Spectral energy distribution as modeled using the EMD in Fig. C.3, shown here for the quiescent state in Visit A (left panel) and the flaring peak phase in Visit F (right panels). Upper panels use the coronal data from the XMM-Newton observation of GJ 3470 alone. Lower panels use the coronal EMD adapted from AD Leo quiescent and flaring stages. The strongest line at high energies corresponds to He II 304 Å.