UVS_DECONTAMINATION | Not a true observation, but included so other instruments are aware that our heaters are on | UVS |
UVS_CALIBRATION | Generic calibration observation - may include star stare, flip ridealong, or dark/radiation observations. Data rate is an estimated average. | UVS |
UVS_IO_TORUS_SCAN | Map emissions from the Io torus. Slit aligned parallel with Jupiter's equator, scanned N-S across one ansa of the torus, then move in four steps to the other ansa, repeating the N-S motion each time | UVS |
UVS_JUP_MONITORING_HP | As above, more of an auroral focus. 2-hour observations fit in between the AP monitoring observations | UVS |
UVS_JUP_MONITORING_AP | Replaces previous monitoring stare. We perform a slow scan across the disk: assume 3 seconds per slit width, so 0.033 / s scan rate | 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_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_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_IO_TORUS_STARE | Monitor emissions from the Io torus. Slit aligned parallel with Jupiter's equator. | 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_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_IRR_SAT | Obtain reflectance spectra of irregular satellites | 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_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_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 |
UVS_SAT_SURF_HP | As UVS_SAT_SURF_AP but using the high resolution port for improved spatial resolution in key surface regions | UVS |
UVS_SAT_SURF_AP | Pushbroom observations near flyby closest approach to investigate surface composition | UVS |
UVS_SAT_SOL_OCC | UVS solar port stares at Sun as the satellite occults it. | UVS |
UVS_SAT_STELL_OCC | UVS airglow port stares at a fixed RA and DEC as the satellite occults the star. | UVS |
UVS_JUP_DEFAULT | default pointing to be inserted at the start and end of the timeline | 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_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_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 |
UVS_JUP_HP_LIMB_SCAN | Same as UVS_JUP_AP_LIMB_SCAN but through the HP port | 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_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 |
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_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_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_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_GCO_HP | High spatial resolution observations of Ganymede's aurora to look for small scale features | 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 |