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tokens: expected from the measured absorption. A soft excess produced by soft Comptonization in a secondary, warm corona was proposed in previous works (Marshall et al. 2003 ; Guainazzi et al. 2004 ). However, similarly to the partial covering interpretation, the variations in this model fail to reproduce the observed PCA. This is likely due to the fact that the soft and hard Comptonization components are almost independently responsible for the variability at low and high energies, which is contrary to the changes in normalization of a single component suggested by the variability analysis and shape of the PCA. As seen in Section 4.3 , the model is also unable to explain the high fluxes observed in the UV band, even when testing different black hole spins. The Δα ox values suggest an X-ray normal state for Mrk 478 at all epochs, so it is unlikely that the UV data are intrinsically extreme. One crucial disagreement between models is on the shape of the primary continuum. In the partial covering model, the power law slope is extremely steep, with Γ = 2.99 ± 0.02 for all epochs. Although NLS1 galaxies typically feature steeper spectra than other AGNs (e.g. Boller, Brandt Fink 1996 ; Brandt, Mathur Elvis 1997 ; Grupe, Thomas Beuermann 2001 ), this value is high. In the soft Comptonization model, the spectrum is much flatter, with the index ranging from 2.0 to 2.2 between epochs. These values are average among NLS1 AGNs. The blurred reflection models require intermediate slopes, steeper than those of typical NLS1 galaxies, but not so extreme as the partial covering model. reflionx suggests slopes in the 2.6–2.8 range, and relxill measures this to be lower, with slopes of around 2.4–2.6. Although the variations in slopes between models are all able to explain the spectra, they differ at . The partial covering and blurred reflection models predict fluxes below the BAT survey limit. Owing to the very shallow power law measured in the optxagnf model, the predicted flux for this model is the highest (∼2 × 10 −12 ) and just at the threshold limit of the BAT survey (Oh et al. 2018 ). All spectra are consistent with null detections using Suzaku PIN. One of the most curious features revealed by the spectral analysis is the unique iron line profile of Mrk 478. AGNs typically show evidence of both narrow and broad lines, with the broad line likely produced by reflection of the primary emission off of neutral material (e.g. the torus). However, no evidence for such a feature is detected in any of the presented models. There are some plausible explanations for this – the spectrum is very steep, meaning that a narrow line may be buried below the continuum at these high energies if the reflection off of neutral material was sufficiently weak. Additionally, only XMM5 has high signal-to-noise ratio at these high energies; the other data sets suffer from short exposure and high background making it difficult to model narrow features at high energies. The emission line,