Table 1
Stellar and disk properties of the targets of this work, sorted by right ascension.
| Source | Ref. | d | Teff | AV | Group | L* | M* | t | Md | NIR | FIR |
|---|---|---|---|---|---|---|---|---|---|---|---|
| n. | (pc) | (K) | (mag) | (L⊙) | (M⊙) | (Myr) | (M⊕) | (%) | (%) | ||
| CI Tau | 1 | 137.0 | 4400 | 1.9 | I/II | 1.3 ± 0.2 | 1.1 ± 0.2 | 1.5–5 | 135 | 20.7 | 9.9 |
| HD 287823 | 2 | 347.2 | 8375 | 0.0 | I/II | 11.7 ± 0.7 | 1.8 ± 0.2 | 8–16 | – | 17.3 | 9.5 |
| HD 245185 | 3 | 414.9 | 10 000 | 0.4 | I | 26.7 ± 1.3 | 2.1 ± 0.2 | 7–11 | 50 | 10.4 | 13.1 |
| HD 290770 | 4 | 398.4 | 10 500 | 0.0 | II | 34.3 ± 1.9 | 2.2 ± 0.2 | 6–15 | – | 14.8 | 5.1 |
| TW Cha | 5 | 183.1 | 3955 | 0.8 | I/II | 0.64 ± 0.04 | 1.1 ± 0.1 | 1.5–5 | 24 | 17.2 | 8.6 |
| DI Cha | 6 | 189.0 | 5860 | 1.8 | II | 10.5 ± 0.8 | 2.3 ± 0.2 | 0.5–2 | 10 | 17.0 | 5.1 |
| HD 98922 | 7 | 653.6 | 10 500 | 0.1 | II | 1219 ± 63 | 5.5 ± 0.6 | 0.2–0.7 | – | 20.3 | 2.2 |
| GW Lup | 8 | 155.3 | 3630 | 0.8 | II | 0.43 ± 0.06 | 0.7 ± 0.1 | 1–3 | 50 | 11.5 | 7.1 |
| HD 142666 | 9 | 146.4 | 7500 | 0.9 | II | 11.9 ± 1.3 | 1.7 ± 0.2 | 7.5–11.5 | 44 | 15.7 | 5.3 |
| HD 144432 | 10 | 155.0 | 7500 | 0.4 | II | 13.7 ± 0.9 | 1.7 ± 0.2 | 6.5–10.5 | 30 | 15.7 | 4.7 |
| V1003 Oph | 11 | 114.7 | 5770 | 4.5 | I/II | 7.1 ± 0.8 | 1.9 ± 0.2 | 2–6 | 10 | 23.9 | 12.1 |
| WSB82 | 12 | 146.0 | 4800 | 4.5 | I/II | 1.5 ± 0.4 | 1.4 ± 0.2 | 3–7 | 120 | 35.3 | 9.2 |
| HD 150193 | 13 | 150.8 | 9000 | 1.5 | II | 26.7 ± 4.8 | 2.2 ± 0.2 | 4–7 | 24 | 19.0 | 4.6 |
| AK Sco | 14 | 139.9 | 6250 | 0.7 | II | 2 × (3.2 ± 0.6) | 2 × (1.3 ± 0.2) | >12 | 16 | 10.9 | 5.9 |
| HD 179218 | 15 | 260.4 | 9640 | 0.4 | I/II | 115 ± 8 | 2.9 ± 0.2 | 1.5–3.5 | 140 | 6.4 | 8.5 |
Notes. Columns are: source name, reference number in figures, distance, effective temperature, optical extinction, group based on Fig. 1, stellar luminosity, mass, age, dust mass in the disk, NIR and FIR excess normalized to the stellar luminosity. Distances are from Gaia EDR3 (Gaia Collaboration 2021). Effective temperatures of Herbig stars are from Fairlamb et al. (2015), of CI Tau from Herczeg & Hillenbrand (2014), of GW Lup from Alcalá et al. (2017), of TW Cha and DI Cha from Luhman (2007), and of V1003 Oph and WSB82 from Luhman & Rieke (1999). The other properties are calculated in this work as described in Appendix A. The dust mass in the disk is obtained under standard assumptions (see Appendix A) and should be regarded as an indicative value.
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