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Giampaolo PiottoDipartimento di Astronomia - Università di [email protected]
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
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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)
Roma, Jan 29, 2009 G. Piotto
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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
Roma, Jan 29, 2009 G. Piotto
The evolution of exoplanetary systems = comparative exoplanetology
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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
Roma, Jan 29, 2009 G. Piotto
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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
Roma, Jan 29, 2009 G. Piotto
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PLATO Science Consortium (DLP)
Science Requirements
Science Requirements
Roma, Jan 29, 2009 G. Piotto
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S: Planet detection and characterization (HR)
Roma, Jan 29, 2009 G. Piotto
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S2: Planet detection and statistics (WB; CAF)
Roma, Jan 29, 2009 G. Piotto
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S3: Characterization of Planets and Planetary system evolution (HR; HL; LG; RN)
Roma, Jan 29, 2009 G. Piotto
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F: Field selection and simulation (GP)
Roma, Jan 29, 2009 G. Piotto
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F1: Input Parameters (GP)
Roma, Jan 29, 2009 G. Piotto
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F2: Image simulation (TA)
Roma, Jan 29, 2009 G. Piotto
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F3: Light Curve Analysis
Roma, Jan 29, 2009 G. Piotto
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P: Characterization of host stars (CA)
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D: Data Base Interface (HR)
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U: Ground Base Observations (SU)
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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
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New baseline designfour-l.o.s.
42 telescopes
3.60 m
40 normal telescopes
2 fast telescopes
56°
Roma, Jan 29, 2009 G. Piotto
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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
Roma, Jan 29, 2009 G. Piotto
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Performance of baseline design
magnitude for noise 27 ppm in 1 hr
compliantcompliant non compliant
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Performance of baseline design
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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
Roma, Jan 29, 2009 G. Piotto
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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
Roma, Jan 29, 2009 G. Piotto
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Roma, Jan 29, 2009 G. Piotto
Carina Field Standard field
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Roma, Jan 29, 2009 G. Piotto
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Roma, Jan 29, 2009 G. Piotto
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Roma, Jan 29, 2009 G. Piotto
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Roma, Jan 29, 2009 G. Piotto