A simple model of dust extinction in gamma-ray burst host galaxies

Open Access

Table A.1.

The 38 GRBs analyzed in this paper.

GRB	z	A_V, Gal (mag)	N_{H_tot, Gal} (10²¹ cm⁻²)	Optical/NIR bandpasses	Epoch (h)	best-fit model afterglow/ext. curve	A_V, host (mag)
150301B	1.517	0.210	0.640	g’r’i’z’JH	5.000	-	-
090102	1.547	0.125	0.463	g’r’i’z’JHK_s	3.090	bknpow/MW¹	0.41±0.03
080605	1.640	0.365	1.030	g’r’i’z’JHK_s	2.785	pow/FM90²	0.50 $_{- 0.10}^{+ 0.12}$ $^{+0.12}_{-0.10}$
191011A	1.722	0.043	0.143	g’r’i’z’JHK_s	0.100	SMC³	0.43±0.03
120119A	1.728	0.296	1.035	g’r’i’z’JHK_s	0.058	pow/FM07⁴	1.02±0.11
121027A	1.773	0.053	0.162	g’r’i’z’JH	49.200	pow/SMC⁵	1.1
080514B	1.800	0.151	0.425	g’r’i’z’JHK_s	21.768	SMC^† ⁶	≤0.14
170113A	1.968	0.304	1.079	g’r’i’z’JH	372.004	SMC^† ⁷	0.00 $_{- 0.00}^{+ 0.00}$ $^{+0.00}_{-0.00}$
081230	2.000	0.038	0.155	g’r’i’z’JHK_s	5.44	SMC⁸	0.22 $_{- 0.08}^{+ 0.14}$ $^{+0.14}_{-0.08}$
150206A	2.087	0.042	0.185	g’r’i’z’J	10.300	-	-
180325A	2.248	0.046	0.126	g’r’i’z’JHK_s	1.626	pow/FM90⁹	1.58 $_{- 0.12}^{+ 0.10}$ $^{+0.10}_{-0.12}$
121024A	2.298	0.272	0.702	g’r’i’z’JHK_s	29.722	pow/SMC¹⁰	0.18±0.04
120815A	2.358	0.308	1.168	g’r’i’z’JHK_s	2.163	bknpow/SMC¹¹	0.32 $_{- 0.02}^{+ 0.02}$ $^{+0.02}_{-0.02}$
070802	2.450	0.071	0.265	g’r’i’z’JHK_s	0.708	pow/FM86¹²	0.8-1.5
090812	2.452	0.064	0.213	g’r’i’z’J	2.183	bknpow/SMC¹³	0.23 $_{- 0.06}^{+ 0.08}$ $^{+0.08}_{-0.06}$
081121	2.512	0.136	0.420	g’r’i’z’JHK_s	3.945	bknpow/SMC¹	0.07 $_{- 0.01}^{+ 0.01}$ $^{+0.01}_{-0.01}$
081118	2.580	0.118	0.396	g’r’i’z’JHK_s	10.93	-	-
090426	2.609	0.045	0.150	g’r’i’z’JH	12.852	pow/SMC^† ¹⁴	0.0
080210	2.641	0.217	0.693	g’r’i’z’JHK_s	1.001	bknpow/SMC¹⁵	0.18±0.03
161023A	2.708	0.091	0.291	g’r’i’z’JHK_s	27.249	pow/SMC¹⁶	0.09±0.03
110731A	2.830	0.480	1.510	g’r’i’z’JH	65.7696	pow/SMC¹⁷	0.24±0.06
120404A	2.876	0.131	0.392	g’r’i’z’JH	19.451	pow/MW¹⁸	0.22±0.05
081028	3.038	0.093	0.452	g’r’i’z’J	31.300	SMC¹⁹	< 0.22
120922A	3.100	0.396	1.152	g’r’i’z’JHK_s	1.500	-	-
081228	3.440	0.431	1.269	r’i’z’JHK_s	0.719	pow/SMC²⁰	0.12 $_{- 0.08}^{+ 0.06}$ $^{+0.06}_{-0.08}$
160203A	3.520	0.187	0.725	g’r’i’z’JHK_s	0.154	FM90²¹	< 0.10
081029	3.848	0.082	0.293	g’r’i’z’JHK_s	5.823	pow/SMC^† ²²	0.03 $_{- 0.03}^{+ 0.02}$ $^{+0.02}_{-0.03}$
131117A	4.042	0.050	0.134	g’r’i’z’JHK_s	0.102	bknpow/FM90⁴	< 0.11
090516	4.109	0.134	0.536	g’r’i’z’JHK_s	14.803	pow/SMC²³	0.19 $_{- 0.03}^{+ 0.03}$ $^{+0.03}_{-0.03}$
120712A	4.175	0.112	0.389	g’r’i’z’JHK_s	9.582	bknpow/SMC²³	0.08 $_{- 0.08}^{+ 0.03}$ $^{+0.03}_{-0.08}$
140614A	4.233	0.330	1.148	r’i’z’JHK_s	0.647	bknpow/SMC²³	0.11 $_{- 0.05}^{+ 0.17}$ $^{+0.17}_{-0.05}$
151112A	4.270	0.036	0.149	r’i’z’JHK_s	11.397	bknpow/LMC²³	0.50 $_{- 0.11}^{+ 0.21}$ $^{+0.21}_{-0.11}$
090205A	4.650	0.312	1.012	r’i’z’JHK_s	6.485	pow/LMC²³	0.14 $_{- 0.05}^{+ 0.04}$ $^{+0.04}_{-0.05}$
100219A	4.667	0.203	0.791	r’i’z’JHK_s	9.513	pow/SMC²⁴	0.24±0.06
140428A	4.680	0.026	0.095	r’i’z’JHK_s	2.601	bknpow/SMC²³	0.30 $_{- 0.23}^{+ 0.32}$ $^{+0.32}_{-0.23}$
140311A	4.954	0.099	0.235	r’i’z’JHK_s	9.339	pow/SMC²³	0.07 $_{- 0.03}^{+ 0.03}$ $^{+0.03}_{-0.03}$
111008A	4.990	0.014	0.084	r’i’z’JHK_s	6.848	bknpow/FM90⁴	0.12±0.04
130606A	5.931	0.064	0.214	r’i’z’JHK_s	8.370	pow/FM90⁴	< 0.07

Notes: Columns 7-8 are the best-fit models found in the literature for each GRB with the corresponding total amount of extinction in the V-band. When different sources are found, spectroscopic studies are preferred. For analysis with only optical data, the shape of the SED, whether fit with a broken power law or a power law, is not indicated. ^† SMC law was assumed since the different extinction laws could not be distinguished.

¹Schady et al. (2012a); ²Zafar et al. (2012); ³Heintz et al. (2023)²⁰; ⁴Zafar et al. (2018b); ⁵Nakauchi et al. (2013); ⁶Rossi et al. (2008); ⁷Gompertz et al. (2018); ⁷Krühler et al. (2011); ⁹Zafar et al. (2018a); ¹⁰Varela et al. (2016); ¹¹Japelj et al. (2015); ¹²Zafar et al. (2011); ¹³Covino et al. (2013); ¹⁴Nicuesa Guelbenzu et al. (2011); ¹⁵De Cia et al. (2011); ¹⁶de Ugarte Postigo et al. (2018); ¹⁷Ackermann et al. (2013); ¹⁸Guidorzi et al. (2014); ¹⁹Margutti et al. (2010); ²⁰Greiner et al. (2011); ²¹Heintz et al. (2019); ²²Nardini et al. (2011); ²³Bolmer et al. (2018); ²⁴Thöne et al. (2013)

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