dust, and shows an excess of emission in the submm, as unveiled by [*APEX*]{}/LABOCA and [*Herschel*]{}, which is often seen in low metallicity starbursting dwarf galaxies [@galliano-2003; @galliano-2005; @galametz-2009; @galametz-2011; @remy-2012]. The origin of the excess is not well determined and several hypotheses described in [@galametz-2011], including a change of dust emissivity, spinning dust grains, or a cold dust component, are invoked in current dust models to explain the submm excess. [@galametz-2009] present a detailed dust modeling of Haro11 in which they derive a total dust mass of $\rm{6 \times 10^{6}~M_{\odot}}$ if the submm excess is ignored, and of $\rm{2 \times 10^{7}~M_{\odot}}$ if the submm excess is interpreted as cold dust. Assuming the excess as cold dust (T$\sim$10 K) is however difficult to reconcile with the observed dust and gas mass budgets, and the expected lower dust-to-gas mass ratios [DGR; @galametz-2011]. Integrating the SED from 3 to 1100 $\mu$m, the total IR luminosity L$\rm{_{TIR}}$ is 1.4 $\times$ 10$^{11}$ L$\rm{_{\odot}}$ [@galametz-2009]. We will use this value of L$\rm{_{TIR}}$ throughout this paper.

Spectroscopic observations show bright lines in the FIR with [*ISO*]{}/LWS, while both the H [i]{} 21-cm line, and the CO (J=1-0) line, the most common tracer of molecular gas in 