Table A.2
Constraints on the dust vertical concentration in different radial domains, local dust mass, and total dust mass.
| Name | Mdust (10−4 M⊙) | Domain (au) | Hd,R (au) | Hd,R/R (−) | Method (−) | aMCFOST (μm) | Σd, median (10−3 g.cm−2) | Σd, max (10−3 g.cm−2) |
|---|---|---|---|---|---|---|---|---|
| AA Tau | 0.7 ± 0.1 | 43 − 93 | ≤ 2.3 | ≤ 0.033 | G | 88 | 6.8 | 17.3 |
| 93 − 160 | ≤ 1.2 | ≤ 0.009 | O | 88 | 1.9 | 13.6 | ||
| AS209 | 2.6 ± 0.3 | 39 − 97 | ≤ 1.4 | ≤ 0.021 | R | 88 | 13.3 | 61.6 |
| 97 − 141 | ≤ 0.9 | ≤ 0.007 | R | 88 | 7.6 | 66.8 | ||
| CI Tau | 4.2 ± 1.0 | 40 − 130 | ≤ 3.9 | ≤ 0.046 | G/R | 88 | 18.3 | 42.1 |
| 130 − 234 | ≤ 12.2 | ≤ 0.067 | R/O | 88 | 7.0 | 16.1 | ||
| DL Tau | 5.8 ± 1.2 | 46 − 78 | ≤ 1.7 | ≤ 0.028 | G | 88 | 30.9 | 66.8 |
| DoAr25 | 6.4 ± 1.7 | 69 − 86 | ≥ 0.9 | ≥ 0.012 | G | 88 | 25.3 | 52.1 |
| 86 − 165 | ≤ 3.0 | ≤ 0.024 | G/R/O | 88 | 18.8 | 101.0 | ||
| DS Tau | 0.5 ± 0.1 | 55 − 85 | ≤ 1.4 | ≤ 0.020 | O | 88 | 12.1 | 32.4 |
| Elias24 | 4.0 ± 0.4 | 37 − 123 | ≤ 1.5 | ≤ 0.019 | R | 88 | 10.0 | 73.4 |
| GM Aur | 5.6 ± 1.6 | 40 − 125 | ≤ 1.7 | ≤ 0.021 | G/R/O | 77 | 18.4 | 60.8 |
| GO Tau | 1.7 ± 0.5* | 73 − 150 | ≤ 4.1 | ≤ 0.037 | G/R/O | 88 | 6.8 | 33.5 |
| GW Lup | 1.2 ± 0.2* | 62 − 141 | ≤ 1.3 | ≤ 0.013 | G/R/O | 88 | 3.7 | 22.5 |
| Haro 6-5B | 3.5 ± 0.9g | 110 − 190 | ≤ 5.5 | ≤ 0.036 | O | 59 | 4.3 | 21.3 |
| HD142666 | 0.9 ± 0.1 | 11 − 30 | ≥ 0.2 | ≥ 0.010 | G | 88 | 51.2 | 59.2 |
| 40 − 60 | ≤ 1.3 | ≤ 0.027 | O | 88 | 28.3 | 43.8 | ||
| HD163296 | 2.0 ± 0.2 | 49 − 85 | 0.4 − 4.5 | 0.006 − 0.067 | R | 88 | 6.5 | 48.0 |
| 85 − 155 | ≤ 0.6 | ≤ 0.005 | R | 88 | 3.9 | 30.7 | ||
| HL Tau | 3.2 ± 0.5 | 61 − 150 | ≤ 5.5 | ≤ 0.053 | G/R/O | 59 | 18.6 | 55.0 |
| ISO-Oph 17 | 1.5 ± 0.2 | 26 − 46 | ≤ 2.4 | ≤ 0.068 | G | 88 | 29.8 | 81.8 |
| J1608 | 0.2 ± 0.0 | 60 − 82 | ≤ 1.0 | ≤ 0.014 | R | 88 | 4.6 | 12.2 |
| J1610 | 0.2 ± 0.0 | 29 − 78 | ≤ 1.5 | ≤ 0.028 | G/O | 88 | 6.6 | 22.0 |
| LkCa 15 | 2.1 ± 0.3 | 47 − 89 | ≥ 4.5 | ≥ 0.067 | R | 88 | 8,1 | 29.3 |
| 89 − 200 | ≤ 4.9 | ≤ 0.034 | R | 88 | 6.4 | 22.7 | ||
| MYLup | 2.8 ± 0.8 | 40 − 100 | ≤ 2.0 | ≤ 0.029 | O | 88 | 41.3 | 127.7 |
| Oph163131 | 0.6 ± 0.1* | 107 − 150 | ≤ 1.4 | ≤ 0.011 | O | 88 | 3.8 | 7.3 |
| PDS70 | 0.5 ± 0.0 | 50 − 105 | ≤ 1.3 | ≤ 0.017 | R/O | 59 | 6.5 | 22.0 |
| RY Tau | 2.1 ± 0.4 | 28 − 90 | ≤ 1.4 | ≤ 0.023 | O | 88 | 51.2 | 116.3 |
| V1094Sco | 6.2 ± 1.3 | 107 − 164 | ≥ 8.9 | ≥ 0.068 | R | 88 | 6.7 | 51.7 |
| 201 − 280 | ≤ 10.7 | ≤ 0.046 | R/O | 88 | 8.4 | 18.3 | ||
| HD163296 | 67.9 | ≥ 3.8 | ≥ 0.056 | (1) | ||||
Notes. In the “Method” column, G indicates that the gap contrast was determinant to put the constraint, O marks that the outer edge effect was mostly used, and R indicates that it is the azimuthal variation in the ring that was critical. The seventh column aMCFOST indicates the grain size which has the maximum opacity at the respective wavelength of the observations and for which the constraints on Hd,R and Hd,R/R were obtained. The last two columns indicate the median and maximum surface density of each region. In the Mdust column, indicating the total dust mass, (*) and (g) highlight sources where the stellar radius was modified to lead to optically thinner dust emission (see Sect. 3.3, Table A.1), potentially affecting the dust mass estimate.
References. (1) Doi & Kataoka (2021).
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