The dust extinction curves of gamma-ray burst host galaxies

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Table 1

The 49 GRBs chosen by our selection criteria to have well-sampled afterglow SEDs.

GRB	z	N_H,Gal	A_V,Gal	Epoch^†	UV/optical/NIR bandpasses	Rest-frame band	Best-fit model
		(10²¹ cm^-2)	(mag)	(ks)		coverage (Å)


050319	3.24^a	0.13	0.03	7	I¹²R¹²³v b	920–2090	bknp/MW
050525A	0.606^b	0.91	0.29	20	K⁴⁵H⁴J⁴⁶I⁴⁷R⁴⁸⁹v b u w1 m2 w2	1000–14 540	pow/SMC
050730	3.969^c	0.30	0.16	10	(KJIr)¹⁰v b	790–4700	pow/MW
050802	1.71^d	0.19	0.06	2	v b u w1 m2 w2	590–2160	pow/MW
050820A	2.615^e	0.44	0.14	10	J¹¹(zIRg)¹²v b u w1	620–3710	bknp/LMC
050922C	2.198^f	0.54	0.32	5	R¹³¹⁴¹⁵¹⁶¹⁷¹⁸v b u w1	710–2360	pow/MW
060206	4.048^g	0.09	0.04	20	(KHJ)¹⁹R²⁰²¹²²v b	770–4630	bknp/MW
060418	1.49^h	0.88	0.69	5	(KHJ)²³z²³²⁴I²⁵R²⁶v b u w1 m2 w2	640–9380	bknp/SMC
060502A	1.51ⁱ	0.35	0.10	5	R²⁷v b u w1	900–3010	pow/SMC
060512	2.1^j	0.15	0.05	5	Ks²⁸J²⁹R³⁰³³v b u	1240–7530	pow/SMC
060526	3.21^k	0.50	0.21	6.5	I³²³³R³³³⁴³⁵³⁶³⁷³⁸³⁹⁴⁰v b	930–2100	pow/MW
060607A	3.082^l	0.24	0.09	8	H²³(irg)⁴¹v b u	950–4200	pow/SMC Ä
060729	0.54^m	0.45	0.17	70	i^mR⁴²v b u w1 m2 w2	1040–5650	bknp/SMC
060904B	0.703ⁿ	1.13	0.53	5	(KJI)⁴³R⁴⁴v b u w1 m2 w2	940–13710	pow/LMC
060908	2.43^o	0.23	0.09	6	R^v b u w1	660–2200	pow/SMC
060912	0.937^p	0.39	0.16	1	v b u w1 w2	830–3020	pow/MW
061007	1.262^q	0.18	0.06	0.7	(iR)⁴⁷v b u w1 m2 w2	710–3850	pow/SMC
061121	1.314^r	0.40	0.14	6	I⁴⁸⁴⁹⁵⁰R⁵¹v b u w1 m2 w2	690–3830	bknp/LMC
061126	1.159^s	1.02	0.56	2	i⁵²R^s⁵³⁵⁴v b u w1 m2	740–4030	bknp/LMC
070110	2.352^t	0.16	0.04	10	R⁵⁵v b u	1150–2250	bknp/SMC
070318	0.836^u	0.14	0.05	6	v b u w1 m2 w2	870–3190	pow/SMC
070810A	2.17^v	0.18	0.07	5	R^vv b u	1220–2380	pow/MW
071112C	0.823^w	0.74	0.36	1.3	(KJ)⁵⁶I⁵⁷R⁵⁷⁵⁸⁵⁹v g⁵⁷b u w1 m2 w2	880–12810	pow/SMC
080210	2.641^x	0.55	0.26	5	KHJ z′ i′ r′ g′	1060–6370	bknp/LMC
080319B	0.937^y	0.11	0.03	200	(ir)⁶⁰b u w1 m2 w2	830–4490	pow/SMC

Notes. Columns list GRB redshift, Galactic column density, N_H,Gal, and visual extinction, A_V, Gal, in the line-of-sight to the GRB, the corresponding SED epoch, the UV/optical/NIR band passes included in the GRB afterglow SED, the rest-frame coverage of the SED, and the best-fit SED model. In this last column we indicate both the best-fit continuum (power-law or broken power-law abbreviated to pow and bknp respectively) and host galaxy dust extinction model, where we have used the abbreviation MW to indicate Milky Way extinction curve model.

^(†)

Relative to time that BAT triggered on the GRB.

References.

^(a)

Fynbo et al. (2005a);

^(b)

Foley et al. (2005);

^(c)

Starling et al. (2005);

^(d)

Fynbo et al. (2005b);

^(e)

Ledoux et al. (2005);

^(f)

Jakobsson et al. (2005a);

^(g)

Prochaska et al. (2006);

^(h)

Dupree et al. (2006);

⁽ⁱ⁾

Cucchiara et al. (2006);

^(j)

Starling et al. (2006);

^(k)

Berger & Gladders (2006);

^(l)

Ledoux et al. (2006);

^(m)

Thoene et al. (2006);

⁽ⁿ⁾

Fugazza et al. (2006);

^(o)

Rol et al. (2006);

^(p)

Jakobsson et al. (2006a);

^(q)

Jakobsson et al. (2006b);

^(r)

Bloom et al. (2006);

^(s)

Perley et al. (2008a);

^(t)

Jaunsen et al. (2007a);

^(u)

Jaunsen et al. (2007b);

^(v)

Thoene et al. (2007);

^(w)

Jakobsson et al. (2007);

^(x)

Jakobsson et al. (2008a);

^(y)

Vreeswijk et al. (2008a).

⁽¹⁾

Huang et al. (2007);

⁽²⁾

Kamble et al. (2007);

⁽³⁾

Woźniak et al. (2005);

⁽⁴⁾

Cobb & Bailyn (2005);

⁽⁵⁾

Rosenberg & Garnavich (2005);

⁽⁶⁾

Flasher et al. (2005);

⁽⁷⁾

Yanagisawa et al. (2005);

⁽⁸⁾

Homewood et al. (2005);

⁽⁹⁾

Mirabal et al. (2005);

⁽¹⁰⁾

Pandey et al. (2006);

⁽¹¹⁾

Macomb et al. (2005);

⁽¹²⁾

Cenko et al. (2006b);

⁽¹³⁾

Durig & Price (2005);

⁽¹⁴⁾

Jakobsson et al. (2005b);

⁽¹⁵⁾

Andreev & Pozanenko (2005);

⁽¹⁶⁾

Henych et al. (2005);

⁽¹⁷⁾

Piranomonte et al. (2005);

⁽¹⁸⁾

D’Elia et al. (2005);

⁽¹⁹⁾

Alatalo et al. (2006);

⁽²⁰⁾

Curran et al. (2007);

⁽²¹⁾

Stanek et al. (2007);

⁽²²⁾

Woźniak et al. (2006);

⁽²³⁾

Molinari et al. (2007);

⁽²⁴⁾

Nysewander et al. (2006);

⁽²⁵⁾

Cobb (2006a);

⁽²⁶⁾

Koppelman (2006);

⁽²⁷⁾

Cenko et al. (2006a);

⁽²⁸⁾

Hearty et al. (2006);

⁽²⁹⁾

Sharapov et al. (2006);

⁽³⁰⁾

⁽³¹⁾

⁽³²⁾

⁽³³⁾

⁽³⁴⁾

Baliyan et al. (2006);

⁽³⁵⁾

Covino et al. (2006);

⁽³⁶⁾

Dai et al. (2007);

⁽³⁷⁾

Greco et al. (2006);

⁽³⁸⁾

Khamitov et al. (2006);

⁽³⁹⁾

Morgan & Dai (2006);

⁽⁴⁰⁾

Rumyantsev et al. (2006);

⁽⁴¹⁾

Nysewander et al. (2009);

⁽⁴²⁾

Quimby & Rykoff (2006);

⁽⁴³⁾

Cobb & Bailyn (2006);

⁽⁴⁴⁾

Skvarc (2006);

⁽⁴⁵⁾

Antonelli et al. (2006);

⁽⁴⁶⁾

Wiersema et al. (2006);

⁽⁴⁷⁾

Mundell et al. (2007);

⁽⁴⁸⁾

Cenko (2006b);

⁽⁴⁹⁾

Cobb (2006c);

⁽⁵⁰⁾

Torii (2006);

⁽⁵¹⁾

Uemura et al. (2006);

⁽⁵²⁾

Gomboc et al. (2008);

⁽⁵³⁾

Smith et al. (2006);

⁽⁵⁴⁾

Williams & Milne (2006);

⁽⁵⁵⁾

Malesani et al. (2007);

⁽⁵⁶⁾

Uemura et al. (2007);

⁽⁵⁷⁾

Yoshida et al. (2007);

⁽⁵⁸⁾

Dintinjana et al. (2007);

⁽⁵⁹⁾

Burenin et al. (2007);

⁽⁶⁰⁾

Racusin et al. (2008).

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