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tokens: is one possible strategy, it is important to remember that not all input features provide insight in all evolutionary phases (i.e. the small separation loses its diagnostic potential in subgiants, White et al. 2011 ). Furthermore, not all quantities can be defined in every system. We can improve the accuracy of spi if a priori knowledge of the evolutionary stage can be supplied. This ensures that the input features and training data are exploited optimally. We have implemented an RF classifier in the spi pipeline to determine the evolutionary phase based on ν max , T eff , Δν, and . Evolutionary phases were divided according to three sampling regimes listed in Section 4.1 . Detailed results are presented in Appendix C , however, we note here that the classifier accurately distinguishes between main-sequence and subgiant stars thus ensuring with high probability that the correct phase is included in the training data. 5 OBSERVATIONAL SURVEYS AND TARGETS The new spi input features have been designed to better extract information from the stellar interior. Moreover, in this work, one of the aims is to determine how asteroseismic precision impacts the determination of key CBM properties, which amongst other things is crucial for reliable stellar ages. To this end, we have reprocessed the results from Bellinger et al. ( 2019 ) with the new pipeline which include data from the KAGES (Silva Aguirre et al. 2015 ; Davies et al. 2016 ) and Legacy (Lund et al. 2017 ; Silva Aguirre et al. 2017 ) surveys. A majority of stars in the TESS field will be observed for 27 d, far shorter than the four-year timeseries of Kepler . The duration and cadence will reveal ridges in the echelle diagram although not with the precision required to probe the interior in detail. Many targets, however, will lie in the repeated/continuous viewing zones resulting in timeseries longer than 54 d. For these stars, we can expect a comparable frequency resolution to previously studied RV targets (e.g. Procyon A, α Cen A) or solar-like oscillators in the CoRoT field which we analyse with spi below. We summarize the main properties of these stars in Table 4 , while in Fig. 4 , we compare their measurement precisions with the precision obtained for 16 Cyg A – one of the Kepler benchmarks. The combination of different surveys, precisions, and observations essential for our scientific goal. Figure 4. The frequency precision for oscillation modes with different spherical degrees as a function of radial order. Here, we compare seven CoRoT stars, α Cen A, and Procyon A with the Kepler Star 16 Cyg A. The shaded regions indicate the uncertainty stemming from different mode identifications in the oscillation spectra (see Table 4 ). Table 4. An overview of CoRoT and RV stars analysed in this study. a In the supplementary online material. b Denotes that the star is likely a subgiant. c We have used these frequencies but relabelled the radial order based on an expected regular pattern. 6 RESULTS