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9 km deep penetration mode
RIME observations up to 9 km deep




Antenna pattern (apparent FOV) is ideally a uniform toroid around the dipole, but recent analysis shows high pattern dependency on solar panel rotation. Worst case is when solar panels are parallel to the antenna, the pattern gets deformed (up to ~50% directivity on +Z boresight for some frequencies, ~1.2dB). This is currently under analysis/discussion with Project/Airbus to find solutions. SOC/PS to be aware and maybe track this for operational implications.
any rule that is used to schedule the observation: repetition rules, continuous (plasma instruments), one-off, every orbit, every day, etc
conditions that make the observation not possible (e.g. thruster firing)
RIME must be operated on the anti-Jovian side of Ganymede since it is affected by Jupiter radio emission. The part of the surface shielded from Jupiter radio emission is a roughly circular area centred at 180°E, 0°N having a ~3000 Km radius. Because of the intermittent nature of Jupiter radio emission, and the possibility to produce predictions of its intensity, observations on the Jovian side of Ganymede are in principle also possible. RIME has to be switched on five minutes before beginning data acquisition to allow the warm-up of the master oscillator and will be switched off as soon as data acquisition ceases (TBC). It is recommended that the instrument is not switched off between acquisitions, if the time interval between them is less than a few to several hours (TBC). Note: having a pointing change from pushbroom nadir to power-optimized nadir during RIME observations is acceptable. The observation strategy for GCO500 is based on the following assumptions: – Distribute observations as evenly as possible in time. – Produce an average of 280 Mbits/day. – Restrict the total data volume to less than 40 Gbits