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Core-collapse supernovae (SNe) are the inevitable fate of most massive stars.Since most stars form in groups, SN progenitors can be constrained withinformation of their environments. It remains challenging to accurately analysethe various components in the environment and to correctly identify theirrelationships with the SN progenitors. Using a combined dataset of VLT/MUSEspatially-resolved integral-field-unit (IFU) spectroscopy and HST/ACS+WFC3high-spatial resolution imaging, we present a detailed investigation of theenvironment of the Type II-P SN 2004dg and Type IIb SN 2012P. The two SNeoccurred in a spiral arm of NGC 5806, where a star-forming complex is apparentwith a giant H II region. By modelling the ionised gas, a compact star clusterand the resolved stars, we derive the ages and extinctions of stellarpopulations in the vicinity of the SNe. The various components are consistentwith a sequence of triggered star formation as the spiral density wave sweptthrough their positions. For SNe 2004dg and 2012P, we identify their hoststellar populations and derive initial masses of $10.0^{+0.3}_{-0.2}~M_\odot$and $15.2^{+2.0}_{-1.0}~M_\odot$ for their progenitors, respectively. Bothresults are consistent with those from pre-explosion images or nebular-phasespectroscopy. SN 2012P is spatially coincident but less likely to be coevalwith the star-forming complex. As in this case, star formation bursts on smallscales may appear correlated if they are controlled by any physical processeson larger scales; this may lead to a high probability of chance alignmentbetween older SN progenitors and younger stellar populations.

Toward a better understanding of supernova environments: a study of SNe 2004dg and 2012P in NGC 5806 with HST and MUSE