tokens: We also find a large extinction of A V = 1.56 mag for this target. HD 38043, sectors 1–3, 5–6, 8–13 The TESS light curve spans 357 d and includes all sectors except 4 and 7. The data are at 2-min cadence in all available sectors. The p modes appear to be dominated by two nearly equally spaced multiplets: the first contains the strongest three modes – the same ones for which frequencies and amplitudes are provided in Table 1 – with a spacing of ∼0.51 d −1 . The second is slightly lower in frequency and amplitude and has a spacing of ∼0.55 d −1 . These could be rotationally split multiplets of modes with similar but non-identical n and l. This star is highly multiperiodic at lower frequencies, consistent with g-mode pulsation, though we could not identify any clear period spacings. HD 41958, sectors 1, 4–5. 7–8, 11 The three strongest p modes have similar amplitudes (7.5–8.2 mmag). They do not have any obvious harmonic relationship, nor do they have the frequency ratio (0.77–0.78) expected of the fundamental mode and first radial overtone modes. HD 42503, sectors 5–7 The mutliperiodic nature of the light curve at frequencies near 5 d −1 is rather unusual. The frequency content does not strongly resemble that of γ Dor stars, but is also quite different from typical δ Sct stars. No radial modes could be identified from frequency ratios of the stronger peaks. The peaks at 0.99 and 2.00 d −1 are not perfect harmonics, and another peak at 3.94 d −1 also falls on this near-harmonic pattern. HD 43533, sectors 6–7 The star is a γ Dor variable and the light curve is dominated by low-frequency variability, with dozens of significant peaks below 6 d −1 , and this variability spills into the δ Sct frequency domain. Excluding this variability, which presumably does not include independent p modes, there are only a few peaks in the Fourier transform that make this a δ Sct star. All three extracted peaks are significant, with SNR>4, despite their low amplitudes. The low amplitudes perhaps suggest these peaks belong to a contaminating source, but the Gaia DR2 data show no likely contaminant. It is noteworthy that this star is located below the ZAMS compared to tracks of solar metallicity. HD 44930, sector 5 The Fourier transform is dominated by several p modes of mmag amplitude. A group of weaker peaks with frequencies between 2 and 3 d −1 might be g modes. The absence of peaks at even lower frequencies would then suggest these are l = 1, m = 1 prograde modes, which suggests the near-core region rotates rapidly. This star is in the Octans association and has a measured Δν of 6.03 d −1 (Bedding et al. 2020 ). The échelle diagram (Fig A1 ) suggests f 1 = 18.15 d −1 is the fundamental mode, even though this is not in agreement with the P–L prediction. HD 47425, sectors 6–7 The two dominant p modes are too close in frequency to be the fundamental mode and first radial overtone. Indeed, it is not possible to clearly identify radial modes by period ratios in
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