Giampaolo PiottoDipartimento di Astronomia - Università di PadovaGiampaolo.Piotto@unipd.it

PLAnetary Transits & Oscillations of stars

Search for and characterisation of exoplanets + asteroseismology

going beyond CoRoT & Kepler

PLATO KOM+1 meeting & Telescope Group MeetingRoma, January 29, 2009

Agenda: 09:15-09:30 Giampaolo Piotto - Welcome and Communications 09:30-10:00 Claude Catala - PPLC: Status and future steps 10:00-10:30 Roberto Ragazzoni - TOU: Status and future steps 10:30-10:45 Break 10:45-11:15 Andrea Baruffolo - ICU: Status and future steps 11:15-11:45 Giampaolo Piotto (Silvano Desidera) - PSC: Status and future steps 11.45-12:00 Isabella Pagano - PLATO Management in Italy: info 12:00-13:00 Discussion 13:00 - 14:00 lunch 14:00 - 14:20 Demetrio Magrin - Report on Optical Design 14.20 - 14:40 Daniele Piazza - Report from Mechanical Design 14:40 - 15:00 Stefano Basso - Report from Thermo-mechanical Analysis 15:00 - 15:30 Jose Luis San Juan - I/F between FPA and TOU 15:30 - 15:45 Mauro Ghigo - Report from Optical Material Analysis 15:45 - 16:00 Matteo Munari - Report from Straylight Analysis & Baffling 16:00 - 17:00 Plans for future activities (chair Ragazzoni)

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Science Objectives

The evolution of planets and that of their stars are intimately linked.

A complete and precise characterization of host stars is necessary to: Measure exoplanet properties: mass, radius, age Compare planetary systems of various ages Observe exoplanets at different stages of dynamical

evolution and at different stages of physical and chemical evolution

Correlation of planet evolution with that of their hosts stars

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The evolution of exoplanetary systems = comparative exoplanetology

Mission Objectives

The Search for, and characterization of, exoplanets and their host stars

Logical step forward after CoRoT and Kepler (and TESS?)

Search for exoplanetary transits and asteroseismology for the same star samples

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The PLATO Science Consortium

PI: Don PollaccoCo-PIs: Connie Aerts Heike Rauer Giampaolo Piotto Stephane Udry

Kick-Off meeting, Paris, Nov 13, 2009

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PLATO Science Consortium (DLP)

Science Requirements

Science Requirements

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S: Planet detection and characterization (HR)

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S2: Planet detection and statistics (WB; CAF)

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S3: Characterization of Planets and Planetary system evolution (HR; HL; LG; RN)

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F: Field selection and simulation (GP)

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F1: Input Parameters (GP)

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F2: Image simulation (TA)

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F3: Light Curve Analysis

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P: Characterization of host stars (CA)

D: Data Base Interface (HR)

U: Ground Base Observations (SU)

Evolution of Scientific Requirements

high level science requirements redefined by PSST and PSC

- P1: > 20,000 bright (~ mV≤11) cool dwarfs (>F5V); noise < 27 ppm in 1hr

- P2: > 80,000 bright cool dwarfs; noise < 80 ppm in 1hr during long pointing

but < 27 ppm in 1 hr during step & stare phase

- P3: ~ 1000 very bright stars (4 ≤mV≤ 8) for 3 years

- P4: ~ 3000 very bright stars (4 ≤mV≤ 8) for > 5 months

- P5: > 250,000 cool dwarfs; noise < 80 ppm in 1 hr for 3 years

New baseline designfour-l.o.s.

42 telescopes

3.60 m

40 normal telescopes

2 fast telescopes

56°

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10 10

10 10

20 20

20

20

40

pupil size 120mmpixel size 15 arcsec 40+2 telescopestotal field of view (2 pointings) = 3600 sq deg

42° as proposed by optics/telescope team

PLATO 4 OVERLAPPING L.O.S CONCEPT

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Performance of baseline design

magnitude for noise 27 ppm in 1 hr

compliantcompliant non compliant

Performance of baseline design

Simulations

Main goal for the Assessment phase is to test the PLATO photometric performances

Should be a tool for an independent test of the PLATO onboard and GB software

It is a tool for both the PPLC and the PSC

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Simulations start-up

We started from the Eddington Simulation Tool (Torben Arentoft)

We used PSFs from the TG (D. Magrin) We simulated 2 512x512pxs sets of

images at center of the field, with a 12.5 and a 15 arcsec/pixel PSFs

2 fields: a “crowded” Carina field, and “less crowded” field

CCD noise and Jitter from Eddington Unweighted mask aperture photometry

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Carina Field Standard field

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