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Interaction of supernova (SN) ejecta with the optically thick circumstellarmedium (CSM) of a progenitor star can result in a bright, long-lived shockbreakout event. Candidates for such SNe include Type IIn and superluminous SNe.If some of these SNe are powered by interaction, then there should be arelation between their peak luminosity, bolometric light-curve rise time, andshock-breakout velocity. Given that the shock velocity during shock breakout isnot measured, we expect a correlation, with a significant spread, between therise time and the peak luminosity of these SNe. Here, we present a sample of 15SNe IIn for which we have good constraints on their rise time and peakluminosity from observations obtained using the Palomar Transient Factory. Wereport on a possible correlation between the R-band rise time and peakluminosity of these SNe, with a false-alarm probability of 3%. Assuming thatthese SNe are powered by interaction, combining these observables and theoryallows us to deduce lower limits on the shock-breakout velocity. The lowerlimits on the shock velocity we find are consistent with what is expected forSNe (i.e., ~10^4 km/s). This supports the suggestion that the early-time lightcurves of SNe IIn are caused by shock breakout in a dense CSM. We note thatsuch a correlation can arise from other physical mechanisms. Performing such atest on other classes of SNe (e.g., superluminous SNe) can be used to rule outthe interaction model for a class of events.

Interaction-powered supernovae: Rise-time vs. peak-luminosity correlation and the shock-breakout velocity