Table 2
Radius and mass upper limits and temperature of potential dusty disks around brown dwarf and planets with nondetections.
| Name | Rout(a) (au) | Td (K) | Mdust(b) (M⊕) | Mdust,20K(c) (M⊕) | Fν(d) observed with |
|---|---|---|---|---|---|
| G196-3 B | 29.5 | 5.3 | 0.014 | 0.0015 | NOEMA (1.3 mm) |
| VHS J1256–1257 b | 18.1 | 4.5 | 0.028 | 0.0019 | NOEMA (1.3 mm) |
| 0.005 | 0.00019 | ALMA 0.87 mm) | |||
| 0.500 | 0.098 | VLA (0.9 cm) | |||
| 4.889 | 1.06 | VLA (3 cm) | |||
| 29.535 | 6.5 | VLA (5 cm) | |||
| 4519.046 | 1015.1 | VLA (21.4 cm) | |||
| CT Cha B | 32.0 | 10.9 | 0.111 | 0.040 | ALMA(0.88 mm) |
| 1 RXS1609 b | 16.9 | 7.4 | 0.118 | 0.018 | ALMA(0.88 mm) |
| ROXs 12 B | 15.1 | 10.1 | 0.092 | 0.029 | ALMA(0.88 mm) |
| ROXs 42B b | 8.2 | 11.1 | 0.052 | 0.020 | ALMA(0.88 mm) |
| DH Tau B | 21.7 | 11.7 | 0.037 | 0.016 | ALMA(0.88 mm) |
| FU Tau B | 101.0 | 8.7 | 0.060 | 0.014 | ALMA(0.88 mm) |
| PZ Tel B | 2.0 | 60.7 | 0.001 | 0.0053 | ALMA(1.3 mm) |
| 51 Eri b | 0.3 | 128.5 | 3×10−4 | 0.0021 | ALMA(1.3 mm) |
| AB Pic b | 15.0 | 6.4 | 0.035 | 0.0056 | ALMA(1.3 mm) |
| κ And b | 2.2 | 113.4 | 0.002 | 0.014 | ALMA(1.3 mm) |
| β Pic b | 0.4 | 152.1 | 4×10−5 | 0.00039 | ALMA(1.3 mm) |
| GSC 6214-2010 B | 18.5 | 7.5 | 0.047 | 0.0076 | ALMA(0.88 mm) |
| GQ Lup B | 13.9 | 18.9 | 0.022 | 0.020 | ALMA(0.88 mm) |
| HD 95086 b | 1.8 | 60.9 | 0.002 | 0.0064 | ALMA(1.3 mm) |
| 2M 1207 b | 5.1 | 12.1 | 0.005 | 0.0023 | ALMA(0.89 mm) |
| HR 8799 b | 2.5 | 51.2 | 7×10−4 | 0.0023 | ALMA(1.3 mm) |
| HR 8799 c | 1.7 | 65.3 | 6×10−4 | 0.0023 | ALMA(1.3 mm) |
| HR 8799 d | 1.0 | 84.0 | 4×10−4 | 0.0023 | ALMA(1.3 mm) |
| HR 8799 e | 0.6 | 110.6 | 3×10−4 | 0.0023 | ALMA(1.3 mm) |
Notes. (a) Dust disk radii derived in this work as described in Sect. 4. (b) Dust masses were computed using Eq. (1) and Td, computed using the approach described in Sect. 4 and listed here. (c) Dust masses were computed using Equation 1 and a constant Td = 20 K as in Testi et al. (2022). (d) The instruments employed for collecting the information on Fν were used for the calculation of Mdust.
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