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Investigating the Escape of Lyα from High-Z Galaxies: Insights from Cosmological Simulations

This presentation at the DFS Annual Meeting 2009, led by Anja C. Andersen and Jesper Sommer-Larsen, explores the mechanisms behind Lyα escape in high-redshift galaxies, a critical aspect for understanding the early Universe. Employing analytical and numerical approaches, including Monte Carlo simulations, the study delves into factors such as gas and dust density, temperature, and ionized regions that facilitate Lyα escape. The findings indicate that environmental parameters significantly influence the luminosity profiles and the cosmic reionization process.

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Investigating the Escape of Lyα from High-Z Galaxies: Insights from Cosmological Simulations

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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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