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Table 1

Dust-to-metal ratios normalized by the Galactic value () derived with the method described in this paper and Savaglio’s (2001, S01).

GRB z A V log  [X/H]a [X/Fe] X [X/H]totb log c log Z/Z⊙d Je
(mag) N(H i) (new) N(Fe)dust (S01)
990123 1.60  < 0.25 2.01 ± 0.18 Zn 1.12 ± 0.00 all
000926 2.04 0.38 ± 0.05 21.30 ± 0.20  −0.11 ± 0.21 1.06 ± 0.21 Zn 1.06 ± 0.04 D
010222 1.48 1.30 ± 0.17 Zn 1.09 ± 0.02 H
020813 1.25 0.90 ± 0.07 Zn 1.02 ± 0.03 D
030226 1.99 0.05 ± 0.01 20.50 ± 0.30  −0.94 ± 0.30 0.17 ± 0.04 Si 0.47 ± 0.09 DW
030226s2f 1.96 0.05 ± 0.01 20.50 ± 0.30  −1.04 ± 0.30 0.45 ± 0.03 Si 0.86 ± 0.06 DW
030323 3.37 21.90 ± 0.07  −1.26 ± 0.27 0.18 ± 0.27 Si 0.49 ± 0.43  < 16.46 HDW
050401 2.90 0.45 ± 0.03 22.60 ± 0.30  −0.93 ± 0.42 1.14 ± 0.36 Zn 1.07 ± 0.05 H
050730 3.97  < 0.17 22.10 ± 0.10  −2.14 ± 0.10 0.12 ± 0.05 Si 0.36 ± 0.12 HWC
050820A 2.62 0.27 ± 0.04 21.05 ± 0.10  −0.72 ± 0.10 0.98 ± 0.12 Zn 1.04 ± 0.03 HWC
050922C 2.20 21.55 ± 0.10  −2.09 ± 0.12 0.35 ± 0.27 Si 0.76 ± 0.24 DW
051111 1.55 0.99 ± 0.04 Zn 1.04 ± 0.02 all
060418 1.49 0.71 ± 0.03 Zn 0.95 ± 0.04 D
070802 2.45 21.50 ± 0.20  −0.16 ± 0.24 0.37 ± 0.18 Zn 0.70 ± 0.19 C
071031 2.69  < 0.11 22.15 ± 0.05  −1.76 ± 0.05 0.03 ± 0.03 Zn 0.08 ± 0.07 all
080330 1.51  < 0.19 0.93 ± 0.11 Zn 1.03 ± 0.04 all
080413A 2.43  < 0.88 21.85 ± 0.15  −1.63 ± 0.16 0.12 ± 0.07 Zn 0.30 ± 0.14 HWC
090323s1f 3.58 0.10 ± 0.04 19.62 ± 0.33  + 0.33 ± 0.35 0.51 ± 0.14 Si 0.91 ± 0.10 D
090323s2f 3.57 0.10 ± 0.04 20.72 ± 0.09  + 0.22 ± 0.10 1.41 ± 0.06 Zn 1.10 ± 0.01 H
090926A 2.11  < 0.15 21.73 ± 0.07  −2.27 ± 0.27 0.57 ± 0.30 Si 0.94 ± 0.16 HDW

Notes. Uncertainties refer to a 1σ confidence level, while 3σ limits are reported for unconstrained measurements.

(a)

Observed abundance of the element X relative to solar.

(b)

Abundances corrected for dust depletion. When available, [Zn/H]tot is considered to be the metallicity of the gas.

(c)

Column density of iron in dust-phase (see text).

(d)

Metallicity as fitted with the S01 method (Eq. (1)), when H is unconstrained and Zn constrained.

(e)

Galactic environments fitted with the S01 method: halo (H), disk + halo (D), warm disk (W) and cool disk (C), as characterized by Savage & Sembach (1996). When more than one environment is possible, (S01) and log Z/Z⊙ are averaged among the allowed values.

(f)

Different absorbing systems toward the same GRB are reported separately.

References. All column densities, z and AV are taken from the compilation by Schady et al. (2011).

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