Dust Formation in the Early (z>6) Universe

S. V. Marchenko

Western Kentucky University

General importance

~50% of the optical radiation emitted since the Big Bang by all sources in the universe has been ‘reprocessed’ by dust

cooling (e.g. [CII] 157.7 m) accretion star formation rates (massive, M> 30 M stars) IMF

assembly of H2 on dust grains is far more efficient than in the gas phase

dust in Lyman break galaxies at z~5 ? (Ando et al. 2004; Ouchi et al. 2004)

CMB distortions; far-IR (=0.4-1.0 mm: Elfgren & Desert 2004) background

SFR and dust

Star formation rates and dust attenuation: GALEX/UV (Schiminovich et al. 2005)

Dust z~0: gen. Info

Stars Dust (MW Galaxy: Gehrz 1989)

AGB (C, OH/IR, Miras)

RSG ~ 10-3 M/yr each

SNe

PNe ~ 10-4 M/yr each

Wolf-Rayet

Presently, WRs produce <1% of the dust galaxy-wide.

Molecular clouds: 1-5times the stellar rate

Dust z>>0 - 1

Stars Dust (z>>0) M(ini) Dust M mass/* (M ) composition size__________________________________________________________________

SNe(PopIII) 140-260 ? ? ?

SNe II 8 0.1-0.3, Z<<Z ? ? 3 , Z~Z Si, C, Fe(?) ‘standard’?, ~1m

LBVs 75-85 ? Z<<Z ? ? 30(?) 0.01-0.25, Z~Z Si, PAH, Al(??), ~1m + C ‘small’

WCd 60-70 ? Z<<Z ? ? 30 10-3 -10-2 , Z~Z

C(amorph.) ~1m+ ‘small’

Dust z>>0 - 2

Stars Dust (z>>0) M(ini) Dust M mass/* (M) composition size__________________________________________________________________ sgB[e] ? ? Z<<Z ? ? 30-60 ? Z~Z Si ~1m

B[e]WD 5(?) ? ? ?

RSG 8-50 ? Z<<Z ? ? 8-25 10-4 -10-3, Z~Z Si ~0.5m+ ‘standard’ AGB 1-(5-6) Mini(Z/Z), Z<<Z ? ? (OH/IR) 1-6 ~10-3 Mini

, Z~Z Si, C, ice ‘stand.’(?)

SN - facts

Dust in core-collapse SNe

Evidence:

- isotopic abundance ratios of grains in meteorites (excess of

13C, 15N, 18O, etc. - Travaglio et al. 1999)

- near-mid-IR (~1-2 yrs after explosion), sub-mm excesses

- blueshifted emission lines

HOW MUCH DUST ??

Theory: up to ~1M/expl. (Todini & Ferrara 2001)

Observations:

~10-3-10-2 M (mid-IR: Dwek 1993; Pozzo et al. 2004)

~1-2 M [sub-mm: Dunne 2003, Morgan 2003]

Primordial (WR, LBV, RSG) dust? – SN2002hh [Barlow et al.2005],

SN 2002ic (Kotak et al., 2005)

SN – 1987A

Preexisting dust?

Light echoes in SN1987A: HST/WFPC2, F656N (Sugerman et al. 2005)

LBVs

LBVs: preexisting dust (RSG/BSG)?

AG Car: 12.5 μm (Voors et al. 2000)

η Car: L band, Chesneau et al. 2005

η Car: Smith et al. 2002

RSG

RSGs: in situ dust

VY CMa (M5e Ia): Smith et al., 2001

WR104, pinwheel

_______________________

150 mas

April-June1998,

Keck, H-K interferometry:

Tuthill et al. (1999)

WR104: WC9d+B0.5V(+VB), P = 220 d

WR48a, Gem

WR48a: WC8ed+?

March 2004, Gemini-South/TReCS, 12.3 m

WR112, animation

Gemini, 12.5 m:

2001 vs. 2004

P ~ 12 y, D ~ kpc7.18.00.2

WR 112 (WC9d+OB?)

WR112, july 2004

July 2004, Gemini-South/TReCS; 12.3 m

WR112, model

WR112, dust survival

… at least 20% of the initially formed dust survives the first ~100 years of

expansion in a shocked environment… (Marchenko et al. 2002)

Z-depend. For WRs

Meynet & Maeder (2005)

Does dust production depends on Z?

Binaries? – some [limited] help?

Model-1

MODEL: modified from Loeb & Haiman (1997)

- dust absorption coefficient - dust opacity - for SMC (Cartledge et al. 2005) - for MWG (Mathis 1990)- dust density

i - different categories of dust-producers: SN, massive stars, AGB

- mass fraction of the deposited dust or 10 z 20 z 10

)(),(),( ZZzZz dust

)(Z

),()()1(),( ,,3 ZffzFzZz idustidepi

icbdust 30107.9 c,044.0b

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dmm

dmm

fZM

ZM

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M

M

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5.0x 35.1x

Model-2

- mass fraction of dust (efficiency of dust formation): - Z-dependent for massive stars (Vink et al. 2001), AGBs (van Loon 2000, C-rich class]

- efficiency of star formation (BH, NS, WD)

- from Drory et al. (2005)

- mass fraction of collapsed barions

- standard CDM cosmology (Haiman & Loeb 1997)

- evolutionary timescales 1, for z zcr,i

0, for z > zcr,i

zdzfT

tt

zd

dFzzF star

z

zzcolii

)()exp()()(20

)(, Zf idust

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Model-3

dzz

Zz

H

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szz

sdust

32/5

)1(

0 )1(

),(),,(

SMCvsMWG

Chemistry: SMC vs. MWG

Z-depend.

Dust outp.: SN

Dust output from SNII; theory: Todini & Ferrara 2001

Dust yields

Left – pessimistic:SNII – 1/10 theory,Massive st. - )(ZfM dust

Right – optimistic (realistic?):SNII – 1/30 theory,Massive st. - )(ZfM dust

Conclusions

Conclusions:

Dominance of SNII at z>3 …IF dust can form in SN

ejecta…

~10 overestimated theoretical for SNII

(cf. SN 2002hh: Barlow et al. 2005)

Fairly short dust-survival times, T 0.4 Gyr, in line

with Jones et al. (1994)

dustM

Things to do

Things to do:

Dust formation and dust survival in the SN ejecta

(SEEDS collaboration, PI M.J. Barlow)

Dust formation/survival in the winds of massive stars

Dust formation (efficiency) and dust chemistry at Z~0

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