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OBSOLETE_RPWI_In_situ_low_Radio_burstThe 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
OBSOLETE_RPWI_In_situ_low_Radar_mode_3The 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 TBDRPWI
RPWI_In_situ_low_Radio_FullThe 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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SWI_SAFEMode used for USO stabilization prior to warm-up. As it takes several weeks to stabilize the USO, the latter should remain ON all the time in the science phase. Mode into which the instruments switches autonomously in case of an instrument anomaly is detected or if no more science operations are in the queue. Mode to be used during downlink. Only housekeeping telemetry is generated in this mode.SWI
SWI_NADIR_STARE_FSSame 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_MOON_NADIR_STARE_FSSame as SWI_MOON_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. Flyby: Two CTS spectra are recorded for 30 sec over 210 channels (16 bits coding). GCO: Two CTS spectra are recorded for 10 sec over 130 channels (16 bits coding). In both cases, two CCH measurements (20 bits coding) are recorded for 0.1 sec. Solar occultation: Two CTS spectra are recorded for 60 seconds over 10000 channels (16 bits coding), and two CCH measurements (20 bits coding) are recorded for 0.1 second. 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_MOON_LIMB_SCAN_FSSame as SWI_MOON_LIMB_SCAN_PS, except a frequency-switch calibration mode is used instead of position-switch. It enables spending ∼100% of the integration time on-source. Flyby: The atmospheric limb is rapidly scanned to achieve 5km vertical resolution. Two CTS spectra are recorded for 1.5 sec over 210 channels (16 bits coding). GCO: Page 16/156 Sub Millimetre Wave Instrument for JUICE (SWI) The atmospheric limb is scanned up and down rapidly with 10 km altitude steps and with 1.5 sec integration time for two CTS spectra over 130 channels (16 bits coding). 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_MOON_LIMB_STARE_FSSame as SWI_MOON_LIMB_STARE_PS, except a frequency-switch calibration mode is used instead of position-switch. It enables spending ∼100% of the integration time on-source. Flyby: Two CTS spectra are recorded for 30 sec over 210 channels (16 bits coding). GCO: Two CTS spectra are recorded for 30 sec over 130 channels (16 bits coding) and a different altitude (5, 10, 20, 40, and 50 km) is scanned every orbit. 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_JUP_LIMB_RASTER_FSSame as SWI_JUP_LIMB_RASTER_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_JUP_LIMB_RASTER_PSInvestigation of Jupiter’s stratospheric winds, temperature and composition, targeting one (or more) molecular line(s) at the planetary limb with a 3◦ resolution in latitude. The investigation of Jupiter’s stratospheric dynamics (winds) requires measuring the Doppler shifts induced by zonal winds on strong lines. The observations require a very high signalto-noise ratio (∼100) and a very high spectral resolution (100kHz). Similar requirements for the investigation of Jupiter’s stratospheric chemical inventory and temperature as a function of latitude. At each limb position, a short ∼10-point across-limb scan of the continuum emission is performed with the CCH to derive a posteriori the instrument pointing. Two CTS spectra are recorded for 60 seconds over 10000 channels (16 bits coding), and two CCH measurements (20 bits coding) are recorded for 0.1 second. Position-switch calibration method.SWI
SWI_JUP_LIMB_STARE_FSSame as SWI_JUP_LIMB_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 precompute ON-OFF for the CTS before downlink.SWI
SWI_JUP_LIMB_STARE_PSInvestigation of Jupiter’s stratospheric composition and temperature by targeting one (or more) molecular line(s) at the planetary limb. The retrieval of vertical profiles require a very high signal-to-noise ratio (∼100) and a very high spectral resolution (100kHz). A coarser spectral resolution (i.e. 500kHz) is sufficient for detections. This mode is nominally meant for deep integrations and implies numerous repetitions. A short ∼10-point across-limb scan of the continuum emission is performed with the CCH to derive a posteriori the instrument pointing. Two CTS spectra are recorded for 60 seconds over 10000 channels (16 bits coding), and two CCH measurements (20 bits coding) are recorded for 0.1 second. Position-switch calibration method.SWI
SWI_SPECTRAL_SCAN_CTS_FSSame as SWI_SPECTRAL_SCAN_CTS_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 precompute ON−OFF for the CTS before downlink. A single execution can cover up to 9 tuningsSWI
SWI_SPECTRAL_SCAN_ACS_PSInvestigation of the atmospheric composition of Jupiter and the Galilean moons. The whole frequency range available to SWI is scanned. This mode is nominally meant for deep integrations and requires numerous repetitions (e.g. monitoring of the moons). Two ACS spectra are recorded every 60 seconds over 1024 channels (16bit coding). Position-switch calibration method.SWI
OBSOLETE_SWI_SOLAR_OCCULTATION_PSUse a solar occultation to observe a weak molecular line in the atmosphere of Jupiter or the Galilean Moons. This mode can also be used for Europa torus solar occultations. Two CTS spectra are recorded every 60 seconds over 10000 channels (16 bits coding), and two CCH measurements (20 bits coding) are recorded every 0.1 second. Position-switch calibration method.SWI
SWI_2D_MAP_PSThis 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 every 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 every 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 every 30 seconds over 210 channels (16 bits coding).SWI
SWI_5POINT_CROSS_PSInvestigation of the Jovian and Galilean moon atmospheric composition, and Galilean surface properties by means of rough raster mapping. The stepsize is such that the opposite ends of the cross are separated by the size of the target in the given direction. For Jupiter, two CTS spectra are recorded every 60 seconds over 10000 channels (16 bits coding). For moon monitoring, two CTS spectra are recorded every 30 seconds over 210 channels (16 bits coding). For both cases, and in parallel, two CCH measurements (20 bits coding) are recorded every 0.1 second. Position-switch calibration method.SWI
SWI_5POINT_CROSS_FSSame as SWI 5POINT CROSS 12 PS, except a frequency-switch calibration mode is used instead of position-switch. It enables spending ~100% of the integration time on-source. For Jupiter, two CTS spectra are recorded every 60 seconds over 10000 channels (16 bits coding). For moon monitoring, two CTS spectra are recorded every 30 seconds over 210 channels (16 bits coding). For both cases, and in parallel, two CCH measurements (20 bits coding) are recorded every 0.1 second. If the purity of the spectral band is good enough, there is an option to pre-compute ON-OFF for the CTS before downlink. Frequency-switch calibration method for CTS data.SWI
PEP_IDLEPEP in IDLE mode PEP
PEP_CALLISTO_DEPARTURE_NIMAll sensors on. NIM in a different mode than during approachPEP
JMAG_DLThis 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
RPWI_DLRPWI observation during downlink windowsRPWI
PEP_JUPITER_EQUATORIAL_DLMode for ensuring continuous coverage for in-situ particle plasma measurements while optimizing power and data volume. Should be on during downlink too. JDC and JEI on. Applies also to Jupiter High Inclination for now.PEP
UVS_JUP_DEFAULTdefault pointing to be inserted at the start and end of the timelineUVS
UVS_EUR_LIMB_HIGH_RESAlign the slit with Europa's equatorUVS
OBSOLETE_RPWI_EUR_BURSTObservation with set up for closest approachRPWI
OBSOLETE_RPWI_EUR_FULLThe full mode for RPWI observationRPWI
OBSOLETE_RPWI_EUR_NORMNormal RPWI modeRPWI
OBSOLETE_RPWI_EUR_LOWObservation combining the modes required when 'far' from the CA, typically before and after 8.5 h from CARPWI
PEP_SCIENCE_LPAn observation with a low power mode for PEP PEP
PEP_SENSORS_STBYPEP in standbyPEP
UVS_EUR_NAD_HIGH_RESUVS observation of satellite surfaceUVS
PEP_GCO500_LOW_RATELow-rate mode to ensure continuous plasma measurements and to be on during off-nadir downlinks.PEP
PEP_GCO500_HIGH_RATEPEP high-resolution mode for detailed measurements over regions of interest such as polar cap boundariesPEP
PEP_GCO5000_LOW_RATELow-rate mode to ensure continuous plasma measurements and to be on during off-nadir downlinks.PEP
PEP_GCO5000_HIGH_RATEPEP Mode focussed on in-situ measurements of upstream plasma conditions and boundaries in Ganymede’s magnetospherePEP
PEP_GEO_LOW_RATELow-rate mode to ensure continuous plasma measurements and to be on during off-nadir downlinks.PEP
PEP_GEO_HIGH_RATEPEP Mode focussed on in-situ measurements of upstream plasma conditions and boundaries in Ganymede’s magnetospherePEP
PEP_GANYMEDE_FAR_DEPARTUREFor now same as Far Approach Mode. All sensors on except JNA.PEP
PEP_GANYMEDE_DEPARTUREAll sensors on except NIM.PEP
PEP_GANYMEDE_CLOSEST_APPROACHMode centered around CA, all sensors onPEP
PEP_GANYMEDE _APPROACHMode before CA Mode, All sensors onPEP
PEP_GANYMEDE_FAR_APPROACHMode 8-12h before CA of Ganymede All sensors on, except JNA.PEP
PEP_CALLISTO_FAR_DEPARTUREFor now same as Far Approach Mode. All sensors on except JNA. PEP
PEP_CALLISTO_DEPARTUREAll sensors on except NIM.PEP
PEP_CALLISTO_CLOSEST_APPROACHMode centered around CA, all sensors onPEP
PEP_CALLISTO_APPROACHMode before CA Mode, All sensors onPEP
PEP_CALLISTO_FAR_APPROACHMode 8-12h before CA of Europa. All sensors on, except JNA.PEP
PEP_EUROPA_FAR_DEPARTUREFor now same as Far Approach Mode. All sensors on except JNA.PEP
PEP_EUROPA_DEPARTUREAll sensors on except NIM.PEP
PEP_EUROPA_CLOSEST_APPROACHMode centered around CAPEP
PEP_EUROPA_APPROACHMode before CA Mode, All sensors onPEP
PEP_EUROPA_FAR_APPROACHMode 8-12h before CA of Europa All sensors on, except JNA.PEP
PEP_JUPITER_LOW_RATE_IMAGING High inclination ENA imaging mode (JNA/JENI on + simultaneous in-situ monitoring by JDC/JEI/JoEE) PEP
PEP_JUPITER_HIGH_RATE_IMAGINGHigh inclination ENA imaging mode (JNA/JENI on + simultaneous in-situ monitoring by JDC/JEI/JoEE) PEP
PEP_JUPITER_MEDIUM_RATE_IMAGINGHigh inclination ENA imaging mode (JNA/JENI on + simultaneous in-situ monitoring by JDC/JEI/JoEE) PEP
OBSOLETE_PEP_JUPITER_HIGH_INCLINATION_HIGH_RATEFor now same as PEP_JUPITER_EQUATORIAL_MEDIUM_RATE_IN_SITUPEP
PEP_JUPITER_EQUATORIAL_TORUS_CROSSINGAll sensors, except JNA, on in medium to low rates. Prime objective is for NIM to measure torus composition in-situ. Other sensors to measure indicators that can be used to constrain the densities. Applies also to Jupiter High Inclination for now.PEP
PEP_JUPITER_EQUATORIAL_LOW_RATEMode for ensuring continuous coverage while optimizing power and data volume. Consists of three sub-modes each of which is run separately: Plasma (JDC and JEI), energetic particles (JENI and JoEE) or ENA (JENI and JNA). Applies also to Jupiter High Inclination for now. PEP
PEP_JUPITER_EQUATORIAL_MEDIUM_RATE_IMAGINGJENI and JNA in imaging modes. In-situ as above.PEP
PEP_JUPITER_EQUATORIAL_MEDIUM_RATE_IN_SITUTargets are plasma moments, flows, pressure, etc…JENI in ion mode and JNA off.PEP
PEP_JUPITER_EQUATORIAL_HIGH_RATEHigh-resolution mode for resolving boundary crossings, fast flow bursts, etc. All sensors in in-situ mode except JNA.PEP
PEP_JOIPlasma and energetic particles measurements throughout closest approach with TBD ENA imaging.PEP
PEP_JUPITER_APPROACHPEP will monitor solar wind while imaging the Jovian magnetosphere in ENAs for 6 months before JOI-JDC or JEI / JNA and JENI onPEP
RIME_CALLISTO_FLYBYRIME flyby observations or observations without on-board processingRIME
RIME_ORBITAL15RIME observations up to 15 km deepRIME
RIME_ORBITAL9RIME observations up to 9 km deepRIME
RIME_STANDBYN/ARIME
SWI_MOON_LIMB_SCAN_PSInvestigation of Galilean Moons’ atmospheric composition, temperature, and winds. Flyby: The atmospheric limb is rapidly scanned to achieve 5km vertical resolution. Two CTS spectra are recorded for 1.5 sec over 210 channels (16 bits coding). GCO: The atmospheric limb is scanned up and down rapidly with 10 km altitude steps and with 1.5 sec integration time for two CTS spectra over 130 channels (16 bits coding). Position-switch calibration method.SWI
SWI_MOON_LIMB_STARE_PSInvestigation of Galilean Moons’ atmospheric composition, temperature, and winds). Flyby: Two CTS spectra are recorded for 30 sec over 210 channels (16 bits coding). GCO: Two CTS spectra are recorded for 30 sec over 130 channels (16 bits coding) and a different altitude (5, 10, 20, 40, and 50 km) is scanned every orbit. Position-switch calibration method.SWI
SWI_MOON_NADIR_STARE_PSInvestigation of Galilean Moons’ surface properties and atmospheric composition, temperature, and winds, and surface properties. This mode can also be used to characterize surface polarization by pointing 45◦off-nadir, after rotating the S/C by 90◦ around its nadir axis. It can also serve for solar occultation experiments to observe a weak molecular line in the atmosphere of Jupiter, a Galilean Moon, or the Europa torus. Flyby: Two CTS spectra are recorded for 30 seconds over 210 channels (16 bits coding). GCO: Two CTS spectra are recorded for 10 seconds over 130 channels (16 bits coding). In both cases, two CCH measurements (20 bits coding) are recorded for 0.1 sec, so that they are separated by maximum 1/2 beam at 1200 GHz. Solar occultation: Two CTS spectra are recorded for 60 seconds over 10000 channels (16 bits coding), and two CCH measurements (20 bits coding) are recorded for 0.1 second. Position-switch calibration method.SWI
OBSOLETE_SWI_SOLAR_OCCULTATION_FSSame as SWI SOLAR OCCULTATION 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 precompute ON-OFF for the CTS before downlink.SWI
SWI_2D_MAP_FSSame 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
SWI_SPECTRAL_SCAN_CTS_PSInvestigation of the atmospheric composition of Jupiter and the Galilean moons. The whole frequency range available to SWI is scanned. 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 (16bit coding). Position-switch calibration method. A single execution can cover up to 13 tunings.SWI
SWI_NADIR_STARE_PSInvestigation 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 every 60 seconds over 10000 channels (16 bits coding). Position-switch calibration method.SWI
SWI_SPECTRAL_SCAN_ACS_FSSame as SWI_SPECTRAL_SCAN_ACS_PS, except a frequency-switch calibration mode is used instead of position-switch. It enables spending ~100% of the integration time on-source. The ACS does not allow to pre-compute ON-OFF before downlink.SWI
SWI_WARMUPWarm-up mode.SWI
SWI_SOFTWAREIn this mode, only the DPU is powered and commanded to perform software maintenance and to perform a software update.SWI
SWI_STANDBYOnly the instrument DPU will be switched on and be able to accept instrument commands. Only housekeeping telemetry is generated in this mode.SWI
SWI_OFFAll 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
JMAG_CALROLLCampaign 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
JMAG_BURSTOperation 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
JMAG_CONTINOPmeasure the magnetic field in normal mode (at a rate of 32 vectors/s) continuouslyJMAG
UVS_IO_TORUS_SCANMonitoring Slit held along Jupiter’s North/South UVS
UVS_JUP_SP_SOL_OCCThe 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
UVS_JUP_HP_STELL_OCCFor 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
UVS_JUP_AP_STELL_OCCFor 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 mode”, but pixellist or histogram mode low or high possible.UVS
UVS_JUP_HP_LIMB_SCANSame as UVS_JUP_AP_LIMB_SCAN but through the HP portUVS
UVS_JUP_AP_LIMB_SCANMonitoring 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
UVS_JUP_HP_FEATURE_SCANTo assess the evolution of discrete phenomena (e.g., H Ly-alpha bulge, plumes, auroral features,…) using the HP port and pixellist mode.UVS
UVS_JUP_HP_SCAN_MAPSame 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
UVS_JUP_AP_SCAN_MAPScan 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
UVS_JUP_HP_AIRGLOW_STARESame 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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