to follow-up

• follow-up observations confirmation or rejection of candidates

• transit fitting tools planet parameters

Leger et al. 2009

11

Groundbased follow-up

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

⇒ planet confirmation and mass measurement

- 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 needed to confirm earth-like planet

12

CoRoT 7

PLATOlimGround

lim

Exoplanets: state of the art

PLATO super-Earthslim: transit + RV

PLATO Space

PLATO and super-Earthsorbiting bright stars: many candidates for follow-up:High precision data

PLATO results on planet models

►constraint on planet formation

►What is the bulk density distribution of low-mass,

terrestrial planets?

►What is the observed critical core mass for giant

planet formation?

►Can super-massive rocky planets exist and how are

they formed?

►How do these parameters depend on stellar type,

metallicity, chemical composition or age?

Note the scarce number of points for Earth mass planets.

PLATO well known radii and masses

-

Wagner et al. 2009, also: Valencia et al. 2007

5%

10%

5%

maximum acceptable

PLATO error bar

standard error bar

Impact of radius and mass measurementImpact of radius and mass measurement

maximum acceptable error bars

10%

10%

5%

PLATO and the composition of low-mass planets

PLATO and the atmospheres of exoplanets

► Diversity of albedos present in exoplanetary

atmospheres? How does the albedo correlate with the

other properties of the exoplanet (incident flux, metallicity,

etc)?

► What are the dominant, inert molecules present in

exoplanetary atmospheres? What are the mean molecular

weights?

► When are clouds present in exoplanetary

atmospheres? What is the diversity of the cloud properties

(particle size, reflectivity, etc)?

• What are the dominant, inert molecules present in exoplanetary atmospheres? What are the mean molecular weights?

• When are clouds present in exoplanetary atmospheres? What is the diversity of the cloud properties (particle size, reflectivity, etc)?

PLATO and other astrophysical science goals – 1

► seismology è stellar structure & evolution

Masses < 10%; radii < 1-2%; ages to 10%; 105 stars

► PMS, WDs, subdwarfs, red giants, O-B, MS...

► ages from PLATO + distances from GAIA + chemical

composition (spectroscopic surveys) èè chemical

gradients & their time evolution ≡ galactic evolution

► (differential) rotation, activity & gyrochronology +

Doppler imaging (bright stars) è surface physics

► Classical stellar pulsations

► Binary zoo

PLATO and other astrophysical science goals – 2

► All-sky accessibility + optical photometric cadence of

25 and 2.5 seconds è è physical processes

involved in disc accretion of compact objects in sample

of selected optically bright CVs and XRBs.

► mass loss and mass exchange in binaries

► SNs, GRBs, microlensing searches for black holes

► Kuiper-belt and Oort clouds objects

O catálogo produzido pelo PLATO servirá de input

para os futuros telescópios gigantes e o JWST.

BRAZIL PARTICIPATION2013: AEB agreement

May 2014: Comitê PLATO Brasil

Software & hardware Instituto Mauá de Tecnologia (S. Bernardo do Campo, SP) + LAC - EPUSP

► jitter photometric correction► PSF + sky background modelling► telescope calibration► Front End Electronic Simulator: reading system► On-board software?

BRAZIL PARTICIPATION (Cont.)

b) Science:

u Plato field selection, input catalogue (PIC)► transit detection, planet parameters, ► stellar physics, oscillation modes, stellar evolution models,► follow-up observations,► additional science program.

c) Science/instrumentation:

project for follow-up:

“Infrared Super-HARPS” (precision in Vr: ~ ≈10 cm/s)

UFRN/ USP/Obs. de Genève/Canada/ Germany/...

èè NTT La Silla

OPPORTUNITIES FOR BRAZILIAN PEOPLE2014 – 20??

MSc, PhDs, sandwiches etc. in

Science & enginereeing (software + hardware)

$ from FAPESP, CNPq, FINEP, etc...

OBRIGADO

DANKE

THANK YOU

MERCI

GRAZIE

GRACIAS

KÖSZÖNÖM ...