Supernova Siblings and Spectroscopic Host-Galaxy Properties

Over the past century, supernova (SN) searches have detected multiple supernovae (SNe) in hundreds of individual galaxies. So-called SN siblings discovered in the same galaxy present an opportunity to constrain the dependence of the properties of SNe on those of their host galaxies. To investigate whether there is a connection between sibling SNe in galaxies that have hosted multiple SNe and the properties of galaxies, we have acquired integrated optical spectroscopy of 59 galaxies with multiple core-collapse SNe. Perhaps surprisingly, a strong majority of host-galaxy spectra fall within the composite region of the Baldwin-Phillips-Terlevich (BPT) diagram. We find a statistically significant difference (KS test p-value = 0.044) between the distributions of the [NII] $\lambda$6583/H$\alpha$ of galaxies that have hosted a majority SN Ibc and those that have hosted a majority SN II, where the majority SN Ibc galaxies have, on average, higher ratios. The difference between the distributions of [NII] $\lambda$6583/H$\alpha$ may arise from either increased contribution from AGN or LINERs in SN Ibc host galaxies, greater metallicity for SN Ibc host galaxies, or both. When comparing the inferred oxygen abundance and the ionization parameter for the galaxies in the Star-Forming region on the BPT diagram, we find statistically significant differences between the distributions for SN Ibc hosts and SN II hosts (p=0.008 and p=0.001, respectively), as well as SN Ib hosts and SN II hosts (p=0.030 and p=0.006, respectively). We also compare the H$\alpha$ equivalent width distributions, also integrated across the galaxies, and find no significant difference.