Table 4
Summary of detected signals and derived planetary parameters assuming that the emission originates from the planet (see Sect. 6 for a discussion of the arguments for and against a planetary origin for the signals).
| Planet | LOFAR | ν | Polarization | Q# | Signifi- | Figure | Flux | Power | TB | Magnetic |
|---|---|---|---|---|---|---|---|---|---|---|
| name | Obs ID | (MHz) | (|V |, V+, V-) | cance (σ) | (mJy) | (W) | (K) | field (G) | ||
| τ Boo b | L570725 | 21-30 | |V |, V+ | Q1a | 6.9 | 5 | 190 ± 30 | 6.3 × 1014−15 | 4.2 × 1017 | 7.5-10.7 |
| τ Boo b | L570725 | 21-30 | |V |, V+ | Q1b | 8.6 | 5 | 430 ± 30 | 1.4 × 1015−16 | 1.0 × 1018 | 7.5-10.7 |
| τ Boo b | L569131 | 15-21 | |V |, V- | Q4f | 3.2 | 4 | 890 |
2.0 × 1015−16 | 2.0 × 1018 | 5.4-7.5 |
Notes. Column 1: planet name. Column 2: LOFAR observation ID. Column 3: frequency range of the detection. Column 4: polarization signature of the emission. Column 5: observable quantity that found the detection. Column 6: statistical significance derived using Gaussian simulations. Column 7: respective figures showing the detected signals. Column 8: estimated flux density of the emission. Column 9: estimated power of the emission. Column 10: brightness temperature of the tentative emission. Column 11: maximum polar surface magnetic field of the planet derived using the maximum frequency, assuming CMI emission.
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