Modeling z ~ 3 Lyα spectra to gain insight into high redshift Lyα emitters

Details Modeling z ~ 3 Lyα spectra to gain insight into high redshift Lyα emitters Modeling z ~ 3 Lyα spectra to gain insight into high redshift Lyα emitters

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...7e..27v&link_type=abstract

The Universe at z > 6, 26th meeting of the IAU, Joint Discussion 7, 17-18 August 2006, Prague, Czech Republic, JD07, #27

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We have developed a 3D Monte Carlo Lyα radiation transfer code to understand the diversity of Lyα line profiles observed in star forming galaxies and related objects (Verhamme et al. 2006, A&A, submitted). Our code allows for prescribed arbitrary hydrogen density, ionisation, temperature structures, and dust distribution, and arbitrary velocity fields and UV photon sources. We will present the modelling of Lyα spectra of a sample of z ~ 3 Lyman break galaxies observed by Steidel and collaborators (Pettini et al., 2002, Shapley et al., 2005) and taken from the FORS Deep Field (Tapken et al., 2006) with our code. A simple model of an expanding neutral shell surrounding a starburst region can reproduce the whole variety of spectra ranging from double-peaked profiles to asymetric emission lines, P-Cygni profiles or broad absorption. The main determining parameters are the outflow velocity and the dust content. Other parameters such as the hydrogen column density, the intrinsic Lyα emission and hence SFR, and the intrinsic Lyα line widths can be determined consistently taking all radiation transfer effects into account. We will also discuss the origin of several observed correlations between Lyα, interstellar lines, and other observables in Lyman break galaxies. This study has also implications on the interpretation of very high-z galaxies and Lyα emitters.

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