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

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Presentation transcript:

IAP Ly  workshop 2007, Paris Dust in Young Galaxies DARK Cosmology Centre | Niels Bohr Institutet | Københavns Universitet

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

3 Lyman  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 Cosmological simulations Sommer-Larsen et al. (2003) Sommer-Larsen (2006) The movie

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

10 Emit photon Monte Carlo

11  Emit photon Determine  Monte Carlo

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

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

14 Radiative transfer

15 Observations

16 Surface brightness maps

17 Surface brightness profiles

18 Spectra

19 Significance of the velocity field

20 Fitting a Neufeld profile

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

22 Adaptive Mesh Refinement

23 Adaptive Mesh Refinement

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

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

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

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

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

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

30 Properties of dust Laboratory experiments

31 Properties of dust Laboratory experiments