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
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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
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Model-3
dzz
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sdust
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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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