Massive stars formed in atomic hydrogen reservoirs: H I observations of gamma-ray burst host galaxies

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Table 1

Properties of our sample of GRB hosts.

GRB	z_opt	Ref.	SFR_IR/Rad	Ref.	SFR_UV	Ref.	log (M_∗/M_⊙)	Ref.	log (M_d/M_⊙)	Ref.	log (M_H₂/M_⊙) ^a	Ref.	Met	Ref.
			(M_⊙yr^-1)		(M_⊙yr^-1)

980425	0.0085	1	0.26	7	0.14	9	8.68	7	6.57	7	<8.05	12	8.60	13
031203	0.1050	2	2.8	8	2.4	10	9.47	10	<8.00^d	8	···	···	8.27	14
060505	0.0889	3	0.69	‡	1.1	10	9.64	11	···	···	···	···	8.30	11
100316D	0.0591	4,5	1.7	‡	0.30^b	5	8.93^c	‡	···	···	···	···	8.30	15
111005A	0.0133	‡,6	0.42	‡	0.16^b	‡	9.68	‡	6.57	‡	···	···	8.70	16

Notes. Unless otherwise stated, the properties are adopted from the references given in the Ref columns. The metallicities are 12 + O/H, where the solar value is 8.69 (Asplund et al. 2004).

^(a)

Converted to the CO-to-H₂ factor of α_CO = 5.

^(b)

We calculated the SFR from the ultraviolet flux using the conversion of Kennicutt (1998a).

^(c)

We calculated the stellar mass from ultraviolet, optical and near-infrared fluxes reported in Starling et al. (2011), Cano et al. (2011) and Olivares E. et al. (2012) using Grasil (see Sect. 2).

^(d)

We calculated the dust mass using the submm flux limit and assuming T_d = 30 K and β = 1.5.

Reference. ‡: this work, 1) Tinney et al. (1998)2) Prochaska et al. (2004)3) Ofek et al. (2006)4) Vergani et al. (2010)5) Starling et al. (2011)6) Levan et al. (2011)7) Michałowski et al. (2014b)8) Watson et al. (2011)9) Michałowski et al. (2009)10) Castro Cerón et al. (2010)11) Thöne et al. (2008)12) Hatsukade et al. (2007)13) Sollerman et al. (2005)14) Levesque et al. (2010a)15) Levesque et al. (2011) 16) Michałowski et al. (in prep.)

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