Cold gas in the early Universe - Survey for neutral atomic-carbon in GRB host galaxies at 1 < z< 6 from optical afterglow spectroscopy

K. E. Heintz; C. Ledoux; J. P. U. Fynbo; P. Jakobsson; P. Noterdaeme; J.-K. Krogager; J. Bolmer; P. Møller; S. D. Vergani; D. Watson; T. Zafar; A. De Cia; N. R. Tanvir; D. B. Malesani; J. Japelj; S. Covino; L. Kaper

doi:10.1051/0004-6361/201834246

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Volume 621 (January 2019)

A&A, 621 (2019) A20

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Table 1.

GRB afterglow sample properties.

GRB	z_GRB	log N(H I) (cm⁻²)	W_r (λ 1560) (Å)	W_r (λ 1656) (Å)	[X/H]	Ion	A_V (mag)	Refs.
F09 sample

050730	3.9693	22.10 ± 0.10	< 0.03	< 0.03	−2.18 ± 0.11	S	0.12 ± 0.02	(1, 2)
050820A	2.6147	21.05 ± 0.10	< 0.12	< 0.13	−0.39 ± 0.10	Zn	0.27 ± 0.04	(3, 4)
050922C	2.1995	21.55 ± 0.10	< 0.03	< 0.03	−1.82 ± 0.11	S	0.09 ± 0.03	(3, 5)
060210	3.9133	21.55 ± 0.15	0.78 ± 0.03	⋯	> − 0.83	Si	0.57 ± 0.08	(6, 5)
060607A	3.0749	16.95 ± 0.03	< 0.05	< 0.07	⋯	⋯	0.08 ± 0.08	(7, 8)
061121	1.3145	⋯	0.49 ± 0.04	0.25 ± 0.04	⋯	⋯	0.55 ± 0.10	(5)
070802^b	2.4511	21.50 ± 0.20	0.70 ± 0.35	1.36 ± 0.32	−0.46 ± 0.63	Zn	1.19 ± 0.15	(9, 2)
071031	2.6918	22.15 ± 0.05	< 0.03	< 0.03	−1.73 ± 0.05	Zn	< 0.07	(3, 2)
080310	2.4274	18.70 ± 0.10	< 0.11	< 0.14	−1.20 ± 0.20	Si	0.19 ± 0.05	(10, 8)
080413A	2.4330	21.85 ± 0.15	< 0.03	< 0.03	−1.60 ± 0.16	Zn	< 0.59	(3, 11)
080605^b	1.6403	⋯	0.64 ± 0.23	0.38 ± 0.15	⋯	⋯	0.50 ± 0.13	(12)
080607^a,^b	3.0368	22.70 ± 0.15	2.17 ± 0.08	2.03 ± 0.04	> − 0.20	O	2.33 ± 0.46	(13, 2)

X-shooter sample

090926A	2.1069	21.60 ± 0.07	< 0.05	< 0.06	−1.85 ± 0.10	S	< 0.04	(14, 15)
100814A	1.4390	⋯	< 0.06	< 0.06	⋯	⋯	< 0.07	(15)
120119A	1.7288	22.44 ± 0.12	0.51 ± 0.05	0.77 ± 0.06	−0.96 ± 0.28	Zn	1.02 ± 0.11	(16, 15)
120327A^a	2.8148	22.01 ± 0.09	< 0.03	< 0.03	−1.17 ± 0.11	Zn	< 0.03	(17)
120815A^a	2.3581	21.95 ± 0.10	(0.12 ± 0.08)^c	(0.21 ± 0.05)^c	−1.15 ± 0.12	Zn	0.19 ± 0.04	(18, 15)
121024A^a	2.3024	21.88 ± 0.10	(0.08 ± 0.05)^c	(0.11 ± 0.07)^c	−0.70 ± 0.10	Zn	0.26 ± 0.07	(19, 15)
130408A	3.7579	21.70 ± 0.10	< 0.05	< 0.06	−1.24 ± 0.12	S	0.21 ± 0.05	(6, 20)
130606A	5.9129	19.91 ± 0.02	< 0.10	< 0.10	−1.30 ± 0.08	Si	< 0.07	(21, 15)
141028A	2.3334	20.55 ± 0.07	< 0.14	< 0.21	−0.73 ± 0.34	Zn	0.13 ± 0.09	(16)
141109A	2.9944	22.10 ± 0.20	< 0.11	< 0.11	−1.40 ± 0.22	Zn	0.11 ± 0.03^d	(22, 23)
150403A	2.0571	21.80 ± 0.20	0.34 ± 0.03	0.50 ± 0.04	−0.80 ± 0.35	S	0.12 ± 0.02^d	(22, 23)
151021A	2.3299	22.20 ± 0.20	< 0.17	< 0.28	−1.11 ± 0.20	Si	0.20 ± 0.03^d	(22, 23)
151027B	4.0647	20.50 ± 0.20	< 0.09	< 0.09	−1.62 ± 0.24	Si	0.10 ± 0.05	(22, 23, 20)
160203A	3.5185	21.75 ± 0.10	< 0.03	< 0.03	−1.26 ± 0.11	S	< 0.10^d	(24)
161023A	2.7106	20.97 ± 0.01	< 0.03	< 0.03	−1.11 ± 0.07	Zn	0.09 ± 0.03	(25)
170202A	3.6450	21.55 ± 0.10	< 0.10	< 0.08	−1.15 ± 0.13	S	< 0.12	(22, 23, 20)

180325A^b	2.2486	22.30 ± 0.14	0.58 ± 0.05	0.85 ± 0.05	> − 0.98	Zn	1.58 ± 0.12	(26)

Notes. All GRB afterglows with spectral coverage of the C Iλλ 1560,1656 line transitions listed here are selected within a completeness limit of W_r(λ 1560)> 0.2 Å. GRB 180325A is listed separately since it is not part of the F09 or XS–GRB sample papers.

^(a)

GRB afterglows where a detection of H₂ in absorption has been reported in the literature.

^(b)

Bursts with a prominent detection of the 2175 Å dust extinction feature.

^(c)

Tentative detection of C I below the imposed detection threshold.

^(d)

A_V measurements from this work.

References. The H I column densities, metallicities and visual extinctions are from: (1) D’Elia et al. (2007); (2) Zafar et al. (2011a); (3) Ledoux et al. (2009); (4) Schady et al. (2012); (5) Covino et al. (2013); (6) Cucchiara et al. (2015); (7) Fynbo et al. (2009); (8) Kann et al. (2010); (9) Elíasdóttir et al. (2009); (10) De Cia et al. (2012); (11) Zafar & Watson (2013); (12) Zafar et al. (2012); (13) Prochaska et al. (2009); (14) D’Elia et al. (2010); (15) Zafar et al. (2018c); (16) Wiseman et al. (2017); (17) D’Elia et al. (2014); (18) Krühler et al. (2013); (19) Friis et al. (2015); (20) Zafar et al. (2018b); (21) Hartoog et al. (2015); (22) Selsing et al. (2018); (23) Thöne et al. (in prep.); (24) Pugliese et al. (in prep.); (25) de Ugarte Postigo et al. (2018); (26) Zafar et al. (2018a).

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