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Home All issues Volume 508 / No 2 (December III 2009) A&A, 508 2 (2009) 645-664 Full HTML
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Table 8:

Dust masses derived from SED models using different shapes of ISRFs.
Synthesized ISRF NGC 1705 a Haro 11 a Mrk 1089
  $M_{\rm warm}$$_{\rm dust}$ b $M_{\rm dust}$c $\bar{\chi}$2 $M_{\rm warm}$$_{\rm dust}$ b $M_{\rm dust}$c $\bar{\chi}$2 $M_{\rm dust}$ $\bar{\chi}$2
Milky Way 2.6 $\times$ 104 1.7 $\times$ 105 2 5.9 $\times$ 106 2 $\times$ 107 13 5.2 $\times$ 107 5.7
Non-ionising cluster 2.5 $\times$ 104 1.7 $\times$ 105 5 6.5 $\times$ 106 2.1 $\times$ 107 25 5.0 $\times$ 107 21
He 2-10 3.3 $\times$ 104 1.75 $\times$ 105 20 8.7 $\times$ 106 2.19 $\times$ 107 45 7.0 $\times$ 107 52
IIZw40 2.8 $\times$ 104 1.71 $\times$ 105 12 8.7 $\times$ 106 2.24 $\times$ 107 36 4.9 $\times$ 107 41
NGC 1140 2.8 $\times$ 104 1.72 $\times$ 105 12 8.1 $\times$ 106 2.2 $\times$ 107 38 4.7 $\times$ 107 46
NGC 1569 2.6 $\times$ 104 1.69 $\times$ 10 5 2 6.6 $\times$ 106 2.02 $\times$ 107 14 5.0 $\times$ 107 16
a The models used for NGC 1705 and Haro 11 include an independent, very cold dust component at 10 K with an emissivity $\beta $ = 1.
b $M_{\rm warm}$ $_{\rm dust}$is the dust mass without including the 10 K dust mass (but with cold dust included in the fit).
c $M_{\rm dust}$ is the total dust mass of the galaxy, 10 K dust mass included for Haro 11.

Source LaTeX | All tables | In the text

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