Table 2.
Properties of the 12 CP stars for which rotation periods could not be extracted using K2 observations.
| EPIC ID | HD | Camp. | ΔT (d) | N |
|---|---|---|---|---|
| 202061199 | 255134 | 00 | 36.18 | 1594 |
| 202061263 | − | 00 | 36.18 | 1602 |
| 206026652a | 215766 | 03 | 69.16 | 2785 |
| 214133870b | 177562 | 07 | 81.30 | 3494 |
| 214503319c | 177765 | 07 | 81.24 | 3432 |
| 219353144 | 181004 | 07 | 81.32 | 3196 |
| 224332430 | 162759 | 09 | 71.34 | 3002 |
| 224351176 | 167700 | 09 | 71.34 | 2924 |
| 224487047 | 165321 | 09 | 71.34 | 3034 |
| 225382260 | 161342 | 09 | 71.34 | 2927 |
| 227365417 | 168187 | 09 | 71.34 | 2919 |
| 246016562d | 219831 | 12 | 78.83 | 3089 |
Notes. Columns are EPIC and HD numbers, K2 campaign number, length of useable K2 data ΔT, and number of data points N. Literature values for rotation and magnetic field strength.
A possible rotation period of Prot = 5.2310 ± 0.0087 d was measured by Wraight et al. (2012), but we find no evidence of this in the K2 photometry.
Non-detection of a magnetic field by Buysschaert et al. (2018b), and poor quality K2 photometry caused by significant loss of flux in the subraster of the TPF.
A known magnetic star with a literature rotation period of Prot ≫ 5 yr (Mathys et al. 1997; Mathys 2017), and roAp pulsations at v = 61.02 d−1 (Alentiev et al. 2012).
No obvious rotation period found by Wraight et al. (2012).
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