Table 2.
Correlations between absorbers’ properties and Lyα luminosity of isolated LAEs and groups.
| Line | LAEs | Wr (Å) | Δv90 (km s−1) |
|---|---|---|---|
| Mg II | Closest | ρ = 0.43 p = 0.05 | ρ = 0.34 p = 0.31 |
| Brightest | ρ = 0.54 p = 0.03 | ρ = 0.04 p = 0.89 | |
| Full | ρ = 0.06 p = 0.72 | ρ = 0.47 p = 0.64 | |
| Isolated | ρ = 0.89 p = 0.02 | ρ = 0.31 p = 0.54 | |
| C IV | Closest | ρ = 0.43 p = 0.01 | ρ = 0.42 p = 0.01 |
| Brightest | ρ = 0.33 p = 0.06 | ρ = 0.33 p = 0.06 | |
| Full | ρ = 0.26 p = 0.01 | ρ = 0.29 p = 0.01 | |
| Isolated | ρ = 0.16 p = 0.33 | ρ = 0.01 p = 0.95 | |
Notes. Results of the Spearman’s test on the correlation between the rest-frame equivalent width and the kinematics, traced by the width in velocity space, of the Mg II and C IV absorbers and the Lyα luminosity of isolated galaxies and groups. In the case of multiple galaxies connected to the same absorber, we consider the full sample, the brightest, or the closest member only.
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