Table 3
Main spectral peculiarities, and spectroscopic classification of our sample stars.
| ID | St. | He str. | Sp. var. | Sp. | Notes | Class |
| comp. | distor. | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
|
|
||||||
| HD 66765 | strong | high | yes | He-strong | ||
| HD 67621 | weak | faint | yes | He-weak | ||
| HD 109026 | P | solar ? | faint ? | no ? | Normal | |
| S | (...) | high | no ? | Very strong metallic lines | Ap | |
| HD 121743 | strong | high | yes | He-strong | ||
| HD 133518 | strong | no | no ? | He-strong | ||
| HD 147932 | faint | high | yes | He-weak | ||
| HD 156324 | P | strong | high ? | yes ? | He-strong | |
| S | (...) | (...) | (...) | (...) | ||
| T | weak ? | (...) | (...) | Numerous strong P ii/iii lines | He-weak PGa | |
| HD 156424 | strong | faint | no | He-strong | ||
Notes. Column (1): star identification. Column (2): spectroscopic stellar component in the cases of a multiple spectroscopic system (P for primary, S for secondary, T for tertiary). Column (3): apparent strength of the He lines relative to a solar abundance. Column (4): variability of the spectral lines. Column (5): distortion of the spectral lines. Column (6): additional notes on the peculiarities of the spectra. Column (7): classification of the star in terms of spectral peculiarity. “(...)”: cannot be determined using our data. “?”: not accurate due to the blending of the spectral lines by the companion (for multiple spectroscopic systems), or because of the absence of rotational Doppler resolution (for HD 133518).
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