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We show model light curves of superluminous supernova 2006gy on theassumption that the supernova is powered by the collision of supernova ejectaand its dense circumstellar medium. The initial conditions are constructedbased on the shock breakout condition, assuming that the circumstellar mediumis dense enough to cause the shock breakout within it. We perform a set ofnumerical light curve calculations by using a one-dimensional multigroupradiation hydrodynamics code STELLA. We succeeded in reproducing the overallfeatures of the early light curve of SN 2006gy with the circumstellar mediumwhose mass is about 15 Msun (the average mass-loss rate ~ 0.1 Msun/yr). Thus,the progenitor of SN 2006gy is likely a very massive star. The density profileof the circumstellar medium is not well constrained by the light curve modelingonly, but our modeling disfavors the circumstellar medium formed by steady massloss. The ejecta mass is estimated to be comparable to or less than 15 Msun andthe explosion energy is expected to be more than 4e51 erg. No 56Ni is requiredto explain the early light curve. We find that the multidimensional effect,e.g., the Rayleigh-Taylor instability, which is expected to take place in thecool dense shell between the supernova ejecta and the dense circumstellarmedium, is important in understanding supernovae powered by the shockinteraction. We also show the evolution of the optical and near-infrared modellight curves of high-redshift superluminous supernovae. They can be potentiallyused to identify SN 2006gy-like superluminous supernovae in the future opticaland near-infrared transient surveys.

Light Curve Modeling of Superluminous Supernova 2006gy: Collision between Supernova Ejecta and Dense Circumstellar Medium