GRB 140606B / iPTF14bfu: Detection of shock-breakout emission from a cosmological gamma-ray burst?

TL;DR

This paper analyzes the properties of GRB 140606B and its associated supernova, suggesting the gamma-ray emission may originate from shock-breakout rather than a jet, based on multi-wavelength observations and modeling.

Contribution

It provides the first detailed analysis indicating shock-breakout emission as a possible origin of gamma-rays in GRB 140606B, challenging the typical jet model for such bursts.

Findings

GRB 140606B's supernova properties align with other GRB-SNe.

Its gamma-ray emission is an outlier of the Amati relation, similar to low-luminosity GRBs.

Evidence suggests shock-breakout may explain the gamma-ray emission.

Abstract

We present optical and near-infrared photometry of GRB~140606B ($z=0.384$), and optical photometry and spectroscopy of its associated supernova (SN). The results of our modelling indicate that the bolometric properties of the SN ($M_{\rm Ni} = 0.4\pm0.2$~M$_{\odot}$, $M_{\rm ej} = 5\pm2$~M$_{\odot}$, and $E_{\rm K} = 2\pm1 \times 10^{52}$ erg) are fully consistent with the statistical averages determined for other GRB-SNe. However, in terms of its $\gamma$-ray emission, GRB~140606B is an outlier of the Amati relation, and occupies the same region as low-luminosity ($ll$) and short GRBs. The $\gamma$-ray emission in $ll$GRBs is thought to arise in some or all events from a shock-breakout (SBO), rather than from a jet. The measured peak photon energy ($E_{\rm p}\approx800$ keV) is close to that expected for $\gamma$-rays created by a SBO ($\gtrsim1$ MeV). Moreover, based on its position in the $M_{V,\rm p}$--$L_{\rm iso,\gamma}$~plane and the $E_{\rm K}$--$\Gamma\beta$~plane, GRB~140606B has properties similar to both SBO-GRBs and jetted-GRBs. Additionally, we searched for correlations between the isotropic $\gamma$-ray emission and the bolometric properties of a sample of GRB-SNe, finding that no statistically significant correlation is present. The average kinetic energy of the sample is $\bar{E}_{\rm K} = 2.1\times10^{52}$ erg. All of the GRB-SNe in our sample, with the exception of SN 2006aj, are within this range, which has implications for the total energy budget available to power both the relativistic and non-relativistic components in a GRB-SN event.