Comparison of blue and red bump features in M4327 with SSP models and empirical templates. Upper panels: M4327 spectrum is compared with a set of SSP models from BPASS v2.2.1 for different burst ages, assuming a stellar metallicity of 20% Z_⊙, a Chabrier (2003) IMF, an alpha-enhancement [α/Fe] = 0.4, and including binary evolution. The broad He II feature, if assumed purely stellar in origin, is well reproduced by a t ∼ 6 Myr-old burst (solid line), although these models under-predict the strength of the blue nitrogen features at ≈4620 − 4640 Å. Middle and bottom panels: M4327 spectrum is fitted with a combination of empirical WR template spectra from Crowther et al. (2023). The best-fit model in the middle panels include only stars of the WN type, whereas in the bottom panels we have included also WC stars; nebular emission lines are fitted separately with individual Gaussian components.