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Monte Carlo techniques based on indivisible energy packets are described forcomputing light curves and spectra for 3-D supernovae. The radiative transferis time-dependent and includes all effects of O(v/c). Monte Carlo quantizationis achieved by discretizing the initial distribution of 56Ni into radioactivepellets. Each pellet decays with the emission of a single energy packetcomprising gamma-ray photons representing one line from either the 56Ni or the56Co decay spectrum. Subsequently, these energy packets propagate through thehomologously-expanding ejecta with appropriate changes in the nature of theircontained energy as they undergo Compton scatterings and pure absorptions.  The 3-D code is tested by applying it to a spherically-symmetric SN in whichthe transfer of optical radiation is treated with a grey absorptioncoefficient. This 1-D problem is separately solved using Castor's co-movingframe moment equations. Satisfactory agreement is obtained.  The Monte Carlo code is a platform onto which more advanced treatments of theinteractions of matter and radiation can be added. Some of these have alreadybeen developed and tested in previous papers and are summarized here.Comment: 14 pages, 5 figures. Accepted by A&

Monte Carlo techniques for time-dependent radiative transfer in 3-D supernovae