Table 1
Physical properties and information of millimeter and submillimeter observations of brown dwarfs and planetary-mass objects with nondetected disks.
| Name | d(a), pc | age, Myr | Lc(a), L⊙ × 10−3 | Mc, MJup | a, au | Fν (Зσ), mJy | Fv observed with | Refs.(b) |
|---|---|---|---|---|---|---|---|---|
| G196-3 В | 21.81±0.01 | 50–100 | 0.0927±0.0001 |  |
~350(c) | 0.108 | NOEMA (1.3 mm) | this work |
| VHS J1256–1257 b | 21.15±0.21 | 150–300 | 0.027±0.0001(d) |  |
~170(c) | 0.153 | NOEMA (1.3 mm) | this work |
| 0.060 | ALMA 0.87 mm) | this work | ||||||
| 0.030 | VLA (0.9 cm) | this work(e), 1 | ||||||
| 0.009 | VLA (3 cm) | this work(e), 1, 2 | ||||||
| 0.012 | VLA (5 cm) | this work(e), 1 | ||||||
| 0.024 | VLA (21.4 cm) | this work(e), 1, 2 | ||||||
| CT Cha В |  |
1–3 | 2.38 | 17±5 | ~511 | 0.156 | ALMA(0.88 mm) | 3 |
| 1 RXS 1609 b |  |
5–14 | 0.41 | 12±2 | ~309 | 0.135 | ALMA(0.88 mm) | 3 |
| ROXs 12 В |  |
4–10 | 1.75 | 18±3 | ~243 | 0.213 | ALMA(0.88 mm) | 3 |
| ROXs 42В b |  |
1–3 | 0.83 | 9±2 | ~168 | 0.129 | ALMA(0.88 mm) | 3 |
| DH Tau В |  |
1–3 | 1.82 | 14±3 | ~317 | 0.123 | ALMA(0.88 mm) | 3 |
| FU Tau В |  |
1–3 | 3.13 | 20±4 | ~747 | 0.117 | ALMA(0.88 mm) | 3 |
| PZ Tel В | 47.25±0.05 | 20–25 | 2.6±0.6 | 38–72 | ~23 | 0.084 | ALMA(1.3 mm) | 4, 5,6 |
| 51 Eri b | 29.91±0.07 | 20–25 |  |
2.5–1.5 |  |
0.081 | ALMA(1.3 mm) | 4,7, 8 |
| AB Pic b | 50.14±0.03 | 30–55 |  |
11–18 | ~252 | 0.078 | ALMA(1.3 mm) | 4,9 |
| κ And b | 52.0±0.5 | 40–50 |  |
 |
~55 | 0.18 | ALMA(1.3 mm) | 4, 10 |
| β Piс b |  |
20–25 |  |
 |
 |
0.036 | ALMA(1.3 mm) | 4, 11-13 |
| GSC 6214-2010 В | 108.78±0.25 | 5–14 | 0.447 | 15±2 | 320 | 0.09 | ALMA(0.88 mm) | 14, 15 |
| GQ Lup В | 154.1±0.7 | 3±2 | 3.306 | 10–36 | ~220 | 0.12 | ALMA(0.88 mm) | 14, 16 |
| HD 95086 b | 86.46±0.14 | 17±4 | 0.017 | 4.4±0.8 |  |
0.03 | ALMA(1.3 mm) | 4, 17 |
| 2M 1207 b | 64.7±0.5 | 10±3 | 0.225 | 5±2 | ~40 | 0.078 | ALMA(0.89 mm) | 18 |
| HR 8799 b | 40.88±0.08 |  |
0.007 | 5.8 | 70 | 0.048 | ALMA(1.3 mm) | 4, 19 |
| HR 8799 с | 40.88±0.08 |  |
0.013 | 7–9 | 43 | 0.048 | ALMA(1.3 mm) | 4, 19 |
| HR 8799 d | 40.88±0.08 |  |
0.013 | 7–9 | 26 | 0.048 | ALMA(1.3 mm) | 4, 19 |
| HR 8799 e | 40.88±0.08 |  |
0.013 | 7–9 | 15 | 0.048 | ALMA(1.3 mm) | 4, 19 |
Notes. (a) All the distances were computed from Gaia DR3 (Gaia Collaboration 2016; Lindegren et al. 2021) and the luminocities have been updated accordingly. (b) References for the observed fluxes and systems’ physical parameters. (c) The separation was computed using the latest Gaia DR3 distance. (d) The luminosity of VHS J1256–1257 b was obtained by integrating the photometric observed fluxes (blue dots in Fig. 1) over the extended wavelength range 0.3–100 μm (Simpson’s rule). For more details, readers can refer to Eq. (1) in Zakhozhay et al. (2017). (e) For more details, readers can refer to Climent et al. (2022).
References. (1) Guirado et al. (2018) (2) Climent et al. (2022) (3) Wu et al. (2020); (4) Pérez et al. (2019); (5) Miret-Roig et al. (2018); (6) Maire et al. (2018); (7) Dupuy et al. (2022); (8) De Rosa et al. (2020); (9) Neuhäuser & Schmidt (2012); (10) Currie et al. (2018); (11) Brandt et al. (2021); (12) Chilcote et al. (2017); (13) Matrà et al. (2019); (14) Wu et al. (2017); (15) Bowler et al. (2015); (16) MacGregor et al. (2017); (17) Su et al. (2017); (18) Ricci et al. (2017); (19) Booth et al. (2016).
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