Probing dust-obscured star formation in the most massive gamma-ray burst host galaxies

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Table 3

Physical parameters of GRB host galaxies: the first block is our observed sample; the second block is taken from the literature (upper limits are only included if they are not more than a factor 100 above SFR_opt.

GRB	z	log(M_⋆)	Z/Z_⊙	SFR_UV	SFR_OII	SFR_Hα	SFR_Radio ^b)
		M_⊙		M_⊙/yr	M_⊙/yr	M_⊙/yr	M_⊙/yr

000210	0.846	9.31 ± 0.08		2.1 ± 0.2	≈3		<86
020127	1.9ph	11.51 ± 0.20	0.5–1.0	≈6			<1380
020819B	0.41	10.50 ± 0.14	≈1	6.9		10.2	20.2 ± 5.2
030528	0.782	10.3	0.1–0.6	4–17	6–37		<58
050219	0.211	9.98		<0.1	0.06		<7
080319C	1.95	≪12.22					<976
080605	1.640	9.9 ± 0.1	0.6	49	55	47	<821
081109	0.979	9.82 ± 0.09	1.17 ± 0.24	33	40	11.8	<114
090113	1.749	10.6				18	<266
090926B	1.24	10.1	0.45 ± 0.18	80		26	<171
100621A	0.542	8.98	0.68 ± 0.17	13		8.7 ± 0.8	<30
110918A	0.982	10.68 ± 0.16	≈1			41	<84
970228	0.695	8.65 ± 0.05 (1)			0.53 (1)		<72 (2) [<58]
980425	0.008	9.21 ± 0.52 (1)			0.19 (1)	0.21 (1)	0.23 ± 0.02 (2) [0.10 ± 0.01]
980703	0.967	10.00 ± 0.15 (1)	0.6 (1)				750 ± 180 (3) [187 ± 18]
990705	0.842	10.20 ± 0.76 (1)		3.31 (8)	6.96 (1)		<23 (9) [<46]
990712	0.433	9.29 ± 0.02 (1)		0.76 (1)	3.01 (1)	2.39 (1)	<10.1 (5) [<28]
991208	0.706	8.53 ± 0.37 (1)			4.52 (1)		<35 (2) [<29]
000418	1.119	9.26 ± 0.14 (1)					330 ± 75 (4) [268 ± 58]
000911	1.058	9.32 ± 0.26 (1)			1.57 (1)		<608 (2) [<490]
010222	1.477	8.82 ± 0.26 (1)					300 ± 115 (4) [<296]
010921	0.451	9.69 ± 0.13 (1)			4.26 (1)	2.5 (1)	<32 (2) [<26]
011121	0.360	9.81 ± 0.17 (1)			2.65 (1)	2.24 (1)	<68 (2) [<55]
020405	0.691	9.75 ± 0.25 (1)			3.74 (1)		<165 (2) [<133]
020903	0.251	8.87 ± 0.07 (1)			2.51 (1)	2.65	<5.4 (2) [<4.3]
021211	1.006	10.23 ± 0.63 (1)				3.1 (6)	825 ± 77 (2) [998 ± 94] ^c)
030329	0.168	7.74 ± 0.06 (1)			0.09 (1)	0.11 (1)	<17 (2) [<14]
031203	0.105	8.82 ± 0.43 (1)			4.08 (1)	12.68 (1)	4.8 (5) [11.1 ± 2.6]
040924	0.859	9.20 ± 0.37 (1)			1.88 (1)		<274 (2) [<221]
041006	0.716	8.66 ± 0.87 (1)			0.34 (1)		<27 (9) [<54]
050223	0.591	10.02 (7)		4.3 (8)	1.44 (1)		93 ± 31 (10) [217 ± 72]
050416A	0.654	9.17 ± 0.12 (11)	0.6 ± 0.3 (11)		2.5 ± 0.7 (12)	4.5 (13)	[<22]
050525A	0.606	8.1 ± 0.6 (11)				0.07 (13)	<53 (10) [<172] ^d)
050801	1.560						[<97]
050824	0.830	7.45 (8)	0.25 (13)			1.20 (13)	[<24]
050915	2.527						<1204 (2) [<985]
051006	1.059	10.11 ± 0.03 (14)		98 (14)			51 (14) [54 ± 19] ^e)
051016B	0.936	7.76 (8)	0.37 (13)			10.2 (13)	[<35]
051022	0.809	10.29 (7)	0.6 (13)	58.19 (1)	36.46 (1)	60 (13)	74 ± 20 (15) [60 ± 17] ^f)
051117B	0.481		2.0 (13)			4.7 (13)	[<10]
060218	0.033	7.78 ± 0.08 (1)		0.05 (8)	0.06 (1)	0.05 (1)	[<0.02]
060505	0.089	9.41 ± 0.01 (1)		1.1 (16)	0.74 (1)	0.43 (1)	0.69 ± 0.40 (17) [0.69 ± 0.40]
060614	0.125	7.95 ± 0.13 (1)				0.01 (1)	<2.4 (2) [<1.6]
060729	0.540	9.13 (18)				0.96 (13)	<60 (2) [<48] ^g)
060814	1.923	10.20 (14)		209 (14)		54 (13)	256 (14) [267 ± 74]
060912A	0.937	9.23 (11)	0.8 (13)			5.1 (13)	[<28]
061021	0.346	8.5 ± 0.5 (11)	0.5 ± 0.4 (11)			0.05 (13)	[<3]
061110A	0.758					0.23 (13)	[<33]
061121	1.314	10.18 (14)		27 (14)			160 (14) [168 ± 54]
070306	1.496	10.70 (14)		17 (14)		101 (13)	143 (14) [150 ± 38] ^h)
070318	0.836						<223 (2) [<180]
071003	1.604		0.7 (13)				< 83 (10) [<211]
080207	2.086	11.51 ± 0.11 (6)		46 (15)			846 ± 124 (15) [738 ± 108]
080413B	1.101		0.4 (13)			2.1 (13)	< 39 (10) [<95]
080517	0.089	9.58 (19)		0.43 ± 0.07 (19)		15.5 ± 0.4 (19)	7.6 ± 1.4 (19) [7.2 ± 1.3]
081007	0.529	8.78 (11)	0.6 ± 0.3 (11)			0.36 ± 0.07 (20)	< 35 (10) [<99]
090424	0.544	9.38 (11)	1.0 ± 0.3 (11)			2.88 ± 1.14 (20)	< 38 (10) [<110]
091208B	1.063						< 33 (10) [<78]
100316D	0.059	8.93 (17)		0.30 (17)			1.73 ± 0.08 (17) [1.73 ± 0.08]
100901A	1.408						< 42 (10) [<105]
111005A	0.013	9.68 (17)		0.16 (17)			0.08 ± 0.02 (17) [0.08 ± 0.02]

Notes.

^(a)

References are given between parentheses, except for the first block for which these are given in the Appendix, together with more extensive notes on the table entries. SFR values are always meant to be extinction corrected (thus the uncorrected SFR_UV values tabulated in Michałowski et al. (2012) are not included).

^(b)

The additional values in brackets for the literature sample are re-computed values from the original papers, or from Perley et al. (2015) who only provided flux limits for the radio non-detections.

^(c)

The upper limit of Hatsukade et al. (2012) is marginally inconsistent; see discussion in Michałowski et al. (2012).

^(d)

Perley et al. (2015) provides a substantially deeper limit of <10 M_⊙/yr.

^(e)

This is consistent with the upper limit of <38 M_⊙/yr of Perley et al. (2015).

^(f)

The <53 M_⊙/yr upper limit of Hatsukade et al. (2012) is marginally consistent, if the spectral slope is flatter than −0.75.

^(g)

Stanway et al. (2014) claim a 2σ detection with 55 ± 24 M_⊙/yr which translates to 128 ± 54 M_⊙/yr with our re-calculation, and is thus consistent with Michałowski et al. (2012).

^(h)

This detection is inconsistent with the upper limit of <77 M_⊙/yr of Perley et al. (2015) which we will use henceforth.

Reference. (1) Savaglio et al. (2009); (2) Michałowski et al. (2012); (3) Berger et al. (2001); (4) Berger et al. (2003); (5) Stanway et al. (2010); (6) Savaglio (2015); (7) Hunt et al. (2014); (8) Svensson et al. (2010); (9) Hatsukade et al. (2012); (10) Stanway et al. (2014); (11) Vergani et al. (2015); (12) Soderberg et al. (2007); (13) Krühler et al. (2015); (14) Perley et al. (2015); (15) Perley & Perley (2013); (16) Castro Ceron et al. (2010); (17) Michałowski et al. (2015); (18) Cano et al. (2011); (19) Stanway et al. (2015); (20) Japelj et al. (2016).

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