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Long ($>2$ s) gamma ray bursts (GRBs) are associated with explosions ofmassive stars, although in three instances, supernovae (SNe) have not beendetected, despite deep observations. With new HI line and archival opticalintegral field spectroscopy data, we characterize the interstellar medium (ISM)of the host galaxy of one of these events, GRB 111005A, in order to shed lighton the unclear nature of these peculiar objects. We found that the atomic gas,radio continuum, and rotational patterns are in general very smooth throughoutthe galaxy, which does not indicate a recent gas inflow or outflow. There isalso no gas concentration around the GRB position. The ISM in this galaxydiffers from that in hosts of other GRBs and SNe, which may suggest that theprogenitor of GRB 111005A was not an explosion of a very massive star (e.g. acompact object merger). However, there are subtle irregularities of the GRB111005A host (most at a $2\sigma$ level), which may point to a weak gas inflowor interaction. Since in the SE part of the host there is 15% more atomic gasand twice less molecular gas than in NW part, the molecular gas fraction islow. In the SE part there is also a region with very high H$\alpha$ equivalentwidth. There is more continuum 1.4 GHz emission to the SE and an S-shaped warpin the UV. Finally, there is also a low-metallicity region 3.5" (1 kpc) fromthe GRB position. Two galaxies within 300 kpc or a past merger can beresponsible for these irregularities.

The interstellar medium in the environment of the supernova-less long-duration GRB 111005A