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Table 5.
CIGALE best-fit parameters of the spectroscopic members in the G237 field.
| ID | ℳ | SFR | Log(SFR/SFRMS) (a) |
|---|---|---|---|
| (1010 M⊙) | (M⊙ yr−1) | ||
| ss1: z = 2.15–2.164 | |||
| 55326 (b) | 1.64 ± 0.46 | 119 ± 10 | 0.46 |
| 55687 | 17.01 ± 0.85 | 5.3 ± 1.8 | −1.66 |
| 56014 | 0.28 ± 0.06 | 14 ± 2 | 0.14 |
| 56915 | 1.26 ± 0.17 | 30 ± 4 | −0.05 |
| 57557 | 0.80 ± 0.14 | 43 ± 5 | 0.26 |
| 58020 | 2.12 ± 0.26 | 44 ± 4 | −0.05 |
| 58057 (b) | 5.08 ± 1.00 | 143 ± 26 | 0.17 |
| 58173 | 0.61 ± 0.08 | 14 ± 2 | −0.14 |
| 58200 | 0.54 ± 0.18 | 9.4 ± 8.3 | −0.27 |
| 58206 | 1.79 ± 0.51 | 51 ± 15 | 0.06 |
| 58266 | 1.22 ± 0.13 | 10.7 ± 6.1 | −0.48 |
| 59504 | 0.36 ± 0.04 | 14.7 ± 1.3 | 0.06 |
| 60718 | 0.75 ± 0.11 | 10.4 ± 2.4 | −0.33 |
| 60811 | 2.03 ± 0.29 | 91 ± 14 | 0.28 |
| L710971 | 3.78 ± 1.10 | 52 ± 30 | −0.18 |
| SL01 | 12.60 ± 1.67 | 34 ± 23 | −0.76 |
| SL03 | 18.67 ± 1.09 | 158 ± 19 | −0.22 |
| 54698 | 0.49 ± 0.08 | 26 ± 3 | 0.20 |
| 57138 | 0.94 ± 0.15 | 76 ± 8 | 0.45 |
| 57730 | 0.73 ± 0.21 | 57 ± 12 | 0.41 |
| 2.164 < z < 2.19 | |||
| 54765 | 0.53 ± 0.08 | 9 ± 1 | −0.31 |
| 55951 | 1.30 ± 0.17 | 18 ± 3 | −0.29 |
| 56005 | 0.60 ± 0.10 | 29 ± 5 | 0.18 |
| ss2: z = 2.19–2.20 | |||
| 54677 | 2.65 ± 0.56 | 37 ± 24 | −0.21 |
| 56950 | 0.87 ± 0.35 | 35 ± 19 | 0.13 |
| 57695 | 0.64 ± 0.19 | 47 ± 12 | 0.37 |
| 59496 | 0.57 ± 0.12 | 18 ± 3 | −0.02 |
| 59906 | 0.64 ± 0.09 | 23 ± 2 | 0.05 |
| 60026 | 0.21 ± 0.04 | 8 ± 1 | −0.03 |
| 60355 | 0.91 ± 0.12 | 15 ± 2 | −0.26 |
| 60984 | 14.47 ± 1.45 | 247 ± 24 | 0.05 |
| full: 2.15 < z < 2.20 | |||
| Total | 96 ± 3 | 1485 ± 71 | 0.22 |
Notes.
(a)
Logarithm of the ratio between the estimated SFR and the expected SFR assuming the main sequence relation (Speagle et al. 2014) at the source redshift and stellar mass corrected for a Chabrier (2003) IMF.
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