Table 4.
Resulting parameters for our sample of absorbing galaxies.
| Quasar field | Host-galaxy identifiers |
Modelled parameter |
||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| θ⋆ (") | b (kpc) |  |
 |
log10[M⋆ (M⊙)] | SFR[O II] (M⊙ yr−1) | SFRHβ (M⊙ yr−1) | σ (km s−1) | [O/H] (dex) | [M/H]em (dex) | |||
| (mag) SED | (mag) BDEC | (mag) SFR | ||||||||||
| HE 1122-1649 | 3.6a | 25.6 | 0.68249(3) | 0.11 | – |  |
 |
1.68 ± 0.23 | 1.55 ± 0.19 |  |
 † |
−0.84 ± 0.05 |
| Q 0153+0009 | 4.9b | 36.6 | 0.77085(3) | 0.00 |  |
– |  |
– | 16.14 ± 1.54 |  |
 †† |
0.04 ± 0.20 |
| Q 1209+107 PA2 | 7.2b | 38.3 | 0.39238(1) | 0.68 |  |
≤0 |  |
3.20 ± 0.12 | 3.34 ± 0.09 |  |
∼8.05‡ | 0.30 ± 0.20 |
| Q 1323–0021 | 1.4b | 10.2 | 0.71717(8) | 0.68 | – | – |  § |
0.27 ± 0.03 | – |  |
– | 0.62 ± 0.35 |
| Q 1436–0051 | 6.2c | 45.5 | 0.73749(3) | 0.68 | – | ≤0 |  |
1.02 ± 0.07⋆⋆ | 0.48 ± 0.10 |  |
 †† |
0.21 ± 0.12 |
| Q 1436–0051 | 4.4b | 34.9 | 0.92886(2) | 1.02 | – | – |  |
– | – |  |
– | 0.21 ± 0.55 |
| Q 2328+0022 | 1.7b | 11.9 | 0.65194(6) | 0.00 | – | – |  |
0.47 ± 0.05 | – |  |
– | −0.23 ± 0.22 |
| Q 2335+1501 | 3.8d | 27.0 | 0.67989(2) | 1.36 | – |  |
 |
4.47 ± 0.17 | 6.31 ± 2.51 |  |
 † |
0.33 ± 0.34 |
Notes. Values for 
refer to the heliocentric rest-frame corrected measurement, with the bracket notation reflecting the uncertainty in the profile-fit. θ is the angular separation between quasar and host, measured in arcsec from known photometry. θ is translated into an impact parameter (b) measured in kpc using the the spectroscopically determined emission-line redshift and the assumed cosmology. 
refers to the nebular extinctions (SED, BDEC, SFR) derived from the χ2-minimising SED solution; the Balmer decrement; and based on the ratio of the SFR in Hα and [O II] under the assumption that they trace similar time-scales, respectively. Stellar mass estimates were determined from the maximum likelihood analysis of the SEDs χ2-distributions. The star-formation rate estimates were corrected for intrinsic and Galactic extinction, and were converted to a Chabrier IMF. σ corresponds to the velocity dispersion based on the profile fits to the emission lines after resolution correction using Eq. (1), and [O/H] to the preferred oxygen abundance derived from emission line ratios according to the M 08 prescriptions. [M/H]em refers to the metallicity in emission, inferred by applying a correction factor and truncation radius to the absorption metallicity.
Upper limit on EB−V imposed from dust-content priors (Sect. 3.6).
References.
this work, based on Rao et al. (2011) K-band image (Sect. 2.4);
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