Survey
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Ly Scattering in Young Galaxies Galaxy Formation and Evolution etc., etc., UCI, Irvine, 2008 www.dark-cosmology.dk/~pela DARK Cosmology Centre Universitet | Niels Bohr Institutet | Københavns Motivation Surface brightness map Surface brightness profile Fynbo et al. (2003) 2 Lyman Cooling radiation (~10%) Stellar sources (~90%) Metagalactic field (~1%) Young galaxies should be visible (Partridge & Peebles, 1967) 3 Analytical models Osterbrock (1962) Harrington (1973) Neufeld (1990) 4 Analytical models Dijkstra (2006) 5 Reality 6 Numerical models 7 Cosmological simulations Razoumov & Sommer-Larsen (2006) Sommer-Larsen et al. (2003) Sommer-Larsen (2006) 8 Monte Carlo L,T,nHI ,vbulk ,Z 9 Monte Carlo Emit photon 10 Monte Carlo Emit photon Determine t 11 Monte Carlo Emit photon Determine t Determine uatom 12 Monte Carlo Emit photon Determine t Determine uatom Determine ^ n Escape! 13 Spectra 14 Surface brightness maps 15 Surface brightness profiles 16 Surface brightness profiles 17 Galaxies. Multifarious. Like birds. Damped Ly absorbers, DLAs Ly emitters, LAEs Lyman-break galaxies, LBGs Sub-mm galaxies, SMGs Distant red galaxies, DRGs 18 Building the bridge Evolutionary sequence? DLA LAE LBG DRG SMG? Selection effects? LBGs/DLAs probe two diff. ends of hi-z LF Viewing angle? 19 Dust and IGM absorption AGBs: e.g., Draine (2003) SNe: e.g., Sugerman et al. (2006) QSOs: e.g., Elvis, Marengo, & Karovska (2002) 20 Inhomogeneous medium 21 Adaptive Mesh Refinement 22 Adaptive Mesh Refinement 23 Adaptive Mesh Refinement 24 Properties of dust n: Metals condense to dust , P(,): 25 Properties of dust n: Metals condense to dust , P(,): In principle easy: 26 Properties of dust n: Metals condense to dust , P(,): In principle easy: 27 Properties of dust n: Metals condense to dust , P(,): In principle easy: 28 Properties of dust Laboratory experiments 29 Properties of dust Laboratory experiments 30 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 31