Table 2
Image sensitivities and inferred planetary radio luminosity limits.
| Epoch | Center | Stokes I | Stokes I | Stokes V | Luminosity |
|---|---|---|---|---|---|
| frequency | global | local | global | limit (3σ) | |
| (MHz) | (mJy beam−1) | (erg s−1) | |||
| 2015 August 30 (off) | 54 | 1.2 | 1.6 | 1.0 | … |
| 42 | 2.0 | 2.6 | 1.5 | … | |
| 2015 October 24 (pre-periastron)(a) | … | … | … | … | … |
| 2015 October 25 (pre-periastron) | 54 | 2.3 | 4.0 | 1.7 | 1.8 × 1023 |
| 42 | 3.9 | 6.9 | 2.7 | 2.3 × 1023 | |
| 2015 October 27 (post-periastron) | 54 | 3.6 | 7.1 | 2.5 | 2.6 × 1023 |
| 42 | 6.8 | 13.2 | 4.3 | 3.7 × 1023 | |
| 2015 October 30 (post-periastron) | 54 | 1.6 | 1.9 | 1.3 | 1.4 × 1023 |
| 42 | 2.6 | 3.3 | 2.1 | 1.8 × 1023 | |
Notes. Values for the full band (30–78 MHz) are referenced to a center frequency of 54 MHz; values for the lower half of the band (30–54 MHz) are referenced to a center frequency of 42 MHz. Luminosity limits are obtained from the Stokes V images. In converting from flux density to luminosity, isotropic radiation and an emission bandwidth on the order of the observing frequency are assumed. (a)Because of ionospheric conditions, no good data were obtained on 2015 October 24.
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