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 7:

Parameters of the SED models introducing a cold dust component at 10 K.
	NGC 1705			Haro 11
	Fiducial modelling	Cold dust component		Fiducial modelling	Cold dust component
		$\beta$ = 1	$\beta$ = 2		$\beta$ = 1	$\beta$ = 2
$\bar{\chi}$ ²	15.7	2.4	3.3	17.2	11.3	11.5
$M_{\rm dust}$ ( $M_\odot$ ) ^a	1.3 $\times$ 10⁶ ( $\pm$ 50 $\%$ )	1.7 $\times$ 10⁵ ( $\pm$ 28 $\%$ ) ^b	1.3 $\times$ 10⁶ ( $\pm$ 21 $\%$ )	1.7 $\times$ 10⁷ ( $\pm$ 40 $\%$ )	2 $\times$ 10⁷ ( $\pm$ 17 $\%$ )	1.3 $\times$ 10⁸ ( $\pm$ 17 $\%$ )
$M_{\rm dust}$ / $M_{\rm HI}$	3.2 $\times$ 10^-2	4.1 $\times$ 10^-3	2.8 $\times$ 10^-2	0.17	0.2	1.3
$M_{\rm PAH}$ / $M_{\rm dust}$	2 $\times$ 10^-3	8.1 $\times$ 10^-4	8 $\times$ 10^-5	1.04 $\times$ 10^-2	3.1 $\times$ 10^-3	6.2 $\times$ 10^-4

^a This mass includes the cold (10 K) dust mass for NGC 1705 and Haro 11; ^b bold numbers represent the dust mass and D/G values of our prefered SED models.

Source LaTeX | All tables | In the text

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