Table 1.
Stellar and pulsational properties of the newly discovered pulsators with TESS and CoRoT.
| Designation | TIC ID | Magnitude | ST | Teff | log g | Source | Type | Frequency range(s) | |
|---|---|---|---|---|---|---|---|---|---|
| V | Tess | (K) | (d−1) | ||||||
| BD+65 1637 | 322312832 | 10.53 | 9.53 | B3 | 18 000 ± 1000 | 4.0 ± 0.5 | A13 | SPB | 3−5.5, 8 |
| HD 152822 | 247980805 | 9.07 | 8.84 | B5/6 | 18 236 ± 625 | 4.3 ± 0.07 | A18 | SPB | 0.8−2.5, 4.8 |
| HD 152799 | 247981153 | 8.74 | 8.67 | B2/3 | 22 919 ± 1577 | 4.31 ± 0.04 | A18 | SPB | 0.7−4.5 |
| HD 329271 | 247981406 | 10.65 | 10.51 | B4 | 18 074 ± 623 | 4.26 ± 0.06 | A18 | SPB | 2.5 |
| HD 317861 | 102141335 | 9.83 | 9.52 | B3 | 20 473 ± 822 | 4.23 ± 0.09 | A18 | SPB | 1.2, 2.5, 5.2, 7.3 |
| HD 76534 | 30051402 | 7.5 | 8.07 | B2 | 19 000 ± 500 | 4.1 ± 0.2 | F15 | SPB | 2.5, 5, 9 |
| HD 287823 | 459990291 | 9.74 | 9.58 | A0 | 8375 ± 125 | 4.23 ± 0.15 | F15 | δ Sct | 16.1−23.75 |
| HD 290500 | 50656450 | 11.04 | 10.75 | A2 | 9500 ± 500 | 3.8 ± 0.4 | F15 | δ Sct | 17.6−23.76 |
| V599 Ori | 332914217 | 13.7 | 11.66 | A8/9 | 8000 ± 250 | 3.72 ± 0.13 | F15 | δ Sct | 17.5−23.3 |
| TYC 8581-2002-1 | 355320922 | 10.91 | 10.55 | A5 | 9750 ± 250 | 4.0 ± 0.1 | F15 | δ Sct | 11.1−22.3 |
| HD 144432 | 67671603 | 8.19 | 7.8 | A9/F0 | 7500 ± 250 | 4.05 ± 0.17 | F15 | δ Sct | 13.1−23.2 |
| HD 135344A | 307606851 | 7.76 | 7.71 | A0 | 6750 ± 250 | 4 | A13 | δ Sct | 60.5−80.9 |
| HD 317859 | 102141942 | 9.52 | 9.04 | F3 | 7300 ± 163 | 4.35 ± 0.01 | A18 | γ Dor | 1.2, 2.7, 5.4 |
| Cl⋆ NGC 2264 VAS 196 | 231147340 | 10.07 | 10.80 | F0/2 | 6784 ± 150 | 4.0 ± 0.2 | this work | γ Dor | 0.8−2.75 |
| Cl⋆ NGC 2264 VAS 219 | 231147743 | 12.09 | 11.85 | A7 | 7170 ± 150 | 4.3 ± 0.3 | this work | γ Dor | 0.5−3.8 |
| Cl⋆ NGC 2264 VAS 230 | 231147556 | 12.37 | 11.66 | A5 | 7520 ± 150 | 4.3 ± 0.4 | this work | hybrid | 2.1−3.3, 8−12 |
Notes. The column source refers to the stellar parameter and the shortcuts refer to the following articles: A13: Alecian et al. (2013), F15: Fairlamb et al. (2015), A18: Aidelman et al. (2018). Sources for the spectral types can be found in the main text.
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