Table 1
Stellar parameters of KFR08 stream members.
| Names | T eff | log g | [Fe/H] | v mic | v mac | v sin i |
|
log g′ | [Fe/H]′ |
|
|
v sin i′ | ||
| HIP | (K) | (km s-1) | (km s-1) | (km s-1) | (K) | (km s-1) | (km s-1) | (km s-1) | ||||||
|
|
||||||||||||||
| 5336 | 5304 | 4.52 | –0.77 | 1.0 | 2.0 | 0.7 | 5354 | 4.60 | –0.76 | 0.7 | 2.0 | 0.6 | ||
| 15495 | 5029 | 4.60 | –0.57 | 0.6 | 1.0 | 0.6 | 5119 | 4.79 | –0.55 | 0.7 | 0.7 | 0.8 | ||
| 18235 | 4980 | 3.33 | –0.68 | 0.6 | 3.2 | 1.0 | 4976 | 3.30 | –0.71 | 1.1 | 3.3 | 0.7 | ||
| 19143 | 4803 | 4.76 | –0.88 | 1.0 | 0.9 | 0.5 | 4939 | 5.07 | –0.84 | 0.5 | 0.3 | 0.4 | ||
| 54469 | 5948 | 4.20 | –0.45 | 1.0 | 3.0 | 2.7 | 6093 | 4.42 | –0.42 | 1.2 | 1.8 | 3.5 | ||
| 55988 | 4096 | 4.65 | –0.82 | 0.4 | –0.1 | 0.1 | 4071 | 5.08 | –0.54 | 0.2 | 0.0 | 0.1 | ||
| 58357 | 4898 | 3.20 | –0.67 | 0.6 | 3.3 | 0.9 | 4912 | 3.25 | –0.68 | 1.1 | 3.4 | 0.8 | ||
| 58708 | 4869 | 3.41 | –0.60 | 1.0 | 3.0 | 0.9 | 4924 | 3.37 | –0.56 | 1.1 | 3.1 | 0.8 | ||
| 58843 | 5649 | 4.37 | –0.76 | 1.0 | 2.9 | 0.5 | 5636 | 4.39 | –0.79 | 1.0 | 2.9 | 0.5 | ||
| 59785 | 4620 | 1.98 | –0.63 | 1.5 | 4.9 | 1.9 | 4808 | 2.52 | –0.48 | 1.7 | 4.7 | 1.5 | ||
| 60747 | 5268 | 4.54 | –0.85 | 0.5 | 1.5 | 0.6 | 5319 | 4.65 | –0.84 | 0.6 | 1.6 | 0.6 | ||
| 64920 | 4672 | 2.47 | –0.58 | 1.2 | 0.9 | 4.1 | 4701 | 2.51 | –0.57 | 1.2 | 0.7 | 4.3 | ||
| 74033 | 5657 | 4.03 | –0.73 | 1.1 | 3.5 | 1.3 | 5646 | 4.02 | –0.75 | 1.1 | 3.3 | 1.8 | ||
| 81170 | 5069 | 4.23 | –1.22 | 0.8 | 0.0 | 0.1 | 5280 | 4.78 | –1.13 | 0.5 | –0.2 | 0.1 | ||
| 87101 | 5485 | 3.14 | –1.68 | 1.5 | –0.2 | 0.1 | 5875 | 4.23 | –1.43 | 1.3 | –0.5 | 0.1 | ||
| 117720 | 5141 | 4.58 | –0.56 | 0.6 | 0.5 | 1.5 | 5150 | 4.63 | –0.65 | 0.8 | 1.0 | 0.8 | ||
Notes. Columns 2–7 give the global parameters obtained through a purely spectroscopic approach (Procedure 1, L15), while Cols. 8–13 give the six parameters obtained from Procedure 2 in L15. The unprimed quantities are the preferred values that are used to estimate the stellar masses and ages.
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