Dust Evolution in IllustrisTNG
Yu-Hsiu Huang (ASIAA/NTU)
H. Hirashita (ASIAA), Y.-H. Hsu (ASIAA/NTHU), Y.-T. Lin (ASIAA), D. Nelson (MPA), and A. P. Cooper (NTHU)
with
Why?
- Depletion of metals in ISM
- Catalyst of H2 formation
- Interaction with starlight
- heating and cooling in ISM
Dust affect galactic evolution and our understanding of galaxies
De Cia+ 2016
\delta_X = [X/H] - [X/H]_{\rm tot}
\delta_X
Metal depletion from gas phase
Grain catalyst dominates H2 formation
Chen+ 2018
Surface density of molecular gas with different grain size distribution
Large
Small
Andromeda in different wavelength
NOAO, Spitzer
absorption
thermal radiation
Y.-H. Ling with SKIRT
Effect of dust on a galaxy SED
What do we want to know?
grain size distribution
abundance
composition
Dust properties mainly depend on the following three things:
Dust Formation & Evolution
Five dust evolution processes
- stellar production
- sputtering in hot gas (e.g. SN shock)
- accretion from gas-phase metals
- shattering
- coagulation
Dust Formation & Evolution
gas
dust
Diffuse ISM
Dense ISM
Environment-depend dust evolution processes
Dust Formation & Evolution
Diffuse ISM
Dense ISM
Environment-depend dust evolution processes
Depend on stellar feedback
Motivation
Understand how grain size distributions (GSDs) evolve in galaxies
What do we want to know?
grain size distribution
abundance
composition
direct calculation
Dust properties mainly depend on the following three things:
cosmological simulation
Research Strategy
IllustrisTNG
dust model
MWA
Analysis
\rm M_\star
\rm SFR
\rm Z
\rm M_{gas}
Select MWA from TNG
206 galaxies
similar metallicity and SFR
Research Strategy
IllustrisTNG
dust model
MWA
Analysis
\rm M_\star
\rm SFR
\rm Z
\rm M_{gas}
Dust Model
- One-zone model to save computational cost
- Include gas accretion and galaxy mergers
time
Research Strategy
IllustrisTNG
dust model
MWA
Analysis
\rm M_\star
\rm SFR
\rm Z
\rm M_{gas}
Analysis
D_{\rm tot}=\displaystyle\int_{0}^{\infty}n(a)da
A_\lambda = 2.5\log_{10} e \sum\limits_i \displaystyle \int _0^\infty n_i(a) \pi a^2 Q_{\rm ext}^{(i)}(a,\lambda) da
-dependent extinction curve
dust abundance
Mie Theory
These two quantities are observables.
\lambda
- Dust – Metallicity Scaling Relation
- Evolution of grain size distributions
- Evolution of extinction curves
First Results on MWAs
Dust–Metallicity Scaling Relation
Rémy-Ruyer+ 2014
The DZ distribution predicted by model roughly covers the measurement from nearby galaxies
Evolution of Grain Size Distributions
GSD converges to certain shape at .
z\sim1
Evolution of Grain Size Distributions
GSD converges to certain shape at .
z\sim1
coagulation
shattering
depends on ratio of dense and diffuse ISM
Evolution of Extinction Curves
Pei 1992
We reproduce the bump feature and covers the MW extinction curve at .
1/\lambda \lesssim 6\,{\rm \mu m^{-1}}
Current Challenges
- Dust geometry is important in recovering galaxy SED.
- GSD should be different in different regions.
- CGM inflow/outflow and its effects on dust evolution
Dust Geometries
How dust distributes in galaxies with respect to stars?
Narayanan+ 2018
GSD in different regions
The dust evolution processes depend on environments.
Aoyama+ 2020
Summary
- We implement dust post-processing model on TNG and validate the DZ scaling relation.
- Our model broadly reproduce the MW extinction curve.
- Shattering and coagulation are important to fully recover the MW GSD.
Some graph
How?
Numerical
Simulations
Multiwavelength
Observations
Attenuation Curves
- model dust distribution
- do radiative transfer simulations and calculate galaxy SED
To work on geometric effect, we have to
Vogelsberger+ 2020
Dust Formation & Evolution
stellar production
(stellar wind or SNe ejecta)
Stellar production forms large grains ( )
\sim 0.1 {\rm \mu m}
Dust Formation & Evolution
sputtering
(hot gas destruction)
more intermediate-size grains
Remove metals from dust grains
Dust Formation & Evolution
accretion
(from gas-phase metals)
increase large grains
Accrete gas-phase metals onto small grains to form larger grains
Dust Formation & Evolution
shattering
(high-speed collision)
increase small
remove large
Fragment larger grains into smaller pieces
Dust Formation & Evolution
coagulation
(low-speed collision)
increase large
remove small
Small grains stick together to form larger grains
Evolution of Extinction Curves
We reproduce the bump feature and covers the MW extinction curve at .
1/\lambda \lesssim 6\,{\rm \mu m^{-1}}
Dust in Galaxies
By Yvonne Huang
