Table 1
Solar twin candidates within the volume-limited sample observed with HARPS presented in this work.
| Star ID | Teff | log gspec | ξt | [Fe/H] | N(Fe i, Fe ii) | Agep | Massp |
| [K] | [cm s-2] | [km s-1] | [Gyr] | [M⊙] | |||
|
|
|||||||
| HD 19641 | 5806 ± 61 | 4.39 ± 0.10 | 0.94 ± 0.01 | -0.01 ± 0.05 | 255, 35 | 4.6 ± 3.4 | 0.992 ± 0.039 |
| HD 29263 | 5780 ± 65 | 4.35 ± 0.10 | 0.94 ± 0.03 | 0.03 ± 0.05 | 259, 35 | 7.0 ± 2.8 | 0.995 ± 0.030 |
| HD 76440 | 5764 ± 63 | 4.43 ± 0.10 | 0.89 ± 0.02 | -0.01 ± 0.05 | 260, 35 | 3.7 ± 3.2 | 0.983 ± 0.038 |
| HD 96116 | 5832 ± 63 | 4.52 ± 0.10 | 0.96 ± 0.03 | -0.01 ± 0.05 | 260, 35 | 2.7 ± 2.5 | 1.005 ± 0.036 |
| HD 134702 | 5782 ± 64 | 4.50 ± 0.11 | 0.74 ± 0.04 | -0.04 ± 0.05 | 259, 36 | 3.2 ± 3.0 | 0.979 ± 0.037 |
| HD 145927 | 5819 ± 62 | 4.41 ± 0.10 | 0.93 ± 0.02 | -0.03 ± 0.05 | 254, 35 | 2.7 ± 2.5 | 0.994 ± 0.036 |
| HD 216008 | 5773 ± 62 | 4.38 ± 0.10 | 0.91 ± 0.02 | -0.04 ± 0.05 | 257, 35 | 6.1 ± 3.9 | 0.967 ± 0.037 |
Notes. log gspec the spectroscopic surface gravity; ξt is the microturbulance speed; N(Fe i, Fe ii) is the number of lines used in the spectroscopic analysis; Massp and Agep are the mass and age determined directly from the Padova web interface using the Hipparcos parallax. The error presented here are the assumed “accuracy” errors, which were used to select solar twin candidates within the full sample.
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