| MAJ_HEATER_SURVIVAL | The FPEs (IR/VISNIR) shall be kept at T > 120K. This function is covered by the Survival Heater lines that are controlled by the S/C.
Two cases can be foreseen: the two heaters are activated and only one is ON (most realistic case based on thermal analysis) | MAJIS |
|---|
| MAJ_JUP_RING | Observations of the main rings (2 ansa) at a given phase (backscattering to forward scattering light), no tracking of azimuthal structure, no spatial binning to increase spatial resolution | MAJIS |
|---|
| JAN_SCI_STARE | 1 frame observation
Children observation defined during scenarios (derived from list in JAN_SCI_RASTER):
│ ├── JAN_SCI_STARE_AMALTHEA
│ ├── JAN_SCI_STARE_AURORAS
│ ├── JAN_SCI_STARE_FEATURES
│ ├── JAN_SCI_STARE_IO
│ ├── JAN_SCI_STARE_LIGHTNING
│ ├── JAN_SCI_STARE_POLAR_SOUTH | JANUS |
|---|
| RPW_20_T11_4_HF_BURST_MIME_OFF | Input by RPWI pending. | RPWI |
|---|
| RPW_19_T11_1_HF_BURST_MM_TRACKING_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_18_T11_3_HF_BURST_MM_TRACKING_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_17_T11_3_HF_SWEEP_FULL_MM_WIDE_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_16_T11_2_HF_BURST_MM_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_15_T11_2_HF_SWEEP_FULL_MM_WIDE_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_14_T11_4_HF_SWEEP_FULL_MIME_OFF | Input by RPWI pending. | RPWI |
|---|
| RPW_13_T10_2_HF_SWEEP_FULL_MIME_OFF | Input by RPWI pending. | RPWI |
|---|
| RPW_12_T11_1_HF_SWEEP_FULL_MM_TRACKING_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_11_T11_2_HF_SWEEP_FULL_MM_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| 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 |
|---|
| RPW_10_T11_1_HF_SWEEP_FULL_MM_BFIELD_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_9_T11_1_HF_PSSR3_MM_TRACKING_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_8_T11_2_HF_PSSR3_MM_WIDE_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_7_T11_1_HF_PSSR3_MM_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_6_T11_1_HF_PSSR2_MM_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_5_T11_1_HF_PSSR1_MM_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_4_T11_2_HF_SWEEP_FULL_MM_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| RPW_3_T10_1_HF_SWEEP_FULL_MIME_OFF | Input by RPWI pending. | RPWI |
|---|
| RPW_2_T11_1_HF_BURST_MM_TRACKING_ID | Input by RPWI pending | RPWI |
|---|
| RPW_1_T11_1_HF_BURST_MM_SWEEP_ID | Input by RPWI pending. | RPWI |
|---|
| 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 |
|---|
| JAN_CONFIG_ALLON | No observations, but instrument ON for thermal stabilization of the complete electronics (PEU and detector are ON) and for setting the observation sequences and between two observation sequences that are too close to switch the detector OFF. | JANUS |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_LOW_2 | Far approach from moon (flyby), setting up NIM filament | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_IMAGING_BURST_2 | *Burst in-situ mode, magnetosphere
*CA of moon flybys with JNA/JENI imaging and high time (plume) resolution for NIM | PEPLO |
|---|
| PEH_IDLE_1 | IDLE may include a sensor on HV but not taking science data, values to be updated
* Macro: 100 | PEPHI |
|---|
| PEH_STBY_1 | Different STBY versions may include different sensors on, in Low voltage
* Macro: 100 | PEPHI |
|---|
| PEH_OFF_1 | PEP-Hi off
* Macro: 0 | PEPHI |
|---|
| PEH_GANYMEDE_IN_SITU_NOMINAL_1 | * Regular in-situ mode, ganymede phase
*CA of moon flybys later in the mission (higher power consumption)
*Good for high quality, extended survey
* Macro: 118
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_GANYMEDE_IN_SITU_BURST_1 | *Burst in-situ mode, ganymede phase
*CA of moon flybys
*Short duration events (e.g. boundary crossings)
* Macro: 122 | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_IMAGING_LOW_1 | *Low power in-situ & ENA imaging mode (e.g. downlink, non-prime/low priority science sgments
* Macro: 142
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_LOW_1 | *Low power in-situ mode
(e.g. downlink, non-prime/low priority science sgments)
* Macro: 110
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_BURST_1 | *Burst in-situ mode, magnetosphere
*CA of moon flybys
*Short duration events (magnetopause/bow shock crossings, injection events, moon wakes/microsignatures)
* Macro: 121
Sensors: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_IMAGING_BURST_1 | *Regular magnetosphere in-situ
& ENA imaging monitoring mode
* Macro: 148b
Sensors ON: JENI, JoEE. | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_NOMINAL_1 | *Regular magnetosphere in-situ
monitoring mode
*Can work on flybys
* Macro: 117
Sensors ON: JENI, JoEE | PEPHI |
|---|
| PEH_JUPITER_IN_SITU_IMAGING_NOMINAL_1 | *Low power in-situ & ENA imaging mode (e.g. downlink, non-prime/low priority science sgments
* Macro: 142
Sensors ON: JENI, JoEE | PEPHI |
|---|
| UVS_DECONTAMINATION | Not a true observation, but included so other instruments are aware that our heaters are on | UVS |
|---|
| UVS_CALIBRATION | Generic calibration observation - may include star stare, flip ridealong, or dark/radiation observations. Data rate is an estimated average. | UVS |
|---|
| UVS_IO_TORUS_SCAN | Map emissions from the Io torus. Slit aligned parallel with Jupiter's equator, scanned N-S across one ansa of the torus, then move in four steps to the other ansa, repeating the N-S motion each time | UVS |
|---|
| UVS_JUP_MONITORING_HP | As above, more of an auroral focus. 2-hour observations fit in between the AP monitoring observations | UVS |
|---|
| UVS_JUP_MONITORING_AP | Replaces previous monitoring stare. We perform a slow scan across the disk: assume 3 seconds per slit width, so 0.033 / s scan rate | UVS |
|---|
| SWI_2D_MAP_OTF_CCH_V1 | Similar to SWI 2D MAP PS, but using an on-the-fly recording sequence,
i.e. the OFF position per map row is only observed once. | SWI |
|---|
| SWI_2D_MAP_OTF_V1 | Similar to SWI 2D MAP PS, but using an on-the-fly recording sequence,
i.e. the OFF position per map row is only observed once. | SWI |
|---|
| SWI_NADIR_STARE_FS_V1 | Same as SWI NADIR STARE 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 |
|---|
| SWI_NADIR_STARE_PS_V1 | 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 |
|---|
| SWI_TSYS_ACS_CCH_V1 | Spectral scan to measure the system temperature spectra of the 2 bands with
the ACS & CCH 1 & 2 by observing the hot load and cold sky. Integration time on ACS is 1
second. A single execution can cover up to 15 tunings. | SWI |
|---|
| UVS_SAT_LIMB_SCAN_HP | Similar to disc scan observations, but holding the pointing relative to the limb during flyby sequences. | UVS |
|---|
| UVS_SAT_LIMB_SCAN_AP | Similar to disc scan observations, but holding the pointing relative to the limb during flyby sequences. | UVS |
|---|
| UVS_SAT_LIMB_STARE_HP | Search for faint atmospheric emissions by building signal to noise through long integrations. | UVS |
|---|
| UVS_SAT_LIMB_STARE_AP | Search for faint atmospheric emissions by building signal to noise through long integrations. | UVS |
|---|
| UVS_SAT_DISK_SCAN_HP | Construct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics. | UVS |
|---|
| UVS_SAT_DISK_SCAN_AP | Construct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics. | UVS |
|---|
| UVS_NC_STARE | Characterize the Io/Europa neutral clouds in the immediate vicinity of the satellite. Center satellite in slit. Align the slit with the satellite orbital plane | UVS |
|---|
| UVS_IO_TORUS_STARE | Monitor emissions from the Io torus. Slit aligned parallel with Jupiter's equator. | UVS |
|---|
| UVS_GCO_HISTOGRAM_003 | Similar to observation 001 but with increased spectral resolution to achieve < 2 nm resolution between 100 and 200 nm as specified in SciRD | UVS |
|---|
| 3GM_BISTATIC_RADAR | Characterization of the surface by determination of roughness, dielectric constant of surface material and material density. The chosen antenna points towards surface, radio signal reflects from surface and received on ground. USO unmuted. The HAA shall be in SCIENCE to calibrate the sloshing potentially excited by pointing the HGA toward a moon’s Surface. | 3GM |
|---|
| 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 |
|---|
| 3GM_GRAVITY_TOUR | Gravity measurement during flyby requires the use of the HGA.
KaT and HAA should be operating during gravity measurement
USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach.
HAA should be in CONFIGURATION mode at least 48 hours before the gravity measurement.
The observation should start with 1 hour of HAA in SELF_CALIBRATION mode. KaT starts with 10min of warm-up.
Additional X/X and X/Ka (DST) link may be required whenever the Sun-
Earth-Spacecraft angle is < 60 deg to cancel noise due to the solar wind plasma | 3GM |
|---|
| 3GM_GRAVITY_GCO500_200 | Gravity measurement during GCO500 and GCO200 will use the HGA during downlink sessions. If not possible, it will use the MGA. KaT and HAA should be operating during gravity measurement. USO is OFF during this phase (except in case of BSR opportunity). HAA should be in STANDBY mode at least 48 hours before the gravity measurement. The observation should start with 1 hour of HAA in SELF_CALIBRATION mode. KaT starts with 10min of warm-up. | 3GM |
|---|
| 3GM_GRAVITY_FLYBYS | Gravity measurement during flyby requires the use of the MGA.
KaT and HAA should be operating during gravity measurements
USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach.
HAA should be in CONFIGURATION mode at least 48 hours before the gravity measurement.
The observation should start with 1 hour of HAA in SELF_CALIBRATION mode. KaT starts with 10min of warm-up.
Additional X/X and X/Ka (DST) link may be required whenever the Sun-
Earth-Spacecraft angle is < 60 deg to cancel noise due to the solar wind plasma. | 3GM |
|---|
| UVS_JUP_ROLL_SCAN | Point to nadir. Rotate about nadir so that we scan a circle (or a fraction of a circle - e.g. covering the auroral regions) over Jupiter's disk. Rotation rate ~0.1 degree per second | UVS |
|---|
| GAL_GAN_OFF_POINTING | science mode for Ganymede off-nadir operations. | GALA |
|---|
| GAL_WARMUP_GAN | Active operation for laser warmup. This observation shall be used before real science measurements, e.g. before closest approach. | GALA |
|---|
| JAN_SCI_INERTIAL | TBW | JANUS |
|---|
| JAN_SCI_LIMB | Children observations defined during scenarios
│ ├── JAN_SCI_LIMB_HAZES
│ ├── JAN_SCI_LIMB_HIGHPHASE
│ ├── JAN_SCI_LIMB_POLAR_SOUTH | JANUS |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_7 | Mode with only NIM on (ion) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the ionosphere.
PEPLo Sensors ON: NIM ion on, only | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_6 | Mode with only NIM on (neutral) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the exosphere.
PEPLo Sensors ON: NIM neutral on, only | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_NOMINAL_3 | Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey in charged particles. NIM, JNA off.
PEPLo Sensors ON: JDC, JEI on, JNA & NIM off | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_NOMINAL_2 | Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey. All instruments on, NIM in ion mode (response of ionosphere to charged particles).
PEPLo Sensors ON: All sensors ON, NIM, JNA ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_NOMINAL_1 | Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey. All instruments on, NIM in neutral mode (response of exosphere to charged particles).
PEPLo Sensors ON: All sensors ON, NIM neutral mode, JNA ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_BURST_1 | Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ
PEPLo Sensors ON: All sensors ON, NIM neutral mode, JNA ion mode | PEPLO |
|---|
| RIM_GANYMEDE_O1_1 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_O1_2 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_O1_4 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N4 | Passive Radar Acquisitions on Jovian side of Ganymede. | RIME |
|---|
| RIM_GANYMEDE_N3_1 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N3_2 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N3_4 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N2_1 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N2_2 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N2_4 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N1_1 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N1_2 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N1_4 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_FLYBY | RIME flyby observations or observations without on-board processing. | RIME |
|---|
| NAVCAM_DVOL_BLOCK | | JUICE |
|---|
| 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 |
|---|
| 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 |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_2 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JE 4 sectors, JDC low power). NIM neutral, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments.
PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Neutral mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_5 | Same as PEP_GANYMEDE_IN_SITU_LOW_1 but with lowest performance in JDC, JEI for max power savings while PEP-Lo is no (JEI 4 sectors, JDC low power). NIM, JNA off. Low power mode for Ganymede, good for long duration surveys.
PEPLo Sensors ON: JDC_LP, JEI 4 sectors, JNA & NIM off | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_LOW_1 | Low power in-situ mode (e.g. downlink, non-prime/low priority science sgments)
PEPLo Sensors ON: JDC_LP, JEI (8 sectors) | PEPLO |
|---|
| PEL_JUPITER_IN_SITU_BURST_1 | Burst in-situ mode for magnetosphere, CA of moon flybys (if NIM offl), Short duration events (magnetopause/bow shock crossings, injection events, moon wakes/microsignatures)
PEPLo Sensors ON: JDC, JEI | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_3 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JEI 4 sectors, JDC low power). NIM ion, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments.
PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_4 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JEI 4 sectors, JDC low power). NIM ion, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments.
PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_BURST_2 | Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ
PEPLo Sensors ON: All sensors ON, NIM, JNA ion mode | PEPLO |
|---|
| PEL_GANYMEDE_IN_SITU_LOW_1 | Same as PEP_GANYMEDE_IN_SITU_NOMINAL_3 but with low performance in JDC, JEI to limit power (JEI 8 sectors, JDC low power). NIM, JNA off. Low power mode for Ganymede, good for long duration surveys
PEPLo Sensors ON: JDC_LP, JEI (8 sectors) | PEPLO |
|---|
| MAG_CONTINOP_FIB_FOB_LIGHT_ONLY | JMAG mode (FIB FOB Light Only), this mode ensures that while FIB and FOB are collecting science the Scalar sensor also has power to its laser but is not collecting science data. This helps to protect the fibres from radiation damage, necessary for the Europa phase due to its radiation environment. | JMAG |
|---|