\[sect:model\] explains the modeling strategy and assumed initial parameters. Section \[sect:results\], \[sect:diffus\], and \[sect:disc\] report the model results and conditions of the ISM components. This study establishes an encompassing picture of the dominant ISM phases in Haro11 and describes the mass budget of the various phases in our model (Section \[sect:buildup\]).

Studies of Haro11 {#sect:haro11}
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Several studies of Haro11 have highlighted its peculiarity as a galaxy and challenged our understanding of star formation. Haro11 – also know as ESO 350-IG38 – is a blue compact dwarf (BCD) galaxy at 84 Mpc, with M$\rm{_{B} =-20.3}$, and metallicity Z$\sim$1/3 Z$_{\odot}$ [@guseva-2012]. It is composed of 3 main star-forming regions, or knots, described in [@vader-1993] and [@kunth-2003], with a morphology presumably resulting from a merger event [@ostlin-2001]. The starbursting nature of Haro11 is visible in Figure \[fig:acs\] with a dominant bright stellar component and dust lanes in front of knot B. These knots host hundreds of young star clusters and $\sim$60 super star clusters (SSC) with ages between 1 and 100 Myr peaking at 3 Myr, and constituting a total stellar mass of $\rm{10^{10}~M_{\odot}}$ [@adamo-2010]. An older stellar population is also present, primarily in knots A and C, as seen in the 