Table 4.
Characteristics of the 22 selected stars.
| Star | Class | [Fe/H] | Mini [M⊙] | Bin | Nab | dRMS |  |
fdil | Macc [M⊙] | Ref. | |
|---|---|---|---|---|---|---|---|---|---|---|---|
| BS 16080−175 | MS | −1.86 | ? | S/L/I | 7 | 0.96 | 0.72 | 0.92 | 4.3 × 10−5 | 1, 2 | |
| BS 17436−058 | RG | −1.90 | ? | S/L/I | 7 | 0.73 | 0.6 | 0.93 | 3.0 × 10−2 | 1, 2 | |
| CS 22880−074 | MS | −1.93 | ? | S/L/I | 11 | 0.95 | 0.65 | 0.995 | 2.5 × 10−6 | 2 − 5 | |
| CS 22887−048 | MS | −1.85 | ? | B | 7 | 0.70 | 0.27 | 0.45 | 6.1 × 10−4 | 1, 6 | |
| CS 29503−010 | MS | −1.69 | 0.86 | S/L/I | 10 | 0.74 | 2.54 | 0.10 | 4.5 × 10−3 | 1, 2, 7 | |
| CS 29513−032 | MS | −1.85 | ? | S/L/I | 12 | 0.65 | 1.56 | 0.99 | 5.1 × 10−6 | 8 | |
| HD 106038 | MS | −1.48 | 0.7 | S/L/I | 7 | 0.79 | 1.22 | 0.992 | 4.0 × 10−6 | 9 − 14 | |
| HD 126681 | MS | −1.17 | 0.7 | S/L/I | 8 | 0.60 | 0.84 | 0.996 | 2.0 × 10−6 | 8, 14 − 20 | |
| HD 166161 | RG | −1.25 | ? | ? | 12 | 0.83 | 0.68 | 0.9997 | 1.2 × 10−4 | 13, 21 − 28 | |
| HD 166913 | MS | −1.93 | 0.73 | S/L/I | 6 | 0.56 | 0.48 | 0.93 | 3.8 × 10−5 | 9, 14, 15, 29, 30 | |
| HD 206983 | RG | −1.00 | ? | ? | 11 | 0.68 | 0.36 | 0.999 | 4.0 × 10−4 | 31, 33 | |
| HD 209621 | RG | −2.00 | ? | B | 12 | 0.52 | 4.32 (2.46 ( * )) | 0.85 | 7.1 × 10−2 | 31, 34 | |
| HD 5223 | RG | −2.00 | ? | B | 14 | 0.63 | 1.93 | 0.95 | 2.1 × 10−2 | 31, 34, 35 | |
| HE 0507−1653 | RG | −1.35 | ? | B | 16 | 0.87 | 2.51 | 0.91 | 4.0 × 10−2 | 31, 32, 36 | |
| HE 1120−2122 | RG | −2.00 | ? | B | 16 | 0.44 | 2.19 (1.25 ( * )) | 0.95 | 2.1 × 10−2 | 31, 32 | |
| HE 2144−1832 | RG | −1.85 | ? | B | 16 | 0.65 | 1.48 | 0.93 | 3.0 × 10−2 | 31, 32 | |
| J130200.0-084328 | RG | −1.95 | ? | S/L/I | 10 | 0.80 | 1.61 | 0.72 | 1.6 × 10−1 | 37 | |
| T6953-00510-1 | RG | −1.93 | ? | ? | 7 | 0.97 | 0.74 | 0.997 | 1.2 × 10−3 | 38 | |
| J053250 | Post-AGB | −1.22 | 1 − 1.5 | ? | 13 | 0.99 | 6.60 (1.13 ( * )) | 0.0 | − | 39 | |
| J052043 | Post-AGB | −1.15 | 1 − 1.5 | ? | 14 | 0.97 | 5.66 (0.51 ( * )) | 0.0 | − | 39, 40 | |
| J051848 | Post-AGB | −1.03 | 1 − 1.5 | ? | 14 | 0.93 | 6.44 (1.66 ( * )) | 0.0 | − | 41 | |
| J004441 | Post-AGB | −1.34 | 1.3 | ? | 15 | 0.81 | 1.14 | 0.0 | − | 40, 42 | |
Notes. Their class is indicated by MS (main sequence), RG (red giant) and post-AGB as well as their metallicity, approximate mass (taken from the literature) and binary status: “B” for detected binary and “S/L/I” for either single (“S”), long-period binary (“L”) or binary systems with a high orbital axis inclination (“I”). The quantity Nab is the number of elements observed between Zn (Z = 30) and Bi (Z = 83), dRMS the average distance to the solar scaled r-process (Eq. (3)), 
the minimum reduced 
value, fdil the dilution factor (Eq. (5)), Macc the amount of mass the observed star must accrete (in the binary case) to reproduce its current level of enrichment (as defined in Sect. 5.6). ( * )The numbers in parenthesis indicate the 
values when excluding Sr, Y and Zr from the adjustment.
References. 1 – Allen et al. (2012); 2 – Tsangarides (2005); 3 – Aoki et al. (2002a); 4 – Preston & Sneden (2001); 5 – Aoki et al. (2002b); 6 – Masseron et al. (2012); 7 – Aoki et al. (2007); 8 – Roederer et al. (2014); 9 – Tan et al. (2009); 10 – Boesgaard et al. (2011); 11 – Fabbian et al. (2009); 12 – Gratton et al. (2003); 13 – Nissen et al. (2007); 14 – Hansen et al. (2012); 15 – Meléndez et al. (2010); 16 – Bensby et al. (2014); 17 – Caffau et al. (2005); 18 – Reddy et al. (2006); 19 – Nissen & Schuster (2011); 20 – Yan et al. (2016); 21 – Gratton et al. (2000); 22 – Simmerer et al. (2004); 23 – Fulbright & Johnson (2003); 24 – Mishenina & Kovtyukh (2001); 25 – Takeda et al. (2011); 26 – Mishenina et al. (2002); 27 – Roederer et al. (2010); 28 – Burris et al. (2000); 29 – Jonsell et al. (2005); 30 – Bihain et al. (2004); 31 – Karinkuzhi et al. (2021); 32 – Jorissen et al. (2016); 33 – Masseron et al. (2010); 34 – McClure & Woodsworth (1990); 35 – Goswami et al. (2006); 36 – Hansen et al. (2016); 37 – Sakari et al. (2018); 38 – Ruchti et al. (2011); 39 – van Aarle et al. (2013); 40 – De Smedt et al. (2014); 41 – De Smedt et al. (2015); 42 – De Smedt et al. (2012).
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