Table 1
Morphology of the inner dust belt based on our MCMC exploration jointly fitting the SPHERE total and polarized intensity data.
| Parameter | Range | Best fit  |
Median ± 1σ |
| r0 (au) | [10,130] | 39.9 | 39.7 ± 0.6 |
| PA (°) | [-120, -60] | -94.1 | -94.1 ± 0.1 |
| i (°) | [0,90] | 78.0 | 77.9 ± 0.4 |
| g | [0.05,0.999] | 0.78 | 0.77 ± 0.01 |
| Scaling (I) | [100,108] | 6.8 × 103 | (6.8 ± 0.3) × 103 |
| Scaling (pI) | [100,108] | 9.6 × 104 | (9.3 ± 0.6) × 104 |
| αout | [-20,-1.1] | -2.17 | -2.18 ± 0.9 |
| SBdisk,I/F⋆,I | 2.0 × 10−3 | (2.0 ± 0.2) × 10−3 | |
| SBdisk, pI/F⋆, pI | 1.2 × 10−4 | (1.2 ± 0.2) × 10−4 | |
Notes. The two last lines correspond to the total surface brightness of the disk in total and polarized intensity, respectively, expressed in terms of contrast, i.e., divided by the total stellar flux. The ranges correspond to the authorized values. The disk models and residuals are shown in Fig. 6, and the corner plot of the posteriors in Fig. D.1. One may wish to compare these results with those from the MCMC exploration independently fitting either the total or polarized intensity, see Tables D.1 and D.2, respectively.
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