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Table 3
Best-fit parameters for the relation between dust and stellar mass.
| Sample | tage (Myr) | αmass | βmass | Ref. |
|---|---|---|---|---|
| PPD, model 1(a) | 2–3 | 1.3 ± 0.2 | 1.1 ± 0.1 | (1) |
| PPD, model 2(a) | 2–3 | 1.9 ± 0.2 | 1.1 ± 0.1 | (1) |
| Debris disks | 10–50 | 1.6 ± 1.0 | −1.9 ± 0.2 | (2) |
| Debris disks | >50 | 1.4 ± 0.9 | −2.6 ± 0.2 | (2) |
| Debris disks | >10 | 1.7 ± 0.7 | −2.3 ± 0.2 | (2) |
Notes. (a)The PPD sample includes objects from Chamaeleon I star-forming region. Model 1 and model 2 correspond to two extremes of the possible relation between the average dust temperature and stellar luminosity. (1) Pascucci et al. (2016); (2) this work.
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