| SWI_2D_MAP_FS_V1 | Same as SWI 2D MAP PS, except a frequency-switch calibration mode is
used instead of position-switch. It enables spending 100% of the integration time on-source. If
the purity of the spectral band is good enough, there is an option to pre-compute ON-OFF for
the CTS before downlink. | SWI |
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| SWI_NADIR_STARE_PS | Investigation of the atmospheric composition (and temperature) of Jupiter
and the Galilean moons. This mode is nominally meant for deep integrations and requires numerous
repetitions (e.g. monitoring of the moons). Two CTS spectra are recorded for 60 seconds
over 10000 channels (16 bits coding). Position-switch calibration method. | SWI |
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| SWI_WARMUP | Warm-up mode. | SWI |
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| SWI_STANDBY | Only the instrument DPU will be switched on and be able to accept instrument commands. Only housekeeping telemetry is generated in this mode. | SWI |
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| SWI_OFF | All instrument subsystems including the DPU will be switched off. Consequently there will be no housekeeping data and no telemetry. The instrument will be in this mode during launch and cruise phase, except during calibration campaigns (e.g. planet flybys). | SWI |
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| MAG_CALROLL | Campaign of spacecraft rolls to allow calibration of J-MAG magnetic field measurements. J-MAG will take data in gradiometer mode continuously while the spacecraft rolls about two principal axes, in regions where the Jovian magnetic field is >100 nT. Spacecraft rolls about two principal axes. 3 rolls of 360° about first axis at 0.5 rev/hr, then 3 rolls about the second axis (also at 0.5 rev/hr). The spacecraft rotation axes must always make an angle with the ambient magnetic field between 20° and 160°. | JMAG |
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| MAG_BURST | Operation of J-MAG in burst mode (measurement at rate of 128 vectors/s) starting 10 minutes before and ending 10 minutes after a predicted crossing of a thin current sheet in Ganymedes magnetosphere (magnetopause/magnetotail current sheet). | JMAG |
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| MAG_CONTINOP | measure the magnetic field in normal mode (at a rate of 32 vectors/s) continuously | JMAG |
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| UVS_IO_TORUS_SCAN | Map emissions from the Io torus. Slit aligned parallel with Jupiter's rotation pole, scanned E-W across the torus | UVS |
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| UVS_JUP_SP_SOL_OCC | The large solar disc and the substantial distance from Jupiter mean that this will not provide the same vertical resolution as stellar occultations, but are useful for measurements of minor/trace constituents due to high S/N. This uses a fixed scan through the Solar Port (SP) at a selected RA and DEC, holding the pointing for an extended amount of time. Note: Here histograms, but pixellist mode possible. | UVS |
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| UVS_JUP_HP_STELL_OCC | For bright stars, use the High spatial resolution port (HP) for higher contrast of star signal to Jupiter background signal. Used also as calibration reference standards. | UVS |
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| UVS_JUP_AP_STELL_OCC | For moderately bright stars. Stars serve as a point source to provide good vertical resolution on Jupiter’s atmosphere. The field of view is pointed to a given RA and DEC and pointing held for an extended amount of time. The majority of the data can be omitted except for that of the star on the detector, so these can be done within a good data budget. Full spectral coverage. Note: Here, “moderate, histogram modeâ€, but pixellist or histogram mode low or high possible. | UVS |
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| UVS_JUP_HP_LIMB_SCAN | Same as UVS_JUP_AP_LIMB_SCAN but through the HP port | UVS |
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| UVS_JUP_AP_LIMB_SCAN | Monitoring auroral and airglow emissions in limb scans which requires a continuous S/C motion to point to limb and scan over planetary limb, using the AP port. Observation performed in pixel list mode to reach a time resolution of 0.001 s. | UVS |
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| UVS_JUP_HP_FEATURE_SCAN | To assess the evolution of discrete phenomena (e.g., H Ly-alpha bulge, plumes, auroral features,…) using the HP port and pixellist mode. | UVS |
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| UVS_JUP_HP_SCAN_MAP | Same as UVS_JUP_AP_SCAN_MAP but for High spatial resolution Port (HP). Scan the UVS slit in the cross slit direction across a region (e.g., auroral (N or S)) or entire disk using the Airglow (AP) port, scan at a constant rate across Jupiter to produce a map. Observation performed in pixel list mode to reach a time resolution of 0.001 s. | UVS |
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| UVS_JUP_AP_SCAN_MAP | Scan the UVS slit in the cross slit direction across a region (e.g., auroral (N or S)) or entire disk using the Airglow (AP) port, scan at a constant rate across Jupiter to produce a map. Observation performed in pixel list mode to reach a time resolution of 0.001 s. | UVS |
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| UVS_JUP_HP_AIRGLOW_STARE | Same as UVS_JUP_AP_AIRGLOW_STARE but for High spatial resolution Port (HP). Monitoring auroral and airglow emissions in stare mode using the Airglow Port (AP). Slit held along Jupiter' s North/South and on the central meridian, while Jupiter rotates below S/C creating a map. Histogram mode. | UVS |
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| UVS_JUP_AP_AIRGLOW_STARE | Monitoring auroral and airglow emissions in stare mode using the Airglow Port (AP). Slit held along Jupiter' s North/South and on the central meridian, while Jupiter rotates below S/C creating a map. Histogram mode. | UVS |
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| UVS_GCO_HP | High spatial resolution observations of Ganymede's aurora to look for small scale features | UVS |
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| UVS_GCO_HISTOGRAM_002 | Similar to observation 001 but with Increased time sampling to capture auroral morphology and variability | UVS |
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| UVS_GCO_HISTOGRAM_001 | Monitoring auroral emissions and surface reflectance during GCO. Limited spectral resolution. | UVS |
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