Transcript Document

Ly Scattering in Young Galaxies
Galaxy Formation and Evolution etc., etc.,
UCI, Irvine, 2008
www.dark-cosmology.dk/~pela
DARK Cosmology Centre
Universitet
| Niels Bohr Institutet | Københavns
Motivation
Surface brightness map
Surface brightness profile
Fynbo et al. (2003)
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Lyman 
Cooling radiation (~10%)
Stellar sources (~90%)
Metagalactic field (~1%)

Young galaxies should be
visible (Partridge & Peebles, 1967)
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Analytical models
Osterbrock (1962)
Harrington (1973)
Neufeld (1990)
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Analytical models
Dijkstra (2006)
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Reality
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Numerical models
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Cosmological simulations
Razoumov & Sommer-Larsen (2006)
Sommer-Larsen et al. (2003)
Sommer-Larsen (2006)
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Monte Carlo
L,T,nHI ,vbulk ,Z
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Monte Carlo
Emit photon
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Monte Carlo
Emit photon

Determine t
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Monte Carlo
Emit photon

Determine t

Determine uatom
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Monte Carlo
Emit photon

Determine t

Determine uatom

Determine ^
n
Escape!
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Spectra
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Surface brightness maps
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Surface brightness profiles
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Surface brightness profiles
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Galaxies. Multifarious. Like birds.
Damped Ly absorbers, DLAs
Ly emitters, LAEs
Lyman-break galaxies, LBGs
Sub-mm galaxies, SMGs
Distant red galaxies, DRGs
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Building the bridge
Evolutionary sequence?
DLA  LAE  LBG  DRG  SMG?
Selection effects?
LBGs/DLAs probe two diff. ends of hi-z LF
Viewing angle?
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Dust and IGM absorption
AGBs: e.g., Draine (2003)
SNe:
e.g., Sugerman et al. (2006)
QSOs: e.g., Elvis, Marengo, & Karovska (2002)
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Inhomogeneous medium
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Adaptive Mesh Refinement
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Adaptive Mesh Refinement
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Adaptive Mesh Refinement
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Properties of dust
n: Metals condense to dust
, P(,):
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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:
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Properties of dust
n: Metals condense to dust
, P(,): In principle easy:
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Properties of dust
Laboratory experiments
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Properties of dust
Laboratory experiments
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Summary
•Ly scattering responsible for extended halo
•Ly line profile may reveal gas kinematics
•Line is broadened ~1000 km s-1
•Anisotropic escape of radiation may explain
differences in observed properties, and may even
link different types of galaxies
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