GRB 050502B optical afterglow: a jet break at high redshift

TL;DR

This study analyzes the optical afterglow of GRB 050502B, identifying a jet break at high redshift through combined optical and X-ray data, and estimates the redshift to be around 5.2, indicating a distant origin.

Contribution

First optical afterglow analysis of GRB 050502B revealing a jet break at high redshift using combined optical and X-ray data.

Findings

Optical afterglow decay index α = 2.1 ± 0.6 with a late break at ~130,000 seconds.

Photometric redshift estimate of z ≈ 5.2, suggesting a high-redshift GRB.

Identification of an achromatic jet break consistent with jet slow cooling model.

Abstract

Aims: GRB 050502B is well known for the very bright flare displayed in its X-ray light curve. Despite extensive studies, however, the optical light curve has never been discussed and its redshift is unconstrained. Possible correlations between optical and X-ray data are analysed. Methods: Photometric data from TNG in the R and I bands were used to compare the optical afterglow with the X-ray light curve. The HyperZ package and a late time VLT host observation were used to derive redshift estimates. Results: The I-band afterglow decay followed a power-law of index {\alpha} = 2.1 $\pm$ 0.6, after a late break at ~ $1.3 \times 10^5$ s. The R - I color is remarkably red and the broadband spectral index {\beta}_OX = $0.9 \pm 0.1$ is consistent with the X-ray spectral slope {\beta}_X. Although a photometric redshift of z > 4 is the most conservative result to consider, a photometric redshift of z = 5.2 $\pm$ 0.3 is suggested with no extinction in the host, based on which an isotropic energy E_{\gamma},iso = $(3.8 \pm 0.7) \times 10^52$ erg and a jet opening angle {\theta} ~ $3.7^{\circ}$ are subsequently derived. Conclusions: The combined X-ray and optical data suggest an achromatic break, which we interpret as a jet break. The post jet break slope obeys roughly the closure relation for the jet slow cooling model. Because of the afterglow's very red color, in order for the redshift to be low (z < 1), extinction, if present in the host, must be significantly high. Since the optical-to-X-ray index is consistent with the X-ray spectrum, and there is no XRT evidence for excess N_H, GRB 050502B was likely at high redshift.