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dark-cosmology.dk /~pela

Ly  Scattering in Young Galaxies. Galaxy Formation and Evolution etc., etc., UCI, Irvine, 2008. DARK Cosmology Centre | Niels Bohr Institutet | Københavns Universitet. www.dark-cosmology.dk /~pela. Motivation. Surface brightness map. Surface brightness profile. Fynbo et al. (2003).

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dark-cosmology.dk /~pela

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  1. Ly Scattering in Young Galaxies Galaxy Formation and Evolution etc., etc., UCI, Irvine, 2008 DARK Cosmology Centre| Niels Bohr Institutet | Københavns Universitet www.dark-cosmology.dk/~pela

  2. Motivation • Surface brightness map • Surface brightness profile • Fynbo et al. (2003)

  3. Lyman a • Cooling radiation (~10%) • Stellar sources (~90%) • Metagalactic field (~1%) •  • Young galaxies should be • visible (Partridge & Peebles, 1967)

  4. Analytical models • Osterbrock (1962) • Harrington (1973) • Neufeld (1990)

  5. Analytical models • Dijkstra (2006)

  6. Reality

  7. Numerical models

  8. Razoumov & Sommer-Larsen (2006) Cosmological simulations • Sommer-Larsen et al. (2003) • Sommer-Larsen (2006)

  9. Monte Carlo • L,T,nHI ,vbulk ,Z

  10. Monte Carlo • Emit photon

  11. Monte Carlo • Emit photon •  • Determine t

  12. Monte Carlo • Emit photon •  • Determine t •  • Determine uatom

  13. Determinen • ^ • Escape! Monte Carlo • Emit photon •  • Determine t •  • Determine uatom • 

  14. Spectra

  15. Surface brightness maps

  16. Surface brightness profiles

  17. Surface brightness profiles

  18. Damped Ly absorbers, DLAs Ly emitters, LAEs Lyman-break galaxies, LBGs Sub-mm galaxies, SMGs Distant red galaxies, DRGs Galaxies. Multifarious. Like birds.

  19. Selection effects? LBGs/DLAs probe two diff. ends of hi-z LF Viewing angle? Building the bridge Evolutionary sequence? DLA  LAE  LBG  DRG  SMG?

  20. Dust and IGM absorption AGBs: e.g., Draine (2003) SNe: e.g., Sugerman et al. (2006) QSOs: e.g., Elvis, Marengo, & Karovska (2002)

  21. Inhomogeneous medium

  22. Adaptive Mesh Refinement

  23. Adaptive Mesh Refinement

  24. Adaptive Mesh Refinement

  25. Metals condense to dust Properties of dust n: , P(,):

  26. In principle easy: Properties of dust n: Metals condense to dust , P(,):

  27. In principle easy: Properties of dust n: Metals condense to dust , P(,):

  28. In principle easy: Properties of dust n: Metals condense to dust , P(,):

  29. Properties of dust • Laboratory experiments

  30. Properties of dust • Laboratory experiments

  31. 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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