Table 5
Relative abundances.
| HIP | Δ[C/H] | σ | Δ[O/H] | σ | Δ[Na/H] | σ | ... |
|
|
|||||||
| wm: late F-dwarfs | |||||||
|
|
|||||||
| 522 | −0.059 | 0.036 | −0.066 | 0.011 | −0.183 | 0.011 | ... |
| 3119 | −0.106 | 0.033 | −0.031 | 0.002 | −0.192 | 0.011 | ... |
| 3236 | −0.213 | 0.044 | −0.117 | 0.003 | −0.242 | 0.003 | ... |
| 3540 | −0.146 | 0.080 | −0.164 | 0.005 | −0.288 | 0.003 | ... |
| 5862 | −0.041 | 0.011 | −0.032 | 0.005 | −0.097 | 0.004 | ... |
| 5985 | −0.157 | 0.060 | −0.136 | 0.005 | −0.228 | 0.008 | ... |
| 7978 | −0.260 | 0.076 | −0.230 | 0.020 | −0.440 | 0.008 | ... |
| 8548 | −0.089 | 0.059 | −0.142 | 0.006 | −0.236 | 0.026 | ... |
| 12653 | −0.106 | 0.036 | −0.032 | 0.012 | −0.179 | 0.030 | ... |
| 12764 | −0.076 | 0.041 | −0.069 | 0.010 | −0.229 | 0.011 | ... |
| . . . | . . . | . . . | . . . | . . . | . . . | . . . | . . . |
| mr: metal-rich solar analogs | |||||||
|
|
|||||||
| 1499 | −0.103 | 0.023 | −0.099 | 0.015 | −0.134 | 0.011 | ... |
| 1803 | −0.215 | 0.031 | −0.086 | 0.021 | −0.206 | 0.015 | ... |
| 5176 | −0.130 | 0.030 | −0.121 | 0.015 | −0.148 | 0.004 | ... |
| 12048 | −0.229 | 0.049 | −0.141 | 0.012 | −0.340 | 0.014 | ... |
| 12186 | −0.253 | 0.029 | −0.155 | 0.008 | −0.298 | 0.031 | ... |
| 17054 | 0.156 | 0.034 | 0.108 | 0.022 | 0.234 | 0.013 | ... |
| 17960 | −0.126 | 0.036 | −0.080 | 0.009 | −0.183 | 0.007 | ... |
| 20723 | −0.027 | 0.020 | −0.031 | 0.023 | −0.059 | 0.026 | ... |
| 20741 | −0.244 | 0.032 | −0.102 | 0.028 | −0.263 | 0.008 | ... |
| 21923 | −0.153 | 0.032 | −0.065 | 0.009 | −0.177 | 0.011 | ... |
| . . . | . . . | . . . | . . . | . . . | . . . | . . . | . . . |
Notes. The Δ values listed here are relative to the reference stars HIP 14954 for the wm sample and HIP 74500 for the mr sample. The σ columns correspond to a simple line-by-line scatter and are not necessarily representative of the true error of our relative, strict differential abundance measurements, which we estimate to be around 0.01 dex.
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