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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
JMAG_BURST_FIB_FOBBurst observation mode without scalar sensor JMAG
JMAG_DL_FIB_FOBThis 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 is operating.JMAG
JMAG_CONTINOP_FIB_FOBJ-MAG will measure the magnetic field in normal mode (at a rate of 32 vectors/s) continuously with SCA not operatingJMAG
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
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
RIME_EUROPA_FLYBYRIME flyby observations or observations without on-board processingRIME
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
RPWI_INITRPWI Transient mode while instrument is initialising after being powered onRPWI
RPWI_STANDBYRPWI Safe mode where the instrument can survive indefinitely and where memory patch, dump and check commands are acceptedRPWI
RPWI_In_situ_burst_Radar_mode_3The 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 TBDRPWI
RPWI_In_situ_burst_Radio_FullThe 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
RPWI_In_situ_burst_Radio_burstThe 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
RPWI_In_situ_slow_Radar_mode_3The RPWI In-situ_slow + Radio_mode_3 mode: - Makes continuous In-situ_slow mode measurement, the basic in-situ modes; - Radio mode TBDRPWI
RPWI_In_situ_slow_Radio_burstThe 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
RPWI_In_situ_slow_Radio_FullThe 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
RPWI_In_situ_normal_Radar_mode_3The 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 TBDRPWI
RPWI_In_situ_normal_Radio_FullThe 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
RPWI_In_situ_normal_Radio_burstThe 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
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
RPWI_DLRPWI observation during downlink windowsRPWI
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
OBSOLETE_RPWI_MAGN_In-situ_BurstN/ARPWI
OBSOLETE_RPWI_MAGN_In-situ_NormalN/ARPWI
OBSOLETE_RPWI_GAN_Radio_BurstUsed for radio occultation of Jovian radio emissions to infer the ionospheric spatial structure. RPWI
OBSOLETE_RPWI_GAN_In-situ_LowTMN/ARPWI
OBSOLETE_RPWI_GAN_In-situ_NormalMakes continuous detailed RPWI observations that satisfy most SciRD requirements below 1.6 MHz. Main science targets here are the ionospheric/magnetospheric electric currents and electrodynamics, including sub-surface ocean characteristics. RPWI
OBSOLETE_RPWI_GAN_Radio_PassiveRadarThere are several ways of doing passive radar under investigation. We have chosen the most resource hungry mode for this table. One of the RWI antenna nulls (X, Y or Z) should point towards Jupiter with +/-1 deg accuracy. Monitoring HOM and DAM Jupiter radiation with reflections from ionosphere, surface and sub-surface layers (ocean/bedrock) to determine ionosphere and ice sheet thickness. Due to lower frequency (below 3 MHz), RPWI will reach deeper than RIME.RPWI
OBSOLETE_RPWI_GAN_Radio_FullMake more detailed radio emissions from Jupiter as well as Ganymede. Will also support RIME measurements, giving the background natural radio emissions. Monitor the radio emission spectrum as well as polarization.RPWI
OBSOLETE_RPWI_GAN_Radio_SlowMake survey of radio emissions from Jupiter as well as Ganymede. Will also support RIME observations, giving the background natural radio emissions. Monitor the radio emission spectrum.RPWI
OBSOLETE_RPWI_GAN_In-situ_BurstMakes 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
SWI_MECHANISMCheck of mechanism response to commands. Integration time on the CTS is 10 seconds.SWI
SWI_POINTING_CCHDetermination of absolute pointing offset between S/C and SWI (for the 2 bands) recording continuum maps with the CCH 1 & 2. Integration time on the CCH is 0.1s.SWI
SWI_POINTING_ACSDetermination of absolute pointing offset between S/C and SWI (for the 2 bands) recording continuum maps with the ACS 1 & 2. Integration time on the ACS is 1s.SWI
SWI_POINTING_CTSDetermination of absolute pointing offset between S/C and SWI (for the 2 bands) recording continuum maps with the CTS 1 & 2. Integration time on the CTS is 1.5s.SWI
SWI_POINTING_ACS_CCH: Determination of absolute pointing offset between S/C and SWI (for the 2 bands) recording continuum maps with the ACS 1 & 2 and the CCH 1 & 2.Integration time on the ACS and CCH are 1s and 0.1s, respectively.SWI
SWI_POINTING_CTS_CCHDetermination of absolute pointing offset between S/C and SWI (for the 2 bands) recording continuum maps with the CTS 1 & 2 and the CCH 1 & 2. Integration time on the CTS and CCH are 1.5s and 0.1s, respectively.SWI
SWI_ALLAN_TOTAL_CCHAllan variance characterization of the CCH 1 & 2 by integrating on the cold sky. Integration time is 0.1 s.SWI
SWI_ALLAN_TOTAL_ACSAllan variance characterization of the ACS 1 & 2 by integrating on the cold sky. Integration time is 1 sSWI
SWI_ALLAN_TOTAL_CTSAllan variance characterization of the CTS 1 & 2 by integrating on the cold sky. Integration time is 1.5 s.SWI
SWI_ALLAN_ACS_FSAllan variance characterization of the ACS 1 & 2 by integrating on the cold sky. Integration time is 1 s. Frequency-switch calibration method.SWI
SWI_ALLAN_CTS_FSAllan variance characterization of the CTS 1 & 2 by integrating on the cold sky. Integration time is 1.5 s. Frequency-switch calibration method.SWI
SWI_TSYS_CCHSpectral scan to measure the Tsys spectra of the 2 bands with the CCH 1 & 2 by observing the hot load and cold sky. A single execution can cover up to 16 tuningsSWI
SWI_TSYS_ACS: Spectral scan to measure the Tsys spectra of the 2 bands with the ACS 1 & 2 by observing the hot load and cold sky. Integration time on ACS is 1 second. A single execution can cover up to 16 tunings.SWI
SWI_TSYS_ACS_CCHSpectral scan to measure the Tsys 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
SWI_TSYS_CTSSpectral scan to measure the Tsys spectra of the 2 bands with the CTS 1 & 2 by observing the hot load and cold sky. Integration time on CTS is 1.5 second. A single execution can cover up to 15 tuningsSWI
SWI_UNLOCK: Launch lock release (on antenna & rocker mechanisms) is allowed only in this mode.SWI
SWI_DIAGNOSTICDiagnostic activity is allowed in this mode, including activation and control of sub-units, and service 6.SWI
SWI_2D_MAP_OTFSimilar 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_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
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
UVS_IRR_SATObtain reflectance spectra of irregular satellitesUVS
UVS_IO_SCANSimilar to UVS_DISK_SCAN, but including extra emission lines e.g. from S and Cl. Also requires different spatial binning since Io is more distantUVS
UVS_SAT_TRANSITMeasure absorption of Jupiter airglow by satellite atmospheres as they transit Jupiter's disk, to constrain satellite atmospheric composition and variability. Pointing: nadir (Point slit N-S on Jupiter's disk and wait for moon to transit)UVS
UVS_EUR_SCAN_HIGH_RESSimilar to UVS_DISK_SCAN but higher resolution. pointing: start at -1.5 satellite radii from the satellite centre, scan in the direction perpendicular to the slit across the disk, ending at +1.5 satellite radii from the centreUVS
UVS_SAT_SURF_HPAs UVS_SAT_SURF_AP but using the high resolution port for improved spatial resolution in key surface regionsUVS
UVS_SAT_SURF_APPushbroom observations near flyby closest approach to investigate surface compositionUVS
UVS_LIMB_SCANSimilar to disc scan observations, but holding the pointing relative to the limb during flyby sequences.UVS
UVS_LIMB_STARESearch for faint atmospheric emissions by building signal to noise through long integrations.UVS

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