PoWR model for PGMW 3053. Several windows are displayed to show the most important He I and He II lines, as well as some metals, in comparison with the final model of the star. The temperature (T_⋆) of the star is determined by modeling the He I-He II ratios (e.g., He I λ4471.5, and He II λ4541.6). Singlet lines of He I (1s2p P) at 4387.9 and 4921.9 Å are identified with blue labels and were not used for diagnostic. Non- photospheric lines (e.g., Na) and features in absorption ([O III]), most likely due to nebular emission subtraction, are indicated with green labels. He II λ4686 is crucial for determining the mass-loss rate (Ṁ) of the star. Rotational broadening and chemical abundances, such as that of nitrogen, are determined from metal lines in absorption (e.g., N III λ4515 and N III λ4518). The observed spectra are shown by a blue line and the PoWR model by a red dashed line. The most important lines are identified.