| MAJ_JUP_EVENT_MONITORING | Study of the evolution of unusual phenomena in Jupiter atmosphere, especially in their zonal evolution MAJIS will acquire several “subcubes” with limited number of lines (about 80) as follows:
1. a series of sub-cubes (from 1 to 4) is acquired with the scan mirror to get the coverage of a limited latitude region at all longitudes on the visible side of the planet. Satellite is re-pointed before acquiring each sub-cube
2. the series at previous point is repeated at fixed time intervals (in the order of 1 h, TBC) to monitor the temporal evolution.
Pointing type: YS, Series of OFF-NADIR pointings (‘off-nadir scan mode’)
satellite orientation: HORIZONTAL
Duration:
160 sec for each sub-cube.
Time between series defines actual temporal sampling and is variable (zero data rate here).
Total duration about 5 h (1/2 of rotation period) | MAJIS |
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| MAJ_GCO5000_GLOBAL | Systematic mapping performed with cross-track binning by 4 during circular phase (~120 days)
3 km/pixel, 300x300 km swaths, spatial binning x 4.
Pointing: YS, Nadir
Satellite orientation: MAJIS slit at a slant with the ground track except at the equator
Duration: 4H per orbit (one cube: 6 min) | MAJIS |
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| JAN_SCI_INERTIAL | TBW | JANUS |
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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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| MAJ_JUP_LIMB_SCAN | The MAJIS pointing mirror is used to scan the atmosphere of Jupiter over the limb up to 1500km. Exposure times are optimized for weak limb emissions.
The scan mirror step of 1/10 MAJIS IFOV shall constrain the spatial sampling provides a spatial supersampling adequate to reconstruct, by deconvolution, the signal vertical profile at sub-pixel scale.
Observations consists in sets of max. 8 cubes at different latitudes, around the limb of the planet.
Duration: Typically 20 min for each cube (110 lines), assuming 11 s per line | MAJIS |
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| MAJ_JUP_HIGH_FREQ_MONITORING | The observing type is designed to study the evolution of atmospheric features at high temporal frequency as well as to map specific atmospheric features at regional scale.
Scanning of features on the Jovian disc, on dayside as well as on nightside, with limited latitudinal coverage.
MAJIS will acquire one or more several “subcubes” with a limited number of lines (about between 64 and 160)
Duration: between 84 and 315 s for each cube, assuming 2.1 s per line | MAJIS |
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| 3GM_IO_PLASMA_TORUS_OCCULTATION | The radio science experiment 3GM will use navigation data in X/X and X/Ka band to characterize the Io plasma torus. The data generated by the DST in 2-way dual-frequency radio links will be the primary observable to perform this investigation. Occultations occur throughout the jovian tour, but their phasing is not always synchronized with the timing of dedicated Jupiter observations by the other orbiter experiments. USO will stay MUTED and HAA in nominal SCIENCE.
Note that other observation strategy would be possible (2-way triple link, 1-way X and Ka link with USO UNMUTED). | 3GM |
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| 3GM_JUPITER_OCCULTATION | The radio science experiment 3GM, with its 1-way dual-frequency radio links (X and Ka-band) referenced to an ultrastable oscillator (USO), is performed as JUICE spacecraft moves in and out of occultation. Occultations occur throughout the jovian tour, but their phasing is not always synchronized with the timing of dedicated Jupiter observations by the other orbiter experiments. USO unmuted, HAA in nominal SCIENCE. | 3GM |
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| RPW_In_situ_burst_Radio_burst | The RPWI In-situ_burst + Radio_burst mode: - Makes continuous In-situ_burst mode measurement. In addtion to in-situ_slow modes, In-situ_burst mode adds continuous measurements of electric and magnetic fields at higher cadence (763 smpl/s) as well as more frequent snapshots at higher frequencies (MF - 50 ksmpl/s and HF - 312 ksmpl/s) - Makes full plasma wave measurements and high-time resolution monitoring up to 1.6MHz as well as cover the low frequency and DC electric field and density measurements. | RPWI |
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| RPW_In_situ_burst_Radio_Full | The RPWI In-situ_burst + Radio_Full mode: - Makes continuous In-situ_burst mode measurement. In addtion to in-situ_slow modes, In-situ_burst mode adds continuous measurements of electric and magnetic fields at higher cadence (763 smpl/s) as well as more frequent snapshots at higher frequencies (MF - 50 ksmpl/s and HF - 312 ksmpl/s); - Makes detailed radio emissions from Jupiter as well as moons (Ganymede, Callisto, Europa). Will also support RIME measurements, giving the background natural radio emissions. Monitor the radio emission spectrum as well as polarization. | RPWI |
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| RPW_In_situ_burst_Radar_mode_3 | The RPWI In-situ_burst + Radio_mode_3 mode: - Makes continuous In-situ_burst mode measurement. In addtion to in-situ_slow modes, In-situ_burst mode adds continuous measurements of electric and magnetic fields at higher cadence (763 smpl/s) as well as more frequent snapshots at higher frequencies (MF - 50 ksmpl/s and HF - 312 ksmpl/s); - Radio mode TBD | RPWI |
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| RPW_OBSOLETE_In_situ_low_Radio_burst | The RPWI In-situ_low + Radio_burst mode: - Makes continuous In-situ_low mode measurement, the lowest in-situ possible power and TM, which implements only the Mutual Impedance sweeps and DC electric field measurements; - Makes full plasma wave measurements and high-time resolution monitoring up to 1.6MHz as well as cover the low frequency and DC electric field and density measurements. | RPWI |
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| RPW_IN_SITU_LOW_RADIO_FULL | The RPWI In-situ_low + Radio_Full mode - Makes continuous In-situ_low mode, the lowest in-situ possible power and TM, which implements only the Mutual Impedance sweeps and DC electric field measurements; - Makes detailed radio emissions from Jupiter as well as moons (Ganymede, Callisto, Europa). Will also support RIME measurements, giving the background natural radio emissions. Monitor the radio emission spectrum as well as polarization. | RPWI |
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| RPW_OBSOLETE_In_situ_low_Radar_mode_3 | The RPWI In-situ_low + Radio_mode_3 mode: - Makes continuous In-situ_low mode measurement, the lowest in-situ possible power and TM, which implements only the Mutual Impedance sweeps and DC electric field measurements; - Radio TBD | RPWI |
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| RPW_In_situ_normal_Radio_burst | The RPWI In-situ_normal + Radio_burst mode: - Makes continuous In-situ_normal mode measurement. In addtion to in-situ modes, In-situ_normal mode adds short durations snapshots if electric and magnetic fields at higher frequencies (LF – 763 smpl/s, MF - 50 ksmpl/s and HF - 312 ksmpl/s - Makes full plasma wave measurements and high-time resolution monitoring up to 1.6MHz as well as cover the low frequency and DC electric field and density measurements. | RPWI |
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| RPW_IN_SITU_NORMAL_RADIO_FULL | The RPWI In-situ_normal + Radio_Full mode: - Makes continuous In-situ_normal mode measurement. In addtion to in-situ modes, In-situ_normal mode adds short durations snapshots if electric and magnetic fields at higher frequencies (LF – 763 smpl/s, MF - 50 ksmpl/s and HF - 312 ksmpl/s - Makes detailed radio emissions from Jupiter as well as moons (Ganymede, Callisto, Europa). Will also support RIME measurements, giving the background natural radio emissions. Monitor the radio emission spectrum as well as polarization. | RPWI |
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| RPW_In_situ_normal_Radar_mode_3 | The RPWI In-situ_normal + Radio_mode_3 mode: - Makes continuous In-situ_normal mode measurement. In addtion to in-situ_slows modes, In-situ_normal mode adds short durations snapshots if electric and magnetic fields at higher frequencies (LF – 763 smpl/s, MF - 50 ksmpl/s and HF - 312 ksmpl/s - Radio mode TBD | RPWI |
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| RPW_In_situ_slow_Radio_burst | The RPWI In-situ_slow + Radio_burst mode: - Makes continuous In-situ_slow mode measurement, the basic in-situ modes; - Makes full plasma wave measurements and high-time resolution monitoring up to 1.6MHz as well as cover the low frequency and DC electric field and density measurements. | RPWI |
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| RPW_IN_SITU_SLOW_RADIO_FULL | The RPWI In-situ_slow + Radio_Full mode: - Makes continuous In-situ_slow mode measurement, the basic in-situ modes; - Makes detailed radio emissions from Jupiter as well as moons (Ganymede, Callisto, Europa). Will also support RIME measurements, giving the background natural radio emissions. Monitor the radio emission spectrum as well as polarization. | RPWI |
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| RPW_In_situ_slow_Radar_mode_3 | The RPWI In-situ_slow + Radio_mode_3 mode: - Makes continuous In-situ_slow mode measurement, the basic in-situ modes; - Radio mode TBD | RPWI |
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| MAJ_JUP_LIMB_SLEW | The scan the atmosphere of Jupiter over the limb up to 3000k is performed with a specific slew of the S/C
Individual lines are largely overlapped to provide actual supersampling (x 10) in the spatial domain and allow sub-pixel resolution by deconvolution.
Typically, we have cubes of about 300 lines by 50 pixels (~7500 km)
Pointing type:
OFF-NADIR (nominal pointing position over the Jupiter limb), continuous tracking (‘track tangent limb’)
satellite orientation:LIMB TANGENT (MAJIS slit tangent to the limb), very slow s/c slew to get oversampling (10 lines corresponding to one pixel IFOV)
Duration: 55 min for each cube (300 lines) | MAJIS |
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| SWI_2D_MAP_PS_V1 | This is a multi-purpose mode that can be used on any science target for
any 2D mapping, and meridional or zonal rasters. This mode will also be used for calibration
purposes (e.g. pointing). The number of rows and columns and the stepsize of the raster map is adaptable to the target angular size. Jupiter: Investigation of the global and regional stratospheric
composition and temperature of Jupiter, and pointing calibration. For 2D maps, meridional
scans and zonal scans, two CTS spectra are recorded for 60 seconds over 10000 channels
(16 bits coding). Moon monitoring: Investigation of the spatial distribution of Galilean moons
atmospheric species (+ monitoring), and calibration. Two CTS spectra are recorded for 60 seconds
over 210 channels (16 bits coding). Flybys: Mapping of Galilean Moons’ surface properties
and atmospheric composition, temperature, and winds. Two CTS spectra are recorded for 30 seconds
over 210 channels (16 bits coding). GCO: (1) Investigation of Ganymede’s atmospheric
composition, temperature, and winds, and surface properties by scanning from limb to limb with
the along-track mechanism across the ground-track using the antenna mechanism ( 72 ). Two
CTS spectra are recorded for 10 seconds over 130 channels (16 bits coding). (2) Tomographic
investigation of Ganymede’s atmospheric and surface composition, temperature, and winds by
scanning along-track from 30km to +30km of the nadir axis with 9 steps, using the rocker
mechanism ( 4.3 ), and with 1.5 sec integration time for two CTS spectra over 130 channels
(16 bits coding). In all cases, two CCH measurements (20 bits coding) are recorded for 0.1
second. During GCO, this implies that two CCH measurements are separated by 1/2 beam at
1200 GHz. Position-switch calibration method (the OFF position is observed after each ON of
the map is observed). | SWI |
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| MAG_DL | This observation is introduced to characterize JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints. Only MAGOBS and MAGIBS are operating. | JMAG |
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| MAG_DL_FOB_LIGHT_ONLY | This observation is introduced to characterise JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints In this particular observation FOB fluxgate is powered on with FSC as light-only. | JMAG |
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| MAG_DL_FOB | This observation is introduced to characterise JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints Only MAGOBS is operating. | JMAG |
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| MAG_DL_LIGHT_ONLY | This observation is introduced to characterise JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints.
In this particular observation FIB & FOB fluxgates powered on with FSC as light-only. | JMAG |
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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_AP_FEATURE_SCAN | To assess the evolution of discrete phenomena (e.g., H Ly-alpha bulge, plumes, auroral features) using the AP port and pixellist mode. | UVS |
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| MAJ_ICU | To monitor the radiometric performances of MAJIS using VISNIR and IR sources Specifically, there are several goals
A) tracking the evolution of the actual levels (before subtracting for CDS) in the digital dynamics (0-65535 at 100 kHz, 0-4095 at 1 MHz). Such an evolution could lead to adjust an offset which can be selected by TC (4 settings) so as to avoid reaching digital saturation for the read image before analog saturation.
B) tracking the evolution of the dark current and cosmetics (new hot / dead pixels)
C) tracking the evolution of the overall photometric response as a function of the signal (needed for the pipeline)
Pointing: MAJIS scan mirror oriented towards the ICU (8.5°)
Satellite orientation: Deep space
Duration: 10min | MAJIS |
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| UVS_SAT_STELL_OCC | UVS airglow port stares at a fixed RA and DEC as the satellite occults the star. | UVS |
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| UVS_SAT_SOL_OCC | UVS solar port stares at Sun as the satellite occults it. | UVS |
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| SWI_WARMUP | Warm-up mode. | SWI |
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