| JAN_SCI_LIMB | | JANUS |
|---|
| NAVCAM_DVOL_BLOCK | | JUICE |
|---|
| PEP_FLYBY_FAR_DEPARTURE | | PEP |
|---|
| 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 |
|---|
| MAJ_JUP_DISK_MOSAIC | A 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 min | MAJIS |
|---|
| MAJ_STANDBY | After 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 6 | MAJIS |
|---|
| SWI_OFF | All 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_OFF | All sensors off, only survival heaters on | PEP |
|---|
| PEP_JUPITER_EQUATORIAL_TORUS_CROSSING | All 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_ACS_FS | Allan 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_ACS | Allan variance characterization of the ACS 1 & 2 by integrating on the cold sky. Integration time is 1 s | SWI |
|---|
| SWI_ALLAN_TOTAL_CCH | Allan variance characterization of the CCH 1 & 2 by integrating on the cold sky. Integration time is 0.1 s. | SWI |
|---|
| SWI_ALLAN_TOTAL_CTS | Allan variance characterization of the CTS 1 & 2 by integrating on the cold
sky. Integration time is 1.5 s. | SWI |
|---|
| SWI_ALLAN_CTS_FS | Allan variance characterization of the CTS 1 & 2 by integrating on the cold sky. Integration time is 1.5 s. Frequency-switch calibration method. | SWI |
|---|
| UVS_SAT_SURF_HP | As UVS_SAT_SURF_AP but using the high resolution port for improved spatial resolution in key surface regions | UVS |
|---|
| PEP_JUPITER_IN_SITU_BURST_1 | Burst in-situ mode for magnetosphere, CA of moon flybys (if NIM offl), Short duration events (magnetopause/bow shock crossings, injection events, moon wakes/microsignatures)
PEPLo Sensors ON: JDC, JEI
PEPHi Sensors ON: JENI_Ion, JoEE | PEP |
|---|
| PEP_GANYMEDE_IN_SITU_BURST_1 | Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ
PEPLo Sensors ON: All sensors ON, NIM neutral mode, JNA ion mode
PEPHi Sensors ON: JENI_Ion, JoEE | PEP |
|---|
| PEP_GANYMEDE_IN_SITU_BURST_2 | Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ
PEPLo Sensors ON: All sensors ON, NIM, JNA ion mode
PEPHi Sensors ON: JENI_Ion, JoEE | PEP |
|---|
| PEP_JUPITER_IN_SITU_IMAGING_BURST_1 | Burst in-situ mode, magnetosphere. CA of moon flybys with JNA/JENI imaging (if NIM off)
PEPLo Sensors ON: JDC, JEI, JNA
PEPHi Sensors ON: Option 1: JENI_Combo, JoEE. Option 2: JENI_ENA, JoEE | PEP |
|---|
| MAG_BURST_FIB_FOB | Burst observation mode without scalar sensor | JMAG |
|---|
| MAG_CALROLL | Campaign 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 |
|---|
| DRAFT_3GM_BSR | Characterisation of the surface by determination of roughness, dielectric constant of surface material and material density. The chosen antenna points towards surface, radio signal reflects from surface and received on ground. USO unmuted.
The HAA shall be ON to calibrate the sloshing potentially excited by pointing the HGA toward a moon’s Surface. | 3GM |
|---|
| 3GM_BISTATIC_RADAR | characterization of the surface by determination of roughness, dielectric constant of surface material and material density. The chosen antenna points towards surface, radio signal reflects from surface and received on ground. USO unmuted | 3GM |
|---|
| UVS_NC_STARE | Characterize the Io/Europa neutral clouds in the immediate vicinity of the satellite. Center satellite in slit. Align the slit with the satellite orbital plane | UVS |
|---|
| SWI_MECHANISM | Check of mechanism response to commands. Integration time on the CTS is 10 seconds. | SWI |
|---|
| UVS_SAT_DISK_SCAN_AP | Construct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics. | UVS |
|---|
| UVS_SAT_DISK_SCAN_HP | Construct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics. | UVS |
|---|
| MAJ_SAT_LIMB_TRACK | Continuous 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: 60min | MAJIS |
|---|
| UVS_JUP_DEFAULT | default pointing to be inserted at the start and end of the timeline | UVS |
|---|
| SWI_POINTING_ACS | Determination 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_CCH | Determination 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_CCH | Determination 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_CTS | Determination 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_DIAGNOSTIC | Diagnostic activity is allowed in this mode, including activation and control of sub-units, and service 6. | SWI |
|---|
| MAJ_GCO5000_REGIONAL | During 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: 6min | MAJIS |
|---|
| MAJ_GEO5000 | During 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 |
|---|
| PEP_FLYBY_DEPARTURE | Europa environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations)
Europa imaging (JNA) & Europa torus (JNA imaging + in-situ)
All sensors on except NIM (in standby or off)
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI) | PEP |
|---|
| PEP_FLYBY_FAR_DEPARTURE_LOW_RATE | Europa environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations)
Europa imaging (JNA) & Europa torus (JNA imaging + in-situ)
All sensors on except NIM (in standby or off).
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI) | PEP |
|---|
| PEP_FLYBY_FAR_DEPARTURE_LOW_RATE_ENA | Europa environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations)
Europa imaging (JNA) & Europa torus (JNA imaging + in-situ)
All sensors on except NIM (in standby or off). JENI in Combo mode (half in ion mode, half imaging)
NIM in ram direction (X-Y S/C plane) | PEP |
|---|
| MAJ_SAT_LIMB_SCAN | Flyby 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: 60min | MAJIS |
|---|
| MAJ_SAT_DISK_SLEW | Flyby 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 min | MAJIS |
|---|
| MAJ_FLYBY_MEDRES | Flyby 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 maximum | MAJIS |
|---|
| UVS_JUP_HP_STELL_OCC | For 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_OCC | For 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 modeâ€, but pixellist or histogram mode low or high possible. | UVS |
|---|
| GAL_MONITORING_GAN | GALA will measure the time of flight between firing and receiving the returned laser signal during Ganymede phase | GALA |
|---|
| GAL_LR_FB_ALBEDO | GALA 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 |
|---|
| RIM_GANYMEDE_N1_1 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N1_2 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N1_4 | Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N2_1 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N2_2 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N2_4 | Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_N3_1 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_N3_2 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_N3_4 | Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 4. | RIME |
|---|
| RIM_GANYMEDE_O1_1 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 1. | RIME |
|---|
| RIM_GANYMEDE_O1_2 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 2. | RIME |
|---|
| RIM_GANYMEDE_O1_4 | Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km processing with presuming factor Np of 4. | RIME |
|---|
| DRAFT_3GM_GRAVITY_FLYBYS | Gravity measurement during flyby requires the use of the MGA.
KaT and HAA should be operating during gravity measurement
USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach.
HAA should be in STANDBY mode at least 48 hours before the gravity measurement.
The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up. | 3GM |
|---|
| DRAFT_3GM_GRAVITY_GCO500_200 | Gravity measurement during GCO500 and GCO200 will use the HGA during downlink sessions. If not possible, it will use the MGA. KaT and HAA should be operating during gravity measurement. USOis OFF during this phase (except in case of BSR opportunity). HAA should be in STANDBY mode at least 48 hours before the gravity measurement. The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up. | 3GM |
|---|
| 3GM_HAA_CALIBRATION | HAA in CALIBRATION mode
Duration: 50min | 3GM |
|---|
| 3GM_HAA_STANDBY | HAA in STANDBY mode | 3GM |
|---|
| GAL_HR_FB | High resolution data acquisition around FB closest approach. GALA will measure the time of flight between firing and receiving the returned laser signal | GALA |
|---|
| MAJ_FLYBY_HR | High 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 sec | MAJIS |
|---|
| UVS_GCO_HP | High spatial resolution observations of Ganymede's aurora to look for small scale features | UVS |
|---|
| MAJ_SAFE | Initiated 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 5min | MAJIS |
|---|
| SWI_MOON_LIMB_SCAN_PS_V1 | Investigation 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_PS_V1 | Investigation 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_FS_V1 | Investigation 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_MOON_NADIR_STARE_PS_V1 | Investigation 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_PS_V1 | Investigation 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_PS_V1 | Investigation 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_PS | Investigation of the atmospheric composition (and temperature) of Jupiter
and the Galilean moons. This mode is nominally meant for deep integrations and requires numerous
repetitions (e.g. monitoring of the moons). Two CTS spectra are recorded for 60 seconds
over 10000 channels (16 bits coding). Position-switch calibration method. | SWI |
|---|
| SWI_NADIR_STARE_PS_V1 | Investigation of the atmospheric composition (and temperature) of Jupiter
and the Galilean moons. This mode is nominally meant for deep integrations and requires numerous
repetitions (e.g. monitoring of the moons). Two CTS spectra are recorded for 60 seconds
over 10000 channels (16 bits coding). Position-switch calibration method. | SWI |
|---|
| SWI_SPECTRAL_SCAN_ACS_PS_V1 | Investigation 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 for 60 seconds over 1024 channels. Position-switch calibration method.
A single execution can cover up to 16 tunings. | SWI |
|---|
| SWI_SPECTRAL_SCAN_CTS_PS_V1 | Investigation 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.
Pointing Type: S/C: nadir or limb. Instrument: nadir or limb, using the SWI mechanism if S/C points
nadir and to reach the moons | SWI |
|---|
| SWI_5POINT_CROSS_PS_V1 | Investigation 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 |
|---|
| MAG_CONTINOP_FIB_FOB | J-MAG will measure the magnetic field in normal mode (at a rate of 32 vectors/s) continuously with SCA not operating | JMAG |
|---|
| MAG_CONTINOP_FIB_FOB_LIGHT_ONLY | JMAG mode (FIB FOB Light Only), this mode ensures that while FIB and FOB are collecting science the Scalar sensor also has power to its laser but is not collecting science data. This helps to protect the fibres from radiation damage, necessary for the Europa phase due to its radiation environment. | JMAG |
|---|
| 3GM_GRAVITY | KaT and HAA for gravity science | 3GM |
|---|
| DRAFT_3GM_GRAVITY_TOUR | KaT and HAA should be operating during gravity measurement
USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach.
HAA should be in STANDBY mode at least 48 hours before the gravity measurement.
The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up. | 3GM |
|---|
| 3GM_GRAVITY_FOR_EPHEMERIDES | KaT ON during communication windows | 3GM |
|---|
| MAJ_GCO5000_LIMB | Latitudinal 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: 600sec | MAJIS |
|---|
| SWI_UNLOCK | Launch lock release (on antenna & rocker mechanisms) is allowed only in this mode. | SWI |
|---|
| PEP_FLYBY_CLOSEST_APPROACH | Local moon-magnetosphere interaction observation: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations)
Europa imaging (JNA). Dense exosphere (NIM)
Sensors on: all
Corotation in JEI or JDC FoV
Full pitch angle coverage (JDC, JEI, JoEE, JENI)
Moon in JNA FoV
Angle of NIM_NEUION_S0 from JUICE_EUROPA_RAM or JUICE_GANYMEDE_RAM or JUICE_CALLISTO_RAM velocity less than 5 deg at CA
Solar panel rotation angle (SADM) SADM > 74° or
SADM < -74°
Moon in JNA FoV | PEP |
|---|
| PEP_JUPITER_IN_SITU_IMAGING_LOW_1 | Low power in-situ & ENA imaging mode (e.g. downlink, non-prime/low priority science segments).
PEPLo Sensors ON: JDC_LP, JEI (4 sectors), JNA
PEPHi Sensors ON: Option 1: JENI_Combo, JoEE. Option 2: JENI_ENA, JoEE | PEP |
|---|
| PEP_JUPITER_IN_SITU_LOW_1 | Low power in-situ mode (e.g. downlink, non-prime/low priority science sgments)
PEPLo Sensors ON: JDC_LP, JEI (8 sectors)
PEPHi Sensors ON: JENI_Ion, JoEE | PEP |
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| MAJ_SERVICE | MAJIS 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 10min | MAJIS |
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| MAJ_JUP_STELLAR_OCC | MAJIS 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 |
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| UVS_IO_TORUS_SCAN | Map emissions from the Io torus. Slit aligned parallel with Jupiter's rotation pole, scanned E-W across the torus | UVS |
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| MAJ_GCO500_LIMB | Mapping 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 cube | MAJIS |
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| UVS_SAT_TRANSIT | Measure 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 |
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| MAG_CONTINOP | measure the magnetic field in normal mode (at a rate of 32 vectors/s) continuously | JMAG |
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| SWI_SAFE | Mode 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 |
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| PEP_GANYMEDE_IN_SITU_LOW_7 | Mode with only NIM on (ion) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the ionosphere. PEP Hi on, all in-situ
PEPLo Sensors ON: NIM ion on, only
PEPHi Sensors ON: JENI_Ion, JoEE | PEP |
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| PEP_GANYMEDE_IN_SITU_LOW_6 | Mode with only NIM on (neutral) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the exosphere. PEP Hi on, all in-situ.
PEPLo Sensors ON: NIM neutral on, only
PEPHi Sensors ON: JENI_Ion, JoEE | PEP |
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| UVS_IO_TORUS_STARE | Monitor emissions from the Io torus. Slit aligned parallel with Jupiter's equator. | UVS |
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| UVS_JUP_AP_LIMB_SCAN | Monitoring 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 |
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| UVS_JUP_AP_AIRGLOW_STARE | 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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| UVS_GCO_HISTOGRAM_001 | Monitoring auroral emissions and surface reflectance during GCO. Limited spectral resolution. | UVS |
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