Observational constraints on the structure of gamma-ray burst jets

TL;DR

This paper uses observational data from gamma-ray bursts, especially GW170817, to constrain the angular structure of GRB jets, finding that gamma-ray emission is likely confined to a narrow, high-Lorentz-factor core.

Contribution

It provides new constraints on the jet angular structure, showing gamma-ray emission is confined to regions with high Lorentz factors and ruling out certain jet models based on observed luminosity distributions.

Findings

High Lorentz factors (Γ > 50) are required at gamma-ray emission angles.

Jets with shallow angular energy distributions are inconsistent with observations.

Steep jet structures produce afterglow light-curves not seen in data.

Abstract

Motivated by GW170817 we examine constraints that observations put on the angular structure of long gamma-ray burst (GRB) jets. First, the relatively narrow observed distribution of $E_{X}/E_{\gamma}$ (the isotropic equivalent early X-ray afterglow to prompt $\gamma$-ray energy ratio) implies that at any angle that $\gamma$-rays are emitted the Lorentz factor must be high. Specifically, the Lorentz factor of $\gamma$-ray emitting material cannot drop rapidly with angle, and must be $\Gamma(\theta)\gtrsim 50$ even if there are angles for which the gamma-ray received energy is lower by three orders of magnitude compared to the jet core. Second, jets with an angular structure of the $\gamma$-ray emission that over-produce events with a $\gamma$-ray luminosity below the peak of the observed luminosity function are ruled-out. This eliminates models in which the $\gamma$-ray energy angular distribution isn't sufficiently steep and the Lorentz factor distribution isn't sufficiently shallow. Finally, models with a steep structure (e.g. Gaussian) which are detected away from the jet core generate afterglow light-curves that were never observed. We conclude that even if the jet kinetic energy distribution drops continuously with latitude, efficient $\gamma$-ray emission seems to be restricted to material with $\Gamma\gtrsim 50$ and is most likely confined to a narrow region around the core. While our study is confined to long GRBs, where the observed sample is larger and more complete, there are indications that similar conclusions may be applicable also to short GRBs. We discuss the possible implications to the $\gamma$-rays observed in GRB 170817A.