Table 5
Derivation of the dust masses for the galaxies in our sample.
Galaxy | h R | h z |
![]() |
![]() |
ref | T d |
![]() |
|
(kpc) | (kpc) | (M⊙) | (K) | (M⊙) | ||||
|
||||||||
NGC 973 | 16.33 | 0.59 | 0.48 | 8.17 | X97 | 20.0 ± 0.6 | 8.11 ± 0.07 | |
UGC 4277 | 12.52 | 0.25 | 0.49 | 7.95 | B07 | 17.3 ± 0.6 | 8.31 ± 0.09 | |
IC 2531 | 13.68 | 0.38 | 0.30 | 7.81 | X99 | 18.5 ± 0.3 | 8.04 ± 0.04 | |
NGC 4013 | 3.93 | 0.21 | 0.67 | 7.08 | X99 | 21.5 ± 0.4 | 7.63 ± 0.04 | |
2.67 | 0.19 | 1.46 | 7.08 | B07 | ||||
NGC 4217 | 6.72 | 0.38 | 1.26 | 7.81 | B07 | 22.1 ± 0.4 | 7.85 ± 0.03 | |
NGC 5529 | 11.87 | 0.52 | 0.65 | 8.02 | X99 | 19.4 ± 0.4 | 8.32 ± 0.05 | |
11.66 | 0.26 | 0.68 | 8.03 | B07 | ||||
NGC 5907 | 7.84 | 0.16 | 0.49 | 7.54 | X99 | 20.0 ± 0.3 | 8.12 ± 0.03 |
Notes. The second, third and fourth columns contain the horizontal scalelength hR, the vertical scaleheight hz, and the face-on optical depth of the dust as derived from radiative transfer fits to V-band images (the scalelength and scaleheights have been rescaled to the distances adopted within HEROES). The fifth column is the optically determined dust mass calculated from these values using Eq. (8). The sixth column contains the reference of the radiative transfer fit: X97 (Xilouris et al. 1997), X99 (Xilouris et al. 1999) or B07 (Bianchi 2007). Dust temperature and dust mass as derived from a modified black-body fit to the Herschel data are reported in the last two columns.
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