CSIC/IEEC - AstroMadrid

The EChO mission
Ignasi Ribas
Institut de Ciències de l’Espai (CSIC/IEEC)
Desarrollo de instrumentación astronómica en España, Madrid, Septiembre 2013
“The Exoplanet Revolution”
9 to 1000 in 15 years!
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Courtesy of Kepler team
Outstanding Science Questions
• Why are exoplanets as they are?
• What are the causes for the observed diversity?
• Can their formation history be traced back from
their current composition and evolution?
• Is the Solar System unique or very common?
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HAT-P7b observed by Kepler
(Borucki et al, 2010)
Transiting planets
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Transit & eclipse spectroscopy
Flux
Individual lightcurves
Different transit depths
Wavelength
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The technique has been proved…
Berta et al. (2012)
Beaulieu, Tinetti, Kipping,
Ribas et al. (2011)
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Spectral coverage
Given the range of T covered, we need a broad wl coverage
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EChO
Exoplanet Characterisation Observatory
ESA M3 mission candidate – March 2011
ESA Science Study
Team
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P. Drossart
P. Hartogh
C. Lovis
G. Micela
M. Ollivier
I. Ribas
I. Snellen
B. Swinyard
G. Tinetti
ESA Study
Team
K. Isaak
L. Puig
M. Linder
Potential launch 2022-2024
Down selection (2014)
EChO in a nutshell
 Telescope entrance pupil: 1.13 m2
 Coverage: 0.55-11 (0.4-16) µm
 < 1µm: Stellar activity monitoring
 1-5 µm: Hot/warm planets (H2O, CO, CO2, CH4)
 > 5 µm: Cooler planets + key molecules
 40% of the sky visible at any time: L2 orbit
 Transiting planets: ~200
 R ≥ 300 (< 5 µm); R ≥ 30 (≥ 5 µm)
 Photometric stability 10-4 (90s, 10 hrs - goal 10-5)
 SNR requirement depends on survey mode
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EChO’s 3 observing modes:
Studying exoplanets as a population & individuals
 3-tier survey:
 Chemical Census: volume-limited sample of transiting planets of
different types with SNR ≈ 5 at R=50 & 30 to detect presence of
molecules (50%)
 Origins: bright gaseous planets with SNR ≈ 10 at R=100 & 30 to
understand detailed physics & chemistry (40%)
 Rosetta Stone: selected targets to enable temporal and spatial
monitoring, benchmarking (10%)
 Wide parameter space coverage, good constraints to planet
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formation & evolution models
 Best exploits EChO capabilities w.r.t. competition (JWST)
 Goal to observe ≥200 planets (130 known today)
Planets studied by EChO
Jupiter
Neptune
Super Earth
Radius
‘Hot’
(800-2500 K)
Easy
GKM stars
‘Temperate’
(250-400 K)
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OK
Temperature
‘Warm’
(400-800 K)
late K & M stars
Tough
late M stars
Very hard
The EChO Instrument Consortium
 Austria
 Netherlands
 Belgium
 Poland
 Denmark
 Portugal
 France
 Spain
 Germany
 Sweden
 Ireland
 UK
 Italy
 In Spain:
 ICE (CSIC-IEEC)
 IAC
 CAB (CSIC-INTA)  IAA
 INTA
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Payload design
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Mechanical Design
& Layout
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Consortium Management Team
Consortium Central Leadership
Consortium
Engineering Manager
TBD
RAL Space
Consortium Project
Manager / UK NPM
Paul Eccleston
RAL Space
France NPM
Jean-Michel Reess
OPM - Lesia
Italy NPM
Emanuele Pace
Uni di Firenze
Spain NPM
Pep Colomé
CSIC - ICE
Germany NPM
Peter Börner
MPS
Netherlands NPM
Jan-Rutger Schrader
SRON
Poland NPM
Miroslaw Rataj
SRC Warsaw
Austria NPM
Roland Ottensamer
Uni of Vienna
Belgium NPM
Etienne Renotte
CSL
Ireland NPM
Ruyman Azzollini
DIAS
National Project Managers (for major HW / SW
Contributions)
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EChO Phase A Study Final Presentations, ESTEC
Consortium PI
Giovanna Tinetti
UCL
Instrument Scientist
Marc Ollivier
IAS
France co-PI
Jean-Philippe
Beaulieu
CNRS IAP
Italy co-PI
Giusi Micela
INAF - Palermo
UK co-PI
Bruce Swinyard
UCL / RAL
Spain co-PI
Ignasi Ribas
CSIC - ICE
Germany co-PI
Paul Hartogh
MPS
Netherlands co-PI
Avri Selig
SRON
Austria co-PI
Manuel Guedel
Uni of Vienna
Poland / Sweden co-PI
Hans Rickman
SRC Warsaw / Uppsala
Observatory
Ireland co-PI
Tom Ray
DIAS
Belgium co-PI
Denis Grodent
Uni de Liege
Denmark co-PI
Hans Ulrik NørgaardNielsen
DTU Space
Portugal co-PI
David Luz
Uni de Lisboa
Consortium Co-PIs
24th September
Consortium Management Team
Lead
Funding
Countries
Major
Contributing
Funding
Countries
Participating
Funding
Countries
2013
Spanish contribution
 CSIC-ICE & IEEC
 Mission Co-PI and NPM
 Ground segment: long-term mission planning tool
 INTA
 SWIR optical module leadership (WP 51, manager: Ana Balado /
Gonzalo Ramos)
 CSIC-IAA
 DPU simulator (WP 84, manager: Luisa M. Lara)
 All
 Science: stellar activity correction, target selection, retrieval of
atmospheric data, interpretation of results
 Possible involvement: on-board software (SWIR channel?) & Data
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processing (SWIR?)
EChO Simulators of Electronics
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Grism
SWiR module
Prism
Camera
optics
Image
Plane
Optical & mechanical design
 Pixel pitch: 18 mm, R~300 or higher
 Input beam: elliptical 25  17 mm2 at
SWiR entrance pupil
 l overlapping solution with prism +
grism
Folding
 Ge except for the grism in ZnSe
Mirror
 Around 88 mm
defocus included for
PSF proper sampling
Slit
Badel 2nd
Mirror
Slit (field stop)
Grism
Prism
Image
Plane
Camera
optics
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Badel Mirrors
Ground segment
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Long-term planning
 Fixed time observations are a new issue for scheduling ESA
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missions
Agreed with ESA that the payload consortium will take
responsibility for long term scheduling
ICE (CSIC-IEEC) is in charge of running scheduling simulations
Mission can be scheduled with fixed downlink windows (2 per
week)
Interactions on-going with SOC and MOC experts on how to
increase flexibility
Timeline
 Payload AO issued September 2012 and resolved in early 2013
 2 competing proposals: UK consortium selected
 Phase 0/A will finished in September 2013
 Payload studies and S/C industrial studies in parallel
 Preliminary Requirements Review in October/November 2013
 Phase B1 after down selection (mid 2014-late 2015)
 Science: delivery of Yellow Book in November 2013
 Presentation to advisory structure in mid January 2014 (Paris)
(EChO, LOFT, Marco Polo-R, STE-Quest, PLATO)
 AWG/SSEWG/SSAC meeting also in Jan
 SPC decision in February 2014
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Conclusions
 The exoplanet field is going through a “revolution”: 1000 planets
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in ~ 15 years, and the Solar System is no longer the paradigm!
To understand the exoplanet diversity and the role of the Solar
System in a broader context, we need to understand how planets
form & evolve in our Galaxy
Our only way to understand these processes is to study the
atmospheres of exoplanets as tracers
We need a large number of exoplanetary atmospheres, and we
need very accurate, coherent, measurements
We need a dedicated mission: EChO is the answer
Spain has a key role in the EChO mission
EChO Phase A Study Final Presentations, ESTEC
24th September 2013