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 | ![]() |
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 former analysis of the Magellan Clay/MIKE echelle spectrum (Chen et al. 2005) suggested a cloud distance d < 100 pc (Prochaska et al. 2006).
We consider the 090426 Lyα variation detection to be marginal and conservatively list this distance estimate as a lower limit.
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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