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The origin of super-luminous supernovae (SLSNe), especially the source oftheir huge luminosities, has not been clarified yet. While a strong interactionbetween SN ejecta and dense circumstellar media (CSM) is a leading scenario,alternative models have been proposed. In this Letter, we suggest newdiagnostics to discriminate the strong SN-CSM interaction scenario from theothers: a decline in the luminosity ('dip') before the main peak of the lightcurve. This dip is an unavoidable consequence of having a dense CSM withinwhich the shock breakout occurs. If a dense CSM shell is located far at largeradii from the progenitor inside, it takes time for the SN ejecta to reach itand the early light curve can be powered by the SN ejecta before the collision.Once the SN ejecta collides with the dense CSM, the electron density and thusthe Thomson scattering opacity suddenly increase. Photons become unable to goout of the shock even if there is a source of emission inside, which results inthe dip in the light curve. This dip is a solid prediction from the stronginteraction scenario irrespective of a power source for the early emission.Eventually the forward shock breaks out from within the dense CSM, and theluminosity increases by the continuous strong SN-CSM interaction, resulting inan SLSN. The possible dip observed in the hydrogen-poor SLSN, 2006oz, could bethe first example of this signature and give support to the SN-CSM interactionas the power source of SLSN 2006oz.

A Dip after the Early Emission of Super-Luminous Supernovae: A Signature of Shock Breakout within Dense Circumstellar Media