Table 1
Stellar and disk parameters for the studied objects.
| Host star | Type(a) | L⋆(a) | M⋆(a) | Age (a) | d (b) | Incl (c) | PA (c) | Rdust(c) | FNIR/F⋆ (d) | FFIR/F⋆ (d) | Ref. |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (L⊙) | (M⊙) | (Myr) | (pc) | (º) | (º) | (AU) | (%) | (%) | |||
| PDS 70 | T Tauri K7 | 0.31 ± 0.02 | 0.8 ± 0.1 |  |
113 | 49.7 | 68.6 | 54 | 4.8 ± 0.6 | 11.3 ± 0.7 | 1 |
| TW Hya | T Tauri K6 | 0.33 ± 0.02 | 0.8 ± 0.1 |  |
60 | 7 | 61/241(e) | 115 | 1.0 ± 1.0 | 14.0 ± 0.9 | 2, 3, 4 |
| RX J1604 | AA Tau K2 | 0.60 ± 0.03 | 1.0 ± 0.1 |  |
150 | 6 | 170/350(e) | 65 | 17.5 ± 3.6 | 26.9 ± 1.9 | 5 |
| RX J1615 | T Tauri K5 | 0.90 ± 0.02 | 0.6 ± 0.1 |  |
155 | 47 | 236 | 197 | 0.0 ± 0.9 | 8.7 ± 1.0 | 6, 7 |
| LkCa 15 | Orion Var K5 | 1.11 ± 0.04 | 1.2 ± 0.1 |  |
158 | 50 | 150 | 47 | 13.4 ± 1.0 | 9.5 ± 0.4 | 8, 9 |
| PDS 66 | T Tauri K1 | 1.26 ± 0.04 | 1.2 ± 0.2 |  |
86 | 31 | 100 | 80 | 7.3 ± 1.4 | 6.5 ± 1.2 | 10 |
| HD 169142 | Herbig F1 | 5.6 ± 1.2 | 1.5 ± 0.2 |  |
114 | 12.5 | 275 | 25 | 10.5 ± 1.0 | 18.2 ± 3.1 | 11 |
| HD 135344B | Herbig F8 | 6.9 ± 0.4 | 1.5 ± 0.1 |  |
136 | 11 | 332 | 25 | 27.2 ± 3.1 | 25.6 ± 1.2 | 12 |
| HD 100453 | Herbig A9 | 8.5 ± 3.5 | 1.6 ± 0.1 |  |
104 | 38 | 52 | 20 | 21.7 ± 2.7 | 19.6 ± 3.5 | 13, 14 |
| MWC 758 | Herbig A8 | 11.8 ± 0.5 | 1.8 ± 0.1 |  |
160 | 21 | 155 | 70 | 27.5 ± 2.9 | 13.1 ± 0.5 | 15 |
| HD 142527 | Herbig F6 | 20 ± 2 | 2.2 ± 0.3 |  |
157 | 24 | 70 | 130 | 34.2 ± 3.3 | 34.8 ± 4.1 | 16 |
Notes. The columns give the name, stellar type, luminosity, mass, age, and distance of the host star, followed by the disk parameters inclination, position angle of the far side of the minor axis, the typical radius for the measured dust reflection, the near-IR excess, and the far-IR excess, and references to previous polarimetric imaging. (a) Taken from Asensio-Torres et al. (2021), except for HD 142527 and HD 100453 taken from their references respectively; (b) from van der Marel (2023); (c) taken from References; (d) from Garufi et al. (2018); (e) not accurately known because of low inclination.
References. 1. Hashimoto et al. (2012); 2. Qi et al. (2004); 3. van Boekel et al. (2017); 4. Sokal et al. (2018); 5. Pinilla et al. (2018a); 6. Pinilla et al. (2018b); 7. de Boer et al. (2016); 8. Thalmann et al. (2015); 9. Thalmann et al. (2016); 10. Wolff et al. (2016); 11. Quanz et al. (2013); 12. Stolker et al. (2016a); 13. Benisty et al. (2017); 14. Fairlamb et al. (2015); 15. Benisty et al. (2015); 16. Verhoeff et al. (2011).
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