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tokens: if using the relationships of the Ca ii triplet due to Paschen blending that may be causing the offset observed between HAeBes and CTTs. Another note of caution is advised when using the He i and O i lines, as their complex line profiles suggest various origins – which may or may not be associated with accretion. The complexities of their profiles are likely the cause of the low detection rate of these lines, as multiple absorption and emission components can contribute to the line equivalent width. An exploration of the line profiles will be presented in a future paper by the authors. 3.3 Emission lines as accretion diagnostics Since all of the emission lines appear to be correlated with the accretion luminosity, it is worth discussing which lines serve as the most sensitive tracers of accretion i.e. most readily detected (and therefore possibly associated directly with accretion). That way the best lines can be prioritized in future observations. In Table 3 , all 32 lines are presented along with details of the number of emission detections. The other columns of the table are split into different categories based on emission detection and UV-excess detection. HAeBe stars that are classed as having an accretion detection are those for which a UV excess was clearly detected in Paper I – 62 stars match this criterion. This includes the seven stars in which an accretion rate could not be determined within the context of MA; it would require an unrealistically high filling factor of shocked material to reproduce their UV excess. The measured Δ D B of these seven objects is likely associated with accretion due to the overall properties of the stars, although the exact mechanism is not known [an alternative could be boundary layer accretion for these hot objects Bertout, Basri Bouvier (see 1988 ); Blondel Djie (see 2006 )]. 2 Table 3. This table details all of the measured emission lines, along with their respective number of detections. The final four columns denote the four categories into which each star of the sample can belong to for a given line; full descriptions are provided in the text. ‘Emis’ denotes emission line, and Δ D B denotes the UV excess. The two categories of emission and accretion can be divided into two outcomes for each case, those with and those without. This gives a total of four possible categories for a star to be in e.g. a star may have a particular line in emission, but no Δ D B was detected in the star. Table 3 gives the number of stars split into each category, for each line, and is presented visually in Fig. 4 . What the four different categories represent are now detailed. The first category contains objects for which both emission lines and a UV excess are detected, represented by the green segments in the diagram. This category measures if the line is a good one to one tracer of accretion i.e. excess is present and so is the emission line. Examples of good tracers are Hα, Brγ and Paβ as their emission detections