Table 1
Disk properties from the ALMA visibility modeling.
| Property | Best value ±3σ | |
|---|---|---|
| 1.3 mm flux [mJy] | FA | 2.00 ± 0.06 |
| FB | 2.00 ± 0.15 | |
| Dust mass [M⊕] | Mdust,A | 1.18 ± 0.16 |
| Mdust,B | 1.18 ± 0.18 | |
| Relative | ΔRASB1 | −47.5 ± 2.5 |
| Astrometry | ΔDecSB1 | −46.2 ± 2.8 |
| DF Tau A-B [mas] | ΔRASB2 | −69.2 ± 21.1 |
| ΔDecSB2 | −29.3 ± 31.9 | |
| ΔRALB1 | −47.4 ± 0.3 | |
| ΔDecLB1 | −47.1 ± 0.4 | |
| ΔRALB2 | −49.9 ± 1.2 | |
| ΔDecLB2 | −44.0 ± 1.5 | |
| Size(*) [mas] | RA,68% | ≤13.8 ± 0.5 |
| RB,68% | ≤13.9 ± 0.7 | |
| RA,90% | ≤20.1 ± 1.0 | |
| RB,90% | ≤ 19.6 ± 1.2 | |
Notes. The disks geometries and relative astrometry are free parameters during the MCMC fitting. The disk sizes and fluxes are not directly fitted, but calculated from the best results shown in Table A.2, where the remaining free parameters are shown. Uncertainties are the 3σ values of the distributions. Dust masses are computed assuming a dust temperature of 20 K, a wavelength of 1.33 mm, an opacity of 2.254 cm2 g−1 (Beckwith et al. 1990), and a distance of 140±10 pc (see Sect. 4). (*)indicates parameters that should be taken with caution. As the emission is only marginally resolved, the values are not well constrained and the uncertainties instead reflect the uncertainties of the model and not the true uncertainties of the data.
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