Supernovae as sources of dustin the early universe
Takaya Nozawa(IPMU, University of Tokyo)
Thanks to:T. Kozasa (Hokkaido Univ.), N. Tominaga (Konan Univ.)
K. Maeda, K. Nomoto, M. Tanaka (IPMU, Univ. of Tokyo)
H. Umeda (Univ. of Tokyo), H. Hirashita (ASIAA)
A. Habe, D. Yamasawa (Hokkaido Univ.)
2011/05/23

1-1. Discovery of massive dust at high redshift
There has been clear evidence for the presence of a large
amount of dust (>108 Msun) in QSOs host galaxies at z > 5
SDSS J1148+5251 at z=6.4

What is the origin of massive dust?
・ Supernovae (Type II SNe)
➔ ~0.1-1 Msun per SN is needed(Morgan & Edmunds’03; Dwek+’07)

・ AGB stars + SNe(Valiante+’09; Dwek & Cherchneff’11)
LIR = 10^13 Lsun

➔ 0.01-0.05 Msun per AGB stars
・ Grain growth in ISM + AGB stars + SNe

Leipski+’10, A&A, 518, L34(Draine’09; Michalowski+’10; Pipino+’11)

1-2. Extinction curves at high-z quasars
Maiolino+’04, Nature, 431, 533
SDSS J1048+4637 at z=6.2High-z extinction curves do notmatch those in the MW and SMC➔ properties of dust at high z may
be different from those at low z

Gallerani+’10, A&A, 523, 85

3.9 < z < 6.4

1-3. Dust formation in primordial SNe
・ Theoretical studies of dust formation in the SN ejecta(e.g. Nozawa+’03; Todini & Ferrara’01; Cherchneff & Dwek’10)－ Mdust=0.1-1 Msun in Type II-P SNe (SNe II-P)－ Mdust=1-60 Msun in pair-instability SNe (PISNe)
dust amount needed to explain massive dust at high-z

He coreFSRSCD2-1. Mass and size of dust ejected from SN II-P
PISNe
SNe II-P

total dust mass surviving thedestruction in Type II-P SNRs;
0.07-0.8 Msun (nH,0 = 0.1-1 cm-3)

size distribution of dust after
RS destruction is domimatedby large grains (> 0.01 μm)

Nozawa+’07, ApJ, 666, 955
at time of dust formation

after destruction of dust
by reverse shock

MW dust model

2-2. Flattened extinction curves at high-z
Hirashita, TN,+’08, MNRAS, 384, 1725

Gallerani+’10, A&A, 523, 85

Dust extinction curves in the early
universe are expected to be flatLi+’08, ApJ, 678, 1136

2-3. Effect of dust on star formation history
efficient formation of H2 molecules on the surface(e.g., Cozaux & Spaans’04)➔ promoting formation of stars (Hirashita & Ferrara’02)

SN dust w/o RS destruction

SN dust with RS destruction

Yamasawa, …, TN,+’11, accepted (arXiv/1104.0728)

Larger size of dust suppresses the formation rate of H2
and thus does not activate star formation significantly

3-1. Dust formation in Type IIb SN○ SN IIb model (SN1993J-like model)－ Meje = 2.94 Msun
MZAMS = 18 Msun
MH-env = 0.08 Msun
－ E51 = 1.0－ M(56Ni) = 0.07 Msun

3-2. Dependence of dust radii on SN typeSN IIb

SN II-P

0.01 μm－ condensation time of dust
300-700 d after explosion－ the radius of dust formedin H-stripped SNe is small－ total mass of dust formed
・ 0.167 Msun in SN IIb
・ 0.1-1 Msun in SN II-P・ SN IIb without massive
H-env ➔ adust < 0.01 μm

Nozawa+’10, ApJ, 713, 356

・ SN II-P with massive
H-env ➔ adust > 0.01 μm

3-3. Destruction of dust in Type IIb SNR
homogeneous CSM (ρ = const)

stellar-wind CSM (ρ ∝ r-2)
330 yrnH,1 = 30, 120, 200 /cc ➔ dM/dt = 2.0, 8.0, 13x10-5 Msun/yr for vw=10 km/s

Almost all newly formed grains are destroyed in shockedgas within the SNR for CSM gas density of nH > 0.1 /cc➔ small radius of newly formed dust
➔ early arrival of reverse shock at dust-forming region
Nozawa+’10, ApJ, 713, 356

3-4. IR emission from dust in Cas A SNR
Nozawa+’10, ApJ, 713, 356

・ total mass of dust formed
Mdust = 0.167 Msun・ shocked dust : 0.095 Msun
Md,warm = 0.008 Msun
・ unshocked dust :Md,cool = 0.072 Msun
with Tdust ~ 40 K

AKARI corrected 90 μm image

AKARI observation
Md,cool = 0.03-0.06 Msun
Tdust = 33-41 K(Sibthorpe+10)

Herschel observation
Md,cool = 0.075 Msun
Tdust ~ 35 K (Barlow+10)

4-1. Dust formation in Type Ia SNe○ Type Ia SN modelW7 model (C-deflagration) (Nomoto+’84; Thielemann+’86)－ Meje = 1.38 Msun

－ E51 = 1.3－ M(56Ni) = 0.6 Msun

4-2. Dust formation and evolution in SNe Ia
average radius

Nozawa+’11, accepted (arXiv/1105.0973)

dust destruction in SNRs
0.01 μm

・ condensation time :100-300 days
・ average radius of dust :aave <~ 0.01 μm
・ total dust mass :Mdust = 0.1-0.2 Msun

newly formed grains arecompletely destroyed for
ISM density of nH > 0.1 cm-3
➔ SNe Ia are unlikely to be
major sources of dust

5-1. Implication on evolution history of dust
〇 metal-poor (high-z or starbust) galaxies
・ massive stars (SNe) are likely to dominate
・ mass loss of massive stars would be less efficient➔ Type II-P SNe might be major sources of dust
necessary for serving the seeds for grain growth in the ISM－ dust mass per SN II-P after the RS destruction
Mdust = 0.1-0.8 Msun for nH,0 = 0.1-1 cm-3
－ average radius of dust is quite large (> 0.01 μm)
・ grain growth in the ISM makes grain size larger➔ dust extinction curve in the early universe might begray (wavelength-independent) if SNe II-P (and graingrowth) are main sources of dust at high redshift5-2. Implication on evolution history of dust
〇 metal-rich (low-z or Milky Way) galaxies
・ low-mass stars are dominate
・ mass loss of massive stars would be more efficient➔ SNe (IIb, Ib/c, Ia) might be minor sources of dustbut, our model treating formation and evolution of dust
self-consistently can reproduce IR emission from Cas A
Dust size distribution at t=5 Myr (nH=1 /cc)

－ dust is almost completely destroyed in the SNRs
since size of newly formed dust is small (< 0.01 μm)
・ How are small dust grains produced?
－ size of dust from AGB stars is unknown－ shattering due to grain-grain collisions
Hirashita, TN, +’10, MNRAS, 404, 1437