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Table 4

GRB absorber distances, as of April 2012.

GRB Instrument z Distance Size Pa log N(H i) [X/H] X Ref.
(pc) (pc)

020813 LRIS+UVES 1.25 50–100 1, 2
050730 UVES 3.97 124 ± 20b E 22.10 ± 0.10 −2.18 ± 0.11 S 3, 4
051111 HIRES 1.55 a few hundred E 5, 6
060418 UVES 1.49 480 ± 56 E  >21.0  <−0.5 Zn 7, 4
080310 UVES 2.43 200–400 0–200 E+I 18.70 ± 0.10 −1.2 ± 0.2 Si 8, 9
080319B UVES 0.94 560–1700 E 10, 4
080330 UVES 1.51 E 11, 4
081008 UVES+FORS 1.97 52 ± 6c E 21.11 ± 0.10 −0.87 ± 0.10 Si 12
090426 LRIS+FORS 2.61 80d I 13
090926 X-shooter 2.11 677 ± 42e E 21.60 ± 0.07 −1.85 ± 0.10 S 14, 4

Notes. Distances derived from a photo-excitation/photo-ionization model of the column density variability, based on high-resolution spectroscopy, highlighted in bold, are considered to be more reliable. The excitation distances have been corrected for according to Vreeswijk et al. (2011).

(a)

Process modelled: photo-excitation (E) or photo-ionization (I).

(b)

A former analysis of the Magellan Clay/MIKE echelle spectrum (Chen et al. 2005) suggested a cloud distance d < 100 pc (Prochaska et al. 2006).

(c)

Component I (Component II lies at pc).

(d)

We consider the 090426 Lyα variation detection to be marginal and conservatively list this distance estimate as a lower limit.

(e)

Main component (the second lies at  ~5 kpc).

References. (1) Dessauges-Zavadsky et al. (2006); (2) Savaglio & Fall (2004); (3) Ledoux et al. (2009); (4) Vreeswijk et al. (2011); (5) Penprase et al. (2006); (6) Prochaska et al. (2006); (7) Vreeswijk et al. (2007); (8) This work; (9) Paper I: De Cia et al. (2012); (10) D’Elia et al. (2009a); (11) D’Elia et al. (2009b); (12) D’Elia et al. (2011); (13) Thöne et al. (2011); (14) D’Elia et al. (2010).

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