Model fits to the spectrum of HESS J1809−193 and HESS J1825−137. For HESS J1809−193 (top panel), the model was fitted to the H.E.S.S. data points only. The emission below 10 GeV is attributed to another component not accounted for in our model framework (see text). For HESS J1825−137 (bottom panel), the model was fitted to Fermi-LAT and H.E.S.S. data points. Upper limits are not shown for clarity but model predictions are consistent with them. In each panel, PWN refers to the emission from particles still trapped in the shocked pulsar wind, SNR refers to the emission from particles that escaped into the remnant and are trapped downstream of the forward shock, and ISM refers to the emission from the halo of particles released in the surrounding medium.