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This article has an erratum: [https://doi.org/10.1051/0004-6361/202453505e]


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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