Late-time observations of SN2006gy: Still Going Strong

TL;DR

SN2006gy remains luminous over a year after explosion, with evidence suggesting its power source is either a pair-instability supernova with dust formation or an IR echo from pre-existing dust, rather than ongoing CSM interaction.

Contribution

This study provides late-time observations of SN2006gy, ruling out CSM interaction and proposing two alternative models for its sustained luminosity.

Findings

SN2006gy is still luminous in near-IR over a year post-explosion.

Weak late-time H-alpha, X-ray, and radio emissions challenge CSM interaction as the main power source.

Data supports either a pair-instability SN with dust or an IR echo from pre-existing dust.

Abstract

Owing to its extremely high luminosity and long duration, SN2006gy radiated more energy in visual light than any other known SN. Two hypotheses to explain its high luminosity -- that it was powered by shock interaction with CSM as implied by its Type IIn spectrum, or that it was fueled by radioactive decay from a large mass of 56Ni synthesized in a pair-instability SN -- predicted different late-time properties. Here we present observations of SN2006gy obtained more than a year after discovery. We were unable to detect it at visual wavelengths, but clear near-IR K and H-band detections show that it is still at least as luminous as the peak of a normal SN II. We also present spectra giving an upper limit to the late-time Ha luminosity of about 1e39 erg/s. Based on the weak late-time Ha, X-ray, and radio emission, combined with the difficulty of explaining the shift to IR wavelengths, we can rule out ongoing CSM interaction as the primary late-time power source. Instead, we propose that the evolution of SN2006gy is consistent with one of two possible scenarios: (1) A pair-instability SN plus modest CSM interaction, where the radioactive decay luminosity shifts to the IR because of dust formation. (2) An IR echo, where radiation emitted during peak luminosity heats a pre-existing dust shell at radii near 1 light year, requiring the progenitor star to have ejected another 10 Msun shell about 1500 yr before the SN.