molecular gas. While evidence for young massive stellar populations and SSCs exist from the optical and IR point of view, evidence for any substantial reservoir of neutral gas, in the form of either atomic or molecular, is non-existent to date. Where is the fuel for the vigorous star formation observed in Haro11? What is the state of the gas reservoirs in Haro11, residing in the ionised, neutral, and molecular form? This study, using a wide variety of tracers of neutral and ionised gas, aims for a more complete description of the enigmatic nature of the ISM of Haro11.

  ----------------------- ----------------------------------------------- ------------------
  RA (J2000)              00h36$^{\prime}$52.5$^{\prime\prime}$           NED $^{(a)}$
  Dec (J2000)             -33$^{\circ}$33$^{\prime}$19$^{\prime\prime}$   NED
  Distance                84 Mpc                                          NED $^{(b)}$
  12+log(O/H)             8.2                                             [@guseva-2012]
  Optical size            0.4$^{\prime}$x0.5$^{\prime}$                   NED
  $L_{\rm TIR}$$^{(c)}$   1.4 $\times \rm{10^{11}~L_{\odot}}$             [@galametz-2009]
  $L_{\rm FUV}$           2 $\times \rm{10^{10}~L_{\odot}}$               [@grimes-2007]
  $L_{\rm X-rays}$        4.4 $\times \rm{10^{7}~L_{\odot}}$              [@grimes-2007]
  $L_{\rm Ly\alpha}$      1.9 $\times \rm{10^{8}~L_{\odot}}$              [@hayes-2007]
  $L_{\rm H\alpha}$       8 $\times \rm{10^{8}~L_{\odot}}$                [@ostlin-1999]
  ----------------------- ----------------------------------------------- ------------------

  : General properties of Haro11.

$(a)$ NASA/IPAC Extragalactic Database.  $(b)$ This distance is derived with a Hubble constant H$_0$ = 73 km/sec/Mpc.  $(c)$ L$\rm{_{TIR}}$ is the integrated SED from 3 to 1100 $\mu$m.  All luminosities are scaled to the distance chosen in this paper of 