dust in the early universe and the contribution of agb stars · 2014-09-01 · dust in the early...
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Dust in the early universe and the contribution of AGB stars
Raffaella Schneider INAF/Osservatorio Astronomico di Roma
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Matteo de Bennassuti (INAF/OAR)
Luca Graziani (INAF/OAR)
Stefania Marassi (INAF/OAR)
Rosa Valiante (INAF/OAR)
In collaboration with: Marcella di Criscienzo (INAF/OAR) Flavia dell’Agli (INAF/OAR) Paolo Ventura (INAF/OAR) Corinne Rossi (La Sapienza) Marco Limongi (INAF/OAR) Alessandro Chieffi (INAF/OAR)
Simone Bianchi (INAF/OAA) Gen Ciaki (Tokyo University) Simona Gallerani (SNS) Takaya Nozawa (IPMU) Kazuyuki Omukai (Tohoku University) Stefania Salvadori (Kapteyn) Naoki Yoshida (Tokyo University)
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dust in the early Universe thermal emission from cold dust has been observed in the rest-frame FIR spectral energy distribution of z > 5 QSOs
24, 199, 169, 259 �m Herschel maps of J1148 @ z = 6.4
Leipski+13,14
dust continuum observations with ALMA @ 250 GHz
J2310 @ z = 6 J1319 @ z = 6.1 J2054 @ z = 6.03
Wang+13
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dust in the early Universe the estimated dust masses are 108 Msun < Mdust < 109 Msun
how are these huge dust masses formed in less than 1 Gyr?
what are the implications for the evolution of the host galaxy?
(Valiante et al. 2009, 2011, 2014; Gall et al. 2010, 2011;
Dwek & Cherchneff 2011; Mattsson 2011; Pipino et al 2011; Calura et al. 2013)
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why do the first galaxies care about dust?
metals and dust increase gas cooling: ! affect star formation efficiency ! allow the formation of the first low-mass stars
RS+2003, 2004; Omukai+ 2005;, RS & Omukai 2010; RS+2011,2012;
Chiaki+13,14
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stellar sources of dust: SNe observations of SNe and SN remnants show signatures of the
presence of dust associated with the ejecta
Schneider+14
Gall+11, Gomez+12, Dunne+09, Barlow+10, Matsuura+11, Otsuka+10
Crab
CasA
1987A
N49 Bianchi & RS 07 no reverse shock
Bianchi & RS 07 with reverse shock
Todini & Ferrara 01; RS+03, Nozawa+03;Bianchi & RS 07; Cherchneff & Dwek 10; Sarangi & Cherchneff 13; Marassi+14
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stellar sources of dust: AGB
Ferrarotti & Gail 01; 02; 06; Zhukovska+08; Nanni+13; Ventura+12a,b; Di Criscienzo+13; Dell’Agli+14; Ventura+14
their role in the early Universe depends on the mass- and metallicity- dependence of the dust yields
• numerical integration of stellar models (ATON code, Ventura+98)
• stationary spherically symmetric wind
• grain growth (olivine, pyroxene, quartz, iron, corundum, silicon carbide, carbon)
Grid of AGB/SAGB stars with 1 Msun ≤ M ≤ 8 Msun and 3x10-4 ≤ Z ≤ 0.008
- Third Dredge Up: surface C enrichment - Hot Bottom Burning: C (and O) surface depletion
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dust yields from AGB stars: stellar mass dependence
transition from carbon dust to silicate production at M ~ 3 Msun
Ventura+12a
Ventura+12a Ferrarotti & Gail 06
Ferrarotti & Gail 06
Z = 0.001
HBB HBB
TDU
TDU
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dust yields from AGB stars: metallicity dependence
Ventura+12b; Di Criscienzo+13
softer HBB higher Si abundance
" Silicates are produced by > 3 Msun stars
" Silicate dust production increases with Z
" No silicates are produced when Z < 0.001
" Carbon dust is produced by < 3 Msun stars and does not depend on Z
" When Z < 10-4 HBB is present even at M < 2 Msun ! no AGB dust
LMC
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dust yields from AGB stars: modelling uncertainties
treatment of mass loss and of convective borders Ventura+13
SMC LMC
Black models: Wachter+08 mass loss; over-shoot (extra-mixing)
extra-mixing
mass loss
Blue models: Blöcker 95 mass loss; no over-shoot (no extra-mixing)
Red models: Blöcker 95 mass loss; over-shoot (extra-mixing)
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AGB dust production rates in the Magellanic Clouds
Observed DPRs inferred by different studies
O-AGB include O-rich and anomalous O-rich AGB stars C-AGB include C-rich and extreme AGB stars
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AGB dust production rates in the Magellanic Clouds
Theoretical DPRs can be computed as:
stellar IMF dust yield star formation history metal enrichment
Zhukovska & Henning 13 RS+14
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AGB dust production rates in the Magellanic Clouds
metallicity – dependent star formation histories (Harris & Zaritsky 2004, 2009)
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AGB dust production rates in the Magellanic Clouds
RS+14
age – metallicity relation
Harris & Zaritsky 09
Carrera+08 Piatti 12
Carrera+08 Piatti & Geisler 13
Harris & Zaritsky 04
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AGB dust production rates in the Magellanic Clouds
Small Magellanic Cloud Large Magellanic Cloud
Blöcker 95 mass loss Wachter+ 08 mass loss Ferrarotti & Gail 06 models (FG)
Blöcker 95 mass loss
Wachter+ 08 mass loss
RS+14
silicate production at Z ≤ 0.004
FG Z =0.008
silicate production at Z ≤ 0.008
Matsuura+ 09,13
Boyer+ 12
Srinivasan+ 09
Riebel+12
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AGB dust production rates in the Magellanic Clouds
Small Magellanic Cloud Large Magellanic Cloud
Blöcker 95 mass loss
Wachter+ 08 mass loss
RS+14
silicate production at Z ≤ 0.004
FG Z =0.008
silicate production at Z ≤ 0.008
" observed DPRs in C-AGBs in the LMC require efficient mass loss (Wachter+ 08)
" observed DPRs in C-AGBs in the SMC require less efficient mass loss (Blöcker 95)
" observed DPRs in O-AGBs in the SMC require silicate dust production at Z ≤ 0.004 as predicted by models with efficient HBB in stars > 3 Msun
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Total dust budget in the Magellanic Clouds
Skibba+12 Gordon+14
Skibba+12 Gordon+14
AGB
AGB+SN AGB
AGB+SN
the existing dust mass can have a stellar origin (if no destruction in the ISM occurs) AGB stars make ~ 15% of the total dust budget in the SMC and ~ 70% in the LMC
RS+14
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the contribution of AGB stars to early dust enrichment
300 Myr 300 Myr 300 Myr
2%
15% 20% 25% 35%
70%
all stars are formed in a single burst at t = 0 with a Salpeter IMF: AGB dust yields from ATON code (Ventura+12,13) SN yields from Bianchi & Schneider (2007)
with ATON yields, AGB contribution to the total dust budget becomes > 30% only when the Z > 0.004 and
becomes dominant in 500 Myr
when Z ≤ 0.004 AGB dust is always sub-dominant wrt to SN dust
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the contribution of AGB stars to early dust enrichment
300 Myr 300 Myr 300 Myr
silicate
silicate silicate
carbon carbon
carbon
2%
15% 20% 25% 35%
70%
all stars are formed in a single burst at t = 0 with a Salpeter IMF: AGB dust yields from ATON code (Ventura+12,13) SN yields from Bianchi & Schneider (2007)
If SN at low Z produce mostly silicate dust, we expect to see only silicate features in young (< 300 Myr) starbursts and the
presence of carbon features may be an indication of the growing AGB contribution to the total dust mass at > 300 Myr
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are stellar sources enough to produce ~ 108 Msun of dust in < 1 Gyr?
Valiante et al. 2009, 2011, 2014; Gall et al. 2010, 2011; Dwek & Cherchneff 2011; Mattsson 2011; Pipino et al 2011; Calura et al. 2013
Mdust do not correlate with Mstar Mdust do correlate with MH2
stellar dust is not enough to reproduce the observed Mdust
the observed Mdust require super-solar metallicities and very efficient
grain growth in dense gas
Matsuoka+ 09,11
Valiante et al. 2014
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Conclusions
" dust enrichment can be fast, t < 1 Gyr " the presence of dust in the first galaxies triggers the formation of the first low-mass stars at Z < 10-4 Zsun " relative role of SN and AGB stars depends on mass- and Z-dependent AGB yields (in addition to SFH, IMF….) " new AGB dust yields suggest that the contribution of AGB stars can dominate the dust budget at t ~ 300 – 500 Myr when Z > 0.004 " at Z ≤ 0.004 the contribution of AGB stars to dust enrichment depends on the mass loss in the C-star stage #! observations of DPRs in the SMC! " existing dust masses in the SMC, LMC can have a stellar origin but in high-z QSO host galaxies grain growth in the ISM is required