1. www.dark-cosmology.dk/~pela IAP Ly  workshop 2007, Paris Dust in Young Galaxies DARK Cosmology Centre | Niels Bohr Institutet | Københavns Universitet

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

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

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

5. 5 Analytical models Dijkstra (2006)

6. 6 Reality

7. 7 Numerical models

8. 8 Cosmological simulations Sommer-Larsen et al. (2003) Sommer-Larsen (2006) The movie

9. 9 Monte Carlo L,T,n HI,v bulk,Z

10. 10 Emit photon Monte Carlo

11. 11  Emit photon Determine  Monte Carlo

12. 12  Emit photon Determine u atom Determine   Monte Carlo

13. 13  Emit photon ^ Determine n Determine u atom Determine    Escape! Monte Carlo

14. 14 Radiative transfer

15. 15 Observations

16. 16 Surface brightness maps

17. 17 Surface brightness profiles

18. 18 Spectra

19. 19 Significance of the velocity field

20. 20 Fitting a Neufeld profile

21. 21 Dust AGBs: e.g., Draine (2003) QSOs: e.g., Elvis, Marengo, & Karovska (2002) SNe: e.g., Sugerman et al. (2006)

22. 22 Adaptive Mesh Refinement

23. 23 Adaptive Mesh Refinement

24. 24 Metals He, C, N, O, Ca, Si, S, Fe at different ionization levels

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

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

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

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

29. 29 n:n: , P( ,  ): Properties of dust In principle easy: Metals condense to dust

30. 30 Properties of dust Laboratory experiments

31. 31 Properties of dust Laboratory experiments