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DUST AT HIGH REDSHIFT

Why do we care?

BAL are the most reddened

sub-class of QSOs R

ed

den

ing!

SMC-like extinction curve!

as for noBAL QSOs at 0<z<2.2!

Reichard et al. 2003; Richards et al. 2003; Hopkins et al. 2004!

dusty wind

EXTINCTION CURVE AT z<4 FROM QSO SPECTRA

Bluer than any BAL at low z (Maiolino et al.04)

EXTINCTION CURVE AT z~6 FROM QSO SPECTRA

A SAMPLE of 33 OPTICAL/NIR SPECTRA OF QSOs AT 4<z<6.4

5.2

)62.1(3000

103000

!"

!!

! AA

templCFF#

#

$%

&'(

)=

F!templ

template by Reichard et al. 2003, having !=-1.62

A3000 absolute extinction at 3000 Å

A! extinction curve normalized at 3000 Å

(Data from Juarez et al. 2009; Jiang et al. 2007; Willott et al. 2009; Mortlock et al. 2008)

GRID OF EXTINCTION CURVES

!

A"

mix= (1# p)A"

SMC+ pA"

SN

170 M!

nH=1cm-3

Todini & Ferrara 01 Bianchi & Schneider 07

Hirashita et al. 08

20 M!

Hirashita et al. 08

SNe type dust

SNe type dust

Pair instability SNe type

dust

Empirical extinction curves

from the local Universe

!

0 " p "1

DUST REDDENING IN 4<z<6.4 QSOs

Extinction curves

at 4<z<6.4

Extinction curve

at 0<z<4

Gallerani et al. (2010)

!"#$%&&$'()$#)**)+)*$,-%.%#$"/$"-#$.%01&)$$

'()$2).'$3'$)45+65"+$6-#7)$8.$+"'$'()$9:;$

THE EXTINCTION LAW AT HIGH REDSHIFT

Evidence for different dust properties in the early Universe (chemical composition? grain size distribution? dust sources?...)

Gallerani et al. (2010)

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CONCLUSIONS

•! Dust extinction in quasars at z<4 is described through

the SMC extinction curve.

•! We infer a mean extinction curve (MEC) from 4<z<6.4

quasar spectra finding that it deviates from the SMC one.

•! Evidence for different dust properties in the early Universe,

(dust sources? chemical composition? grain size?…)

Gallerani et al. (2010)