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

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 ($M_{\mathrm{Ni}}=0.4\pm 0.2$~M${}_{\odot }$, $M_{\mathrm{ej}}=5\pm 2$~M${}_{\odot }$, and $E_{\mathrm{K}}=2\pm 1\times 10^{52}$ 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 ($E_{\mathrm{p}}\approx 800$ keV) is close to that expected for $\gamma$-rays created by a SBO ($\gtrsim 1$ MeV). Moreover, based on its position in the $M_{V,\mathrm{p}}$--$L_{\mathrm{iso},\gamma }$~plane and the $E_{\mathrm{K}}$--$\Gamma \beta$~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 ${\bar{E}}_{\mathrm{K}}=2.1\times 10^{52}$ 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.

Pre-print version: 14 Figs, 9 Tables, accepted at MNRAS. Comments and discussion are welcomed

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