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Lyman α — The Great Escape. DFS Annual Meeting 2009. Supervisors: Anja C. Andersen & Jesper Sommer-Larsen. Dark Cosmology Centre | Niels Bohr Institutet | Københavns Universitet. www.dark-cosmology.dk /~pela. very.

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dark-cosmology.dk /~pela

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  1. Lyman α — The Great Escape DFS Annual Meeting 2009 Supervisors: Anja C. Andersen & Jesper Sommer-Larsen Dark Cosmology Centre| Niels Bohr Institutet | Københavns Universitet www.dark-cosmology.dk/~pela

  2. very Ly is a powerful probe of the early Universe Ly escape from high-z galaxies Why? What? How?

  3. Ly escape from high-z galaxies Why? What? How? very Ly is a powerful probe of the early Universe

  4. Gas density and temperature • Dust density and cross-section Ly escape from high-z galaxies • Analytical attempt (Neufeld 1990)

  5. Ly escape from high-z galaxies • – Why does Ly escape after all? • Multiphase medium? Neufeld (1991); Hansen & Oh (2006) • Outflow? Kunth et al. (1999); Verhamme et al. (2006); Östlin et al. (2008) • Ionized holes? Tenori-Tagle et al. (1999); Mas-Hesse et al. (2003); Kunth et al. (2003); Hayes et al. (2007)

  6. Numerical approach • Cosmological N-body + hydro simulation • + LyRT on AMR grid with dust

  7. Dust Four important quantities: • Density:nd • Cross-section:d() • Albedo: A • Phase function:P()

  8. Dust Four important quantities: • Density:nd • Cross-section:d() • Albedo: A • Phase function:P()

  9. Dust Four important quantities: • Density:nd • Cross-section:d() • Albedo: A • Phase function:P() Pei (1991) + Weingartner & Draine (2001) + Gnedin et al. (2008)

  10. Dust Four important quantities: • Density:nd • Cross-section:d() • Albedo: A • Phase function:P() Calzetti et al. (1995); Lillie et al. (1976); Li & Draine (2001)

  11. Monte Carlo • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe

  12. Monte Carlo • Emit photon • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe

  13. Monte Carlo • Emit photon • Propagate thru ISM • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe

  14. Monte Carlo • Emit photon • Propagate thru ISM • Interact with • gas or dust • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe

  15. Monte Carlo • Emit photon • Propagate thru ISM • Interact with • gas or dust • New and ñ • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe

  16. Monte Carlo • Emit photon • Propagate thru ISM • Interact with • gas or dust • New and ñ • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe • Scatter/absorb

  17. Monte Carlo • Emit photon • Propagate thru ISM • Interact with • gas or dust • New and ñ • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe • New ñ • Scatter/absorb

  18. Monte Carlo • Emit photon • Propagate thru ISM • Interact with • gas or dust • New and ñ • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe • ✞ • New ñ • Scatter/absorb

  19. Monte Carlo • Emit photon • Propagate thru ISM • Interact with • gas or dust • New and ñ • In each cell: • LLy, T, vbulk, nHI, nHII, ZC,N,O,Mg,Si,S,Ca,Fe • ✞ • New ñ • Scatter/absorb • Escape

  20. Results Surface brightness map

  21. Results Surface brightness profile

  22. Results Surface brightness profile: dust helps to make profile look more extended

  23. Results Spectrum

  24. Results fesc(Mvir)

  25. IGM transmission z = 3.6 z = 5.7 z = 6.3 Songaila (2004)

  26. IGM transmission

  27. IGM transmission z = 3.6 z = 5.7 z = 6.3

  28. Summary • Many factors help facilitating the escape of Ly • Spectrum affected in a highly non-grey fashion • fesc decreases with increasing Mvir • Dust makes SB profile even more extended • Problem can be inversed: Predict results of future observations (e.g. Ultra-VISTA) • You cannot escape the raptor

  29. Summary • Many factors help facilitating the escape of Ly • Spectrum affected in a highly non-grey fashion • fesc decreases with increasing Mvir • Dust makes SB profile even more extended • Problem can be inversed: Predict results of future observations (e.g. Ultra-VISTA) • You cannot escape the raptor

  30. Summary • Many factors help facilitating the escape of Ly • Spectrum affected in a highly non-grey fashion • fesc decreases with increasing Mvir • Dust makes SB profile even more extended • Problem can be inversed: Predict results of future observations (e.g. Ultra-VISTA) • You cannot escape the raptor

  31. Summary • Many factors help facilitating the escape of Ly • Spectrum affected in a highly non-grey fashion • fesc decreases with increasing Mvir • Dust makes SB profile even more extended • Problem can be inversed: Predict results of future observations (e.g. Ultra-VISTA) • You cannot escape the raptor

  32. Summary • Many factors help facilitating the escape of Ly • Spectrum affected in a highly non- grey fashion • fesc decreases with increasing Mvir • Dust makes SB profile even more extended • Problem can be inversed: Predict results of future observations (e.g. Ultra-VISTA) • You cannot escape the raptor

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