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

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Table 4

GRB host galaxy properties taken from the literature and based on UV, optical, near- and mid-IR data, as well as the dust mass and temperature derived in this paper from modified blackbody fits to our Herschel data.

GRB	E(B − V) ^a	[O/H]^b	SFR(Hα/Oii)^c	SFR(FIR)	log [ M_∗ ]	A _V ^d	T _d ^e	log [ M_d ] ^f
Host	(mag)		(M_⊙ yr^-1)	(M_⊙ yr^-1)	(M_⊙)	(mag)	(K)	(M_⊙)

000210	0.029	8.3 ± 0.1		<37		0.0	30	<8.6
		8.7 ± 0.1
000418	0.033	8.1 ± 0.2		< 40		1.3	40	<8.3
		8.8 ± 0.2
070306	0.024	8.4 ± 0.1		101 ± 21		0.4	51 ± 0.2	7.9 ± 0.3
081109	0.017	8.8 ± 0.1		<32		1.3	35	<8.5
090926B	0.020	8.2 ± 0.2		<45		1.0	35	<8.7

Notes.

^(a)

Galactic dust reddening in magnitudes from the map of Schlafly & Finkbeiner (2011).

^(b)

Metallicities in the case of GRBH 000210, 000418 and 070306 (Piranomonte et al., in prep.; Vergani et al., in prep.) were derived using the R₂₃ ratio and applying the calibration from Kobulnicky & Kewley (2004). The N ii emission line required to distinguish between the R₂₃ lower and upper branches was not detected in the spectra of GRBH 000210 and 000418, and we therefore report both solutions. Metallicities for GRBH 081109 and 090926B (Krühler et al., in prep.) were derived using the methods from Nagao et al. (2006). For a detailed description on the differences between the individual strong line diagnostics, see Kewley & Ellison (2008).

^(c)

SFRs derived from the O ii line for GRBH 000418 (Piranomonte et al., in prep.), and from the Hα line for the other four GRBHs (Piranomonte et al., in prep.; Krühler et al., in prep.; Vergani et al., in prep.), based on the formulation described in Kennicutt (1998), but converted to a Chabrier IMF (Chabrier 2003). All have been corrected for host galaxy dust extinction derived from the Balmer decrement, with the exception of GRBH 000418, for which we used the average visual extinction given in Col. 7, and assuming the Calzetti dust attenuation law (Calzetti et al. 2000).

^(d)

The quoted value corresponds to the A_V of the best-fit galaxy template.

^(e)

Fixed temperature of the MBB scaled to the data, apart from in the case of GRBH 070306, where it was left as a free parameter in the SED fit.

^(f)

3σ upper limit or best-fit dust-mass resulting from a blackbody scaled to the data with emissivity index β = 1.5 and temperature as given in Col. 8.

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