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}}
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