Table 3
Programme stars observed with IGRINS.
| Star | Teff (K) | log(g) (dex) | [Fe/H] (dex) | ξmicro (km s–1) | Distance (pc) | Stellar pop. | S /N | [Yb/Fe] (dex) | [Eu/Fe](b) (dex) | [Ce/Fe] (dex) |
|---|---|---|---|---|---|---|---|---|---|---|
| α Boo | 4308 | 1.7 | –0.56 | 1.8 | … | Thick | 155 | 0.111 | 0.317 | –0.293 |
| µ Leo | 4494 | 2.5 | 0.29 | 1.5 | … | Thin | 169 | 0.090 | 0.034 | –0.283 |
| є Vir | 5112 | 3.0 | 0.15 | 1.6 | … | Thin | 299 | –0.002 | … | 0.012 |
| βGem | 4809 | 2.8 | 0.00 | 1.4 | … | Thin | 336 | –0.210 | 0.016 | –0.101 |
| HD 102328 | 4442 | 2.5 | 0.30 | 1.5 | 70 ± 1 | Thin | 250 | 0.068 | –0.027 | –0.218 |
| HD 102328 (a) | 4442 | 2.5 | 0.28 | 1.5 | 68 ± 1 | Thin | 125 | 0.127 | –0.027 | –0.223 |
| HIP 50583 | 4292 | 1.7 | –0.49 | 1.7 | … | Thin | 86 | 0.382 | 0.193 | 0.020 |
| HIP 63432 | 4155 | 1.3 | –0.65 | 1.9 | 199 ± 4 | Thick | 275 | 0.317 | 0.292 | –0.039 |
| HIP 72012 | 4077 | 1.4 | –0.19 | 1.5 | 196 ± 3 | Thin | 286 | 0.055 | 0.182 | –0.123 |
| HIP 90344 | 4454 | 2.2 | –0.37 | 1.4 | 91 ± 1 | Thin | 283 | 0.403 | 0.223 | 0.013 |
| HIP 96014 | 4240 | 1.6 | –0.35 | 1.7 | 139 ± 2 | Thin | 414 | 0.052 | 0.086 | –0.149 |
| HIP 102488 | 4742 | 2.5 | –0.16 | 1.6 | … | Thin | 343 | 0.247 | 0.137 | –0.100 |
| 2M17215666 | 4342 | 1.6 | –1.10 | 1.7 | 1900 ± 200 | Halo, s-rich | 165 | 0.424 | 0.511 | 0.207 |
| KIC 3748585 | 4569 | 2.6 | 0.08 | 1.3 | 360 ± 10 | Thin | 205 | 0.008 | –0.037 | –0.105 |
| KIC 3955590 | 4411 | 2.2 | 0.06 | 1.6 | 950 ± 50 | Thin | 140 | –0.114 | –0.079 | –0.232 |
| KIC 4177025 | 4309 | 1.7 | –0.43 | 1.6 | 1200 ± 80 | Thick | 185 | 0.263 | 0.607 | –0.254 |
| KIC 5113910 | 4338 | 1.7 | –0.37 | 1.6 | 1900 ± 200 | Thin | 183 | 0.245 | 0.122 | –0.040 |
| KIC 5709564 | 4687 | 2.2 | –0.35 | 1.7 | 640 ± 20 | Thick | 137 | –0.050 | 0.406 | –0.330 |
| KIC 5779724 | 4303 | 1.6 | –0.48 | 1.7 | 1500 ± 100 | Thick | 215 | 0.197 | 0.417 | –0.225 |
| KIC 5859492 | 4511 | 2.4 | 0.14 | 1.5 | 780 ± 30 | Thin | 181 | –0.262 | 0.030 | –0.288 |
| KIC 5900096 | 4480 | 2.5 | 0.22 | 1.5 | 313 ± 6 | Thin | 179 | –0.047 | 0.071 | –0.210 |
| KIC 6465075 | 4825 | 2.8 | –0.28 | 1.3 | 550 ± 20 | Thin | 146 | 0.300 | 0.169 | 0.071 |
| KIC 6547007 | 4738 | 2.4 | –0.72 | 1.4 | 750 ± 30 | Thick | 281 | 0.201 | 0.397 | –0.149 |
| KIC 6837256 | 4731 | 2.3 | –0.68 | 1.5 | 1250 ± 60 | Thick | 148 | 0.209 | 0.306 | –0.226 |
| KIC 11045542 | 4304 | 1.6 | –0.52 | 1.5 | 1900 ± 200 | Thin | 294 | 0.186 | 0.085 | –0.201 |
| KIC 11342694 | 4509 | 2.8 | 0.21 | 1.3 | 440 ± 10 | Thin | 139 | 0.044 | 0.044 | –0.118 |
| KIC 11444313 | 4630 | 2.3 | –0.09 | 1.5 | 1400 ± 80 | Thin | 160 | 0.070 | 0.146 | –0.144 |
| KIC 11569659 | 4838 | 2.4 | –0.33 | 1.6 | 1510 ± 80 | Thin | 246 | 0.168 | 0.162 | –0.061 |
| KIC 11657684 | 4870 | 2.6 | –0.26 | 1.5 | 1700 ± 100 | Thin, s-rich | 184 | 0.448 | 0.096 | 0.351 |
| 2M14231899 | 4308 | 1.8 | –0.77 | 1.6 | 1900 ± 300 | Thick, s-rich | 284 | 0.639 | 0.547 | 0.179 |
| HD 142091(a) | 4845 | 3.3 | 0.06 | 1.2 | 30 ± 0.1 | Thin | 223 | 0.066 | … | –0.217 |
Notes. The [Yb/Fe] and [Ce/Fe] abundances were determined in this work, whilst the [Eu/Fe] abundances are the ones from Forsberg et al. (2019). The distances are from McMillan (2018). The stellar parameters and classification into different stellar populations are determined in Jönsson et al. (in prep.) (see our Sects. 3.1 and 3.2). The S/N is determined using the code DER_SNR (Stoehr et al. 2008) applied to a set of continuum regions in the H band. We use A(Fe)⊙ = 7.45, A(Yb)⊙ = 1.08 (Grevesse et al. 2007) and A(Ce)⊙ = 1.58, A(Eu)⊙ = 0.52 (Grevesse et al. 2015). (a)Data from the IGRINS Spectral Library (Park et al. 2018) (b)The [Eu/Fe] values in Forsberg et al. (2019) are reported to be systematically too high, possibly originating from systematic uncertainties in log(g) as reported in Jönsson et al. (2017). We lower all these abundances by 0.10 dex both in this table and in subsequent figures, such that the overall thin disk in [Eu/Fe] goes through the solar value, as seen in Fig. 6.
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