Galaxy counterparts of intervening high-z sub-DLAs/DLAs and Mg ii absorbers towards gamma-ray bursts

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Volume 546 (October 2012)

A&A, 546 (2012) A20

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Table 2

Properties of the intervening sub-DLAs and DLAs.

GRB	z _GRB	z _abs		[Si/H]	EW_rest(Si ii λ1526)	Detected lines	References
GRB	z _GRB	z _abs		[Si/H]	(Å)	Detected lines	References

050730	3.969	3.56439	20.3 ± 0.1	<–1.3	<1.01^a	Al ii, Fe ii, Si ii, Si ii^∗, C iv, Si iv	1, 2, 3
050730	3.969	3.02209	19.9 ± 0.1	− 1.5 ± 0.2^b	...	Al ii, Fe ii, Si ii	1, 2, 3
050820A	2.615	2.3598^c	20.1 ± 0.2	–1.5 ± 0.2	0.17 ± 0.01^d	Fe ii, Si ii, C iv, Mg ii	4
050908	3.3467	2.6208	20.8 ± 0.1^d^e	>–1.40^d	2.24 ± 0.06	Al ii, Fe ii, Si ii, C iv	2
070721B	3.6298	3.0939^g	20.1 ± 0.3^d^e	>–0.66^d	2.35 ± 0.69^d	Al ii, Fe ii, Si ii, C iv	2

Notes.

^(a)

This line is blended. The EW listed is the value of the blend.

^(b)

Without ionisation correction.

^(c)

Vergani et al. (2009) reported EW_rest(Mg ii λ2796) < 0.42 Å with a most likely value of 0.31 Å.

^(d)

This work.

^(e)

Fynbo et al. (2009) suggested that the absorber is a sub-DLA.

^(f)

Derived in the optically thin limit.

^(g)

Chen et al. (2009) and Fynbo et al. (2009) proposed that a galaxy 09 SE of the afterglow position is the galaxy counterpart to the intervening absorber.

References. (1) Chen et al. (2005); (2) Fynbo et al. (2009); (3) Starling et al. (2005); (4) Vergani et al. (2009).

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