Search for precursor eruptions among Type IIb supernovae

TL;DR

This study searches for pre-explosion eruptions in Type IIb supernovae using pre-coverage data, finding no significant precursors and setting upper limits on their occurrence, contrasting with higher rates in Type IIn supernovae.

Contribution

It provides the first systematic search for precursor eruptions in Type IIb supernovae using extensive pre-explosion observations, establishing upper limits on precursor rates.

Findings

No precursors detected for Type IIb SNe in the final 3.5 years.

Type IIb SNe have fewer precursors than Type IIn SNe.

Detection of progenitor for SN 2011dh shows no variability before explosion.

Abstract

The progenitor stars of several Type IIb supernovae (SNe) show indications for extended hydrogen envelopes. These envelopes might be the outcome of luminous energetic pre-explosion events, so-called precursor eruptions. We use the Palomar Transient Factory (PTF) pre-explosion observations of a sample of 27 nearby Type IIb SNe to look for such precursors during the final years prior to the SN explosion. No precursors are found when combining the observations in 15-day bins, and we calculate the absolute-magnitude-dependent upper limit on the precursor rate. At the 90% confidence level, Type IIb SNe have on average $<0.86$ precursors as bright as absolute $R$-band magnitude $-14$ in the final 3.5 years before the explosion and $<0.56$ events over the final year. In contrast, precursors among SNe IIn have a $\gtrsim 5$ times higher rate. The kinetic energy required to unbind a low-mass stellar envelope is comparable to the radiated energy of a few-weeks-long precursor which would be detectable for the closest SNe in our sample. Therefore, mass ejections, if they are common in such SNe, are radiatively inefficient or have durations longer than months. Indeed, when using 60-day bins a faint precursor candidate is detected prior to SN 2012cs ($\sim2$% false-alarm probability). We also report the detection of the progenitor of SN 2011dh which does not show detectable variability over the final two years before the explosion. The suggested progenitor of SN 2012P is still present, and hence is likely a compact star cluster, or an unrelated object.