Detection of Low-energy Breaks in Gamma-Ray Burst Prompt Emission Spectra

Abstract

The radiative process responsible for gamma-Ray Burst (GRB) prompt emission has not been identified yet. If dominated by fast-cooling synchrotron radiation, the part of the spectrum immediately below the $νF_ν$ peak energy should display a power-law behavior with slope $α_2=-3/2$, which breaks to a higher value $α_1=-2/3$ (i.e. to a harder spectral shape) at lower energies. Prompt emission spectral data (usually available down to $\sim10-20\,$keV) are consistent with one single power-law behavior below the peak, with typical slope $\langleα\rangle=-1$, higher than (and then inconsistent with) the expected value $α_2=-3/2$. To better characterize the spectral shape at low energy, we analyzed 14 GRBs for which the Swift X-ray Telescope started observations during the prompt. When available, Fermi-GBM observations have been included in the analysis. For 67% of the spectra, models that usually give a satisfactory description of the prompt (e.g., the Band model) fail in reproducing the $0.5-1000\,$keV spectra: low-energy data outline the presence of a spectral break around a few keV.We then introduce an empirical fitting function that includes a low-energy power law $α_1$, a break energy $E_{\rm break}$, a second power law $α_2$, and a peak energy $E_{\rm peak}$. We find $\langleα_1\rangle=-0.66$ ($\rm σ=0.35$), $\langle \log (E_{\rm break}/\rm keV)\rangle=0.63$ ($\rm σ=0.20$), $\langleα_2\rangle=-1.46$ ($\rm σ=0.31$), and $\langle \log (E_{\rm peak}/\rm keV)\rangle=2.1$ ($\rm σ=0.56$).The values $\langleα_1\rangle$ and $\langleα_2\rangle$ are very close to expectations from synchrotron radiation. In this context, $E_{\rm break}$ corresponds to the cooling break frequency.