Rapid-response mode VLT/UVES spectroscopy of super iron-rich gas exposed to GRB 080310 - Evidence of ionization in action and episodic star formation in the host

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Volume 545 (September 2012)

A&A, 545 (2012) A64

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Table A.1

Intervening systems: identified absorption lines.

z	v _host ^a	Transitions	W_rest^b (Å)
	(km s^-1)	λ (Å)	Lyα	C iv 1548	Mg ii 2796	Si ii 1526	Fe ii 2382

2.4200	650	Lyα, C iv 1548, 1550,^c	1.04 ± 0.01	0.05 ± 0.01	<0.05	<0.02	0.05 ± 0.01
		Fe ii 2382

2.4113	1411	Lyα, C iv 1548, 1550^c	0.70 ± 0.01	0.13 ± 0.02	c	<0.03	<0.02

2.2786	13 018	Lyα, C ii 1334, C ii* 1335,	1.62 ± 0.01 (≈ 18.7^d)	1.03 ± 0.02	0.07 ± 0.02	<0.02	<0.02
		C iv 1548, 1550,
		Mg ii 2796, 2803,
		Si ii 1260,^c Si iii 1206,
		Si iv 1393, 1402,
		Al ii 1670, Al iii 1854, 1862

2.1702	22 499	Lyα, C iv 1548, 1550	0.61 ± 0.01	0.07 ± 0.01	c	<0.02	<0.02

2.0685	31 395	Lyα, C iv 1548, 1550	1.22 ± 0.02 (≈ 18.4^d)	0.21 ± 0.01	–	<0.02	<0.02

1.6711	66 155	Lyα, C ii 1334, C ii* 1335,	<0.96	c	0.42 ± 0.01	0.13 ± 0.01	0.04 ± 0.01
		C iv 1548^c, 1550,
		Mg ii 2796, 2803,
		Al ii 1670, Al iii 1854, 1862,
		Si ii 1526, Si iv 1393, 1402,
		Fe ii 1608, 2344, 2382, 2600

1.1788	109 216	Si ii 1526,		<0.18	0.05 ± 0.01	0.24 ± 0.04	<0.04
		Mg ii 2796, 2803

Notes.

^(a)

Blue-shifted velocity with respect to the z = 2.42743 host-galaxy system.

^(b)

Rest W and 1σ error estimate, or 3σ upper limit for non-detections, measured in the highest S/N spectrum for each line. The assumed 2 × FWHM apertures correspond to a b-value of 20 km s^-1, which enabled us to cover each line (except for C iv 1548 at z = 2.41,2.27,2.06,1.67, where an aperture corresponding to b = 100 km s^-1 was necessary and b = 50 km s^-1 for Mg ii 2796 at z = 1.67 and C iv 1548 at z = 1.17).

^(c)

Blended with another line.

^(d)

log N(H i) estimate from the W, assuming a damped regime (N_Lyα [cm^-2] ≈ 1.87 × 10¹⁸ W² [Å] ).

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