Cosmological Simulation with
Dust Evolution
Kuan-Chou Hou (ASIAA/NTU)
Shohei Aoyama, Hiroyuki Hirashita (ASIAA),
Ikko Shimizu, Kentaro Nagamine (Osaka Univ.)
EAYAM in Ishigaki, Japen
15/11/2017

Importance of Dust•

Obscure the starlight (optical—UV) & Re-emit IR•

Shape the SED

Hubblesite’s News Releases on Galaxies(ESA/HERSCHEL/PACS & SPIRE CONSORTIUM, O. KRAUSE, HSC, H.

•Cosmic infrared background••

ALMA starts to resolve the faint IR sources

history of obscured SFR

H. Dole et al., IAS

Fujimoto+ 2016

Motivation•

The nature of the faint IR galaxies•

Evolution of dust in galaxies•The relation between dust and other galaxy properties statistically

Implement all relevant processes driving dust
evolution in cosmological simulation

Dust model + Simulation•

Smoothed Particle Hydrodynamic simulation ➝ GADGET 3•

Springel 2005, modified•

ΛCDM; Star formation & Stellar feedback•

503 (Mpc/h)3; 2 × 5123 particles•

Dust and metal production are treated consistently with star formation•ISM processes: SN destruction, accretion, shattering and coagulation•Grain size distribution is represented by small and large grains (divided at∼0.03 µm; Hou+ 2017)

Dust processes
AGBSN

Stellar production
WindDust (solid)
Metal (gas)Astration
Gas Collapse

Dust processes
Coagulation
Shattering

Low V

DustMetal

High VAccretion
SN destruction
Shock wave

Gas and Dust distribution
Dust50 Mpc/hGas

Gas and Dust distribution at z = 0
Dust

50 Mpc/hGas

Dust Mass Function
z=0•

Agree with observations at
Md ≲108 M⦿.

•Excess in the high mass
end -> A lack of AGN
feedback•

Observation data (Vlahakis+2005, Dunne+ 2011,Clemens+ 2013 and Clark+2015)

Dust and Metal relation•

Condensation efficiency is 0.1
in stellar yield•

Low metallicity galaxies follow
the stellar dust production•

Most of metal condense into
dust in high metallicity
galaxies•

Consistent with observation of
nearby galaxies(Remy-Ruyer+ 2014)

z=0

D=ZStellar dustproduction

Dust and Metal relation•

Condensation efficiency is 0.1
in stellar yield•

Low metallicity galaxies follow
the stellar dust production•

Most of metal condense into
dust in high metallicity
galaxies•Consistent with observation ofnearby galaxies(Remy-Ruyer+ 2014)z=0

Redshift evolution•

Dust Mass Function up toz~5•

Galaxy number density
increases from z ~ 5 to 2;
decreases from z ~ 1 to 0•

Astration and grain growthby accretion cause a bump.

•Galaxies have the mostabundant dust at z ~ 2 - 1

Redshift evolution
Stellar mass function

Dust mass function

Redshift evolution•

Dust Mass Function up toz~5•

Galaxy number density
increases from z ~ 5 to 2;
decreases from z ~ 1 to 0•

Astration and grain growthby accretion cause a bump.

•Galaxies have the mostabundant dust at z ~ 2 - 1

Redshift evolution•Dust and Metal relation•Balance between SF andaccretion•Stronger SN destruction
at higher redshift•Accretion turning point
shift to higher metallicity

Redshift evolution
Mdust/Mstar — Z

DSmall/DLarge — Z

Summary•

Perform the cosmological simulation with the dust enrichment model•

Solving time evolution of dust formation and destruction together with gas
dynamics.

•Predicted dust abundances in galaxies up to z ~ 5•

Produced the dust mass function•Reproduced the nonlinearity of the Dust-to-gas mass ratio and Metallicity relation•Predicted the redshift evolution of the relation between dust and galaxy
quantities, e.g., Z, M鯱Ϟto be tested by future observations

Thank youDust abundances in the i-th particle from t to t + ∆t :!

"D(t)
D(t)
L,XS,XSNe′ ∆Mreturn
DL,X (t + ∆t) = DL,X (t) − ∆DL,X −−∆t + f in,X YX(1 − δ)τSh
τcomg

SNeDS,X (t + ∆t) = DS,X (t) − ∆DS,X +!

"DL,X (t) DS,X (t) DS,X (t)−+∆tτShτcoτacc

•Softening length : 5 kpc•Minimum gas smoothing is 0.1 softening length•

Star formation efficiency : 0.05

12 K. C. Houet al.
Extinction
curvesAdapt silicate-graphite dust species model