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tokens: an external cold medium during the slow cooling regime to derive all the micro-physical and dynamical parameters ( Mészáros Rees 1997 ; Granot Sari 2002 ), and subsequently check for consistency with the slow or fast cooling transition times. Both spectral regimes, that is, , are explained and analysed in detail in the following subsection. The former corresponds to the jet in the light curve being associated with a jet break without energy injection, and the latter corresponds to the jet in the light curve associated with either the end of energy injection into the outflow or with a jet break with an ongoing energy injection during the whole evolution of the afterglow (i.e. the ongoing energy injection is still visible until the last observations). Table 4 Closure relations * . was use in the analysis. Notes. When determining the energy-injection parameter , we use the measured and . The equations used for are for the case when , for both spectral regimes. More details in Racusin et al. (2009) . (*) When and it does not depend on or . We did not include this scenario as it is not compatible with our data at any time. (**) Details on the results and implications of the closure relations are discussed in the outlined section. (a) For , . When we have (). (b) For . When we have (). 4.1. <inline-formula specific-use="simple-math"><italic>ν</italic><sub>c</sub> <italic>ν</italic><sub><italic>K</italic><sub>s</sub></sub></inline-formula>: Jet break Using the closure relations for a decelerating spherical blast wave, we find that the measured temporal slope before the break in the light curve is consistent with for both ISM and wind environments. This implies , as . The only plausible scenario consistent with the measured and corresponds to a non-spreading uniform jet propagating into a wind environment. We therefore associate the achromatic break observed in the light curve with a jet break ( Rhoads 1999 ; Wiersema et al. 2014 ). We proceed by including the post-break sub-mm and radio data in our analysis. The first broadband SED contains GROND, XRT, and APEX data. The best fit to this is a broken power law with both Galactic and host extinction and absorption, with (see Table 5 ). The measured value of Hz is a lower limit because the APEX measurement is an upper limit. The second broadband SED contains XRT, GROND, CARMA, and EVLA detections. Two possible spectral sub-regimes in the slow cooling phase give a good fit to the data: the cooling regime where , and the one where . Because there are only a few data points at radio wavelengths, it is difficult to distinguish between these two cooling regimes. Therefore, we analysed both cases. When (i.e. a hard electron spectrum), there is more energy-per-decade in high-energy electrons. This distribution has important implications for the analysis of the physics in the shock region, specifically requiring an additional high-energy cut-off in the electron population. We based our analysis on the