{ "id": "2210.13052", "version": "v1", "published": "2022-10-24T09:16:44.000Z", "updated": "2022-10-24T09:16:44.000Z", "title": "Measurement of the $\\sim 10^{-16}$~Gauss inter-galactic magnetic field with high energy emission of GRB 221009A", "authors": [ "Zi-Qing Xia", "Yun Wang", "Qiang Yuan", "Yi-Zhong Fan" ], "comment": "5 pages, 3 figures", "categories": [ "astro-ph.HE", "astro-ph.CO" ], "abstract": "The fast evolving TeV-PeV transients and their delayed GeV-TeV cascade emission in principle server as an ideal probe of the inter-galactic magnetic fields which are hard to be measured by other methods. Very recently, LHASSO has detected the very high energy emission of the extraordinary powerful GRB 221009A up to $\\sim 18$ TeV within $\\sim 2000$ s after the burst trigger. Here we report the detection of a $\\sim 400$ GeV photon, without accompanying prominent $\\gamma$ rays down to $\\sim 2$ GeV, by Fermi-LAT in the direction of GRB 221009A at about 0.4 days after the burst. Such a hard spectrum is unexpected in the inverse Compton radiation of the electrons accelerated by the external forward shock. Instead, the inverse Compton scattering of the $e^\\pm$ pairs, produced from the cascade of the early primary $\\sim 20$ TeV $\\gamma$ rays, off the diffuse far-infrared and microwave backgrounds can generate $\\gamma$ rays up to $\\sim 400$ GeV with a rather hard low energy spectrum. We infer that an inter-galactic magnetic field strength of $B_{\\rm IGMF}\\sim 10^{-16}$ Gauss can naturally account for the arrival time of the $\\sim 400$ GeV photon. Such a $B_{\\rm IGMF}$ is comparable to the limits set by the statistical studies of the high energy emission of TeV blazars.", "revisions": [ { "version": "v1", "updated": "2022-10-24T09:16:44.000Z" } ], "analyses": { "keywords": [ "high energy emission", "gauss inter-galactic magnetic field", "grb 221009a", "measurement", "gev photon" ], "note": { "typesetting": "TeX", "pages": 5, "language": "en", "license": "arXiv", "status": "editable" } } }