On The Origin of Lyman-alpha Absorption in Nearby Starbursts and
  Implications for Other Galaxies
  (Abridged) Despite the privileged position that Lyman-alpha (Lya) emission
line holds in the exploration of the distant universe and modern observational
cosmology, the origin of the observed diversity of lya profiles remains to be
thoroughly explained. Observations of nearby star forming galaxies bring their
batch of apparent contradictions between Lya emission and their physical
parameters, and call for a detailed understanding of the physical processes at
work. IZw 18, one of the most metal-poor galaxies known is of particular
interest in this context.
  We use a 3D Lya radiation transfer code to model Hubble Space Telescope (HST)
observations of IZw 18 and to fit its Lya spectrum. Different geometrical
configurations of the source and the neutral gas are explored.
  The integrated Lya profile of NW region of IZw 18 is reproduced using the
observed small amount of dust (E(B-V) ~ 0.05) and a spherical HI shell with
N(HI) = 6.5 x 10^(21) cm^(-2). Such a high column density makes it possible to
transform a strong Lya emission (EW(Lya) = 60 A) into a damped absorption even
with a small extinction. When a slab geometry is applied and a given line of
sight is chosen, the Lya profile can be successfully reproduced with no dust at
all and N(HI) = 3 x 10^(21) cm^(-2). The spatial variations of the profile
shape are naturally explained by radiation transfer effects. In the case of
outflowing Inter Stellar Medium (ISM), as commonly observed in Lyman Break
Galaxies (LBGs), a high N(H) and dust content are required to observe Lya in
absorption. For nearly static neutral gas as observed in IZw 18 and other low
luminosity galaxies only a small amount of dust is required provided a
sufficiently high N(H) covers the galaxy.
