The SEDs and host galaxies of the dustiest GRB afterglows

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Table 5

Afterglow properties.

Afterglow	Redshift^*	T ₉₀^**	β _opt^***	β _X		N _H,X	χ²/d.o.f.
		[s]			[mag]	10²²cm^-2

GRB 070306	1.496	210^(a)	1.00	1.00 ± 0.07			123/108
GRB 070802^(b,c)	2.452	16.4^(d)	0.60		/1.19 ± 0.15	/ < 2.9	15/14
GRB 080605^(b,c)	1.640	20^(e)	0.67	0.67 ± 0.01	0.47 ± 0.03/	/0.71 ± 0.08	428/327
GRB 080607^(c,f)	3.036	79^(g)	0.96		3.3 ± 0.3/	/	70/39
GRB 080805^(b,c)	1.505	78^(h)	0.47	0.97 ± 0.05	/1.53 ± 0.13	/	23/18
GRB 081109	0.979	190⁽ⁱ⁾	1.10				48/63
GRB 090926B^(b)	1.24	110^(j)	0.73				33/31
GRB 100621A	0.542	63.6^(k)	0.79				138/124

Notes. Afterglow measurements were taken from the reference denoted with the superscript in the first line. When two references are given, we quote both values for and N_H,X, but values for β and χ² only from the first one for the sake of clarity.

^(*)

Redshifts from Jaunsen et al. (2008), Elíasdóttir et al. (2009), Fynbo et al. (2009a), Fynbo et al. (2009b) and Milvang-Jensen et al. (2010).

^(**)

T₉₀ is the duration in which the GRB emits from 5% to 95% of its γ-rays, and is used to discriminate between short and long bursts. Typically, long GRBs have T₉₀ > 2 s (Kouveliotou et al. 1993). All GRBs in this work are hence unambigously long events.

^(***)

β_opt is tied to β_X in the fitting, and hence has the same error.

References. (a) Barthelmy et al. (2007), (b) Greiner et al. (2011), (c) Zafar et al. (2011), (d) Cummings et al. (2007), (e) Cummings et al. (2008), (f) Perley et al. (2011b), (g) Stamatikos et al. (2008), (h) Palmer et al. (2008), (i) Markwardt et al. (2008), (j) Baumgartner et al. (2009), (k) Ukwatta et al. (2010a).

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