Table A.1
Source parameters used to calculate the dust masses, used for Keplerian masking, and the obtained dust and gas radii.
| Name | RA | Dec | Dist. | M⋆ | L⋆ | Age | Sp.Tp. | Group | Vsys | Vint | inc | PA | Ref. |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (h:m:s) | (deg:m:s) | (pc) | (M⊙) | (L⊙) | (Myr) | (km s−1) | (km s−1) | (°) | (°) | ||||
| AK Sco | 16:54:44.8 | −36:53:19.0 | 140 | 1.52 | 6.94 | 8.57 | F5 | I | 5.4 | 2.5 | 109 | 128 | 1,a |
| Ass ChaT2-21 | 11:06:15.3 | −77:21:56.7 | 165 | 2.09 | 10.37 | 3.23 | G5 | debris | – | – | – | – | 2 |
| Ass ChaT2-54 | 11:12:42.6 | −77:22:22.9 | 203 | 1.92 | 5.03 | 3.06 | G8 | debris | – | – | – | – | 3 |
| BE Ori | 05:37:00.1 | −06:33:27.3 | 392 | 1.86 | 7.95 | 4.55 | G3 | II | – | – | – | – | 2 |
| Brun 656 | 05:35:21.3 | −05:12:12.7 | 467 | 2.72 | 27.4 | 1.53 | G2 | debris | – | – | – | – | 2 |
| CO Ori | 05:27:38.2 | +11:25:39.1 | 400 | 2.97 | 43.82 | 1.48 | F7 | II | – | – | – | – | 4 |
| CR Cha | 10:59:06.9 | −77:01:40.3 | 186 | 1.62 | 3.72 | 1.51 | K4 | II | 5.2 | 2.5 | 31 | −36 | 5, b |
| CV Cha | 11:12:27.6 | −76:44:22.3 | 192 | 1.85 | 4.63 | 3.44 | K0 | II | – | – | – | – | 2 |
| DI Cha | 11:07:20.6 | −77:38:07.3 | 190 | 1.95 | 9.82 | 4.08 | G2 | II | – | – | – | – | 2 |
| GW Ori | 05:29:08.4 | +11:52:12.7 | 398 | 3.02 | 35.47 | 1.00 | G5 | I | 13.8 | 2.5 | 37 | −176 | 6, c |
| Haro 1-6 | 16:26:03.0 | −24:23:36.6 | 134 | 2.04 | 12.78 | 3.50 | G1 | I | – | – | – | – | 2 |
| HBC 442 | 05:34:14.2 | −05:36:54.2 | 382 | 1.9 | 13.2 | 4.75 | F8 | II | – | – | – | – | 7 |
| HBC 502 | 05:46:07.9 | −00:11:56.9 | 411 | 2.01 | 10.71 | 0.53 | K3 | I | – | – | – | – | 2 |
| HD 34700 | 05:19:41.4 | +05:38:42.8 | 353 | 2.46 | 24.34 | 2.41 | G0 | I | 5.1 | 4.5 | 0 | 0 | 2 |
| HD 35929 | 05:27:42.8 | −08:19:38.5 | 384 | 3.25 | 80.78 | 1.14 | F2 | II | – | – | – | – | 8 |
| HD 135344B | 15:15:48.4 | −37:09:16.4 | 135 | 1.5 | 8.09 | 9.07 | F8 | I | 7.1 | 1.5 | 10 | −62 | 2, d |
| HD 142527 | 15:56:41.9 | −42:19:23.7 | 157 | 2.06 | 19.31 | 3.80 | F6 | I | 3.6 | 1.5 | 27 | 26 | 9, e |
| HD 142666 | 15:56:40.0 | −22:01:40.4 | 148 | 1.62 | 11.81 | 8.37 | A8 | II | 4.1 | 1.5 | 62 | 18 | 2, f |
| HD 144432 | 16:06:57.9 | −27:43:10.1 | 155 | 1.64 | 12.5 | 8.14 | A9 | II | – | – | – | – | 10 |
| HD 288313 | 05:54:03.0 | +01:40:22.1 | 418 | 3.47 | 38.47 | 0.52 | K2 | – | – | – | – | – | 2 |
| HD 294260 | 05:36:51.3 | −04:25:40.0 | 407 | 1.68 | 8.74 | 6.72 | G1 | II | 12.0 | 2.5 | 0 | 0 | 11 |
| HQ Tau | 04:35:47.3 | +22:50:21.4 | 158 | 1.85 | 4.63 | 3.44 | K0 | II | – | – | – | – | 2 |
| HT Lup | 15:45:12.8 | −34:17:31.0 | 154 | 1.8 | 5.95 | 0.95 | K3 | II | 5.4 | 2.5 | 48 | 14 | 2, g |
| LkHA 310 | 05:47:11.0 | +00:19:14.8 | 422 | 1.87 | 6.8 | 4.25 | G6 | I | – | – | – | – | 2 |
| LkHA 330 | 03:45:48.3 | +32:24:11.8 | 308 | 1.93 | 14.39 | 4.66 | F7 | I | 9.0 | 0.8 | 28 | −49 | 2, h |
| PDS 156 | 18:27:26.1 | −04:34:47.6 | 398 | 2.61 | 21.12 | 1.80 | G5 | II | 13.0 | 2.5 | 0 | 0 | 2 |
| PDS 277 | 08:23:11.8 | −39:07:01.5 | 343 | 1.59 | 9.68 | 8.66 | F3 | I | 1.6 | 2.5 | 0 | 0 | 2 |
| PR Ori | 05:36:24.8 | −06:17:30.6 | 408 | 2.5 | 10.83 | 1.05 | K1 | I/II | – | – | – | – | 2 |
| RY Ori | 05:32:09.9 | −02:49:46.8 | 365 | 1.69 | 9.01 | 6.65 | F7 | II | – | – | – | – | 7 |
| RY Tau | 04:21:57.4 | +28:26:35.1 | 134 | 1.69 | 11.97 | 4.29 | K1 | II | 6.6 | 2.5 | 65 | −23 | 6, i |
| EM* SR 21 | 16:27:10.3 | −24:19:13.1 | 138 | 1.64 | 7.03 | 6.71 | G1 | I | 2.75 | 2.5 | 15 | −16 | 12,j |
| SU Aur | 04:56:00.4 | +30:34:01.1 | 158 | 2.22 | 12.75 | 2.92 | G4 | I | 5.8 | 1.5 | 53 | 123 | 2, k |
| SW Ori | 05:34:15.8 | −06:36:04.7 | 376 | 1.51 | 3.28 | 7.10 | G8 | I | – | – | – | – | 2 |
| T Tau | 04:21:59.4 | +19:32:06.2 | 144 | 1.94 | 8.88 | 4.01 | K0 | I | – | – | – | – | 6 |
| UX Tau | 04:30:04.0 | +18:13:49.2 | 139 | 2.34 | 8.91 | 1.26 | G8 | I | 5.4 | 2.5 | 40 | −167 | 2, 1 |
Notes. Object coordinates, distances, stellar masses, luminosities, ages, and groups are taken from Valegård et al. (2021) and references therein. See Valegård et al. (2021) for the uncertainties on these values. The spectral types are taken from: (1) Houk (1982), (2) Valegård et al. (2021), (3) Daemgen et al. (2013), (4) Mora et al. (2001), (5) Torres et al. (2006), (6) Herbig (1977), (7) Manoj et al. (2006), (8) Houk & Swift (1999), (9) Houk (1978), (10) Houk (1982), (11) Rydgren & Vrba (1984), (12) Suárez et al. (2006). The inclinations and position angles are taken from: (a) Czekala et al. (2015), (b) Kim et al. (2020), (c) Bi et al. (2020), (d) Cazzoletti et al. (2019), (e) Kataoka et al. (2016), (f) Huang et al. (2018), (g) Kurtovic et al. (2018), (h) Pinilla et al. (2022), (i) Long et al. (2018), (j) Pérez et al. (2014), (k) Ginski et al. (2021), (l) Francis & van der Marel (2020). For the disks with no detection no parameters are given, as indicated by the dashed lines. For the disks with a zero degree inclination and position angle no values were found in the literature, but a mask was applied. The velocities of the Keplerian masks were determined by fitting by eye, such that all emission was enclosed.
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