The Remarkable Late-time Flux Excess in Hubble Space Telescope Observations of the Type Iax Supernova 2012Z

Abstract Type Iax supernovae (SNe Iax) are thermonuclear explosions of white dwarfs (WDs), peculiar and underluminous compared to the normal Type Ia supernovae (SNe). Observations of SNe Iax provide insight into the physics of WD explosions and suggest that some may not be terminal events. Late-time photometry (∼1400 days postpeak) of the SN Iax SN 2012Z, the only WD SN with a preexplosion detection of a progenitor system, revealed a flux excess that may be explained by a gravitationally bound remnant driving a radioactively powered wind. We present further late-time Hubble Space Telescope photometry of SN 2012Z, ∼2500 days after the explosion, and find that the SN is still brighter than, but trending toward, the preexplosion flux. Additionally, we observe that the excess F555W flux seen in previous data has grown more pronounced. The color of the excess flux disfavors a light echo or interaction with the circumstellar material. The decline rate of the excess flux is consistent with energy deposition from 55 Fe, but the luminosity is higher than expected from models of the ejecta, further suggesting evidence for a bound remnant. Combining our data with future observations should allow for the detection of emission from the ejecta shock-heating of the companion He star seen in the progenitor system.