Can we build a complete set of tools ? RT Can we build a complete - - PowerPoint PPT Presentation

Can we build a complete set of tools ?

RT

Can we build a complete set of tools ?

RT SEDs Images

Interfero: nIR + mm (CASA)

Spectra, 
 Channel maps

→ PIONIER/Gravity, ALMA, SPHERE/GPI → Herschel, ALMA, JWST, SPICA

Can we build a complete set of tools ?

RT

Chemistry, gas thermal balance

SEDs Images

Interfero: nIR + mm (CASA)

Spectra, 
 Channel maps

→ PIONIER/Gravity, ALMA, SPHERE/GPI → Herschel, ALMA, JWST, SPICA

Can we build a complete set of tools ?

RT

Model fitting : grid of models, MCMC

Fostino

Chemistry, gas thermal balance

SEDs Images

Interfero: nIR + mm (CASA)

Spectra, 
 Channel maps

→ PIONIER/Gravity, ALMA, SPHERE/GPI → Herschel, ALMA, JWST, SPICA

Can we build a complete set of tools ?

RT

Hydro models, dust evolution


Model fitting : grid of models, MCMC

Fostino

Chemistry, gas thermal balance

SEDs Images

Interfero: nIR + mm (CASA)

Spectra, 
 Channel maps

→ PIONIER/Gravity, ALMA, SPHERE/GPI → Herschel, ALMA, JWST, SPICA

Can we build a complete set of tools ?

RT

Hydro models, dust evolution


Model fitting : grid of models, MCMC

Fostino

Chemistry, gas thermal balance

SEDs Images

Interfero: nIR + mm (CASA)

Spectra, 
 Channel maps

→ PIONIER/Gravity, ALMA, SPHERE/GPI → Herschel, ALMA, JWST, SPICA

Feedback ?

Can we build a complete set of tools ?

RT

Hydro models, dust evolution


Model fitting : grid of models, MCMC

Fostino

Chemistry, gas thermal balance

SEDs Images

Interfero: nIR + mm (CASA)

Spectra, 
 Channel maps

→ PIONIER/Gravity, ALMA, SPHERE/GPI → Herschel, ALMA, JWST, SPICA

Feedback ?

Inclined binary with a disc:
 1 million phantom SPH particules ➔ 1 million MCFOST Voronoi cells

Example of post-processing

Scattered light : 1.6μm Thermal emission : 1.3mm

mcfost <para_file> -phantom <dump>

Fargo model

Coupling hydro + chemistry + RT

+
 Astrochem

Live coupling hydro + RT

• mcfost is now available as a library (libmcfost.a)
• pass SPH particles (position, velocity, n(a))
• MCFOST performs

Voronoi tessellation + radiative transfer and returns Tdust + radiation pressure vectors without interpolation

• takes ~ few minutes for 106 particles :
• can be performed every few time steps yo get

full hydro+RT simulations

syntax specific to phantom (thanks Daniel) so far, 
 but trivial to extend to other code

MCFOST + phantom : 
 recovering hydrostatic equilibrium

MCFOST + phantom : 
 recovering hydrostatic equilibrium

Gas temperature

mcfost + ProDiMo (Woitke 2009) model

Gas heating & cooling

Chemical abundances

Estimating Tgas via Machine Learning

Also predicts election density (-> MHD), molecular abundances Prediction from 100 ProDiMo models training set

ALMA and SPHERE views of IM Lupi

1"

100 150 200 100 150 200

ALMA 1.3mm + 12CO
 0.3” 0.1km/s SPHERE H band DPI ~ 0.03”

Avenhaus et al, in prep. i = 50 deg

100au 1" IM Lup

Pinte et al, 2017

12CO (2-1)

1"

Upper surface Lower surface Upper surface Lower surface

dv=−1.28km/s dv=−0.96km/s dv=−0.64km/s dv=−0.32km/s dv=−0.00km/s dv=0.32km/s dv=0.64km/s dv=0.96km/s dv=1.28km/s

5 15 25 35 Tb [K]

13CO (2-1)

1"

Upper surface Lower surface Upper surface Lower surface

dv=−1.28km/s dv=−0.96km/s dv=−0.64km/s dv=−0.32km/s dv=−0.00km/s dv=0.32km/s dv=0.64km/s dv=0.96km/s dv=1.28km/s

5 10 15 20 Tb [K]

Upper surface Far side Upper surface Near side Lower surface Far side Lower surface Near side

vertical snow line T

• p of the CO layer
• bserved in 12CO

Bottom of the CO layer

• bserved in

12CO

Bottom of the CO layer observed in 13CO and C18O gas CO layer atomic and ionized layer

1"

dv=−1.28km/s dv=−0.96km/s dv=−0.64km/s dv=−0.32km/s dv=−0.00km/s dv=0.32km/s dv=0.64km/s dv=0.96km/s dv=1.28km/s

5 15 25 35 Tb [K]

Reconstructing the altitude, velocity and temperature of the CO emitting layers

Tex ≈ Tgas for 
 low J CO lines

δx yb − yc h sin i (xc, yc) (x , y ) F (x, yf) N (x, yn)

1"

Upper surface far side Upper surface near side Lower surface near side N F Position along vertical axis Flux

∆ v = 0.80 km/s

r = r (x − x?)2 + ✓yf − yc cos i ◆2 . The altitude h of the orbit

emis- as h = yc − y? sin i .

3 = (3obs − 3syst) r (x − x?) sin i.

Tb = Tex(1 − e−τ)

The CO layers

12CO 13CO

C18O

100 200 300 400 50 100 150

r [au] hCO [au]

Vertical velocity gradient & sub-Keplerian rotation

vKep(r,z=0) vKep(r,z) v(r,z), with dP/dr

100 200 300 400 1 2 3 4

r [au] v [km.s−1]

32 r = GM?r (r2 + h2)3/2 + 1 ⇢gas @P @r .

Mapping the vertical
 snow line

T = 21K Flux dilution Flux dilution

12CO upper surface 12CO lower surface 13CO upper surface

C18O upper surface

100 200 300 400 10 20 30

r [au] max(Tb) [K]

Upper surface Far side Upper surface Near side Lower surface Far side Lower surface Near side

vertical snow line T

• p of the CO layer
• bserved in 12CO

Bottom of the CO layer

• bserved in

12CO

Bottom of the CO layer observed in 13CO and C18O gas CO layer atomic and ionized layer

Comparison with models

100 200 300 400 500 0.1 0.2 0.3 0.4 0.5 5 10 15 20 25 30 35 40 45 50

r [au] h/r

T [K]

CO layers vs scattered light layer

IM Lup

12CO 13CO

C18O

100 200 300 400 50 100 150

r [au] hCO [au]

Avenhaus et al, in prep.

Concluding remarks

• New ALMA and adaptive optics observations

require advanced models coupling hydro + RT + chemistry

• Modern continuum RT codes can be coupled

efficiently with hydro codes

• Tgas, ionisation chemistry can be estimated via

Machine Learning trained on databases of thermo-chemical models