Table 4
Summary table of all the relations derived in the paper.
| Observed | Derived | Slope | Intercept | z | Notesa | Sects.b |
|
|
||||||
| β spec | A IRX | 1.10 ± 0.23 | 3.33 ± 0.24 | 1.6 <z< 3.0 | spectral coverage: 1200−2600 Å | 5.1, A |
| β phot | A IRX | 1.45 ± 0.25 | 3.63 ± 0.26 | 1.6 <z< 3.0 | 5.1 | |
| (B − z) | A IRX | 1.64 ± 0.13 | 0.77 ± 0.13 | 1.4 <z< 2.5 | 5.3 | |
| β phot | A IRX | 1.03 ± 0.26 | 3.54 ± 0.25 | 1.0 <z< 1.6 | 5.4 | |
| log(EW[OII])c | β phot | −1.35 ± 0.20 | 0.91 ± 0.30 | 1.0 <z< 1.6 | [OII]λ3727 emission line | 6.1 |
| log(EW[OII])c | A IRX d | −1.39 ± 0.26 | 4.48 ± 0.35 | 1.0 <z< 1.6 | [OII]λ3727 emission line | 6.1 |
Notes. For each relation, observed and derived quantities are indicated, as well as slope and intercept of the linear relation, with associated uncertainties. Relations are given in the form: Derived = Slope × Observed + Intercept.
AIRX is the attenuation towards the stellar continuum at λ = 1500 Å. The attenuation for the [OII]λ3727 line is defined as A[OII] = AIRX × (κHα/κ1500 Å) × f-1, where κλ is the reddening curve. Assuming a Calzetti law for both the stellar continuum and nebular emission we estimate f = 0.50. Assuming instead a Cardelli et al. (1989) law for nebular emission and Calzetti law for the stellar continuum we estimate f = 0.37 (Sect. 6.2).
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