Spectral energy distribution of the G292.0+1.8 PWN emission, fitted with the one-zone electron model described in Sect. 4. The dataset includes radio emission from Gaensler & Wallace (2003) and Sect. 2, the total PWN X-ray spectrum from Hughes et al. (2001), the VHE upper limit from (H. E. S. S. Collaboration 2018), and the Fermi-LAT spectrum obtained from our analysis. Two models, Model 1 and Model 2, fit the data; their parameters are summarized in Table 3. The inverse Compton (IC) emission (black line) accounts for contributions from the CMB (dashed line), starlight (dotted line), and dust (dotted-dashed line) targets, following the energy density estimates from Porter et al. (2006) and Shibata et al. (2011) for Model 1, and Zhu et al. (2018) for Model 2.