First Galaxies Ringberg, 26 June 1 July 2011 from dust to galaxies: testing the evolution of the stellar IMF Raffaella Schneider INAF/Osservatorio Astronomico di Roma
http://www.arcetri.astro.it/david Simone Bianchi INAF/OAArcetri BenedeEa Ciardi MPA PraIka Dayal SISSA Carmelo Evoli SISSA Andrea Ferrara SNS Simona Gallerani INAF/OARoma Fabio Iocco IAP Francisco Shu Kitaura MPA Antonella Maselli INAF/OAArcetri Stefania Salvadori Kapteyn InsItute Ruben Salvaterra Univ. Milano Bicocca Raffaella Schneider INAF/OARoma Sunghye Baek SNS Marcos Valdes IPMU Tokyo Rosa Valiante Univ. Firenze Livia Vallini Univ. Pisa
OUTLINE observations of dust at high-z stellar sources of dust: SN and AGB stars implications for the IMF at very low-metallicities test the stellar IMF in QSOs host galaxies
OUTLINE observations of dust at high-z stellar sources of dust: SN and AGB stars implications for the IMF at very low-metallicities test the stellar IMF in QSOs host galaxies
Dust in high redshift QSOs dust emission has been detected in 10 QSO at z 6 (Wang et al 2008, 2010), among which SDSS J1148+5251 at z=6.43 (Bertoldi et al. 2003). MAMBO-2 (1.2 mm) SCUBA (450 & 850 µm) SHARC II (350 µm) Bertoldi et al (2003) Robson et al. (2004) Beelen et al. (2006)
Estimating the mass of dust 1.86 x 10 8 M sun < M dust < 4.78 x 10 8 M sun a = Bertoldi et al. (2003) b = Robson et al. (2004) c = Beelen et al. (2006) d = Weingartner & Draine (2001) SMC e = SN dust Bianchi & Schneider (2007)
redshift evolution in dust properties? SN dust extinction curve observed in the quasar SDSS1048+46 at z=6.2 Maiolino et al. 2004
Mean Extinction Curve (MEC) of QSOs at z > 4 Gallerani et al 2010 BAL nobal The MEC for BAL deviates from the SMC at a confidence level 95% The MEC for nobal is intermediate between the BAL MEC and the SMC Different dust production mechanism at z > 4? Different dust processing into the ISM?
OUTLINE observations of dust at high-z stellar sources of dust: SN and AGB stars implications for the IMF at very low-metallicities test the stellar IMF in QSOs host galaxies
dust yields from AGB/SAGB stars Dust produced by AGB stars: synthetic AGB models+nucleation theory Ferrarotti & Gail (2006); Zhukovska et al. (2008) graphite SiC+Fe silicates Dust produced by AGB & SAGB stars: physical models+nucleation theory Di Criscienzo et al. in prep m d [10-3 10-2 ] M sun
supernovae as stardust sources Courtesy of Takaya Nozawa Tanaka et al. (2011) Young Supernovae Supernova Remnants Young Supernovae: Ercolano+07, Wooden+93,Dwek+92,Pozzo+04,Elmhamdi+03,Meikle+07, Szalai+10,Kotak +09,Mattila+08,Sakon+09 Supernova Remnant: Rho+08,Sibthorpe+10,Barlow+10,Nozawa+ 0,Morton+07,Green+04,Temim+06,Rho +09,Sandstrom+09,Williams+08,Temim+10
what theory predicts Kozasa & Hasegawa 1987; Todini & Ferrara 2001; Nozawa et al 2003 Schneider, Ferrara & Salvaterra 2004; Bianchi & Schneider 2007; Chercheneff & Dwek 2010 dust mass in young SN: [10-3 1] M sun dust mass SN remnants: < 0.1 M sun 20% survives 7% 2% Bianchi & Schneider 2007
supernovae as stardust sources Courtesy of Takaya Nozawa Tanaka et al. (2011) what theory predicts what theory predicts Young Supernovae: Ercolano+07, Wooden+93,Dwek+92,Pozzo+04,Elmhamdi+03,Meikle+07, Szalai+10,Kotak +09,Mattila+08,Sakon+09 Supernova Remnant: Rho+08,Sibthorpe+10,Barlow+10,Nozawa+ 0,Morton+07,Green+04,Temim+06,Rho +09,Sandstrom+09,Williams+08,Temim+10
the cosmic dust yield Valiante, Schneider, Bianchi, Andersen 2009 continuous SFR burst-like SFR AGB stars dominate dust-production in a timescale which ranges 150 Myr 500 Myr
OUTLINE observations of dust at high-z stellar sources of dust: SN and AGB stars implications for the IMF at very low-metallicities test the stellar IMF in QSOs host galaxies
critical metallicity scenario dust grains and metals drive a transition in mass scales of prestellar gas clouds 1 High mass Low mass f dep = M dust /(M met +M dust ) 0.8 0.6 0.4 0.2 Pop III Pop II 100 M sun 0.1 M sun 0.01 M sun 0 - Z cr (f dep ) -6-4 -2 0 Log (Z/Z sun ) RS+2003, 2004, Omukai+ 2005, RS & Omukai 2010, RS+2011
exploring different f dep = M dust /(M dust +M met ) norev f dep = 20% rev1 4% rev2 1.5% rev3 0.5% norev f dep = 85% rev1 26% rev2 10% rev3 3.4% RS, Omukai, Bianchi, Valiante in prep
thermal evolution with different f dep Z = 10-7 Z sun Z = 10-6 Z sun Z = 10-5 Z sun primordial rev3 rev2 rev1 norev f dep Total metallicity RS, Omukai, Bianchi, Valiante in prep
low mass star formation: critical metallicity or % dust-to-gas ratio? RS, Omukai, Bianchi, Valiante in prep 20 M sun Z = 0 35 M sun Z = 10-4 Z sun 20 M sun Z = 10-4 Z sun CCSN Schneider+06 PISN Schneider+06 Local ISM Omukai+05 no frag D cr = 4.4 10-9 frag Energy transfer rate between gas and dust > Compressional heating rate cr total grain cross section per unit dust mass
OUTLINE observations of dust at high-z stellar sources of dust: SN and AGB stars implications for the IMF at very low-metallicities test the stellar IMF in QSOs host galaxies
GAlaxyMErgerTree&Evolution Salvadori, RS, Ferrara (2007) GAMETE with BH evolution/feedback and dust formation/processing in the ISM Valiante, RS, Salvadori & Bianchi (2011) 50 merger histories of a 10 13 M sun halo @ z =6.4 star formation in quiescent and/or merger-driven bursts BH growth via gas accretion and mergers BH feedback chemical enrichment (metals and dust) on the stellar characteristic timescales
GAlaxyMErgerTree&Evolution Valiante, RS, Salvadori & Bianchi (2011) GAMETE interpret SDSS J1148 observed properties averaging over different merger trees and exploring different SF histories
GAlaxyMErgerTree&Evolution Valiante, RS, Salvadori & Bianchi (2011) GAMETE Chemical evolution with dust
chemical evolution of the QSO host Valiante, RS, Salvadori & Bianchi (2011) GAMETE gas Low stellar mass models metals stars dust low-f * models with standard IMF (m ch = 0.35 M sun ) of metals (M Z ) and dust (M d ) the mass
chemical evolution of the QSO host Valiante, RS, Salvadori & Bianchi (2011) GAMETE gas metals stars dust intermediate- and high-f * models with standard IMF (m ch = 0.35 M sun ) the mass of metals (M Z ) and dust (M d )
chemical evolution of the QSO host Valiante, RS, Salvadori & Bianchi (2011) GAMETE 1.15 x 10 11 M sun M star (<25kpc) 9.4 x 10 11 M sun chemical properties of the host galaxy seem to require a M star that would shift the BH closer/onto the local M bh -M star correlation
chemical evolution of the QSO host Valiante, RS, Salvadori & Bianchi (2011) GAMETE gas stars metals dust low-f * models with top-heavy IMF (m ch = 5 M sun ) metals (M Z ) and dust (M d ) the mass of
evolution of dust components Valiante, RS, Salvadori & Bianchi (2011) GAMETE stardust (AGB, SN) only can not reproduce the observed dust mass dust growth in MCs is required
Summary Observations of distant QSOs indicate rapid dust enrichment at z > 6 AGB stars and SN contribute to dust production at high redshift: evolution in dust properties Dust grains appear to dominate the thermal evolution of low-metallicity gas clouds: lowmass star formation requires a minimum dust-to-gas ratio, cr The chemical properties (dust & metal masses) of QSOs host galaxies allow to constrain the star formation history and stellar IMF at z > 6 Observed properties of J1148 at z = 6.4 are reproduced if the IMF is top-heavy (m ch = 5 M sun ) or the stellar mass is a factor 3 10 larger than inferred by observations, shifting J1148 onto the local M bh -M star relation