  Superluminous supernovae (SLSNe) are the most luminous supernovae in the
universe. They are found in extreme star-forming galaxies and are probably
connected with the death of massive stars. One hallmark of very massive
progenitors would be a tendency to explode in very dense, UV-bright, and blue
regions. In this paper we investigate the resolved host galaxy properties of
two nearby hydrogen-poor SLSNe, PTF~11hrq and PTF~12dam. For both galaxies
\textit{Hubble Space Telescope} multi-filter images were obtained.
Additionally, we performe integral field spectroscopy of the host galaxy of
PTF~11hrq using the Very Large Telescope Multi Unit Spectroscopic Explorer
(VLT/MUSE), and investigate the line strength, metallicity and kinematics.
Neither PTF~11hrq nor PTF~12dam occurred in the bluest part of their host
galaxies, although both galaxies have overall blue UV-to-optical colors. The
MUSE data reveal a bright starbursting region in the host of PTF~11hrq,
although far from the SN location. The SN exploded close to a region with
disturbed kinematics, bluer color, stronger [OIII], and lower metallicity. The
host galaxy is likely interacting with a companion. PTF~12dam occurred in one
of the brightest pixels, in a starbursting galaxy with a complex morphology and
a tidal tail, where interaction is also very likely. We speculate that SLSN
explosions may originate from stars generated during star-formation episodes
triggered by interaction. High resolution imaging and integral field
spectroscopy are fundamental for a better understanding of SLSNe explosion
sites and how star formation varies across their host galaxies.
