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Dust in Young Galaxies
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Ebeltoft, 2008
www.dark-cosmology.dk/~pela
DARK Cosmology Centre
Universitet
| Niels Bohr Institutet | Københavns
How to find them?
Damped Ly absorbers, DLAs
Ly emitters, LAEs
Lyman-break galaxies, LBGs
Sub-mm galaxies, SMGs
Distant red galaxies, DRGs
2
Building the bridge
Evolutionary sequence?
DLA  LAE  LBG  DRG  SMG?
Selection effects?
LBGs/DLAs probe two diff. ends of hi-z LF
Viewing angle?
3
Monte Carlo
Emit photon

Determine t

Determine uatom

Determine ^
n
Escape!
4
Radiative transfer
5
Non-isotropic <ESC>
6
How about dust?
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Inhomogeneous medium
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Adaptive Mesh Refinement
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Adaptive Mesh Refinement
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Metals
He, C, N, O, Ca, Si, S, Fe at different ionization levels
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Properties of dust
n: Metals condense to dust
, P(,): In principle easy:
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Properties of dust
n: Metals condense to dust
, P(,): In principle easy:
13
Properties of dust
n: Metals condense to dust
, P(,): In principle easy:
14
Properties of dust
n: Metals condense to dust
, P(,): In principle easy:
15
Properties of dust
n: Metals condense to dust
, P(,): In principle easy:
16
Properties of dust
Laboratory experiments
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Properties of dust
Laboratory experiments
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