Annie Baglin, Natal, October 30th 2004 1 The origin of the mission The scientific requirements The global programme The focal plane and the targets The scientific organisation COnvection, ROtation and planetary Transits COnvection, ROtation and planetary Transits An introduction to the CoRoT mission http://www. astrsp - mrs . fr /projets/ coro http://cnes.mission.fr/coro
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Annie Baglin, Natal, October 30th 2004
1
The origin of the missionThe scientific requirements
The global programmeThe focal plane and the targets
The scientific organisation
COnvection, ROtation and planetary TransitsCOnvection, ROtation and planetary Transits
* Ultra high precision stellar variability* Very long duration of observations * without interruption* on a large variety of starsRelative variations of stellar quantitiesmainly in the optical domain,Analysis in the time/frequency space
Photometry from Space Ministallite World wide pioneerWorld wide pioneer
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The early days of the space adventure
First Colloquium Observatoire de Paris in 1984
Workshop on Improvements to photometry San Diego 1984
Stating the importance of space for stellar seismology and activity
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2
3
4
5
6
7
0 1 2 3 4 5 6
rel power /10**4 μHz
mHz
scintillation
transparency
+ scintillation transparency
from E. Fossat, San Diego Workshop,
• High resolution Spectroscopy Large telescopes Limited to low Vr
• Photometrylimited by scintillation on the ground
Goal: < ppm in 5 days : ~ 2 10-7 / μHz~ 1000 times less !
2 10-4 / μHz
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EVRIS
Telescope 15 cm, Built in Meudon, Marseille and Austria
On board the Soviet spacecraft Mars 96
Observation of 10 very bright stars During the cruise to Mars
MOST (μ sat Canada), analogous to EVRIS is now flying…..
CRASH!But…….
After many proposals on different programmesEVRIS accepted by CNES…… in 89
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Several european projects
Combining seismology and activity (visible and UV instruments)
PRISMA(1993)
1m visible, 3° FoVFar UV 10cm monitor CII
Large phot (40,1.5°)Small phot (15 cm, 3°)
UVSpectro (57cm, R=30 000)XUV tel (40cm, 13nm)
STARS (1996)
But not selected
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The long way to go….
But……. crash of Mars 96, ……..discovery of exoplanets in 95 ……..improvement of detectors
…..New proposal in 97
Started in 93 as an answer to a AO for minisats by CNES
As a second generation mission……
Preselected in 98Selected in 2000 launch in 2004..!Confirmed in 2002 after some threat…..European
and Brasilian partners
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Seismology requirements/1
The solar template(only star observed in photometry)
Secondary science with CoRoT ?Described e.g. in Weiss et al 2004 Palermo Eddington colloquium
Wide variety of subjects and interest
*Large and complete stellar data base of more than 100000 stars11 < V < 16
*Also a few selected targets
Creation of the Additional Programmes
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Browsing in the exoplanet data
Measuring limb darkening with binaries
Defining the Dor domain
COROT
Detecting infalling comets
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Observing specific objects
EX: NGC 2264
from WEBDA
• v<8.5• 8.5<v<9.5• 9.5<v<12+ v>12
Up to 10 stars inCCDA1 and CCDA2Or many faint ones in exo field
8
8.5
9
9.5
10
10.5
11
9999.5100100.5101
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The global programme
Core programmeSeismology +Exoplanet(In the corresponding focal planes)
Central programme ≥ 5 long runs (150 days)
50 S targets mv < 9.5 60 000 E targets mv < 15.5
Exploratory programme ~ 4 short runs (10 to 20 days)
50 S targets mv < 9.5 60 000 E targets mv < 15.5
Restricted to Co-Is and their teams
Additional programmes Any scientific field
except Core Programme
• ~ 4 specific short runs50 S targets mv < 10.5 ? 60 000 E targets mv < 16 ?
• A few targets in the exoplanet field
• Use of the data of the core programme
Open AO, GIs
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The eyes of COROT
C1: density dwarfs ≥ 1500 per square degree
at mv<15.5
C2: ≥ 5 main targets FGK IV, V mv< 6.5 Delta scuti < 9
Scientific Constraints
=102.5 and 282.5
Early feasibility studies based on catalogues and plates
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Ground based complementary observations
Effort supported by Laboratories and Participating Countries
Collection of data on potential targets to determine the fundamental parameters (Teff, logg, [Fe/H], Vsini..)select the targetsprepare ground-based support and follow-up
Bright for the seismology field > 250 nights > 250 nights 0.9 to 3.5 m telescopes0.9 to 3.5 m telescopes > 1500 stars> 1500 starsData base: GAUDI at LAEFF
Faint stars for the exoplanet field ≥ 2.5m telescopes 100 million starsData base: EXODAT at LAM
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Seismology GBO
1-Photometric & spectroscopic observations of targets up to mV=8 for scenarii 1.2.3.4
• All observations complete: about 1500 stars .Data in GAUDI• Teff, log g, MV, [Fe/H], vsini, VR derived from these data, in Corotsky and GAUDI
Stromgren photometry from OSN, SpainHigh res. spectroscopy from ELODIE/OHP
FEROS (ESO+BRASIL) SARG/TNG +Coralie + Tautenburg
2- New targets to be observed because of possible drift of orbital plane(552 new targets, 68 near primary objects)
• Work started on ESO/FEROS (Renan)
3- Observations of targets with 8 ≤ mV ≤ 9.5 in 1.4° x 2.8° field around main targets
(386 stars)photometric Stromgren observations: IAA/OSN in 2004/2005spectroscopic observations:proposal for CFHT/Espadons for 2005A (all 386 stars in 3 nights)additional proposal for ESO/FEROS
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Preselected fields for long runs
-10-50510
-10
-5
0
5
10
171834
177552
181555
170580
18064243587
49434
49933
522651Winter 2006/7
2Summer 2007
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Seismology targets
-2
-1
0
1
2
3
4
5
6
3.63.73.83.944.1
43318
43587
45067
49434
49933
46558
52265
171834
177552
175726
181555
171234
180642
log teff
2.4Mo
2.0Mo
1.8Mo
1.4Mo
1.0Mo
170580 ?
Principal targets A possible choice for secondary targets
Need of more precise fundamental parameters
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A possible HD 49933/49434 long run
Exobasket
Rrange contam E1 E2 Total
11-15 0.1 2630 2221 4851
11-15 0.2 425 265 690
15-16 0.1 1845 1200 3045
15-16 0.2 601 926 1527
11-16 0.2 5501 4612 10113
11-14 > 0.2 181 173 354
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Next steps
1- CW7 in Granada December 2004- confirm the two first fields for the long runs: LR1a, LR1c
star densities for exo, set of secondary targets for sismo
2- January 2005 AO for AP CoRoT year 1
3- CW8 in Toulouse June 2005- prepare the first short runs SR0a (split in 2? Also technical), SR1a- define the next two other long runs: LR2a, LR2c- select the AP for CoRoT year 1
4- CW9 December 2005- Selection of the first short runs SR0a, SR1a, SR1c: AP?- define the next two other long runs: LR3a, LR3c
5- January 2006 AO for AP CoRoT year 2……….
Still preliminary…….subject to modifications
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The COROT Team
• RSSD/ESTEC: MDP Unit
• SPAIN: Ground segment
• AUSTRIA: participation to the DPU
• ESA Scientific programme: Optics and AIT contribution
• BELGIUM: Baffle, cover, mechanics of the service module
participating countries(• Chairs of the Working Groups (5) • Project Manager (invited)
In charge of
- the scientific specifications - the programme of observations - the data distribution policy - the list of Co-Is and Gis - Programme of CWs - Public relations
COROT WEEKS twice a year
Open scientific Meetings + CS and WGs
7th in Granada (Spain), Dec 14th to 17th
Meetings:Twice a year or more At each CW
Nice 1999
Marseille 2003
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The data policy
Public release
Observation
Data reduction
Distribution of I(t)to the CoIs and GIs
150 days
~ a few months
~ 1 yearResponsability: Project Team
*
Publications will be put on a secured siteTo be Referred by the SC within 15 days (TBC)
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Do sonho ate a realidade
~ Junho 2006…..!
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MOST a pionner microsat
1st canadian microsatelliteLaunched June 30th 2003Suitcase size15 cm collectorMono-objectHeliosynchroneus LEO
A few bright stars , 30 days mv = [ 0,5] of all types
Procyon, amplitude spectrum a) observed by MOST for 32 days
b) simulated signal: p modes 10ppm and 3 days lifetime
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KEPLER
Terrestrial planets findingNASALaunch 2008?
95 cm Schmidt telescopeFOV 100deg2 100 CCDs Trailing orbit
5 years on one field
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EDDINGTON: the mission
4 identical co-aligned60 cm Schmidt telescopesOn a Herschel busFOV = 35 deg2
At L2
Programmatic difficulties….???
Culmination of the European effortsHorizon 2000 + medium size mission
Seismology + Planet finding
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GAIA
ESA Cornerstone 2010-2012
Stellar physics
Fundamental parametersLuminosity calibrationVariability levelsBinaries……