The 300 TeV photon from GRB 221009A: a Hint at Non-linear Lorentz Invariance Violation?

TL;DR

This paper investigates whether Lorentz invariance violation (LIV) can explain the detection of a 300 TeV photon from GRB 221009A, addressing puzzles about photon absorption and delayed detection, and constrains LIV parameters.

Contribution

It demonstrates that second-order subluminal LIV can reconcile the observations, providing new constraints on LIV energy scales based on GRB data.

Findings

Second-order LIV is consistent with the observed 300 TeV photon.

First-order LIV is incompatible with the data.

The study constrains the LIV energy scale to approximately 10^{-7} times the Planck energy.

Abstract

The air shower array Carpet-3 detected a 300 TeV photon from the direction of GRB 221009A at 4536 s after the Fermi-GBM trigger for this event. If the association with this gamma-ray burst is real, it poses two puzzles. First, why was this photon not absorbed by the extragalactic background light? ``New physics'' beyond the Standard Model is required to explain how it managed to reach Earth from a cosmological distance. Second, why was this photon detected when the VHE afterglow observed by LHAASO already faded? A novel astrophysical mechanism is required to explain this delay. In this work we show that Lorentz invariance violation (LIV), which arises as a low-energy limit of certain quantum gravity theories, can solve both puzzles. It shifts thresholds of particle interaction and changes the opacity of the extragalactic background, and cause energy-dependent variations of the photon velocity, which changes the photon time of flight. We investigate the LIV parameter space assuming that the 300 TeV photon is a part of the VHE afterglow detected by LHAASO in the TeV range. We identify viable solutions and place stringent two-sided constraints on the LIV energy scale required to resolve the observational puzzles. First-order LIV appears to be incompatible with the constraints set by analyzing the TeV afterglow of this GRB. Viable solutions emerge for higher orders. In particular, the commonly studied second-order subluminal LIV with $E_{\rm LIV2} = 1.30_{-0.35}^{+0.56} \times 10^{-7} E_{\rm Pl}$ (95.4% credibility level; $E_{\rm Pl}$ is the Planck energy) is consistent with all the observed data.