Probing the dust properties of galaxies up to submillimetre wavelengths - I. The spectral energy distribution of dwarf galaxies using LABOCA

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Table 1:

General properties of the sample.
Name	Ra (2000)	Dec (2000)	$12+\log({\rm O/H})^{a}$	Distance (Mpc)^b	M(HI)^c	Apparent size
NGC 1705	04h54'13.5''	-53 $^{\circ}$ 21'40''	8.46	4.7	5.1 $\times$ 10⁷	1.9' $\times$ 1.4'
Haro 11	00h36'52.5''	-33 $^{\circ}$ 33'19''	7.9	92	$\sim$ 10⁸	0.5' $\times$ 0.5'
Mrk 1089	05h01'37.8''	-04 $^{\circ}$ 15'28''	8.0	59.8	2.7 $\times$ 10¹⁰	0.61' $\times$ 0.23'
UM 311	01h15'34''	-00 $^{\circ}$ 51'32''	8.3	21.3	2.3 $\times$ 10⁹	0.11' $\times$ 0.11'

^a References for metallicities: NGC 1705: Meurer et al. (1992), Haro 11: Bergvall & Östlin (2002), Mrk 1089 and UM 311: Hopkins et al. (2002).
^b References for distances: NGC 1705: Meurer et al. (1992), Haro 11: Bergvall et al. (2000), Mrk 1089 and UM 311: Hopkins et al. (2002).
^c References for the HI mass: NGC 1705: 8.9 $\times$ 10⁷ $M_\odot$ for D = 6.2 Mpc (Meurer et al. 1998), Haro 11: upper limit derived from the HI detection (Bergvall & Östlin 2002), Mrk 1089: 2.1 $\times$ 10¹⁰ $M_\odot$ for D=53 Mpc (Williams et al. 1991), UM 311: 3.1 $\times$ 10⁹ $M_\odot$ for D = 24.7 Mpc (Smoker et al. 2000). The HI masses were scaled according to the distances we used.

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