Binary interactions can result in delayed SNe and displace SNe far from their parent clusters and molecular clouds. Top panels: stacked histograms separated by progenitor type. Effectively single stars had no binary interaction prior to SN (no Roche-lobe overflow and <5% wind mass accretion). Primary (secondary) stars were the initially more (less) massive star in a binary that did not undergo a merger. Merger products are the result of a merger between two stars prior to SN in a binary. Bottom panels: fractional complementary cumulative distribution also separated by progenitor type. Pie charts shows the relative contribution from each progenitor type. Left panels: histograms show the SN rate as a function of time since cluster birth. Dashed lines indicate time beyond which no SN occur in FIRE simulations. Right panels: histograms show the distance between an SN and its parent cluster at the time of the SN. The inset panel highlights the tail of SNe at extremely long distances. Solid markers on the top axis of the top panel indicate the median value for each progenitor type. The black circle in the bottom panel shows the overall median distance. An interactive version of the top-right panel of this figure is available. The interactive version allows the reader to view this figure for all model variations, instead of just the fiducial model. One can also use a slider to see how the distribution changes as a function of time, as well as buttons to change between a stacked histogram and separate (semitransparent) histograms for each progenitor type.

An interactive version of this figure is available in the online article.

An interactive version of this figure is available.

An interactive version of this figure is available in the online journal.