Table 2
Comparison of the mode identifications of our work and the Gaia survey.
| Star | Period | GDR3 | R23 | This work |
|---|---|---|---|---|
| CK Cam | 3.29 | F | F | U/F |
| BD Cas | 3.65 | 10 | 10 | U/10 |
| V1726 Cyg | 4.24 | 10 | 10 | U/10 |
| FF Aql | 4.47 | 10 | F | 10 |
| CE Cas A | 5.14 | F | F | U/F |
| X Lac | 5.44 | F | 10 | 10 |
| V924 Cyg | 5.57 | F | 10 | U/10 |
| MY Pup | 5.69 | F | 10 | 10 |
| GH Car | 5.73 | F | 10 | 10 |
| V495 Cyg | 6.72 | F | F | 10 |
| V440 Per | 7.57 | F | 10 | 10 |
| V636 Cas | 8.38 | F | F | U/F |
| GH Lup | 9.28 | F | F | U/F |
Notes. For each star, we indicate the mode identification (fundamental or first overtone) as given by the SOS Cep&RRL pipeline (Gaia Collaboration 2023) (GDR3), the reclassification by Ripepi et al. (2023) (R23), and finally our mode identification based on Fourier phase ϕ21 of the RV curve. When the pulsation mode is uncertain or undetermined according to our criteria (U), we indicate the mode identification resulting from the PL–ABL relation (see Fig. 7b).
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