Table 1.
Summary of the best-fit model setups for HESS J1809−193 and HESS J1825−137.
| Source | HESS J1809−193 | HESS J1825−137 |
|---|---|---|
| Data set | HESS | LAT+HESS |
| Pulsar age tage (yr) | 16 475 | 20 930 |
| Pulsar spin-down time scale τ0 (yr) | 34 525 | 470 |
| Ejecta energy Eej (erg) | 1051 | 5 × 1050 |
| Ejecta mass Mej (M⊙) | 15 | 15 |
| Interstellar medium density n0 (H cm−3) | 0.1 | 0.01 |
| Interstellar magnetic fieldBISM (μG) | 5 | 5 |
| Turbulence scale κT | 0.02 | 0.01 |
| Turbulent energy injection efficiency ηT | 0.075 | 0.2 |
| Magnetic energy injection efficiency ηB | 0.025 | 0.02 |
| Particle energy injection efficiency ηe | 0.90 | 0.78 |
| Particle injection spectrum low-energy index α1 | 1.2 | 1.0 |
| Particle injection spectrum high-energy index α2 | 2.4 | 2.5 |
| Particle injection spectrum break energy Eb (GeV) | 800 | 210 |
| Particle injection spectrum cutoff energyEc (TeV) | 1000 | 1000 |
Particle escape maximum momentum  (GeV/c) |
1.5 × 105 | 1.0 × 103 |
| Particle escape indexξ | 2.5 | 2.5 |
| χ2/Nd.o.f. | 15.2/22 | 30.4/30 |
Notes. Parameters in italics were set and fixed at the beginning of the fitting procedure. In addition, we emphasise that tage was not explicitly fitted and was deduced from τ0 and τc. The same applies to ηe, which was deduced from ηB and ηT. Last, 
was fixed to 1 TeV/c for HESS J1825−137 because the SNR was found to have a minor contribution to the signal.
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