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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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