Table 5
Summary of the stellar and disk properties for the best-fitting dust models for our 13 disks.
| Source | Robitaille model | Isella model | |||||||||
| A v | M ⋆ | M d | R d | i | F 1.3mm | M ⋆ | M d | R d | i | F 1.3mm | |
| [mag] | [M⊙] | [10-2 M⊙] | [AU] | [°] | [mJy] | [M⊙] | [10 ] |
[AU] | [°] | [mJy] | |
|
|
|||||||||||
| CI Tau | 1.80 (1.80) | 0.4 | 1.9 | 91 | 57 | 105 | – | – | – | – | – |
| CW Tau | – | – | – | – | – | – | – | – | – | – | – |
| CY Tau | 0.05 (0.03) | 0.9 | 1.4 | 97 | 32 | 23 | 0.4 | 6.92 | 197 | 51 | 117 ± 20 |
| DG Tau | 1.60 (1.41) | 1.5 | 3.9 | 158 | 50 | 254 | 0.3 | 41.7 | 89 | 18 | 317 ± 28 |
| DN Tau | 0.49 (0.49) | 0.6 | 1.0 | 92 | 32 | 39 | 0.4 | 1.86 | 125 | 30 | 93 ± 8 |
| DO Tau | 4.88 (2.23) | 0.8 | 3.2 | 104 | 57 | 103 | – | – | – | – | – |
| DQ Tau | – | – | – | – | – | – | – | – | – | – | – |
| DR Tau | 0.51 (0.51) | 0.8 | 3.2 | 104 | 18 | 103 | 0.4 | 6.31 | 86 | 37 | 109 ± 11 |
| FT Tau | 0.00 (–) | 0.2 | 0.8 | 62 | 50 | 36 | – | – | – | – | – |
| GO Tau | – | – | – | – | – | – | 0.6 | 7.10 | 670 | 25 | 57 ± 8 |
| IQ Tau | 1.44 (1.44) | 1.0 | 3.0 | 101 | 63 | 74 | – | – | – | – | – |
| UZ Tau | – | – | – | – | – | – | 0.3 | 4.79 | 260 | 43 | 126 ± 12 |
| V806 Tau | – | – | – | – | – | – | – | – | – | – | |
Notes. For the Robitaille models, the visual interstellar extinction Av magnitudes are for the best model fit, only using the measured values from White & Ghez (2001) as an input parameter to the SED fitting tool (in parenthesis). The M⋆ values listed for both models are the derived values for each method. For the Isella models, the outer dust radius Rd is from Table 5 in Isella et al. (2009), defined as where the disk becomes optically thin to the stellar radiation. For UZ Tau, the Isella model in fact concerns only the spectroscopic binary component UZ Tau E. The 1.3 mm continuum fluxes (F1.3mm) listed for our best-fitting Robitaille model are the SED values of the fit; and for the Isella models we list the resolved (interferometric) dust continuum measurement.
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