HST/STIS UV spectra of MWC 656 obtained on four observing dates. A PoWR stellar atmosphere model with T_* = 21 kK, log g_* = 3.4, and v sin i = 300 km s⁻¹ is shown in black for comparison. The top and bottom panels show the full spectral range, split into blue and red halves, while the middle row displays zoom-ins on key diagnostic lines: the N Vλλ1238, 1241 doublet, the C IVλλ1548, 1551 doublet, and the He IIλ1640 line. Shaded grey regions mark known ISM absorption features. The zoom-in panels reveal prominent high-ionisation features, not present in the Be star model, suggesting they originate from a hotter source within the system.