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Table 1.
Physical parameters of the program stars.
| IDs | Sp. Type | Vrad, km s−1 | Reference | Teff, K | log g | [Fe/H] | Reference |
|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
| HD 057060 | O7e... | 20.0 ± 1.7 | Pourbaix et al. (2004) | 32508 ± 1928 | 3.39 ± 0.26 | 0.24 ± 0.14 | Koleva & Vazdekis (2012) |
| 33215 ± 2674 | 3.28 ± 0.16 | −0.03 ± 0.20 | Prugniel et al. (2011) | ||||
| HD 064332 | S | −1.3 ± 0.5 | Gontcharov (2006) | 3399 ± 44 | 0.61 ± 0.40 | −0.04 ± 0.18 | Prugniel et al. (2011) |
| HD 067507 | CNv... | 23 ± 10 | Wilson (1953) | 2680 | ... | ... | Bergeat et al. (2002) |
| HD 085405 | C | 3.50 ± 1.6 | Gontcharov (2006) | 2769 | ... | −0.10 | Soubiran et al. (2016) |
| 2645 | ... | ... | Bergeat et al. (2002) | ||||
| HD 096446 | B2IIIp | 6.1 ± 0.8 | Gontcharov (2006) | 20086 ± 530 | 3.59 ± 0.08 | 0.06 ± 0.04 | Koleva & Vazdekis (2012) |
| HD 099648 | G8Iab | −8.82 ± 0.19 | Gaia Collaboration (2018a) | 4970 ± 75 | 2.25 ± 0.43 | −0.01 ± 0.15 | Koleva & Vazdekis (2012) |
| 4977 ± 49 | 2.24 ± 0.12 | −0.03 ± 0.06 | Prugniel et al. (2011) | ||||
| HD 099998 | K3.5III | 18.43 ± 0.37 | Gaia Collaboration (2018a) | 4001 ± 32 | 1.56 ± 0.20 | −0.24 ± 0.07 | Prugniel et al. (2011) |
| HD 100733 | M3III | 21.07 ± 0.29 | Gaia Collaboration (2018a) | 3530 | ... | ... | Wright et al. (2003) |
| HD 306799 | M0Iab | −16.38 ± 0.19 | Mermilliod et al. (2008) | 3650 | ... | ... | Wright et al. (2003) |
| HD 101712 | M3Iab | −0.70 ± 1.23 | Mermilliod et al. (2008) | 3200 | ... | ... | Wright et al. (2003) |
| HD 102212 | M1III | 50.28 ± 0.09 | Famaey et al. (2009) | 3738 ± 6 | 1.55 ± 0.10 | −0.41 ± 0.05 | Koleva & Vazdekis (2012) |
| HD 114960 | K5III | 7.35 ± 0.16 | Gaia Collaboration (2018a) | 4000 | ... | ... | Wright et al. (2003) |
| IRAS 15060+0947 | M9III | −8.2 ± 2.6 | Engels & Bunzel (2015) | 3281 | ... | ... | Gaia Collaboration (2018b) |
| HD 147550 | B9V | −24.1 ± 0.9 | Gontcharov (2006) | 9830 ± 279 | 3.70 ± 0.66 | −0.38 ± 0.11 | Koleva & Vazdekis (2012) |
| HD 160365 | F6III | 8.14 ± 2.31 | Massarotti et al. (2008) | 6009 | ... | ... | Soubiran et al. (2016) |
| HD 160346 | K3V | 17.856 ± 0.784 | Kunder et al. (2017) | 4808 ± 65 | 4.53 ± 0.22 | 0.03 ± 0.10 | Koleva & Vazdekis (2012) |
| HD 163810 | G3V | 185.99 ± 0.22 | Latham et al. (2002) | 5818 ± 15 | 4.35 ± 0.06 | −1.20 ± 0.04 | Koleva & Vazdekis (2012) |
| HD 164257 | A0 | 5.5 ± 0.9 | Gontcharov (2006) | 9792 ± 691 | 3.70 ± 2.11 | 0.41 ± 0.30 | Koleva & Vazdekis (2012) |
| [B86] 133 | M4 | 44 ± 5 | This work | 4637 | ... | −0.21 | Gaia Collaboration (2018b), |
| 2645 | ... | ... | Ivanov et al. (2004) | ||||
| HD 167278 | F2 | −14.7 ± 0.9 | Gontcharov (2006) | 6563 ± 18 | 4.14 ± 0.08 | −0.21 ± 0.04 | Koleva & Vazdekis (2012) |
| HD 170820 | K0III | 2.84 ± 0.06 | Mermilliod et al. (2008) | 4707 ± 57 | 1.65 ± 0.13 | 0.17 | Prugniel et al. (2011) |
| HD 172230 | A5 | −36.8 ± 0.8 | Gontcharov (2006) | 7772 ± 102 | 3.76 ± 0.44 | 0.55 ± 0.14 | Koleva & Vazdekis (2012) |
| HD 173158 | K0 | 14.06 ± 0.32 | Gaia Collaboration (2018a) | 5164 ± 121 | 0.87 ± 0.43 | 0.04 ± 0.20 | Koleva & Vazdekis (2012) |
| HD 174966 | A3 | 5.6 ± 0.9 | Gaia Collaboration (2018a) | 7874 ± 57 | 4.09 ± 0.16 | 0.03 ± 0.10 | Koleva & Vazdekis (2012) |
| HD 175640 | B9III | −26.0 ± 4.3 | Gontcharov (2006) | 12067 ± 326 | 4.07 ± 0.55 | 0.22 ± 0.18 | Koleva & Vazdekis (2012) |
| 12077 ± 453 | 3.94 ± 0.21 | 0.17 ± 0.15 | Prugniel et al. (2011) | ||||
| HD 179821 | G5Ia | 81.78 ± 3.71 | Gaia Collaboration (2018a) | 6997 | 0.62 | 0.44 | Soubiran et al. (2016) |
| 7107 | 1.00 | 0.45 | Soubiran et al. (2016) | ||||
| HD 232078 | K3IIp | −388.34 ± 0.27 | Soubiran et al. (2008) | 4295 ± 48 | 0.82 ± 0.27 | −1.08 ± 0.11 | Koleva & Vazdekis (2012) |
| 4014 ± 48 | 0.81 ± 0.20 | −1.22 ± 0.11 | Prugniel et al. (2011) | ||||
| HD 193256* | A8Vn... | 6 ± 2 | This work | 7860 | 3.74 | −0.95 | Soubiran et al. (2016) |
| HD 193281A | A2III | 0.3 ± 0.5 | Gontcharov (2006) | 8623 ± 345 | 4.30 ± 0.33 | −0.68 ± 0.28 | Koleva & Vazdekis (2012) |
| 8597 ± 218 | 4.11 ± 0.14 | −0.37 ± 0.13 | Prugniel et al. (2011) | ||||
| HD 193281B* | F5:V: | −43.13 ± 0.97 | Gaia Collaboration (2018a) | 8080 | 3.58 | −1.00 | Soubiran et al. (2016) |
| 8080 | 3.58 | −1.00 | Soubiran et al. (2016) | ||||
| 8414 | ... | ... | Soubiran et al. (2016) | ||||
| K2III | 4354 ± 57 | ... | ... | This work | |||
| HD 193896 | G5IIIa | −15.23 ± 0.18 | Gaia Collaboration (2018a) | 4900 | ... | ... | Wright et al. (2003) |
| HD 196892 | F6V | −34.498 ± 0.004 | Santos et al. (2011) | 6028 ± 22 | 4.17 ± 0.10 | −0.99 ± 0.07 | Koleva & Vazdekis (2012) |
| HD 200081 | G0 | 7.67 ± 0.27 | Soubiran et al. (2008) | 5526 ± 71 | 3.25 ± 0.43 | 0.02 ± 0.12 | Koleva & Vazdekis (2012) |
| HD 204155 | G5 | −84.60 ± 0.16 | Latham et al. (2002) | 5704 ± 28 | 3.89 ± 0.16 | −0.70 ± 0.07 | Koleva & Vazdekis (2012) |
| 5718 ± 56 | 3.93 ± 0.11 | −0.69 ± 0.06 | Prugniel et al. (2011) | ||||
| HD 209290 | M0.5V | 18.144 ± 0.069 | Soubiran et al. (2013) | 4031 | ... | −0.06 | Ammons et al. (2006) |
Notes. The columns contain: (1) object ID (asterisks mark non-XSL objects); (2) SIMBAD spectral type; (3−4) radial velocity and reference; (5−8) effective temperature, surface gravity, iron abundance and reference. Our estimated spectral type and effective temperature for HD 193281B are also listed.
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