Table 4
Summary of the emission of the YSOs.
| # | Source | Spectral | Dust | Ionized emission | X-ray |  |
||
|---|---|---|---|---|---|---|---|---|
| index | VLBA | Variability(3) | Fully or | detection(5) | (1040 | |||
| α(1) | detection | partially | erg s−1) | |||||
| at 5 GHz(2) | non-thermal | |||||||
| emission(4) | ||||||||
| Class 0 | ||||||||
| 1 | J162626.31-242 430.7 | 3.3 ± 0.7/1.2 ± 0.3 | ≤21% | N | Y | Y | ||
| 2 | J162626.39-242 430.8 | 2.9 ± 0.8/1.5 ± 0.5 | ≤21% | N | ||||
| 3 | J162627.83-242 359.3 | ≥4.8/ ≥1.7 | ≤27% | Y | Y | |||
| Class I | ||||||||
| 4 | J162617.24-242 346.0 | ≥2.9/ ≥1.7 | ≤28% | |||||
| 5 | J162621.36-242 304.7 | ≥2.3/ ≥1.0 | ≤8% | |||||
| 6 | J162621.72-242 250.9 | 0.6 ± 0.5/0.5 ± 0.2 | ≤23% | N | Y4.5GHz (†) | Y | ||
| 7 | 162622.27-242 407.1 | … | … | |||||
| 8 | J162623.58-242 439.9 | >4.2/0.8 ± 0.3 | ≤0.2% | N | Y | Y | Y | |
| 9 | 162625.49-242 301.6 | … | ≤100% | |||||
| 10 | J162625.63-242 429.4 | 1.2 ± 0.7/0.3 ± 0.2 | ≤10% | Y | Y7.5GHz (†) | Y | ||
| 11 | 162630.47-242 257.1 | … | ≤100% | Y | ||||
| Class II | ||||||||
| 12 | J162610.32-242 054.9 | 2.3 ± 0.6/1.4 ± 0.2 | ≤77% | N | Y (†) | Y | Y | <74 |
| 13 | J162616.85-242 223.5 | − 5.7 ± 1.0∕−1.9 ± 0.4 | ≤2% | Y | Y | Y | Y | |
| 14 | 162617.06-242 021.6 | … | … | Y | ≲7 | |||
| 15 | 162618.82-242 610.5 | … | … | ≲7 | ||||
| 16 | 162618.98-242 414.3 | … | ≤100% | ≲4 | ||||
| 17 | 162621.53-242 601.0 | … | … | Y | ≲7 | |||
| 18 | J162622.39-242 253.4 | − 5.5 ± 0.4∕−2.4 ± 0.2 | ≤0.5% | Y | Y | Y | Y | <71 |
| 19 | J162623.36-242 059.9 | ≥4.0/ ≥1.4 | ≤18% | Y | Y | Y | <45 | |
| 20 | J162623.42-242 101.9 | ≥0.8/ ≥0.3 | ≤34% | ≲21 | ||||
| 21 | J162624.04-242 448.5 | ≥1.9/ ≥0.7 | ≤1% | Y | ≲28 | |||
| 22 | J162625.28-242 445.4 | … | … | Y | ≲6 | |||
| 23 | 162627.81-242 641.8 | … | … | ≲9 | ||||
| 24 | 162637.79-242 300.7 | … | … | ≲10 | ||||
| 25 | 162642.74-242 427.7 | … | … | ≲14 | ||||
| 26 | 162642.89-242 259.1 | … | … | ≲17 | ||||
| 27 | 162643.86-242 450.7 | … | … | ≲21 | ||||
| Class III | ||||||||
| 28 | 162615.81-241 922.1 | … | … | Y | ≲15 | |||
| 29 | 162622.19-242 352.4 | … | … | ≲4 | ||||
| 30 | J162625.23-242 324.3 | ≥0.3/ ≥0.1 | ≤2% | Y | ≲20 | |||
| 31 | 162631.36-242 530.2 | … | … | Y | ≲6 | |||
| 32 | J162634.17-242 328.7 | 0.3 ± 0.3/0.0 ± 0.1 | ≤0.02% | Y | N | Y | Y | |
Notes. (1) The first spectral index is calculated between 7.5 and 10 GHz, the second between 4.5 and 10 GHz. The uncertainties take into account both the fit uncertainty and the calibration uncertainty. The spectral indices can be significantly affected by variability, as the measurements were carried out at several epochs. (2) Ortiz-León et al. (2017). Y for detection, N for non detection. (3)Dzib et al. (2013) and this study. The sources with the symbol. (†) Correspond to the sources that only present variability (>25%) in Dzib et al. (2013). (4)Y for the sources expected to present non-thermal emission based on the criteria discussed in the text (VLBA detection, variability, and spectral indices). Some of these sources could also be sources with thermal emission but abnormally high variability. (5) Imanishi et al. (2003). (6) EUV luminosities reaching the disks calculated from the fluxes or 3σ noise levels measured in our VLA images at 10 GHz (3 cm) and using Eq. (2) of Pascucci et al. (2012) and a distance of 137 pc for the Oph A cluster.
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