ARIEL - Ignasi Ribas Institut d'Estudis Espacials de Catalunya (IEEC) Institut de Ciències de l'Espai (ICE, CSIC) - Carmenes
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ARIEL
Enabling planetary science across light-years
Ignasi Ribas
Institut d’Estudis Espacials de Catalunya (IEEC)
Institut de Ciències de l’Espai (ICE, CSIC)
1st meeting of ExoNet, Granada, 22/2/2019
Exoplanets today: huge diversity 3800+ PLANETS, 2700 PLANETARY SYSTEMS KNOWN IN THE GALAXY
Huge diversity: why?
Formation & evolution processes?
Migration? Interaction with star?
Accretion
Gaseous planets form here
Interaction with star
Planet migration
Ices, dust, gas
Key exoplanet questions
• How diverse are exoplanets chemically?
• Does chemical diversity correlate with
other parameters?
• How do planets form?
• How do planets evolve?
The Sun’s planets are cold
SOME KEY O, C, N, S MOLECULES ARE NOT IN GAS FORM
T ~ 150 K
Warm/hot exoplanets
O, C, N, S (TI, VO, SI) MOLECULES ARE IN GAS FORM
Atmospheric
pressure
0.01Bar
H2O gas CO2 gas
CO gas CH4 gas
HCN gas TiO gas
T ~ 500-2500 K Condensates VO gas H2S gas
1 Bar
Gases from interior
Issues with current data
• Low SNR & R observations
• Data are sparse, not enough wavelength coverage
• Broad wavelength coverage is not simultaneous
• Absolute calibration at the level of 10-4 is not
guaranteed!
• Instrument systematics are difficult to disentangle
from the signal
• Stellar activity is the largest source of astrophysical
noise
• We need observations on a population of objects to
draw conclusions
ARIEL – ESA M4 mission • 1-m telescope, spectroscopy from VIS to IR • Satellite in orbit around L2 • ~1000 exoplanets observed (rocky + gaseous) • Launch in 2028 – 3.5-yr mission • Simultaneous coverage 0.5-7.8 micron • Payload consortium: 15 ESA countries + NASA under study
The exoplanet mission timeline
C
B
A 10-4 – 10-5 relative
precision
A B C
Sedaghati et al. 2017A chemical survey of a
large population
SCIENCE REQUIREMENTS: EXOPLANET RADIATION, MOLECULAR &
CLOUD SIGNATURES, STELLAR ACTIVITY
H2 O
CO2
CH4
CO
H +
3
HCN
NH3
SO
2
SiO
TiO
VO
C H
2 2
C H
2
(R /R )
2 4
s
C H
2 6
p PH
3
1 2 3 4 5 6 7 8
Wavelength ( m)
Simultaneous observations in the VIS and IR are neededARIEL 3-tier approach
INDIVIDUAL PLANETS & POPULATION ANALYSIS
• Main atmospheric
component
• Trace gases
SURVEY
• Thermal structure
• Cloud characterization
• What fraction of planets • Elemental composition
D EEP SURVEY
have clouds?
• Have small planets still
retained H/He? BENCHMARK
• Color-color diagrams
• Refinement of ~ 50-100
orbital/planet
parameters in IR • Atmospheric
~ 500 circulation
• Spatial & temporal
~ 1000 PLANETS variabilityChemical diversity
ARIEL WILL CLARIFY CORRELATION WITH THE DENSITY
– 42 –
Density observations Atmospheric composition through
●
ARIEL will clarify the degeneracy
3.0 O 3.0
/ T(K) K-20c H2
4000 2200 K-26b
0%
1600 ▲
K-26c
10
1000
2O
▲●
H
%
400 1200 GJ1214b
50
2O
●
2.5 2.5
H
100 900 HIP116454
%
K-307b
20
▲
40 700 ●
K-307c K-10c
)
ck
●
10 500
▲ HD97658b
(3 ro Fe Rocky Icy
●
55Cnce i O %
gS 25
K-60d
r (R⊕)
2.0
▲
▲ M
% Fe
2.0
Interior Interior
K-60c ● 50
K-60b K-20b
▲ K-21b
●
HD219134b
Fe
●
●
%
100
COROT7b
1.5 K-10b
● ▲ 1.5
H/He
●
K-93b K-36b
Water vapor
▲
K-105c
Atmosphere Atmosphere
●
K-78b
1.0 ● 1.0
● Earth
Venus
0.8 1 1.5 2 3 4 5 6 7 8 910
m (M⊕)
15 20
Same mean density – Different
atmospheric signatures
López-Morales et al. 2016; Valencia et al. 2013
Mass-Radius relation for planets with masses < 20 M , measured with precisionsLarge population of
warm/hot planets
TODAY AND IN THE NEXT DECADE
TESS yields
Sullivan et al. 2015ARIEL sky visibility
Instantaneous Sky 100% 80% 60% 40% Survey
Visibility Deep
BenchmarkARIEL science working groups
Spectral retrieval:
Michiel Min (SRON), Joanna Barstow (UCL), Ingo Waldmann (UCL)
Planet interior:
Ravit Helled (Un. Zurich), Stephanie Werner (Un. Oslo)
Planet formation:
Diego Turrini (INAF)
Disks:
Mihkel Kama (Cambridge), Olja Panic (Leeds)
Atmospheric chemistry:
Olivia Venot (LISA), Yamila Miguel (Un. Leiden), Franck Selsis (Un. Bordeaux)
Mass measurement with RV:
Lars A. Buchhave (DTU), Olivier Demangeon (Un. Porto)
Stellar characterisation:
Camilla Danielski (CEA)
Data challenges:
Subi Sarkar (Un. Cardiff) and Theresa Leuftinger (Un. Vienna) (Stellar activity)
Nikos Nikolaou (UCL) (Data reduction), Michel Min (SRON) (Retrievals)
Stellar activity:
Bart Vandenbussche (Un. Leuven), Ignasi Ribas (IEEC-CSIC), Giusi Micela (INAF)
Data analysis:
Ingo Waldmann (UCL), Angelos Tsiaras (UCL)ARIEL science working groups
Upper atmosphere/star-planet interaction:
Antonio Garcia Muñoz (TU Berlin), Manuel Guedel (U. Vienna), Luca Fossati (U.
Graz)
High-cadence photometry:
Davis Waltham (RH), Gyula Szabo (Un. Eötvös Loránd), Luca Borsato (Un.
Padova)
Ephemerides:
Vincent Coudé du Foresto (Obs. Paris)
Phase-curves:
Benjamin Charnay (Obs. Paris), João Mendonça (DTU)
Albedo and reflected light (+ synergy with other instruments):
Olivier Demangeon (Un. Porto)
Synergy with ELT & ground-based obs.:
Enric Palle (IAC)
Synergy with JWST:
Pierre-Olivier Lagage (CEA)
Synergy with Solar System science:
Gabriella Gilli (Obs. Lisboa), Pedro Machado (Obs. Lisboa)
Synergy with PLATO and CHEOPS:
Isabella Pagano (INAF), Giampaolo Piotto (Un. Padova)ARIEL science working groups
Scheduling:
Juan Carlos Morales (ICEE-CSIC), Andrea Moneti (IAP)
Performance simulations:
Enzo Pascale (La Sapienza/Cardiff), Subi Sarkar (Cardiff), Billy Edwards
(UCL), Lorenzo Mugnai (La Sapienza)
Spectroscopic database:
Clara Sousa-Silva (MIT), Svatopluk Civiš (Heyrovsky Institute)
Other science: brown dwarfs:
Sarah Casewell (Un. Leicester)
Other science: young stellar objects:
Csaba Kiss (Konkoly Obs.), Krisztián Vida (Konkoly Obs.)
Novel methods to handle high-volume, high-dimensional data:
James Cho (QMUL)
Synergy with NGTS, HAT:
Matt Burleigh (Leicester Un.), Gaspar Bakos (Princeton)
Synergy with TESS:
TBA from US
Synergy with amateur astronomers:
Anastasia Konkori (Royal Museums Greenwich), Marco Rocchetto
(Konica Minolta)ARIEL payload + EGSE + mission planning
Our role in the ARIEL consortium
ARIEL Consortium France Co-PI
Italy Co-PI Spain Co-PI Belgium Co-PI Poland Co-PI UK Co-PI
Steering Committee Giusi Micela
Jean-Philippe
Ignasi Ribas Bart Vandenbussche Miroslaw Rataj Matt Griffin
Beaulieu
(MLA Mandated Member INAF - Palermo IEEC – CSIC KU Leuven SRC Warsaw Cardiff University
CNRS IAP
State Representatives)
Consortium PI Austria Co-PI USA Co-PI
Italy Co-PI France Co-PI Spain Co-PI Netherlands Co-PI
Giovanna Tinetti Pino Malaguti Pierre-Olivier Lagage Enric Palle Michiel Min Manuel Güdel Mark Swain
UCL CEA CEA Saclay IAC SRON Uni of Vienna JPL
Consortium Project Czech Rep co-PI
Manager Denmark Co-PI Ireland Co-PI Norway co-PI
Martin Ferus
Paul Eccleston Lars Buchhave Tom Ray Stephanie Warner
Czech Academy of
RAL Space DTU Space DIAS University of Oslo
Science
ARIEL Science Team
Chaired by ESA ARIEL
PS Germany Co-PI Sweden co-PI Portugal Co-PI Hungary co-PI
Paul Hartogh Kay Justtanont Pedro Machado Robert Szabo
MPS Chalmers Uni. Uni de Lisboa Konkoly Obs
Consortium Co-PI Board
ESA ARIEL Project Team
Consortium Project Systems Engineering
Instrument Scientist Telescope Scientist Mission Scientist Consortium PI
Lead
Manager Kevin Middleton
Marc Ollivier Enzo Pascale Matt Griffin Giovanna Tinetti
ESA ARIEL Project ESA ARIEL Project Paul Eccleston IAS Uni di Roma Cardiff University UCL
Manager Scientist RAL Space
RAL Space
Italy NPM France NPM Spain NPM Belgium NPM Poland NPM
ESA ARIEL Payload ESA ARIEL Emanuele Pace Michel Berthe Pep Colome Bart Vandenbussche Miroslaw Rataj
Manager Project Team Uni di Firenze CEA IEEC – CSIC KU Leuven SRC Warsaw
Netherlands NPM UK NPM Ireland NPM Austria NPM USA NPM
Matthijs Krijger Rachel Drummond Deirdre Coffey Manfred Steller Kirk Seaman
SRON RAL Space UCD / DIAS IWF Graz JPL
Czech Rep NPM
Germany NPM Denmark NPM Portugal NPM Norway NPM
Svata Civis
TBD Søren Møller Pedersen Manuel Abreu TBD
Czech Academy of
MPS DTU Space Uni de Lisboa TBD
Science
Consortium Management TeamSpanish consortium organization
+ M.R. Zapatero Osorio
(member of ESA’s
ARIEL Science Team)Conclusions • ARIEL has been conceived to deliver the first chemical survey of ~1000 exoplanets, probing uniformly the gamut of planet and stellar parameters • The Spanish participation in the ARIEL mission science consortium and payload development is very significant • Timeline: Phase B1 (2019-2020), mission adoption (Nov 2020), phase B2 (2021-2022) • Think abut joining the science WGs!
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