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RIME_EUROPA_FLYBYRIME flyby observations or observations without on-board processingRIME
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
MAJIS_STANDBYAfter switch-on of MAJIS, the Boot SW automatically starts, and performs the primary boot from the PROM (Init fugitive BSW mode). After processor modules initialization, the Boot software goes to STANDBY mode. By default, the ASW Image0 (stored in MRAM0 = ASM0) is autonomously loaded after a timeout of 30 seconds. MAJIS then enters into ASW init Mode and then into SAFE mode. In STANDBY Mode, all channels are off, and only DPU HK SID1 are received. MAJIS needs to be maintained in STANDBY mode using the TC(17,1) in the following cases : - upload (using service 6) of new ASW images (or CUSW, or firmware) into MRAM: FCP-MAJ-070 describes the maintenance process. - upload a new BROWSE Table FCP-MAJ-060 into MRAM - select ASW Image1 and then start ASW Image 1 instead of teh default ASW Image0. FCP-MAJ-062 - any other update of MRAM using service 6MAJIS
MAJIS_SERVICEMAJIS in service MODE (1 or 2 channels with FPE/FPA off + AUX w/o loads) SERVICE Mode as soon as one or two channels are switched ON (PE and AUX) From SERVICE, it is possible to return to SAFE mode or to change the status of MAJIS to DIAG2, DIAG3 or SCIENCE Duration: less than 10minMAJIS
MAJIS_SAT_LIMB_TRACKContinuous stare observation of a satellite limb during flyby using inertial pointing from satellite, dayside or nightside. Additional offsets within limb by means of internal pointing mirror. Scanning with MAJIS internal mirror. (--> ‘track limb’). Pointing: S/C limb tracking (‘track limb’) satellite otientation: SLIT tangent to the limb (slit not aligned with S/C motion) Duration: 60minMAJIS
MAJIS_SAT_LIMB_SCANFlyby observations of the satellite dayside or nightside limbs with vertical (N-S) slews across track, during yaw-steering phase. Satellite offsets to limb around Y-axis (E-W) before each observation, then satellite offsets around X axis (N-S) between each slit acquisition or continuous slew pointing. Pointing: S/C slew scan centred a limb ( ‘Limb slew scan mode’). Satelliteo orientation: Slit tangent to the limb Duration: 60minMAJIS
MAJIS_SAT_DISK_SLEWFlyby observations of the satellite surface with vertical (N-S) slews across track, during yaw-steering phase. One or two slews (pole to pole) necessary to complete dayside coverage. Satellite offset around Y-axis (E-W) before each observation, then satellite offsets around X axis (N-S) between each slit acquisition. Pointing: NADIR Pointing, YS, S/C scan (slew) with offset around Y (‘mosaic mode’ tbc). MAJIS slit perpendicular to the ground-track. Satellite orientation: MAJIS slit perpendicular to the ground-track Duration: 30 minMAJIS
MAJIS_SAT_DISK_SCANObservation of a distant satellite dayside or nightside surface. Satellite offset required for pointing then disk coverage is achieved using the internal pointing mirror scanning in the Y (N-S) direction. Pointing: NADIR-P with possible offset around Y, YS, MAJIS scan (‘Nadir scan’). Satellite orientation: MAJIS slit perpendicular to the ground-track Duration: 30minMAJIS
MAJIS_SAFEInitiated after ASW loading All channels are off and no PE HK are generated. Only ME HK are generated (only DPU ON) From SAFE it is possible 1) to switch OFF MAJIS, 2) to change the status of MAJIS to DIAG1 or SERVICE mode Duration: less than 5minMAJIS
MAJIS_Ring_OccultationObservation of a star occulted by the rings Scan windowing of 9 lines centered on the star (1 scan step = 1/3 MAJIS IFOV) possible Pointing: Inertial. For each occultation, transit of TBD min Satellite orientation: Inertial pointing of the S/C towards the position of the star to maintain MAJIS slit fixed on it. These occultation observations need to be consolidated in the future (star atlas, signal, Tint, S/C inertial capabilities). Scan mirror can be used to mitigate APE driftMAJIS
MAJIS_MainRING _PhaseCurveObservations of the main rings at various phase angles (N angles), one ansae (always the same), 20 vertical lines Pointing: S/C pointing ring plane at 1.8 R_J (extremity of main rings) Satellite orientation: OFF-NADIR, Ring plane while maintaining horizontal orientation of MAJIS slit, MAJIS scan mode activated for vertical sampling centered on the rings (20 lines) Duration: 200 sec for one observations at a given phase angleMAJIS
MAJIS_MainRING _LowPhaseObservations of the main rings (2 ansa), no tracking of azimuthal structure, 20 vertical lines pointing: OFF-NADIR, S/C pointing centered on the extremity of main rings, S/C depointing required for the two ansa Satellite orientation: Maintaining the MAJIS slit parallel to radial axis of main rings, MAJIS scan mode activated for vertical sampling centered on the rings (20 vertical lines) Duration:400 sec (excluding the S/C repointing to the other ansae)MAJIS
MAJIS_MainRING _HighPhaseObservations of the main rings (2 ansa) at high phase (forward scattering light), no tracking of azimuthal structure, no spatial binning to increase spatial resolution. Pointing: OFF-NADIR, S/C pointing centered on the extremity of main rings, S/C depointing required for the two ansa Satellite orientation: Maintaining the MAJIS slit parallel to radial axis of main rings, MAJIS scan mode activated for vertical sampling (20 vertical lines) centered on the rings Duration: 400 sec (excluding the S/C repointing to the other ansae)MAJIS
MAJIS_JUP_STELLAR_OCCMAJIS will acquire several “subcubes” (number depends upon planet's speed over the sky) around the (fixed) star position, at different angular distances between the star and the planet's limb during the ingress/egress. Each sub-cube spans over several lines (around 6, less if S/C capability allows it) to compensate for possible pointing inaccuracies. Bright far moons can be used instead of stars as sources to decrease the repetition integration (and therefore spatial sampling) as the orbital velocity ranges from ~ 5 km/s at apojove to ~ 13 km/s at perijove satellite orientation: LIMB TANGENT (preferred, otherwise VERTICAL), to minimize straylight duration: About 10min 66 sec (max) for each subcube. Time interval between sub-cubes as small as possible for better vertical coverage. Total number of cubes depends upon relative angular speed between star and limb.MAJIS
MAJIS_JUP_LIMB_SLEWThe 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
MAJIS_JUP_LIMB_SCANThe MAJIS pointing mirror is used to scan the atmosphere of Jupiter over the limb up to 3000km. The scan mirror step of 1/3 MAJIS IFOV shall constrain the spatial sampling. Typically, we have cubes of about 20 lines by 50 pixels (~7500 km with 1 pixel=150 km) Pointing type: OFF-NADIR (nominal pointing position over the Jupiter limb), continuous tracking (‘track tangent limb’) satellite orientation: LIMB TANGENT (slit tangent to the limb) Duration: 4 min for each cube (20 lines)MAJIS
MAJIS_JUP_HIGH_FREQ_MONITORINGStudy of the evolution of atmospheric features at high temporal frequency. Tracking of features on the Jovian disc, on dayside as well as on nightside, with limited latitudinal coverage. MAJIS will acquire several “subcubes” with limited number of lines (about 40) using the scan mirror centered at one fixed position over the nominal Jupiter coordinate grid and reference surface. Planet rotation is compensated by continuous slew of the spacecraft (stop when acquiring). pointing type: OFF_NADIR, NYS, DISCONTINUOUS SLEW (‘track landmark scan’) satellite orientation: HORIZONTAL Duration: 80 sec for each sub-cube. Total duration about 5 h (1/2 of rotation period)MAJIS
MAJIS_JUP_EVENT_MONITORINGStudy 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
MAJIS_JUP_DISK_SLEWObservations of Jupiter clouds and spectroscopy of minor gases. Scanning the instrument slit over Jovian disk (vertical direction) by means of the S/C slew. aims to cover the entire equatorial region (-30°:+30°) Pointing: OFF_NADIR, CONTINUOUS SLEW (« continuous S/C scan ») Satellite orientation: HORIZONTAL Duration: 20 min per cubeMAJIS
MAJIS_JUP_DISK_SCANObservations of Jupiter clouds and spectroscopy of minor gases. Scanning the instrument slit over Jovian disk (vertical direction) by means of internal pointing mirror, both dayside and nightside. Aims to cover the entire equatorial region (-30°:+30°) pointing type: YS, NADIR with fixed offset around Y (‘nadir offset MAJIS scan’) satellite orientation: HORIZONTAL Duration: 20min/cubeMAJIS
MAJIS_JUP_DISK_MOSAICA series of several MAJIS_JUP_DISK_SCAN or MAJIS_JUP_DISK_SLEW Spacecraft has to be re-pointed between individual acquisitions. POinting type: YS, NADIR with offset around Y (‘ nadir offset MAJIS scan’’) satellite orientation: HORIZONTAL (preferred) Duration: 3 x (scan-duration + turnaround Y duration). Scan duration from 20 to 40 min depending on the distance from Jupiter. Turnaround ~50 minMAJIS
MAJIS_JUP_AURORAL_MAPPINGObservations of Jupiter aurorae. Scanning the instrument slit over Jovian disc by means of internal pointing mirror, 200 lines. Pointing type: YS, NADIR with fixed offset around Y (‘nadir offset MAJIS scan’) satellte orientation: HORIZONTAL Duration: 37 min (200 lines <-> typical size of latitudes where polar ovals are observed)MAJIS
MAJIS_JovianRING_MOSAICMosaicking the 2 ring ansa from 90000 to 230000 km. 3 overlapping cubes of 20 vertical lines performed by the scanner (or S/Cslew if compatible with JANUS). This requires re-pointing between individual cubes. Pointing: OFF-NADIR, S/C pointing projected ring plane, S/C depointing required for the two ansa Satellite orientation: Maintaining the horizontal orientation of MAJIS slit, MAJIS scan mode activated for vertical sampling (20 vertical lines) centered on the rings, S/C depointing required for mosaicking each ansa (3 overlapping cubes to perform a radial mosaic of one ansa of the rings with radial distance from 90000 to 230000 km) Duration: 1200 sec (excluding the S/C repointings)MAJIS
MAJIS_ICUTo 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: 10minMAJIS
MAJIS_GEO5000During elliptical phase (~15 days before and after circular phase), mapping of selected areas (~40) at intermediate to high resolutions: 50 to <750 m/pix, bridging the gap in resolution between systematic mapping (MAJIS_GCO5000_global) and GCO ROIs (MAJIS_GCO500_HR). Pointing: YS, NADIR satellite orientation: MAJIS slit at a slant with the ground track except at the equator Duration: from 35 min to 4H (Table 8 from budget report v2.1)MAJIS
MAJIS_GCO5000_REGIONALDuring circular phase (~120 days), regional mapping of the surface of Ganymede, bridging the gap in resolution between systematic global mapping and HR ROI's observed at GCO-500. 750 m/pix (no spatial binning), 300x300 km swaths Pointing type: YS, NADIR Satellite orientation: MAJIS slit at a slant with the ground track except at the equator Duration: 6minMAJIS
MAJIS_GCO5000_LIMBLatitudinal scanning of the diurnal limb at 1 km at different latitudes; study of the variability of the exospheric processes (sputtering, photodissociation, sublimation). Observe polar (north/south) and equatorial latitudes ; perform long-term and high-temporal-resolution monitoring. Pointing: S/C limb tracking at locations where the slit is tangent to the limb Satellite orientation: Off-nadir orientation, Slit tangent to the limb Duration: 600secMAJIS
MAJIS_GCO5000_GLOBALSystematic 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
MAJIS_GCO5000_AURORAObservations at auroral latitudes (30-35° N-S), at least in the dawn and dusk sides of Jovian magnetosphere. Mapping at spatial resolution of about 1 km using the MAJIS scan Pointing: S/C limb; no requirements on the slit orientation Saletllite orientation: Off-nadir orientationMAJIS
MAJIS_GCO500_LIMBMapping of selected areas on the dayside limb at resolutions of about 300 m at different latitudes (~30° in lat/lon from the nadir) to study variability of the exospheric processes (sputtering, photodissociation, sublimation). MAJIS scanning at different latitudes of the diurnal limb; a minimum of 3 (north,equat,south) x 2 (dawn, dusk) positions. Pointing: S/C limb tracking at locations where the slit is tangent to the limb satellite orientation: Off-nadir orientation, Slit tangent to the limb Duration: 600 sec per cubeMAJIS
MAJIS_GCO500_HRObservations in true push-broom of specific targets on the surface using motion compensation with the scanner 30 km cross-track x 8.7 km along-track @ 75 m/pixel 30 km cross-track x 17.4 km along-track @ 150 m/pixel (spatial binning x2) Pointing: Nadir pointing, NYS ( ‘motion compensation PB’) Satellite orientation: MAJIS slit perpendicular to the ground-track Duration: One acquisition: 60 sec; switch-on procedure: 10 minutes (TBC)MAJIS
MAJIS_FLYBY_MEDRESFlyby observations of the satellite surface with vertical (N-S) slews or MAJIS scan providing medium spatial resolution (e.g.resolution from 3 km to 1 km/pixel for Ganymede). Perform when the S/C moves slowly from approach YS phase to PB phase and during PB phase. Pointing: NYS, NADIR or OFF_NADIR after offset around Y ( ‘motion compensation PB’). Satellite orientation: MAJIS slit across track. Satellite offsets around Y (off-track pointing) axis or around X axis (for slew). Duration: a few minutes maximumMAJIS
MAJIS_FLYBY_HRHigh resolution pubshbroom flyby observations of satellite dayside surfaces bracketing closest approach. Satellite offsets around Y (off-track pointing) axis during or prior to observation allow near-nadir pointing of specific regions. Motion compensation or MAJIS scan is achieved using the MAJIS internal pointing mirror depending on the S/C speed and distance. Binning can be applied may be required near C/A. Pointing: NYS, NADIR or OFF_NADIR after offset around Y (‘motion compensation PB’). Satellite orientation: MAJIS slit across track, Satellite offsets around Y (off-track pointing) axis possible. Duration: 20 to 130 secMAJIS
MAJIS_BORESIGHT_ALIGNEMENTStar sequence for geometrical calibration. A star is initially pointed using the MAJIS boresight, then MAJIS is operated with the scan mechanism at high resolution (1/3 of IFOV) over 18 lines centered in the star. Then this operation is successively observed after 4 S/C repointings of 1.5° around X and Y. Pointing : inertial Satellite orientation: S/C pointing the star and MAJIS scans Duration: 18 to 180 sec per position (5 positions in total)+ stabilization time for repointing not taken into accountMAJIS
MAJIS_AmaltheaS/C pointing Amalthea preferentially near maximal elongation of (2.54 R_J), 2 hemispheres, MAJIS spatial windowing (16 rows) pointing: OFF-NADIR, S/C pointing Amalthea at 2.54 R_J while maintaining horizontal orientation of MAJIS slit satellite orientation: Maintaining horizontal orientation of MAJIS slit, MAJIS scan mode activated for vertical sampling centered on the satellite (10 lines) Duration: 100 sec for one hemisphereMAJIS
GALA_MONITORING_GANGALA will measure the time of flight between firing and receiving the returned laser signal during Ganymede phaseGALA
GALA_LR_FB_ALBEDOGALA will passively measure the reflectance of the illuminated hemisphere of the satellite during flyby nadir phase.GALA will operate in passive albedo mode (DiagRx)GALA
GALA_HR_TARGET_GANRegion of Interest Observation at GanymedeGALA
GALA_HR_FBHigh resolution data acquisition around FB closest approach. GALA will measure the time of flight between firing and receiving the returned laser signalGALA
GALA STANDBYto be schedule before SCIENCE if GALA is OFF and after science before GALA is switched OFF.GALA
3GM_USO_ONUSO is SWON and muted3GM
3GM_RADIO_OCCULTATIONSThe radio science experiment 3GM, with its 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. For instance, there are no occultations by Jupiter during the equatorial phase in 2030 and only 2 during the inclined orbital phase in 2031. The mission phase with the greatest number of Jupiter occultations (26) is the transfer to the Ganymede mission phase in 2032. The current planning tour offers a fairly regular sampling of latitudes between 54° S and 17° N and a rather global longitudinal coverage. USO unmuted, HAA in NOMINAL SCIENCE. Note that 2 other options exist for torus occultations but are not (yet) defined in the database3GM
3GM_HAA_STANDBYHAA in STANDBY mode3GM
3GM_GRAVITY_FOR_EPHEMERIDESKaT ON during communication windows 3GM
3GM_GRAVITYKaT and HAA for gravity science3GM
3GM_BISTATIC_RADARcharacterization 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 unmuted3GM
3GM HAA CALIBRATIONHAA in NOMINAL SCIENCE Duration: 50min3GM
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
PEP_OFFAll sensors off, only survival heaters onPEP
PEP_GANYMEDE_DEPARTURE_NIM All sensors on. NIM in a different mode than during approach.PEP
PEP_EUROPA_DEPARTURE_NIMAll sensors on. NIM in a different mode than during approach.PEP
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
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
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
UVS_DISK_SCANConstruct 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_SOL_OCCUVS solar port stares at Sun as the satellite occults it.UVS
UVS_SAT_STELL_OCCUVS airglow port stares at a fixed RA and DEC as the satellite occults the star.UVS
JANUS_POIObservations of multiple frames with specific inertial pointing to several targets (distant satellites, rings, calibration targets, and for specific observation modes (occultation)). To be used while in J orbit and in cruise.JANUS
JANUS_RAST_SLEWObservations of multiple frames in (m x n) positions targeted with a raster pointing of the S/C made with a continuous slew. The raster is done with continuous slew approach: images are acquired while the S/C is slewing; slew rate shall be adapted with the instrument angular sampling and the integration time. To be used while in J orbit or during FBs (out from CA phase)JANUS
JANUS_RAST_POIObservations of multiple frames in (m x n) positions targeted with a raster pointing of the S/C. The raster is done with a stop-and-go approach: the S/C maintain an inertial pointing allowing images acquisitions, then perform a slew to the new position and repeat the cycle till the (m x n) raster is completed. To be used while in J orbit or during FBs (out from CA phase)JANUS
JANUS_POI_PUSH_FRObservations of single or multiple frames with a pointing offset wrt to nominal S/C pointing (e.g., wrt nadir-looking while in G orbit, during FB or while in Jupiter orbit)JANUS
JANUS_NOM_PUSH_FRObservations of single or multiple frames during nominal S/C pointing (e.g., nadir-looking while in G orbit, during FB or while in Jupiter orbit)JANUS
JANUS_CONFIGNo 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
JANUS_IDLENo observations, but instrument ON for thermal stabilization before observations or between two observation phases that are too close to switch the instrument OFF.JANUS
JANUS_OFFNo observations, instrument OFF.JANUS
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

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