Late-Time HST Photometry of SN 1994I: Hints of Positron Annihilation Energy Deposition

TL;DR

This study presents late-time multicolor HST observations of SN 1994I, revealing that positron annihilation significantly contributed to its energy deposition around 280 days post-maximum, aligning with models of gamma-ray escape.

Contribution

First detailed multicolor late-time photometry of SN 1994I, demonstrating positron energy deposition and providing a framework for comparing supernova light curves.

Findings

Late-time light curve consistent with gamma-ray escape model

Positron annihilation significantly energizes the supernova at late times

Developed a scaling method for comparing supernova light curves

Abstract

We present multicolor Hubble Space Telescope (HST) WFPC2 broadband observations of the Type Ic SN 1994I obtained approximately 280 days after maximum light. We measure the brightness of the SN and, relying on the detailed spectroscopic database of SN 1994I, we transform the ground-based photometry obtained at early times to the HST photometric system, deriving light curves for the WFPC2 F439W, F555W, F675W, and F814W passbands that extend from 7 days before to 280 days after maximum. We use the multicolor photometry to build a quasi-bolometric light curve of SN 1994I, and compare it with similarly constructed light curves of other supernovae. In doing so, we propose and test a scaling in energy and time that allows for a more meaningful comparison of the exponential tails of different events. Through comparison with models, we find that the late-time light curve of SN 1994I is consistent with that of spherically symmetric ejecta in homologous expansion, for which the ability to trap the Gamma-rays produced by the radioactive decay of 56Co diminishes roughly as the inverse of time squared. We also find that by the time of the HST photometry, the light curve was significantly energized by the annihilation of positrons.