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

Raffaella Schneider INAF/Osservatorio Astronomico di Roma

First Galaxies Ringberg, 26 June ‐ 1 July 2011 

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).

Bertoldi et al (2003)

MAMBO-2 (1.2 mm) SCUBA (450 & 850 µm)

Robson et al. (2004)

SHARC II (350 µm)

Beelen et al. (2006)

Estimating the mass of dust

1.86 x 108 Msun < Mdust < 4.78 x 108 Msun

 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

Different dust production mechanism at z > 4? Different dust processing into the ISM?

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

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

silicates

SiC+Fe

Dust produced by AGB & SAGB stars: physical models+nucleation theory

Di Criscienzo et al. in prep

md ≈ [10-3 – 10-2] Msun

supernovae as stardust sources Tanaka et al. (2011)

Courtesy of Takaya Nozawa

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

Bianchi & Schneider 2007 

dust mass in young SN: [10-3 – 1] Msun

20% survives

7%

dust mass SN remnants: < 0.1 Msun

2%

supernovae as stardust sources Tanaka et al. (2011)

Courtesy of Takaya Nozawa

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

f dep

= M

dust

/(M

met

+Mdu

st)

1

0.8

0.6

0.4

0.2

0

-6 -4 -2 0 -∞ Log (Z/Zsun)

Zcr(fdep)

High mass Low mass

100 Msun

0.1 Msun

0.01 Msun

critical metallicity scenario dust grains and metals drive a transition in mass scales of prestellar gas clouds

Pop III

Pop II

RS+2003, 2004, Omukai+ 2005, RS & Omukai 2010, RS+2011

exploring different fdep= Mdust/(Mdust+Mmet)

RS, Omukai, Bianchi, Valiante in prep

norev fdep = 20%

rev1 4%

rev2 1.5%

rev3 0.5%

norev fdep = 85%

rev1 26%

rev2 10%

rev3 3.4%

thermal evolution with different fdep

RS, Omukai, Bianchi, Valiante in prep

primordial rev3 rev2 rev1 norev

f dep

Z = 10-7 Zsun Z = 10-6 Zsun Z = 10-5 Zsun

Total metallicity

low mass star formation: critical metallicity or %dust-to-gas ratio?

20 Msun Z = 0

35 Msun Z = 10-4Zsun

20 Msun Z = 10-4 Zsun

CCSN Schneider+06

PISN Schneider+06 Local ISM Omukai+05

Dcr = 4.4 10-9

no frag frag

Energy transfer rate between gas and dust > Compressional heating rate

RS, Omukai, Bianchi, Valiante in prep

total grain cross section per unit dust mass

cr  

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 GAMETE Salvadori, RS, Ferrara (2007)

with BH evolution/feedback and dust formation/processing in the ISM Valiante, RS, Salvadori & Bianchi (2011)

•  50 merger histories of a 1013 Msun 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 GAMETE Valiante, RS, Salvadori & Bianchi (2011)

interpret SDSS J1148 observed properties averaging over different merger trees and exploring different SF histories

GAlaxyMErgerTree&Evolution GAMETE Valiante, RS, Salvadori & Bianchi (2011)

Chemical evolution

with dust

GAMETE 

Valiante, RS, Salvadori & Bianchi (2011)

chemical evolution of the QSO host

“Low stellar mass models”

low-f* models with standard IMF (mch = 0.35 Msun) the mass of metals (MZ) and dust (Md)

gas 

stars metals 

dust 

GAMETE Valiante, RS, Salvadori & Bianchi (2011)

chemical evolution of the QSO host

gas 

stars metals 

dust 

intermediate- and high-f* models with standard IMF (mch = 0.35 Msun) the mass of metals (MZ) and dust (Md)

GAMETE Valiante, RS, Salvadori & Bianchi (2011)

chemical evolution of the QSO host

chemical properties of the host galaxy seem to require a Mstar that would shift the BH closer/onto the local Mbh-Mstar correlation

1.15 x 1011 Msun ≤ Mstar (<25kpc) ≤ 9.4 x 1011 Msun

GAMETE Valiante, RS, Salvadori & Bianchi (2011)

chemical evolution of the QSO host

gas 

stars metals 

dust 

low-f* models with top-heavy IMF (mch = 5 Msun) the mass of metals (MZ) and dust (Md)

GAMETE Valiante, RS, Salvadori & Bianchi (2011)

evolution of dust components

dust growth in MCs is required

stardust (AGB, SN) only can not reproduce the observed dust mass

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: low-mass star formation requires a minimum dust-to-gas ratio,

•  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 (mch = 5 Msun) or the stellar mass is a factor 3 – 10 larger than inferred by observations, shifting J1148 onto

the local Mbh-Mstar relation

cr