Lyman α – impact of the intergalactic medium

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Outline of the lectures

Lecture 6 Summary and Perspectives

ELLIPTICALS AND HIGH-REDSHIFT UNIVERSE: Discussion

Atomic Physics of Lyman Alpha And Intergalactic Medium

Cosmology With The Lyα Forest

Martin Haehnelt, Matteo Viel, Volker Springel

X-Rays -> see you at COSPAR in July; also Kawai’s talk this conf.

On the implications for the Lya line of an inhomogeneous, dusty medium

Observing galaxies at z = 8.8

Dust. LyGalaxies Nyborg, 2008

Probing Reionization with Lyman Alpha Emitters Pratika Dayal

– or: debunking the Neufeld scenario

Intergalactic transmission and its impact on the Lyman a line

Ly Scattering in Young Galaxies

STRUCTURE FORMATION MATTEO VIEL INAF and INFN Trieste

Modeling Lyα emission from high-z galaxies

Dust in Young Galaxies Peter Laursen Supervisor: Anja C. Andersen

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Presentation transcript:

Lyman α – impact of the intergalactic medium DARS get-together, Ebeltoft, 2010 Dark Cosmology Centre | Niels Bohr Institutet | Københavns Universitet www.dark-cosmology.dk/~pela

Lyman a • Put constraints on the epoch of reionization • Crucial for determing redshifts in the hi-z Universe • Map the Cosmic Web • Explore young galaxies and a multitude of of their properties, e.g • Kinematics and dynamics • Star formation rates • Morphology • Stellar population • Outflows • Gas accretion • Maybe even more I can’t think of right now...

Observed Ly profiles Tapken et al. (2008)

Modeling Ly profiles Verhamme et al. (2008) Various scenarios has been invoked: The fact that Lyα line profiles are often seen to exhibit a P Cygni-like profile has led to the suggestion that high-velocity outflows of gas are needed to enable escape (Kunth et al. 1998; Östlin et al. 2008; Atek et al. 2008). However, at high redshifts many galaxies are still accreting matter, which should result in an increased blue peak. Since this is rarely observed, the shape could be caused by other mechanisms, e.g. IGM absorption. Verhamme et al. (2008)

Numerical approach Cosmological N-body + hydro simulation + galactic Ly RT with dust + IGM RT + hi-res resimulations of interesting regions + ionizing UV RT on AMR grid According to the analytical solution of a homogeneous medium, f_esc should be ~10e-5

IGM transmission

IGM transmission

Ly forest

Gunn-Peterson trough

Homogeneous universe

Retarded Hubble flow

Retarded Hubble flow

Transmission as a function of redshift z = 3.6 z = 5.7 z = 6.3

Impact on the Lya profile

Probing the Epoch of Reionization

Probing the Epoch of Reionization Songaila (2004)

Probing the Epoch of Reionization WMAP: zre = 11.0 ± 1.4 Thomson scattering optical depth:

Probing the Epoch of Reionization

Summary • Retarded Hubble flow may explain at least some of the asymmetric Ly profiles zre,WMAP and zre,QSO could be reconciled through more realistic treatment of the ionization history •