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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_UNLOCK: Launch lock release (on antenna & rocker mechanisms) is allowed only in this mode.SWI
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
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_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
UVS_EUR_LIMB_HIGH_RESAlign the slit with Europa's equatorUVS
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
PEP_OFFAll sensors off, only survival heaters onPEP
PEP_GANYMEDE_DEPARTUREAll sensors on except NIM.PEP
PEP_CALLISTO_DEPARTUREAll sensors on except NIM.PEP
PEP_EUROPA_DEPARTUREAll sensors on except NIM.PEP
PEP_CALLISTO_DEPARTURE_NIMAll sensors on. NIM in a different mode than during approachPEP
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
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
SWI_ALLAN_TOTAL_ACSAllan variance characterization of the ACS 1 & 2 by integrating on the cold sky. Integration time is 1 sSWI
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_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_CTSAllan variance characterization of the CTS 1 & 2 by integrating on the cold sky. Integration time is 1.5 s.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
PEP_SCIENCE_LPAn observation with a low power mode for PEP PEP
UVS_SAT_SURF_HPAs UVS_SAT_SURF_AP but using the high resolution port for improved spatial resolution in key surface regionsUVS
JMAG_BURST_FIB_FOBBurst observation mode without scalar sensor 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
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
SWI_MECHANISMCheck of mechanism response to commands. Integration time on the CTS is 10 seconds.SWI
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
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
UVS_JUP_DEFAULTdefault pointing to be inserted at the start and end of the timelineUVS
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_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_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_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_DIAGNOSTICDiagnostic activity is allowed in this mode, including activation and control of sub-units, and service 6.SWI
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_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_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_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
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
PEP_GANYMEDE_FAR_DEPARTUREFor now same as Far Approach Mode. All sensors on except JNA.PEP
PEP_CALLISTO_FAR_DEPARTUREFor now same as Far Approach Mode. All sensors on except JNA. PEP
PEP_EUROPA_FAR_DEPARTUREFor now same as Far Approach Mode. All sensors on except JNA.PEP
OBSOLETE_PEP_JUPITER_HIGH_INCLINATION_HIGH_RATEFor now same as PEP_JUPITER_EQUATORIAL_MEDIUM_RATE_IN_SITUPEP
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
3GM HAA CALIBRATIONHAA in NOMINAL SCIENCE Duration: 50min3GM
3GM_HAA_STANDBYHAA in STANDBY mode3GM
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
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
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
PEP_JUPITER_EQUATORIAL_HIGH_RATEHigh-resolution mode for resolving boundary crossings, fast flow bursts, etc. All sensors in in-situ mode except JNA.PEP
SWI_SOFTWAREIn this mode, only the DPU is powered and commanded to perform software maintenance and to perform a software update.SWI
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
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
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_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_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_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
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_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
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
PEP_JUPITER_EQUATORIAL_MEDIUM_RATE_IMAGINGJENI and JNA in imaging modes. In-situ as above.PEP
3GM_GRAVITYKaT and HAA for gravity science3GM
3GM_GRAVITY_FOR_EPHEMERIDESKaT ON during communication windows 3GM
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
PEP_GCO500_LOW_RATELow-rate mode to ensure continuous plasma measurements and to be on during off-nadir downlinks.PEP
PEP_GCO5000_LOW_RATELow-rate mode to ensure continuous plasma measurements and to be on during off-nadir downlinks.PEP
PEP_GEO_LOW_RATELow-rate mode to ensure continuous plasma measurements and to be on during off-nadir downlinks.PEP
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_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
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_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_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
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
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
JMAG_CONTINOPmeasure the magnetic field in normal mode (at a rate of 32 vectors/s) continuouslyJMAG
PEP_EUROPA_FAR_APPROACHMode 8-12h before CA of Europa All sensors on, except JNA.PEP
PEP_CALLISTO_FAR_APPROACHMode 8-12h before CA of Europa. All sensors on, except JNA.PEP
PEP_GANYMEDE_FAR_APPROACHMode 8-12h before CA of Ganymede All sensors on, except JNA.PEP
PEP_GANYMEDE _APPROACHMode before CA Mode, All sensors onPEP
PEP_CALLISTO_APPROACHMode before CA Mode, All sensors onPEP
PEP_EUROPA_APPROACHMode before CA Mode, All sensors onPEP
PEP_EUROPA_CLOSEST_APPROACHMode centered around CAPEP
PEP_GANYMEDE_CLOSEST_APPROACHMode centered around CA, all sensors onPEP
PEP_CALLISTO_CLOSEST_APPROACHMode centered around CA, all sensors onPEP
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
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
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
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_AP_AIRGLOW_STAREMonitoring 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
UVS_IO_TORUS_SCANMonitoring Slit held along Jupiter’s North/South UVS
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
RIME_STANDBYN/ARIME

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