Table 1.
Results obtained from spectroscopy and membership analysis.
| Star | V | n | FWHM | Sp. type |  |
 |
P(χ2) | Variability | Cluster | Notes |
|---|---|---|---|---|---|---|---|---|---|---|
| (mag) | (km s−1) | (km s−1) | (km s−1) | (%) | ||||||
| 9 | 9.26 | 22 | 170 | B8V | 33.6 | 1.4 | 0 | var. | NM | |
| 10 | 8.37 | 25 | 52+52 | B8pHgMn+B8pHgMn | 17.8 | 0.1 | – | SB2 | A | 1 |
| 30 | 8.51 | 15 | 100+50 | B7III+B8pSiII | 15.8 | 0.6 | – | SB2 | A | 1 |
| 90 | 9.57 | 2 | 300 | B8III: | 11.0 | 10.9 | 56 | const. | A | |
| 99 | 8.49 | 3 | 66 | K0II | 16.8 | 0.5 | 76 | const. | A | |
| 112 | 9.74 | 2 | 140 | B8IV | 20.0 | 2.6 | 66 | const. | A | |
| 132 | 9.36 | 2 | 310 | B7IV: | 14.2 | 8.0 | 84 | const. | A | |
| 134 | 8.93 | 6 | 40 | B8III | 15.8 | 1.0 | 0 | var. | A | 2 |
| 165 | 9.07 | 3 | 140 | B7V | 14.5 | 2.1 | 64 | const. | A | |
| 201 | 9.53 | 3 | 185 | A0III | 53.6 | 10.9 | 06 | const. | NM | |
| 257 | 9.15 | 14 | 100+35 | B2V+B2V | 25.3 | 0.4 | – | SB2 | B | 1 |
| 259 | 8.37 | 5 | 130 | B1V | 26.6 | 0.6 | 80 | const. | B | |
| 277 | 8.74 | 6 | 280 | B2V | 24.7 | 5.0 | 0 | var. | B | |
| 313 | 8.88 | 2 | 350 | B8IV | 11.8 | 10.1 | 66 | const. | NM | |
| 322 | 9.27 | 2 | 110 | B8IVpSi | 19.4 | 1.7 | 21 | const. | A | 2 |
| 353 | 8.96 | 2 | 440 | B7III: | 13.0 | 6.8 | 63 | const. | A | |
| 354 | 9.67 | 2 | 250 | B8IV | 12.0 | 13.7 | 42 | const. | A | |
| 356 | 8.35 | 5 | 50 | K0II | 15.2 | 0.4 | 96 | const. | A | |
| 380 | 8.34 | 4 | 290 | A2V: | 22.2 | 4.2 | 99 | const. | NM | |
| 448 | 8.95 | 2 | 290 | B6e | 12.9 | 6.4 | 83 | const. | A | |
| 475 | 8.20 | 22 | 40 | B1V | 27.2 | 0.1 | 0 | SB1 | B | 1 |
| 476 | 9.25 | 2 | 290 | B2V | 25.9 | 5.2 | 68 | cont. | B | 3 |
| 477 | 9.53 | 2 | 420 | B2V: | 17.2 | 6.1 | 88 | const. | B? | 3 |
| 540 | 8.19 | 6 | 37 | G5II | 30.2 | 0.5 | 23 | const. | NM | |
| 544 | 8.20 | 5 | 46 | B9IIIpSi | 25.0 | 0.4 | 49 | const. | NM | |
| 575 | 6.39 | 5 | 121 | A7V | 30.6 | 0.8 | 47 | const. | NM | |
| 682 | 6.44 | 6 | 120 | O9.7II | 30.5 | 0.8 | 39 | const. | B | |
| 698 | 9.05 | 2 | 300 | B2V: | 20.3 | 3.1 | 26 | const. | B? | 3 |
Notes. 1: the average RV and its error correspond to the velocity of the center of mass obtained by fitting the orbit. 2: Large “astrometric excess noise” (>0.4 mas) with high significance (>50) in Gaia DR2; astrometric parameters probably not useful. 3: Members of NGC 2546B according to parallax and proper motions. A larger number of spectroscopic observations are needed to discard RV variability and determine a more reliable RV mean.
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