Table 3
CEMP star fraction computed from the SEGUE data in the range −2.5 < [Fe/H] ≤ 2, and computed with our different model sets.
| Model sets and data | FC (%) | FC,gia (%) | FC,TO (%) | FC,dwa (%) | Fgia,CEMP (%) | FTO,CEMP (%) | Fdwa,CEMP (%) |
|
|
|||||||
| SEGUE | 11.46 ± 1.00 | 15.79 ± 1.00 | 10.38 ± 1.00 | 1.67 ± 1.00 | 51.42 ± 2.30 | 47.02 ± 2.16 | 1.56 ± 1.00 |
|
|
|||||||
| A | 8.50 ± 0.02 | 9.59 ± 0.03 | 10.73 ± 0.04 | 7.32 ± 0.02 | 31.95 ± 0.10 | 19.80 ± 0.08 | 48.25 ± 0.13 |
| B | 8.96 ± 0.02 | 10.30 ± 0.03 | 11.01 ± 0.04 | 7.72 ± 0.02 | 32.47 ± 0.10 | 19.23 ± 0.07 | 48.30 ± 0.13 |
| C | 9.48 ± 0.02 | 10.67 ± 0.03 | 11.78 ± 0.04 | 8.24 ± 0.02 | 31.69 ± 0.10 | 19.56 ± 0.07 | 48.75 ± 0.13 |
| D | 12.17 ± 0.02 | 9.94 ± 0.03 | 15.21 ± 0.05 | 12.45 ± 0.02 | 23.12 ± 0.07 | 19.60 ± 0.06 | 57.28 ± 0.12 |
| IK01 | 8.81 ± 0.01 | 9.98 ± 0.03 | 11.12 ± 0.04 | 7.58 ± 0.02 | 31.99 ± 0.10 | 19.75 ± 0.08 | 48.27 ± 0.13 |
| IL05 | 16.47 ± 0.02 | 17.23 ± 0.04 | 18.31 ± 0.05 | 15.40 ± 0.03 | 32.23 ± 0.08 | 19.27 ± 0.06 | 48.50 ± 0.10 |
| Qp4 | 7.87 ± 0.01 | 8.69 ± 0.03 | 9.85 ± 0.04 | 6.90 ± 0.02 | 31.37 ± 0.11 | 19.45 ± 0.08 | 49.18 ± 0.14 |
| Q1 | 11.37 ± 0.02 | 12.18 ± 0.03 | 13.95 ± 0.05 | 10.11 ± 0.02 | 32.27 ± 0.10 | 20.28 ± 0.07 | 47.45 ± 0.13 |
| SDM | 11.16 ± 0.02 | 12.45 ± 0.03 | 14.06 ± 0.04 | 9.67 ± 0.02 | 31.98 ± 0.08 | 19.72 ± 0.06 | 48.29 ± 0.11 |
| S3 | 9.41 ± 0.02 | 10.72 ± 0.03 | 11.82 ± 0.04 | 8.08 ± 0.02 | 31.71 ± 0.09 | 20.05 ± 0.07 | 48.24 ± 0.12 |
| T8 | 9.89 ± 0.01 | 12.14 ± 0.03 | 10.11 ± 0.03 | 8.78 ± 0.02 | 30.91 ± 0.09 | 20.22 ± 0.07 | 48.86 ± 0.12 |
| T12 | 8.14 ± 0.02 | 9.72 ± 0.04 | 13.60 ± 0.08 | 6.43 ± 0.02 | 31.52 ± 0.16 | 19.70 ± 0.12 | 48.78 ± 0.21 |
Notes. The range of V magnitudes adopted in the models is [13.5, 18.5]. FC, FC,gia, FC,TO, FC,dwa indicate, respectively, the CEMP/VMP ratio computed among all/giant/turnoff/dwarf stars. The fraction of giants, turnoff stars and dwarf stars computed among CEMP stars is indicated respectively as Fgia,CEMP, FTO,CEMP, Fdwa,CEMP (the latter fractions add up to 100%). The errors in the models convey only Poisson statistics. A minimum observational uncertainty of 1% is adopted (cf. Lee et al. 2013). CEMP stars have carbon abundance [C/Fe] > + 0.7.
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