| 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 |
|---|
| UVS_SAT_SURF_HP | As UVS_SAT_SURF_AP but using the high resolution port for improved spatial resolution in key surface regions | UVS |
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| UVS_SAT_SURF_AP | Pushbroom observations near flyby closest approach to investigate surface composition | UVS |
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| UVS_SAT_STELL_OCC | UVS airglow port stares at a fixed RA and DEC as the satellite occults the star. | UVS |
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| UVS_SAT_SOL_OCC | UVS solar port stares at Sun as the satellite occults it. | UVS |
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| UVS_SAT_LIMB_STARE_HP | Search for faint atmospheric emissions by building signal to noise through long integrations. | UVS |
|---|
| UVS_SAT_LIMB_STARE_AP | Search for faint atmospheric emissions by building signal to noise through long integrations. | UVS |
|---|
| UVS_SAT_LIMB_SCAN_HP | Similar to disc scan observations, but holding the pointing relative to the limb during flyby sequences. | UVS |
|---|
| UVS_SAT_LIMB_SCAN_AP | Similar to disc scan observations, but holding the pointing relative to the limb during flyby sequences. | 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 |
|---|
| 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_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 |
|---|
| UVS_JUP_SP_SOL_OCC | The large solar disc and the substantial distance from Jupiter mean that this will not provide the same vertical resolution as stellar occultations, but are useful for measurements of minor/trace constituents due to high S/N. This uses a fixed scan through the Solar Port (SP) at a selected RA and DEC, holding the pointing for an extended amount of time. Note: Here histograms, but pixellist mode possible. | UVS |
|---|
| UVS_JUP_ROLL_SCAN | Point to nadir. Rotate about nadir so that we scan a circle (or a fraction of a circle - e.g. covering the auroral regions) over Jupiter's disk. Rotation rate ~0.1 degree per second | UVS |
|---|
| 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_HP_SCAN_MAP | Same as UVS_JUP_AP_SCAN_MAP but for High spatial resolution Port (HP). Scan the UVS slit in the cross slit direction across a region (e.g., auroral (N or S)) or entire disk using the Airglow (AP) port, scan at a constant rate across Jupiter to produce a map. Observation performed in pixel list mode to reach a time resolution of 0.001 s. | UVS |
|---|
| UVS_JUP_HP_LIMB_SCAN | Same as UVS_JUP_AP_LIMB_SCAN but through the HP port | UVS |
|---|
| UVS_JUP_HP_FEATURE_SCAN | To assess the evolution of discrete phenomena (e.g., H Ly-alpha bulge, plumes, auroral features,…) using the HP port and pixellist mode. | UVS |
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| UVS_JUP_HP_AIRGLOW_STARE | Same as UVS_JUP_AP_AIRGLOW_STARE but for High spatial resolution Port (HP). Monitoring auroral and airglow emissions in stare mode using the Airglow Port (AP). Slit held along Jupiter' s North/South and on the central meridian, while Jupiter rotates below S/C creating a map. Histogram mode. | UVS |
|---|
| UVS_JUP_DEFAULT | default pointing to be inserted at the start and end of the timeline | 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 |
|---|
| UVS_JUP_AP_SCAN_MAP | Scan the UVS slit in the cross slit direction across a region (e.g., auroral (N or S)) or entire disk using the Airglow (AP) port, scan at a constant rate across Jupiter to produce a map. Observation performed in pixel list mode to reach a time resolution of 0.001 s. | UVS |
|---|
| UVS_JUP_AP_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 |
|---|
| 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 |
|---|
| UVS_IRR_SAT | Obtain reflectance spectra of irregular satellites | UVS |
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| UVS_IO_TORUS_STARE | Monitor emissions from the Io torus. Slit aligned parallel with Jupiter's equator. | UVS |
|---|
| 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 |
|---|
| UVS_IO_SCAN | Similar to UVS_DISK_SCAN, but including extra emission lines e.g. from S and Cl. Also requires different spatial binning since Io is more distant | UVS |
|---|
| UVS_GCO_HP | High spatial resolution observations of Ganymede's aurora to look for small scale features | UVS |
|---|
| UVS_GCO_HISTOGRAM_003 | Similar to observation 001 but with increased spectral resolution to achieve < 2 nm resolution between 100 and 200 nm as specified in SciRD | UVS |
|---|
| UVS_GCO_HISTOGRAM_002 | Similar to observation 001 but with Increased time sampling to capture auroral morphology and variability | UVS |
|---|
| UVS_GCO_HISTOGRAM_001 | Monitoring auroral emissions and surface reflectance during GCO. Limited spectral resolution. | UVS |
|---|
| UVS_EUR_SCAN_HIGH_RES_OBSOLETE | Similar 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 centre | UVS |
|---|
| SWI_WARMUP | Warm-up mode. | SWI |
|---|
| SWI_UNLOCK | Launch lock release (on antenna & rocker mechanisms) is allowed only in this mode. | SWI |
|---|
| SWI_TSYS_CTS_V1 | Spectral scan to measure the system temperature spectra of the 2 bands with
the CTS 1 & 2 by observing the hot load and cold sky. Integration time on CTS is 2 seconds. A
single execution can cover up to 15 tunings. | SWI |
|---|
| SWI_TSYS_CCH_V1 | Spectral scan to measure the system temperature 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
tunings. | SWI |
|---|
| SWI_TSYS_ACS_V1 | Spectral scan to measure the system temperature 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_CCH_V1 | Spectral scan to measure the system temperature 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_ACS_CCH | Spectral scan to measure the system temperature 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_STANDBY | Only the instrument DPU will be switched on and be able to accept instrument commands. Only housekeeping telemetry is generated in this mode. | 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_SPECTRAL_SCAN_CTS_FS_V1 | Same 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 tunings. | 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_ACS_FS_V1 | Same 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. A single
execution can cover up to 11 tunings. | SWI |
|---|
| SWI_SCIENCE | Place holder:
one of the ASW mode, where the science script will be run ( i.e. from SWI_TSYS_CTS down to SWI_MOON_NADIR_STARE_FS) during the mission | SWI |
|---|
| 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 |
|---|
| 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_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_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_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_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 |
|---|
| 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_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_FS_V1 | Same 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_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_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_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_LIMB_STARE_FS_V1 | Same 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_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_SCAN_FS_V1 | Same 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_MECHANISM | Check of mechanism response to commands. Integration time on the CTS is 10 seconds. | 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_STARE_FS_V1 | Same 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 pre-compute
ON-OFF for the CTS before downlink. | 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_JUP_LIMB_RASTER_FS_V1 | Same 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_DIAGNOSTIC | Diagnostic activity is allowed in this mode, including activation and control of sub-units, and service 6. | 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_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_ACS | Allan variance characterization of the ACS 1 & 2 by integrating on the cold sky. Integration time is 1 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 |
|---|
| 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_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 |
|---|
| SWI_5POINT_CROSS_FS_V1 | Same as SWI 5POINT CROSS PS, except a frequency-switch calibration
mode is used instead of position-switch. It enables spending 100% of the integration time onsource.
For Jupiter, two CTS spectra are recorded for 60 seconds over 10000 channels (16 bits
coding). For moon monitoring, two CTS spectra are recorded for 30 seconds over 210 channels
(16 bits coding). For both cases, and in parallel, 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. Frequency-switch calibration method for
CTS data. | SWI |
|---|
| SWI_2D_MAP_PS_V1 | This 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 for 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 for 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 for 30 seconds
over 210 channels (16 bits coding). GCO: (1) Investigation of Ganymede’s atmospheric
composition, temperature, and winds, and surface properties by scanning from limb to limb with
the along-track mechanism across the ground-track using the antenna mechanism ( 72 ). Two
CTS spectra are recorded for 10 seconds over 130 channels (16 bits coding). (2) Tomographic
investigation of Ganymede’s atmospheric and surface composition, temperature, and winds by
scanning along-track from 30km to +30km of the nadir axis with 9 steps, using the rocker
mechanism ( 4.3 ), and with 1.5 sec integration time for two CTS spectra over 130 channels
(16 bits coding). In all cases, two CCH measurements (20 bits coding) are recorded for 0.1
second. During GCO, this implies that two CCH measurements are separated by 1/2 beam at
1200 GHz. Position-switch calibration method (the OFF position is observed after each ON of
the map is observed). | SWI |
|---|
| SWI_2D_MAP_OTF_V1 | Similar 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_2D_MAP_OTF_CCH_V1 | Similar 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_2D_MAP_OTF | Similar 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_2D_MAP_FS_V1 | Same 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 |
|---|
| RPW_STANDBY | RPWI Safe mode where the instrument can survive indefinitely and where memory patch, dump and check commands are accepted | RPWI |
|---|
| RPW_OBSOLETE_In_situ_low_Radio_burst | The 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 |
|---|
| RPW_OBSOLETE_In_situ_low_Radar_mode_3 | The 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 TBD | RPWI |
|---|
| RPW_INIT | RPWI Transient mode while instrument is initialising after being powered on | RPWI |
|---|
| RPW_IN_SITU_SLOW_RADIO_FULL | The 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 |
|---|
| RPW_In_situ_slow_Radio_burst | The 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 |
|---|
| RPW_In_situ_slow_Radar_mode_3 | The RPWI In-situ_slow + Radio_mode_3 mode: - Makes continuous In-situ_slow mode measurement, the basic in-situ modes; - Radio mode TBD | RPWI |
|---|
| RPW_IN_SITU_NORMAL_RADIO_FULL | The 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 |
|---|
| RPW_In_situ_normal_Radio_burst | The 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 |
|---|
| RPW_In_situ_normal_Radar_mode_3 | The 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 TBD | RPWI |
|---|
| RPW_IN_SITU_LOW_RADIO_FULL | The RPWI In-situ_low + Radio_Full mode - Makes continuous In-situ_low mode, the lowest in-situ possible power and TM, which implements only the Mutual Impedance sweeps and DC electric field measurements; - Makes detailed radio emissions from Jupiter as well as moons (Ganymede, Callisto, Europa). Will also support RIME measurements, giving the background natural radio emissions. Monitor the radio emission spectrum as well as polarization. | RPWI |
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| RPW_In_situ_burst_Radio_Full | The 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 |
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| RPW_In_situ_burst_Radio_burst | The 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 |
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| RPW_In_situ_burst_Radar_mode_3 | The 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 TBD | RPWI |
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| RPW_DL | RPWI observation during downlink windows | RPWI |
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| 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 |
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| 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 |
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| 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 |
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| RIM_GANYMEDE_N4 | Passive Radar Acquisitions on Jovian side of Ganymede. | RIME |
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| 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 |
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