Evolution of matter from the interstellar medium to exoplanets with the JWST - Indico
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Evolution of matter from the interstellar
medium to exoplanets with the JWST
Modeling of protoplanetary disks
Robert Brauer (DAp/IAS)
CSNSM: C. Engrand, J. Duprat, M. Godard, L. Delauche, L. Delbecq, D. Le Du, J. Bourcois, C. Baumier,
C. Bachelet, F. Fortuna, B. Augé, E. Charron, B. Guerin, J. Roja
IAS: A. Abergel, A. Aleon, R. Brunetto, E. Habart, A. Jones, M. Olivier, L. Verstraete, N. Ysard, Z. Djouadi,
O. Mivumbi, K. Dassas, C. Cossou, R. Brauer, T. Bouteraon, Z. Dionnet, T. Schirmer, R. Maupin, R. Urso
ISMO: E. Dartois
IPNO: M. Chabot, G. Martinet, S.Bouneau, N. De Sereville, F. Hamache
DAp/AIM: P. Bouchet, D. Dicken, S. Fromang, P.-O. Lagage, E. Pantin, A. Coulais, R. Gastaud, R. Brauer,
G. Morello, M. Martin-Lagarde
Maison de la Simulation: P. Tremblin
PhD and post-doc since Sept. 2016
Evolution of interstellar dust
Everywhere
Optical ⇒ Infrared
Visible (ESO/S. Brunier) Planck HFI (thermal dust)
Key actor of matter evolution at all angular scales
∼ 50 kpc ∼ 280 AU
Herschel, FIR, M31 NRAO, visible in Orion HST visible, M16 ALMA 1 mm, HL Tau
2
Evolution of interstellar dust
Everywhere
Optical ⇒ Infrared
Visible (ESO/S. Brunier) Planck HFI (thermal dust)
Key actor of matter evolution at all angular scales
∼ 50 kpc ∼ 280 AU
Star and planet formation
Herschel, FIR, M31 NRAO, visible in Orion HST visible, M16 ALMA 1 mm, HL Tau
2
Evolution of interstellar dust
Everywhere
Optical ⇒ Infrared
Visible (ESO/S. Brunier) Planck HFI (thermal dust)
JWST Herschel Planck
Key actor of matter evolution at all angular scales
∼ 50 kpc ∼ 280 AU
Warm dust,
Cold dust
Dust bands
Herschel, FIR, M31 NRAO, visible in Orion HST visible, M16 ALMA 1 mm, HL Tau
Jones et al. 2013 + DUSTEM
2
The JWST: successor of the HST
A 6.5 meter infrared telescope in space
Optimized in the IR
Spring
Launch: ✭ ✭✭2019✭✭ → March 2021
In operation for 5 to 10 years (2021→2031)
3
The JWST: successor of the HST
A 6.5 meter infrared telescope in space
Optimized in the IR
Spring
Launch: ✭ ✭✭2019✭✭ → March 2021
In operation for 5 to 10 years (2021→2031)
Four IR instruments:
NIRIS (0.6 − 5 µm) (Canada)
NIRCAM (1 − 5 µm) (US)
NIRSPEC (1 − 5 µm) (ESA)
MIRI (5 − 28 µm) (Europe – US)
3
The JWST: successor of the HST
A 6.5 meter infrared telescope in space
Optimized in the IR
Spring
Launch: ✭ ✭✭2019✭✭ → March 2021
In operation for 5 to 10 years (2021→2031)
Four IR instruments: Four scientific themes:
NIRIS (0.6 − 5 µm) (Canada) First light and the reionisation
NIRCAM (1 − 5 µm) (US) Assembly of galaxies
NIRSPEC (1 − 5 µm) (ESA) Birth of stars and proto-planetary systems
MIRI (5 − 28 µm) (Europe – US) Planetary systems and the origin of life
3
Overview of work packages
Extraterrestrial JWST data
JWST proposals
material / analogues (from 2021)
Laboratory
Pre-JWST data Data processing
experiments
Simulation of exoplan-
Laboratory data Data analysis
etary atmospheres
Simulations of
Dust modelling Radiative transfer codes
JWST observations
WP2 WP3 WP4 Geometry and chemical JWST simulated
structure of PDRs & disks data processing
4
WP2: Preparation of JWST observations (ongoing work)
5
WP2: Preparation of JWST observations (ongoing work)
Prior to launch (2016-2020)
• Participation to the French Center of Expertise for MIRI
• Simulations of JWST observations
• Participation of test campaigns and pipeline developments and
testing
5WP2: Preparation of JWST observations (ongoing work)
Prior to launch (2016-2020)
• Participation to the French Center of Expertise for MIRI
• Simulations of JWST observations
• Participation of test campaigns and pipeline developments and
testing
Strongly involed in several observing programs
• Eearly Released Science programs
• Guaranteed Time Observations (GTO)
• Open Time Observations (Cycle 1 call in 2019)
5WP3: Modelisation & Simulations (ongoing work)
6WP3: Modelisation & Simulations (ongoing work)
Photodissociation Regions (PDRs) and Disks
• New charge model for dust grains H+ 5’’
H0
• Optical properties of large aggregates H2
• Laboratory-based silicate optical properties
(collaboration with IRAP/Toulouse)
• Dust and radiative transfer models to analyse
pre-JWST data (RT codes: MCRT, MCFOST, POLARIS)
• Nano carbon dust emission in protoplanetary
disks (VLT IR spectroscopy data)
• Dust evolution in PDRs
(Spitzer, Herschel, and HST data) Horsehead nebula
6WP3: Modelisation & Simulations (ongoing work)
Photodissociation Regions (PDRs) and Disks
• New charge model for dust grains H+ 5’’
H0
• Optical properties of large aggregates H2
• Laboratory-based silicate optical properties
(collaboration with IRAP/Toulouse)
• Dust and radiative transfer models to analyse
pre-JWST data (RT codes: MCRT, MCFOST, POLARIS)
• Nano carbon dust emission in protoplanetary
disks (VLT IR spectroscopy data)
• Dust evolution in PDRs
(Spitzer, Herschel, and HST data) Horsehead nebula
Exoplanet atmospheres
• Effect of composition variations
• Influence of the convection
6WP4: Laboratory experiments (ongoing work)
7WP4: Laboratory experiments (ongoing work)
Organic matter
• Analysis of cometary matter (CONCORDIA) and comparison with
Rosetta/COSIMA data
• Measurements at Soleil and at UMET Lille ⇒ N/C, C/Si and O/Si ratios
• Micrometeorites extraction from the 2016 Antarctic campaign
⇒ 3 new UCAMM candidates (2018)
7WP4: Laboratory experiments (ongoing work)
Organic matter
• Analysis of cometary matter (CONCORDIA) and comparison with
Rosetta/COSIMA data
• Measurements at Soleil and at UMET Lille ⇒ N/C, C/Si and O/Si ratios
• Micrometeorites extraction from the 2016 Antarctic campaign
⇒ 3 new UCAMM candidates (2018)
Evolution of chemistry in the ISM and Solar System
• Branching ratios & reaction rates (Cn Ny Hz ) with AGAT (ALTO/IPNO)
⇒ Kida database
• High- (GANIL, GSI, …) and low- (SIDONIE, ARAMIS) energy ion irradiation
7WP4: Laboratory experiments (ongoing work)
Organic matter
• Analysis of cometary matter (CONCORDIA) and comparison with
Rosetta/COSIMA data
• Measurements at Soleil and at UMET Lille ⇒ N/C, C/Si and O/Si ratios
• Micrometeorites extraction from the 2016 Antarctic campaign
⇒ 3 new UCAMM candidates (2018)
Evolution of chemistry in the ISM and Solar System
• Branching ratios & reaction rates (Cn Ny Hz ) with AGAT (ALTO/IPNO)
⇒ Kida database
• High- (GANIL, GSI, …) and low- (SIDONIE, ARAMIS) energy ion irradiation
Mineral matter
• Sample preparation (new microscope for micromanipulation)
• Multi-technique analysis of refractory inclusions from primitive meteorites
(micro-IR, TEM, nano-SIMS)
• IR hyperspectral imaging of meteorites and dust from sample return missions
7PhD students and post-doc
4 two year post-doc (2 in the initial project)
• E. Charron - Cometary matter (CSNSM, P2IO)
• R. Brauer - Disks (DAp/AIM & IAS, P2IO)
• G. Morello - Exoplanets (DAP/AIM, P2IO)
• R. Urso - Laboratory experiments (IAS1)
7 PhD (4 in the initial project, only 21/2 PhD founded by P2IO)
• T. Bouteraon - Disks (IAS, 1/2 P2IO - 1/2 Paris-Sud)
• M. Martin-Lagarde - Exoplanets (DAP/AIS, 1/2 CNES and 1/2 P7)
• T. Schirmer - PDRs (IAS, 1/2 CNES and 1/2 P2IO)
• R. Maupin - Silicate Matter (IAS)
• Z. Dionet - IR and X micro-tomography (IAS, IDEX Paris-Saclay)
• B. Guériin - Cometary matter/matter in disks (CSNSM/ISMO)
• J. Rojas - Analyses isotopiques UCAMMs, Irradiation
(CSNSM/ISMO)
8PhD students and post-doc
4 two year post-doc (2 in the initial project)
• E. Charron - Cometary matter (CSNSM, P2IO)
• R. Brauer - Disks (DAp/AIM & IAS, P2IO)
• G. Morello - Exoplanets (DAP/AIM, P2IO)
• R. Urso - Laboratory experiments (IAS1)
7 PhD (4 in the initial project, only 21/2 PhD founded by P2IO)
• T. Bouteraon - Disks (IAS, 1/2 P2IO - 1/2 Paris-Sud)
• M. Martin-Lagarde - Exoplanets (DAP/AIS, 1/2 CNES and 1/2 P7)
• T. Schirmer - PDRs (IAS, 1/2 CNES and 1/2 P2IO)
• R. Maupin - Silicate Matter (IAS)
• Z. Dionet - IR and X micro-tomography (IAS, IDEX Paris-Saclay)
• B. Guériin - Cometary matter/matter in disks (CSNSM/ISMO)
• J. Rojas - Analyses isotopiques UCAMMs, Irradiation
(CSNSM/ISMO)
8Observations of protoplanetary disks
9Observations of protoplanetary disks
Near-Infrared (λ = 1.65 µm) (Sub-)mm (λ = 1.3 mm)
∼ 100 AU ∼ 240 AU
SAO 206462 (Credit: NAOJ/Subaru) HL Tau (Credit: ESO/ALMA)
(with coronograph)
9Observations of protoplanetary disks
Near-Infrared (λ = 1.65 µm) (Sub-)mm (λ = 1.3 mm)
∼ 100 AU ∼ 240 AU
SAO 206462 (Credit: NAOJ/Subaru) HL Tau (Credit: ESO/ALMA)
(with coronograph)
9Observations of protoplanetary disks
Near-Infrared (λ = 1.65 µm) (Sub-)mm (λ = 1.3 mm)
?
JWST
∼ 100 AU ∼ 240 AU
SAO 206462 (Credit: NAOJ/Subaru) HL Tau (Credit: ESO/ALMA)
(with coronograph)
9Radiative transfer simulations of protoplanetary disks
• Derive constraints from existing observations
• Provide predictions for observations
10Radiative transfer simulations of protoplanetary disks
• Derive constraints from existing observations
• Provide predictions for observations
disk structure
and star(s)
POLArized RadIation Simulator
Dust model (Reissl et al. 2016, Brauer et al. 2017)
For disks ⇒ (Brauer et al. in prep.)
Spectral cube
λ
MIRI simulator
Synthetic observation
10THEMIS
The Heterogeneous dust Evolution Model
for Interstellar Solids
11THEMIS
The Heterogeneous dust Evolution Model
for Interstellar Solids
core/mantle grains (CM)
increasing AV, nH, NH diffuse ISM
a-C a-C a-C
a-SilFe a-SilFe
pyroxene-
olivine-
a-C:H photo-processing
type
type
core/mantle/mantle grains (CMM)
a-C/a-C:H a-C/a-C:H
a-SilFe a-SilFe a-C:H
a-C:H accretion
a-C/a-C:H
coagulation & ice mantle accretion
aggregated core/mantle a-C:H a-SilFe
grains (AMM)
a-C:H a-SilFe
a-SilFe a-SilFe
aggregated core/mantle/ice
a-SilFe a-SilFe grains (AMMI)
dense ISM
Overview of the THEMIS model (Jones et al. 2017)
11THEMIS
The Heterogeneous dust Evolution Model
for Interstellar Solids
aromatic
r = 0.4 nm
r = 0.7 nm
r = 1.0 nm
aliphatic
Optical properties of carbonaceous grains depending on size and structure
(derived from laboratory data)
11Radiative transfer simulations of protoplanetary disks
• Provide predictions for observations
• Derive constraints from existing observations
disk structure
and star(s)
POLArized RadIation Simulator
Dust model (Reissl et al. 2016, Brauer et al. 2017)
For disks ⇒ (Brauer et al. in prep.)
Lab. data Spectral cube
λ
MIRI simulator
Synthetic observation
12Radiative transfer simulations of protoplanetary disks
• Provide predictions for observations
• Derive constraints from existing observations
disk structure
and star(s)
Dust temperature distribution
Dust model Thermal dust emission
Scattered stellar emission
Lab. data Spectral cube
λ
MIRI simulator
Synthetic observation
12Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
13Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
Near-Infrared (λ = 1.65 µm) CO 2-1 line at 1.3 mm Continuum around 1.3 mm
(Yang et al. 2017) (Dutrey et al. 2014)
13Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
Near-Infrared (λ = 1.65 µm) CO 2-1 line at 1.3 mm Continuum around 1.3 mm
(Yang et al. 2017) (Dutrey et al. 2014)
Planet?
13Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
Near-Infrared (λ = 1.65 µm) CO 2-1 line at 1.3 mm Continuum around 1.3 mm
?
JWST
(Yang et al. 2017) (Dutrey et al. 2014)
Planet?
13Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
Dust density as a cut through the midplane
13Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
300
0.010
200 0.008
0.006
100
0.004
FI [Jy/as2 ]
∆y [au]
0
0.002
−100
−200
−300 0.000
−200 0 200
∆x [au]
Dust density as a cut through the midplane Simulated emission (λ = 7.7 µm)
13Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
Near-Infrared (λ = 1.65 µm) CO 2-1 line at 1.3 mm Continuum around 1.3 mm
?
JWST
(Yang et al. 2017) (Dutrey et al. 2014)
13Planet formation in disks around multiple stars
• Multiple star systems are very frequent
• GG Tau A: Unique system with a large disk around
at least 2 stars
Infrared (λ = 7.7 µm)
Near-Infrared (λ = 1.65 µm) 3
0.014 CO 2-1 line at 1.3 mm Continuum around 1.3 mm
0.012
0.010
2 0.008
0.006
1 0.004
FI [Jy/as2 ]
∆y [′′]
0 0.002
−1
−2
−3
0.000
−2 0 2
(Yang et al. 2017) (Dutrey et al. 2014)
∆x [′′]
Synthetic observation
(MIRI simulator)
13Ongoing work and perspectives
Extraterrestrial JWST data
JWST proposals
material / analogues (from 2021)
Laboratory
Pre-JWST data Data processing
experiments
Simulation of exoplan-
Laboratory data Data analysis
etary atmospheres
Simulations of
Dust modelling Radiative transfer codes
JWST observations
WP2 WP3 WP4 Geometry and chemical JWST simulated
structure of PDRs & disks data processing
14Ongoing work and perspectives
Ongoing studies:
Extraterrestrial dust band spectroscopy JWST data
origin of disk structures JWST proposals
material / analogues (from 2021)
other evolutionary states
Laboratory
Pre-JWST data Data processing
experiments
Simulation of exoplan-
Laboratory data Data analysis
etary atmospheres
Simulations of
Dust modelling Radiative transfer codes
JWST observations
WP2 WP3 WP4 Geometry and chemical JWST simulated
structure of PDRs & disks data processing
14Ongoing work and perspectives
Ongoing studies:
Extraterrestrial dust band spectroscopy JWST data
origin of disk structures JWST proposals
material / analogues (from 2021)
other evolutionary states
Continue JWST proposal
Laboratory (to be submitted in 2020)
Pre-JWST data Data processing
experiments Additional JWST proposals
MATISSE/VLTI proposals
Simulation of exoplan-
Laboratory data Data analysis
etary atmospheres
Simulations of
Dust modelling Radiative transfer codes
JWST observations
WP2 WP3 WP4 Geometry and chemical JWST simulated
structure of PDRs & disks data processing
14Ongoing work and perspectives
Ongoing studies:
Extraterrestrial dust band spectroscopy JWST data
origin of disk structures JWST proposals
material / analogues (from 2021)
other evolutionary states
Continue JWST proposal
Laboratory (to be submitted in 2020)
Pre-JWST data Data processing
experiments Additional JWST proposals
MATISSE/VLTI proposals
Simulation of exoplan-
Laboratory data Data analysis
etary atmospheres
Simulations of
Dust modelling Radiative transfer codes
JWST observations
WP2 WP3 WP4 Geometry and chemical JWST simulated
structure of PDRs & disks data processing
Future perspectives:
Continue to work on star and planet formation
Combine gained expertise/knowledge with new topics
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