Prompt emission of GRB 121217A from gamma-rays to the near-infrared

AbstraktAbstract

The mechanism that causes the prompt-emission episode of gamma-ray bursts (GRBs) is still widely debated despite there being thousands of prompt detections. The favoured internal shock model relates this emission to synchrotron radiation. However, it does not always explain the spectral indices of the shape of the spectrum, which is often fit with empirical functions, such as the Band function. Multi-wavelength observations are therefore required to help investigate the possible underlying mechanisms that causes the prompt emission. We present GRB 121217A, for which we were able to observe its near-infrared (NIR) emission during a secondary prompt-emission episode with the Gamma-Ray burst Optical Near-infrared Detector (GROND) in combination with the Swift and Fermi satellites, which cover an energy range of 5 orders of magnitude (10(-3) keV to 100 keV). We determine a photometric redshift of z = 3.1 +/- 0.1 with a line-of-sight with little or no extinction (A(v) similar to 0 mag) utilising the optical/NIR SED. From the afterglow, we determine a bulk Lorentz factor of Gamma(0) similar to 250 and an emission radius of R < 10(18) cm. The prompt-emission broadband spectral energy distribution is well fit with a broken power law with beta(1) = -0.3 +/- 0.1 and beta(2) = 0.6 +/- 0.1 that has a break at E = 6.6 +/- 0.9 keV, which can be interpreted as the maximum injection frequency. Self-absorption by the electron population below energies of E-a < 6 keV suggest a magnetic field strength of B similar to 10(5) G. However, all the best fit models underprcdict the flux observed in the NIR wavelengths, which also only rebrightens by a factor of similar to 2 during the second prompt emission episode, in stark contrast to the X-ray emission, which rebrightens by a factor of similar to 100. This suggests an afterglow component is dominating the emission.

The mechanism that causes the prompt-emission episode of gamma-ray bursts (GRBs) is still widely debated despite there being thousands of prompt detections. The favoured internal shock model relates this emission to synchrotron radiation. However, it does not always explain the spectral indices of the shape of the spectrum, which is often fit with empirical functions, such as the Band function. Multi-wavelength observations are therefore required to help investigate the possible underlying mechanisms that causes the prompt emission. We present GRB 121217A, for which we were able to observe its near-infrared (NIR) emission during a secondary prompt-emission episode with the Gamma-Ray burst Optical Near-infrared Detector (GROND) in combination with the Swift and Fermi satellites, which cover an energy range of 5 orders of magnitude (10(-3) keV to 100 keV). We determine a photometric redshift of z = 3.1 +/- 0.1 with a line-of-sight with little or no extinction (A(v) similar to 0 mag) utilising the optical/NIR SED. From the afterglow, we determine a bulk Lorentz factor of Gamma(0) similar to 250 and an emission radius of R < 10(18) cm. The prompt-emission broadband spectral energy distribution is well fit with a broken power law with beta(1) = -0.3 +/- 0.1 and beta(2) = 0.6 +/- 0.1 that has a break at E = 6.6 +/- 0.9 keV, which can be interpreted as the maximum injection frequency. Self-absorption by the electron population below energies of E-a < 6 keV suggest a magnetic field strength of B similar to 10(5) G. However, all the best fit models underprcdict the flux observed in the NIR wavelengths, which also only rebrightens by a factor of similar to 2 during the second prompt emission episode, in stark contrast to the X-ray emission, which rebrightens by a factor of similar to 100. This suggests an afterglow component is dominating the emission.