from dust to galaxies: testing the evolution of the stellar IMF

Transcription

1 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

2 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

3 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

4 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

5 Dust in high redshift QSOs dust emission has been detected in 10 QSO at z 6 (Wang et al 2008, 2010), among which SDSS J 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)

6 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)

7 redshift evolution in dust properties? SN dust extinction curve observed in the quasar SDSS at z=6.2 Maiolino et al. 2004

8 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?

9 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

10 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 [ ] M sun

11 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

12 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

13 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

14 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

15 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

16 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 ) Pop III Pop II 100 M sun 0.1 M sun 0.01 M sun 0 - Z cr (f dep ) Log (Z/Z sun ) RS+2003, 2004, Omukai+ 2005, RS & Omukai 2010, RS+2011

17 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

18 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

19 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 = frag Energy transfer rate between gas and dust > Compressional heating rate cr total grain cross section per unit dust mass

20 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

21 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 M sun 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

22 GAlaxyMErgerTree&Evolution Valiante, RS, Salvadori & Bianchi (2011) GAMETE interpret SDSS J1148 observed properties averaging over different merger trees and exploring different SF histories

23 GAlaxyMErgerTree&Evolution Valiante, RS, Salvadori & Bianchi (2011) GAMETE Chemical evolution with dust

24 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

25 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 )

26 chemical evolution of the QSO host Valiante, RS, Salvadori & Bianchi (2011) GAMETE 1.15 x M sun M star (<25kpc) 9.4 x 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

27 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

28 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

29 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