passbands are similar to those used on the BRIght-star Target Explorer Constellation (BRITE) which is already operating. We used the OPAL data for the AGSS09 mixture and $Z=0.015$. In the left panel we marked positions of all unstable modes in models with masses $13-18M_\odot$ whereas in the right panel we chose modes excited in models with $16M_\odot$ and $4.21 < \log T_\mathrm{eff} < 4.33$. These temperature range is a typical maximum error and larger than the error for HD 163899 (Saio et al. 2006). With different symbols we discriminate between different values of $\ell$ and evolutionary stages. Their meanings are described in the legend of the plots.

In the diagram for all studied masses, there is a perfect separation between radial and non-radial modes and fairly good separation between dipoles and quadruples. A discrimination between models undergoing shell hydrogen burning and models on the blue loops is not obvious. Modes excited in models on these evolution stages tend to group in slightly different locations but in a plot including such a range of masses their distinction would be uncertain given observational errors in the photometric amplitudes and phases. The situation improves slightly when we are able to constrain the mass 