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

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Volume 508 / No 2 (December III 2009)

A&A, 508 2 (2009) 645-664

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Table 5:

Parameters of our SED models using or not submm constraints and Dust-to-Gas mass ratios of our galaxies.
	Haro 11		Mrk 1089		NGC 1705
	no submm	submm	no submm	submm	no submm	submm
$M_{\rm dust}$ ( $M_\odot$ )	6.2 $\times$ 10⁶	1.7 $\times$ 10⁷ ( $\pm$ 40 $\%$ )	3 $\times$ 10⁷	5.12 $\times$ 10⁷ ( $\pm$ 20 $\%$ ) ^a	2.9 $\times$ 10⁴	1.3 $\times$ 10⁶ ( $\pm$ 50 $\%$ )
$f_{\rm PAH}$	0.22	0.1	0.18	0.18	0.11	4.4 $\times$ 10^-2
$\alpha$	1.88	1.73	2.21	2.18	2.5	1.84
$U_{\rm min}$	12.2	1.44	1.5	0.82	3.68	9 $\times$ 10^-3
$U_{\rm max}$	1.3 $\times$ 10⁵	5.77 $\times$ 10⁴	3.84 $\times$ 10⁵	3.5 $\times$ 10⁵	1.47 $\times$ 10⁴	8.67 $\times$ 10²

$M_{\rm HI}$ ( $M_\odot$ )	$\sim$ 10⁸		2.7 $\times$ 10¹⁰		4.1 $\times$ 10⁷ ^b
$M_{\rm dust}$ / $M_{\rm HI}$	6 $\times$ 10^-2	0.17	10^-3	1.9 $\times$ 10^-3	7 $\times$ 10^-4	3.2 $\times$ 10^-2

^a Bold numbers are the dust mass and the dust-to-gas mass ratio values of our prefered SED for the galaxy Mrk 1089.
^b HI mass associated with the aperture chosen for the dust mass determination, namely 80% of the the total HI mass.

Source LaTeX | All tables | In the text

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