Table 3.
Main absorption properties of extremely strong DLAs with VLT spectroscopic follow-up.
| Quasar | zQSO | zabs | log N(H I) | Inst. (a) | log N(H2) | [X/H] (b) | [Fe/Zn] (b) | AV(c) | Refs. |
|---|---|---|---|---|---|---|---|---|---|
| Homogeneous ESDLA sample: | |||||||||
| J0017+1307 | 2.594 | 2.326 | 21.62 ± 0.03 | XS | 18.3 | −1.50 ± 0.09 | −0.20 ± 0.09 | 0.36 (LMC2) | 1 |
| J0025+1145 | 2.961 | 2.304 | 21.92 ± 0.09 | XS | ∼20 | −0.53 ± 0.11 | −0.90 ± 0.12 | 0.51 (SMC) | 1 |
| J0154+1935 | 2.513 | 2.251 | 21.75 ± 0.15 | UVES | ∼18.0 | −0.72 ± 0.15 | −0.42 ± 0.03 | … | 2 |
| J0816+1446 | 3.846 | 3.287 | 22.00 ± 0.10 | UVES | 18.6 ± 0.4 | −1.10 ± 0.10 | −0.48 ± 0.02 | … | 3 |
| J1143+1420 | 2.583 | 2.323 | 21.64 ± 0.06 | XS | 18.3 ± 0.1 | −0.80 ± 0.06 | −0.54 ± 0.03 | 0.23 (SMC) | 1 |
| J1258+1212 | 3.055 | 2.444 | 21.90 ± 0.03 | XS | 18.3 | −1.43 ± 0.04 | −0.50 ± 0.04 | 0.04 (SMC) | 1 |
| J1349+0448 | 3.353 | 2.482 | 21.80 ± 0.01 | XS | 18.1 | −1.35 ± 0.06 | −0.34 ± 0.08 | 0.07(SMC) | 1 |
| J1411+1229 | 2.713 | 2.545 | 21.83 ± 0.03 | XS | 15.9 | −1.59 ± 0.08 | −0.34 ± 0.11 | 0.09 (SMC) | 1 |
| J1456+1609 | 3.683 | 3.352 | 21.70 ± 0.10 | UVES | 17.10 ± 0.09 | −1.39 ± 0.11 | −0.40 ± 0.07 | … | 2 |
| J1513+0352 | 2.680 | 2.464 | 21.83 ± 0.01 | XS | 21.31 ± 0.01 | −0.84 ± 0.23 | −1.22 ± 0.23 | 0.43 (LMC) | 4 |
| J2140−0321 | 2.479 | 2.339 | 22.41 ± 0.03 | XS/UVES | 20.13 ± 0.07 (d) | −1.52 ± 0.08 | −0.70 ± 0.10 | 0.12 (SMC) | 1,2 |
| J2232+1242 | 2.299 | 2.230 | 21.75 ± 0.03 | XS | 18.56 ± 0.02 | −1.48 ± 0.05 | −0.21 ± 0.04 | 0.01 (SMC) | 1 |
| J2246+1328 | 2.514 | 2.215 | 21.73 ± 0.03 | XS | 16.3 | −1.82 ± 0.63 | −0.17 ± 0.64 | <0.1 (f) | 1 |
| J2322+0033 | 2.693 | 2.477 | 21.58 ± 0.03 | XS | 16.0 | −1.71 ± 0.13 | −0.10 ± 0.14 | <0.1 (f) | 1 |
| Additional ESDLAs: | |||||||||
| HE0027−1836 | 2.560 | 2.402 | 21.75 ± 0.10 | UVES | 17.43 ± 0.02 | −1.59 ± 0.10 | −0.67 ± 0.03 | … | 5,6 |
| Q0458−0203 | 2.290 | 2.040 | 21.70 ± 0.10 | UVES | 14.9 | −1.26 ± 0.10 | −0.67 ± 0.04 | … | 7 |
| J0843+0221 | 2.920 | 2.786 | 21.82 ± 0.11 | UVES | 21.21 ± 0.02 | −1.59 ± 0.10 | −0.91 ± 0.13 | 0.09 (SMC) | 8 |
| J1135−0010 | 2.890 | 2.207 | 22.10 ± 0.05 | XS/UVES | NA (e) | −1.13 ± 0.05 | −0.61 ± 0.03 | 0.11 (SMC) | 9 |
| Q1157+0128 | 1.990 | 1.944 | 21.80 ± 0.10 | UVES | 14.7 | −1.40 ± 0.10 | −0.41 ± 0.01 | … | 7 |
Notes.
Metallicities and depletion factors from the literature have been corrected to use our adopted solar abundances.
Extinction measurements are available for systems observed with X-shooter only, except for J0843+0221, for which an estimate has been obtained directly from the SDSS spectrum (Balashev et al. 2017). The best-fit extinction law is indicated in parentheses. Uncertainties are dominated by systematics due to intrinsic quasar-shape variations and hence are all of the order of 0.1 mag.
UVES-based measurement from Noterdaeme et al. (2015a).
No H2 line is covered for this system due to the Lyman break of a system at higher redshift; see Noterdaeme et al. (2012) and Kulkarni et al. (2012).
These quasars are bluer than the composite spectrum (see Sect. 4.5).
References. (1) This work; (2) Noterdaeme et al. (2015a); (3) Guimarães et al. (2012); (4) Ranjan et al. (2018); (5) Noterdaeme et al. (2007); (6) Rahmani et al. (2013); (7) Noterdaeme et al. (2008); (8) Balashev et al. (2017); (9) Noterdaeme et al. (2012).
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