Herschel observations of gamma-ray burst host galaxies: implications for the topology of the dusty interstellar medium

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Table 1

GRB afterglow properties.

GRB	Redshift	RA	Dec	Offset^†	A _V,GRB	β _OX ^§	N _H,X
		(J2000)^‡		(arcsec)	(mag)		10²² cm^-2

000210	0.846¹	01:59:15.58	−40:39:33.02⁶	¹¹	−	< 0.54	0.17 ± 0.04 ¹⁷
000418	1.118²	12:25:19.30	+20:06:11.6⁷	¹²	0.4–0.9^14,15	−	−
070306	1.496³	09:52:23.31	+10:28:55.26⁸	¹³	^,16	<−0.08	^,16
081109	0.979⁴	22:03:09.72	−54:42:39.5⁹	¹³	^,16	< 0.3	^,16
090926B	1.243⁵	03:05:13.94	−39:00:22.2¹⁰	¹³	^,16	< 0.4	^,16

Notes.

^(‡)

All positions are from the optical afterglow with the exception of GRB 000210, which corresponds to the X-ray afterglow position.

^(†)

Relative offset between the GRB afterglow position and the centre of the host galaxy.

^(§)

GRB afterglow optical-to-X-ray flux spectral index as defined in Jakobsson et al. (2004). Those GRBs with afterglow spectral index β_OX< 0.5 have lower optical-to-X-ray flux ratios than predicted by the standard afterglow synchrotron theory, and as such are referred to as “dark”.

Reference.

⁽¹⁾

Piro et al. (2002);

⁽²⁾

Bloom et al. (2003);

⁽³⁾

Jaunsen et al. (2008);

⁽⁴⁾

Krühler et al. (2011);

⁽⁵⁾

⁽⁶⁾

⁽⁷⁾

⁽⁸⁾

⁽⁹⁾

D’Avanzo et al. (2008);

⁽¹⁰⁾

Malesani et al. (2009);

⁽¹¹⁾

This work;

⁽¹²⁾

Berger et al. (2003);

⁽¹³⁾

Krühler et al. (2011);

⁽¹⁴⁾

Klose et al. (2000);

⁽¹⁵⁾

Berger et al. (2001);

⁽¹⁶⁾

Krühler et al. (2011);

⁽¹⁷⁾

Piro et al. (2002).

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