An Exceptional Very High Energy Gamma-Ray Flare of PKS 2155-304

TLDR

PKS 2155‑304 is a well‑known high‑frequency peaked BL Lac at z = 0.116 that emits very‑high‑energy γ‑rays. The study investigates an extreme γ‑ray outburst detected in the early hours of 2006 July 28 (MJD 53944). The H.E.S.S. stereoscopic array monitored the source since 2002, and the rapid variability implies an emission region comparable to the Schwarzschild radius of a ~10⁹ M☉ black hole, requiring Doppler factors greater than 100.

Abstract

The high-frequency peaked BL Lac PKS 2155-304 at redshift z = 0.116 is a well-known VHE (>100 GeV) γ-ray emitter. Since 2002 its VHE flux has been monitored using the H.E.S.S. stereoscopic array of imaging atmospheric Cerenkov telescopes in Namibia. During the 2006 July dark period, the average VHE flux was measured to be more than 10 times typical values observed from the object. This article focuses solely on an extreme γ-ray outburst detected in the early hours of 2006 July 28 (MJD 53,944). The average flux observed during this outburst is I(>200 GeV) = (1.72 ± 0.05stat ± 0.34syst) × 10-9 cm-2 s-1, corresponding to ~7 times the flux, I(>200 GeV), observed from the Crab Nebula. Peak fluxes are measured with 1 minute timescale resolution at more than twice this average value. Variability is seen up to ~600 s in the Fourier power spectrum, and well-resolved bursts varying on timescales of ~200 s are observed. There are no strong indications for spectral variability within the data. Assuming the emission region has a size comparable to the Schwarzschild radius of a ~109 M☉ black hole, Doppler factors greater than 100 are required to accommodate the observed variability timescales.