Table 1
FT squared visibility best-fit solution for the geometrically thin ring model and the Gaussian-convolved ring model.
| Geometrically thin ring | Gaussian-convolved ring | |||||
|---|---|---|---|---|---|---|
| Parameter | Unit | Fit solution | Parameter | Unit | Fit solution | Scan range |
| Fs | [%] | 93.81 ± 0.07 | Fs | [%] | 93.81 ± 0.07 | [0 ; 100%] |
| Fc | [%] | 6.19 ± 0.07 | Fc | [%] | 6.19 ± 0.07 | 1 - Fs |
| kc | − 0.35 ± 0.21 | kc | − 0.35 ± 0.21 | [−4 ; 4] | ||
| ri | [mas (au)] | 7.40 ± 0.21 (0.81) | ri | [mas (au)] | 7.35 ± 0.21 (0.81) | [0 ; 60] |
| w | [mas (au)] | 0.35 ± 0.35 (0.04) | w | [mas (au)] | 0.24 ± 0.24 (0.03) | [0 ; 100] |
| i | [deg] | 58.47 ± 1.55 | i | [deg] | 58.45 ± 1.55 | [30 ; 80] |
| PA | [deg] | − 1.77 ± 1.11 | PA | [deg] | − 1.78 ± 1.11 | [−40 ; 40] |
 |
4.67 ± 0.33 |  |
4.67 ± 0.33 | |||
Notes. Fs is the stellar flux contribution, Fc the dusty circumstellar environmentflux contribution, kc the dust spectral index at 2.15 μm, ri the ring inner hole radius, w the ring width (ri and w defined in different ways for the two models, see Sect. 4.1), i the ring inclination from face-on, PA the northeast position angle, and 
the reducedchi-square. The uncertainties on the fitted parameter correspond to the 1σ error. Scan ranges refer to both models.
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