Table 1.
Properties of the studied stars.
TIC | Other ID | Resolved | Magnetic | Binarity |
---|---|---|---|---|
lines | field | |||
ssrAp stars | ||||
73765625 | HD 90131 | x | x | |
77038207 | HD 96003 | x | SB1 | |
154786038 | HD 96571 | x | x | SB1 |
165446000 | BD+39 4435 | x | x | |
167695608 | TYC 8912-1407-1 | x | x | |
170419024 | HD 151860 | x | x | SB1 |
202899762 | BD+46 570 | x | x | SB1 |
233539061 | HD 174017 | SB2 | ||
298197561 | HD 340577 | x | ||
301918605 | HD 17330 | x | SB1 | |
444094235 | HD 85284 | x | SB1 | |
Long period Ap stars | ||||
77128654 | HD 97127 | x | x | |
352787151 | BD+35 5094 | |||
468507699 | HD 206977 | x | ||
Ap stars with moderately long periods | ||||
163801263 | HD 203922 | x | x | |
301946105 | HD 7410 | x | SB1 | |
347202840 | HD 236298 | x | ||
461161123 | HD 95811 | |||
Short period Ap star | ||||
403625657 | HD 11187 | x | ||
Stars that are not typical Ap stars | ||||
80486647 | HD 67658 | |||
81554699 | HD 97132 | SB2 | ||
124988213 | HD 44979 | |||
206461701 | HD 209364 | |||
207468665 | HD 148330 | |||
286965228 | HD 127304 | SB(2?) | ||
291561579 | HD 171420 | |||
334505323 | HD 106322 |
Notes. The table is divided in five segments. The top one includes those stars for which the analysis presented in Appendix A indicates that they are in all probability ssrAp stars. The spectroscopic properties of the stars listed in the second segment are consistent with their having either moderately or extremely long rotation periods. The rotation periods of the stars from the third segment definitely or very probably are moderately long (20 d ≲ Prot ≲ 50 d). The fourth segment contains the only magnetic Ap star of this study to have a rotation period of a few days. In the bottom segment, we list those stars whose spectrum does not look like those of typical Ap stars. In each segment, the stars are listed in order of increasing TIC number (Col. 1); an alternative ID is given is Col. 2. The visible range spectrum of those stars for which ‘x’ appears in Col. 3 shows resolved magnetically split lines; the ‘x’ flag in Col. 4 identifies those stars for which a significant detection of the magnetic field was achieved and at least one field moment could be determined, either in this study or in the literature (see text). Finally, Col. 5 indicates which stars are spectroscopic binaries, distinguishing to the extent possible the single-lined (SB1) and double-lined systems.
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