file: torus1:[gll_raw.info.science_summaries]MWG_PRIME_MISSION.OBS taken from information Ian Stewart sent in an email. PDS_VERSION_ID = PDS3 LABEL_REVISION_NOTE = "Karen Simmons, September 1998" OBJECT = DATA_SET DATA_SET_ID = "GO-J-UVS-2-EDR-V1.0" OBJECT = DATA_SET_INFORMATION DATA_SET_NAME = "Galileo Orbiter UVS/EUV Jupiter operations EDR data" DATA_SET_COLLECTION_MEMBER_FLG = "N" DATA_OBJECT_TYPE = SPECTRUM START_TIME = 1995-342T00:00:00 STOP_TIME = 1997-349T08:00:00 DATA_SET_RELEASE_DATE = 1999-01-15 PRODUCER_FULL_NAME = "Karen E. Simmons" University of Colorado, Boulder, CO" DETAILED_CATALOG_FLAG = "Y" DATA_SET_DESC = " Data Set Overview ================= Observations by the group of Galileo science instruments are coordinated by the Project Science Group (PSG). Spacecraft resources are divided between the needs of the three main disciplines: Atmospheres, Satellites and Magnet- ospheres. These disciplines coordinate science operations with their three Galileo Science Working Groups (WGs). These are the Satellite Working Group (SWG), the Magnetospheres WG (MWG) and the Atmospheres WG (AWG). The Ultraviolet Spectrometer (UVS) subsystem obtains science observations in all three of these disciplines. UVS observations are described below, organized by Orbit. Other data, like calibrations, are included where appropriate. The UVS team constitutes the science group from the University of Colorado. The PI is Dr. Charles W. Hord. The instrument consists of two pieces of hardware, the UltraViolet Spectrometer (UVS) and the Extreme UltraViolet (EUV) Spectrometer. The data resource negotiations with the WGs were considered as one team within the WGs. Data for the separate hardware are kept in separate data files. In the descriptions below, UVS may indicate the team, and thus both instruments, or may refer to only the UVS hardware. Separate EUV observation classes do exist and they are described below. Each Science WG has its own set of observations. The observations described in this EDR data set label include all observations from the Nominal Mission period, from Jupiter-Orbit-Insertion until End-Of-Nominal Mission. All Jupiter, Torus, satellite, etc target objects are described. Data from different orbits may contain observations from all or none of the described WG Observation classes. Experiment Data Record (EDR) data for UVS may be in either of two file formats: one for Playback (PB) data and one for the Phase 2 Real-Time-Science (RTS) data. Some of the observations are done only with the on-board summing RTS mode. Playback (PB) observations are recorded on the tape and played back at full, 1000 bps data rate. These PB data are therefore the highest time and spatial resolution data sets obtained by the UVS. Conversely, the RTS data are integrated over time, on-board, and generally represent the search for small optical depth constituents or other magnitude-only observations. EUV obtained only RTS data during the nominal mission. All UVS EDRs are raw, uncalibrated spectra. EDRs have been re-formatted by the team from spacecraft packets. The data set includes all EDR data from orbital operations for the Nominal/Prime Mission. File labels describe the file format of each data file. Each data file record has header information containing time tags, followed by the spectral data. There may be more than one record per file. Generally, each file contains all the data for that individual science Observation_ID, as classed below. UVS RDRs are generally heavily processed data sets and do not normally contain full spectra. EDR calibration is described in the calibration documents and files archived with PDS and discussed in the published papers. A list of recent publications appears at the end of this Description; a full publication list is available from the PDS. The PDS label file, for each data file, contains a PRODUCT_NAME which contains the Galileo Observation ID. These 12-character Observation IDs actually appear in the sequence (SEF) file. These are related to the WG Observation classes described below. An example of a PRODUCT_NAME is G07A_UPB_G7MANS01 ____ is the 4-character Orbit load number _Uxx_ is UPB for UVS Playback or URT for UVS RTS data format __ is the Orbit number (note:'C' load observations are usually grouped with the next encounter orbit period) OR ------ is the observation name __ is the observation series number. As with all well made plans, these Observation_ID rules were not always followed. The observation names might also be proper names of features or other new names. The data files are named by the observation name given in the SEF. The .DAT file extension indicates the file is a binary Vax formatted data file; an .XDR file extension indicates the file is an IEEE standard (transfer format) file. UVS and EUV data files are distinguished by their file names. The UVS Mission science objectives are given, in great detail, in several Galileo JPL mission documents. The Science Requirements Document (625-50) and the Orbit Planning Guides, OPG, (JPL 625-100, Vol 2.) are two. There is an OPG for the Nominal Mission and one for the Galileo Europa Mission. The OPG describes both the instrument objectives and the observation classes as well as specific observation ID names. On-line (web access) copies of the OAPEL (Orbit Activity Planning ELement) planning sheets and graphic designs provide additional information. See http://michelangelo.jpl.nasa.gov/spot/prime.html or http://lasp.colorado.edu/galileo/ . The UVS Prime (Nominal) Mission Observation classes are discussed below. These descriptions come from the planning documents. They are grouped by Working Group (WG). ++++++++++++++++++++++++++++++++++++++ AWG SCIENCE AND OBSERVATION OBJECTIVES ++++++++++++++++++++++++++++++++++++++ KEY QUESTIONS: The UVS atmospheric observations during the Jupiter tour attempt to answer several key questions related to stratospheric aerosol, airglow, and auroral studies. The observational goals and strategy, combined with Galileo's capabilities based upon the Phase 2 flight software, will permit observations which can answer these questions. They are: 1) To improve our understanding of stratospheric solar heating and residual mean meridional circulation: what are the horizontal and vertical distributions and the spectra of UV absorbers in the stratosphere? 2) To understand stratospheric meridional circulation: what is the meridional variation of ammonia and acetylene at high resolution and what can be said of their zonal distributions? 3) To understand the regional and global UV energetics with its temporal variation: what is the morphology of the UV airglow regional and global features as they vary in time? What is the global constituent distribution and its long-term variation (with and without solar influence) as shown in airglow (electroglow, nightglow) and auroral data? What is the regional airglow (electroglow, nightglow) and auroral variability on short and long time-scales with and without solar influence? 4) To understand the regional and global UV energetics with its spatial distribution: what are the UV airglow characteristics of local features at the highest possible resolution? What are the UV airglow characteristics of the Jovian limb? What is the shape of the hydrogen limb-darkening curve? What influences the hydrogen bulge? OBSERVATIONAL GOALS: The UVS atmospheric observations will be conducted during Jupiter approach and during each Jovian orbit with the exception of the non-targeted orbit 5. The principal goal of these observations will be to answer these key scientific questions as well as to support the AWG observations where possible. GALILEO CAPABILITIES: The capabilities for Galileo to conduct the UVS atmospheric observations are outlined in the Phase 2 Level 3 spacecraft requirements document. These capabilities, along with the telecommunication downlink assumed by that document, are used in the observations described in detail below. OBSERVATIONAL STRATEGY: The general UVS atmospheric observational strategy will be to conduct the highest priority UVS/AWG observations using spacecraft resources (bits-to- ground, tape usage, tape start-stop cycles, real-time science downlink, propellant for science turns, and observing time) followed by lower priority observations as resources permit. Observations which will address the science questions are based upon the following detailed prioritized observation descriptions. The observations can be grouped into general science area categories. These are Stratospheric aerosol, Chemistry of the stratosphere, Airglow, Auroral, Calibration, and Targets of opportunity observations. The categories are described below where the capitalized acronyms are the 6-character generic observation names described in detail. * Stratospheric aerosol observations will map the horizontal distribution, UV spectrum, and vertical distribution of UV absorbers in Jupiter's stratosphere and upper troposphere. These measurements enable an understanding of solar heating and the residual mean meridional circulation of the stratosphere. Aerosol properties for small-scale features will be measured, mostly as part of the feature track, FUVFEA, and stratospheric chemistry studies, ACELAT and BRTMAP. Orbits using the partial or full stratospheric aerosol observation sets are G1, G2, C3, E4, E6, G7, G8, C9, and C10. During JA/J0 the FUVPES observation will ridealong with other remote sensing instruments for a study of the Probe Entry Site. * Chemistry of the stratosphere observations (hydrocarbon chemistry and transport tracer studies) are accomplished with a complementary set consisting of ACELAT and, to a very limited degree, CENMAP, EWMAPS, and NEWS. The UVS will map latitudinal gradients of ammonia and acetylene in Jupiter's stratosphere. The meridional gradient of these two constituents will provide unique information on the stratospheric meridional circulation. A dense grid of measurements with good spatial resolution (i.e., an orientation with the UVS slit aligned parallel to latitude bands) is required. Orbits using the partial or full stratospheric chemistry complementary observation set are G1, G2, C3, E4, E6, G7, G8, C9, and C10. * Airglow observations are generally grouped into the complementary obser- vation sets of FUVFEA, CENMAP, BRTMAP, FIXTMD/FIXTMB, FIXLON, EWMAPS, and NEWS in each orbit. These measurements perform the following studies: global coverage of hydrogen bulge and the distribution of other atomic and molecular species using the technique of observing a fixed local time over a Jupiter rotation; latitudinal and meridional coverage of the H limb-darkening curves using East-West maps during short time intervals; global coverage of H, H2, and other atomic and molecular species' abundance using N-S, E-W maps for measuring latitudinal and meridional brightside emissions; regional time variation of Io hot spot and other regional features by observing at fixed longitudes for one-half Jupiter rotation; and high spatial resolution of local features in the feature track campaigns. The DRKNEW observation, which also observes nightglow and global H distribution without solar influence, is done separately at solar occultation. Orbits using the full airglow complementary observation set are G1, G2, G8, C9, and C10 while all other orbits use a subset of these observations. * Auroral observations are generally grouped into the complementary obser- vation sets of AURMAP, AURVAR, DRKMAP, and FIXLON in most orbits. These measurements combine midnight/noon asymmetry mapping, variability in the auroral darkside, long-term zonal survey mapping, and high temporal resolution studies of the variability of local auroral features. Orbits using the full auroral complementary observation set are G1, G2, E4, E6, G8, C9, and C10 while all other orbits use a subset of these observations. * Calibration is done early and late in the mission with star calibrations on previously observed targets using the STRCAL observation. The star kappa Vel is a particularly suitable, though not the only, candidate. The radiation environment on the Jupiter approach is also characterized with five RIMs of recorded data during JA/J0 using the RADMON observation. * Targets of opportunity may exist and will be identified on a case-by-case basis. MEASUREMENT SET PRIORITIES The UVS measurement set priorities, listed by acronym and fully described in the measurement set element description section, are listed. The recorded observations reflect the agreements made between discipline working groups as to bits-to-ground (BTG) and tape track allocations. The realtime observations include the highest priority UVS activities (designed to minimize BTG and tape track allocation resources) and will use realtime BTG during the encounter period in several of the realtime formats. Orbit JA/J0: 1) RADMON recorded 2) FUVPES recorded Orbits G1-E11: 1) AURMAP realtime 2) FUVFEA recorded 3) ACELAT recorded 4) DRKNEW recorded 5) AURVAR recorded 6) CENMAP realtime and recorded 7) BRTMAP realtime and recorded 8) DRKMAP realtime 9a) FIXTMD realtime 9b) FIXTMB realtime and recorded 10) FIXLON realtime 11a) EWMAPS recorded 11b) NEWSMP recorded 12) STRCAL realtime DESCRIPTIONS OF MEASUREMENT SET ELEMENTS Period JA/J0 : RECORDED: 1) RADMON Objective: radiation environment characterization during Jupiter approach; Strategy: G-N channel recorded 1 RIM for each of 5 Rj distances; target to the NEP (North Ecliptic Pole); Location: 100, 50, 25, 15 and 9 Rj ; geometry constrained; 2) FUVPES Objective: FUV feature track campaign (reflectance map) of the Probe Entry Site (PES) for three emission angles near 60 deg phase angle; Strategy: 1 RIM F channel and 5 RIMs G channel recorded for one phase angle and three emission angles during ridealong observations with other remote sensing instruments (F channel with SSI, G channel with NIMS on one emission angle and G channel independently on two emission angles); Location: near 21 Rj during JA/J0; geometry constrained; Orbits G1-E11: REALTIME: 1) AURMAP Objective: Midnight/noon auroral mapping to study asymmetries under the same solar and magnetospheric conditions; higher spatial resolution beginning G7; Strategy: a secondary G channel 10 bps RTS 1.5 hour observation with one-half hour on bright side and 1 hour on dark side; used as a backup observation to FIXTMD, FIXTMB, or FIXLON; use TMC (Target Motion Compensation) in TARGET; Location: 90 deg phase angle; geometry constrained; RECORDED: 2) FUVFEA Objective: FUV feature track campaign (reflectance map) for low to high phase angles and for a variety of emission angles; Strategy: 1 RIM F channel and 5 RIMs G channel recorded per one phase angle and one emission angle; 'stare' mode in ridealong with SSI (and NIMS where applicable); make 3 emission angle observations at each phase angle; record each emission and phase angle observation and deselect from playback those observations which are not of the highest priority to fit within the AWG FUVFEA allocations of BTG described below; [Note: A possible option exists for conducting an emission/phase angle observation in the realtime science mode which places the photon counts into the UVS integration (summation) buffer in the Command Data System (CDS) rather than on the tape recorder. In this case, the RTS telemetry format would begin at a time such that the CDS cycle for flushing the integration buffer would fall between the F and G channel observations. The appropriate detector would be turned on for only those RIMs that data were actually to be taken.]; Location: low to high phase angles at 3 emission angles per phase angle (large phase angle requires 90 deg SITURN); geometry constrained; 3) ACELAT Objective: Ammonia and acetylene latitude map (meridional scan) for hydrocarbon stratospheric chemistry and transport tracer study; excellent opportunity for distinguishing auroral zone from Io footprint on brightside latitudinally; Strategy: F & G channels recorded for 0.5 hours; 45 deg SITURN required for horizontal UVS slit to RA = 90 and Dec = -20 during G2 at 96-250/19:30:00; use TMC in TARGET; Location: 10 deg phase angle and 14-15 Rj; geometry critical; first orbits (G1 or G2); 4) DRKNEW Objective: Darkside north-south scans for detailed, full-disk mapping of nightglow and aurora observing short time scale variations as well as zonal and meridional asymmetries under given magnetospheric conditions; good for mapping global Balmer series hydrogen distribution and detection of H2 continuum emission without direct solar illumination; excellent opportunity for distinguishing auroral zone from Io footprint on darkside latitudinally; Strategy: F/G & N/G channels during C3 recorded for 1.553 hours (average time from POINTER analysis) on this orbit with a solar occultation; large SITURN required; UVS slit oriented horizontally; Location: very high phase angle outbound in solar occultation region; geometry critical; 5) AURVAR Objective: Darkside auroral variability detailed study to look at short time scale variations using Lyman-alpha miniscans at fixed location; 3 orbits late in the mission; Strategy: G channel miniscans recorded in 0.5 hour observations; use TMC in TARGET; Location: as close as possible to Jupiter, depending on radiation; orbits G8, C10, E11; geometry constrained; REALTIME AND RECORDED: 6) CENMAP Objective: Brightside mapping of hydrocarbons along the central meridian at low phase angles for long term variability studies on every orbit possible viewing the brightside on inbound leg; Strategy: G channel 10 bps RTS for 2.5 hours (1 scan with 5 points) and F channel 5 RIMs recorded; use TMC in TARGET; Location: as close as possible to Jupiter, depending on radiation, for spatial resolution and with a bright central meridian; geometry constrained; 7) BRTMAP Objective: Brightside survey mapping of UV global energy budget using a central meridional and equatorial scan for long term variability studies on every orbit possible viewing the brightside on inbound leg; Strategy: G channel 10 bps RTS for 4.5 hours and F channel 9 RIMs recorded; 2 scans (central meridian 5 points and equatorial latitude 4 points) with a total of 9 observation points; use TMC in TARGET for central meridian scan; the central meridian scan can be eliminated when the observation is sequential in time with the CENMAP observations in G2 and G8; slow slews may be substituted for point-and-stare strategy, particularly in east-west direction; Location: as close as possible to Jupiter, depending on radiation, for spatial resolution and with a bright central meridian; geometry constrained; REALTIME: 8) DRKMAP Objective: Darkside survey mapping of nightglow and aurora at specified latitudes or longitudes for 1) long-term zonal variability studies on every close-in orbit where darkside viewing on inbound leg is possible and 2) long-term global variability studies on every further-out orbit where darkside viewing on inbound leg is possible; Strategy: G, F, N channels 10 bps RTS for 1.5 hours; 3 horizontal scans (each at a different latitude); DRKMAP OBSERVING STRATEGY EARLY LATE CLOSE (zonal) E4, E6 G7, G8, C9, C10 FAR (global) G1, G2, C3 E11 Location: where darkside viewing is possible early in mission (farther out global coverage) and later in the mission (closer in zonal coverage); geometry constrained; 9a) FIXTMD Objective: Jupiter fixed local time map of aurora or equatorial electroglow on dark side to study global variation of hydrogen bulge and the distribution of other atomic and molecular species at auroral and equatorial latitudes; Strategy: a primary G channel 10 bps RTS 10 hour observation for one Jupiter rotation; use TMC in TARGET; Location: greater than or equal to phase 90 deg as well as the closest location as possible to Jupiter (G7-E11 when darkside is most visible); REALTIME AND RECORDED: 9b) FIXTMB Objective: Jupiter fixed local time map of aurora or equatorial electroglow on bright side to study global variation of hydrogen bulge and the distribution of other atomic and molecular species at auroral and equatorial latitudes; Strategy: a primary G channel 10 bps RTS 10 hour observation for one Jupiter rotation with F channel 1 RIM recorded per hour to remove overlapping order effects on bright side; use TMC in TARGET; Location: less than phase 90 deg as well as the closest location as possible to Jupiter (G1-E6 when brightside is most visible); REALTIME: 10) FIXLON Objective: Jupiter scans at fixed longitudes to study long- and short-term dark and bright variations of local and regional features such as the Io hot spot and H, H2 plus other atomic and molecular species at auroral and equatorial latitudes on darkside and/or brightside; Strategy: a primary G channel 10 bps RTS 5 hour observation (maximum) for one-half Jupiter rotation; use TMC in TARGET; Location: either bright side or dark side and as close to Jupiter as possible, depending on radiation, for zonal resolution and farther from Jupiter for global/meridional resolution; geometry constrained; RECORDED: 11a) EWMAPS Objective: Dayglow/electroglow study using east-west latitude swath to determine limb-darkening curves of Lyman-alpha, H2 dayglow; Strategy: F, G channels recorded for 0.5 hours; ratio of 1 RIM F to 5 RIMs G; Location: as close to Jupiter as possible, depending on radiation, at about phase 45 deg - 60 deg; 11b) NEWSMP Objective: Dayglow/electroglow study using north-east-west-south swaths to determine limb-darkening curves of Lyman-alpha and global H2 band emission distribution; used with DRKNEW to constrain relative importance of fluorescence versus electron impact in H2 band emissions; Strategy: F, G channels recorded for 0.93 hours (average time from POINTER analysis); combine with ACELAT in G2 by performing the observation 1 Jovian rotation before ACELAT and deleting the central meridian (N-S) swath; possibly use Lyman-alpha miniscan in C10 observation to obtain a hydrogen map of Jupiter; Location: as close to Jupiter as possible, depending on radiation, at about phase 45 deg - 60 deg early and late in mission (G2 and C10); REALTIME: 12) STRCAL Objective: Instrument calibration twice during mission (early and late) on previously calibrated star; alpha Eri not suitable due to variability while kappa Vel is a good candidate; Strategy: F, G channels at 10 bps RTS for 1.5 hours for early in mission (and potentially F & G recorded for up to 30 RIMs in C9 to get AACS coverage); Location: as early in the encounter period as possible; AACS data Recorded: (6 words x 16 bits/word)/0.667 sec = 144 bps added to each recorded observation. Realtime: 2 bps data in engineering data stream are not costed to science bits. Cooperative images SSI frame uncompressed: 5.05 x 106 bits. Can estimate 100:1 compression (0.05 x 106 bits) for edited SSI frames and use for cooperative images requiring knowledge of satellite or atmosphere features. Can be recorded, deselected on playback. OPNAV image: highly compressed SSI frame (about 400:1 = 0.013 x 106 bits) used when only limb crossing information is required. Sent into downlink stream as soon as it is taken with priority above any other downlinked data; AWG priorities = 3, 5, 10, 12, 13, 16. SITURN Estimated 2.8 kg propellant used for each balanced SITURN to 90 deg off Earth point; use for solar occultation, ammonia/acetylene map, and high phase feature campaign; JA/J0 ACTIVITY PLANS 1. RADMON100: UVS radiation monitor (G-N); 1 RIM; 95-333/20:30 at 100 Rj . 2. RADMON050: UVS radiation monitor (G-N); 1 RIM; 95-338/16:30 at 50 Rj . 3. RADMON025: UVS radiation monitor (G-N); 1 RIM; 95-340/14:30 at 25 Rj . 4. RADMON015: UVS radiation monitor (G-N); 1 RIM; 95-341/05:30 at 15 Rj . 5. RADMON009: UVS radiation monitor (G-N); 1 RIM; 95-341/13:30 at 9 Rj . 6. FUVPES1: UVS FUV PES ridealong; 6 RIMs; 95-340/20:00 at 20 Rj. 7. FUVPES2: UVS FUV PES ridealong; 6 RIMs; 95-340/20:00 at 20 Rj . 8. FUVPES3: UVS FUV PES ridealong; 6 RIMs; 95-340/20:00 at 20 Rj . ++++++++++++++++++++++++++++++++++++++ MWG SCIENCE AND OBSERVATION OBJECTIVES ++++++++++++++++++++++++++++++++++++++ GLL EUV/UVS OBSERVATIONS OF THE IO TORUS INTRODUCTION The Voyager UVS investigation discovered bright EUV emissions from what was soon identified as a plasma torus in Io's orbit, and the almost simultaneous prediction and discovery of active volcanism on Io answered the immediate question of where the material and energy of the torus came from. Since then, Io's torus has been the focus of intense interest and of considerable observational and theoretical efforts. The ions S II, S III, S IV, O II, and O III have been observed; neutral Na was known to be present for some time before Voyager; and a vast nebula of Na I surrounding Jupiter has been discovered since. Similar distributions of S I and O I are expected at greater densities than Na I, but have never been detected. The EUV channel was added to the GLL UVS investigation specifically to add to our understanding of the torus. Because of great observational difficulties, little work has been done in the EUV since Voyager. This wavelength region includes most of the energy emitted by the torus, and EUV radiation is the major cooling process for its ions and electrons. We can therefore expect that the EUV offers great diagnostic capabilities, particularly of the secular and periodic behavior of the processes that produce, control, and dissipate the torus. SCIENTIFIC RATIONALE The Jovian magnetosphere rotates past Io at about 55 km/sec. Material sputtered off Io or its atmosphere, or thrown off directly by volcanic activity, is accelerated after ionization to near co-rotation speed as it is picked up by the magnetic field. Radiative energy loss from the torus is severe and without sustained injection of energy, the torus would lose most of its energy content in less than two rotations. Part of the energy supply is provided by ion pickup with subsequent transfer to the electrons. However, a heterogeneous energy source is needed to explain the relatively high temperature of the main part of the torus. There is currently no satisfactory explanation for the additional energy source, and the torus energy budget remains one of the major issues to be resolved. The energy budget can be directly addressed with judicious observations by the Galileo UVS. The torus is trifurcated, with a cold inner region, a very narrow ribbon region near 5.7 Rj, connected to a warm outer plasma region. The inner region has no measurable EUV emission. The ribbon is assumed to be at a temperature high enough to produce EUV emission, but currently is observed only in infrared lines of S II and S III. The outer region presumably in combination with the ribbon region is responsible for the observed EUV emission spectrum obtained by the Voyager UVS. There is a general agreement that the ribbon region may be an important and possibly a key factor in the dynamics of the system, but current information on the energetics and temporal and spatial morphology is limited to the ground based observation. The Galileo UVS can directly address the partitioning, plasma temperature, and energy budget questions. There is a dependence of ion partitioning on electron kinetic distribution. The more highly stripped ions, S IV and O III, are sensitive to the high energy component of the electron population and their mixing ratios can be utilized as measures of how energy is inserted, and limits to the mean input rate can be calculated from limits on the emission lines of these species. The torus is strongly affected by the rotation of Jupiter. Ions are trapped in a potential well formed by the rotation of the magnetic field and the curvature of the field lines; they spread in this potential well to about 1 Rj from the centrifugal equator. The torus wobbles in Jupiter's rotational frame because of the tilt and offset of the magnetic field. It is brighter in the local evening sector than in the morning, implying that the electrons are heated periodically in a region fixed in local time. All these effects require observations that have time resolution substantially greater than Jupiter's rotation period of 10 hrs. The source of material for the torus - Io - rotates around Jupiter with a period of 43 hrs, and the response of the torus to episodic events on Io, such as large volcanic eruptions, may be expected to exhibit this periodicity. Ions are lost from the torus by diffusion, whose timescale is thought to be 60-100 days. Secular changes in torus density and/or temperature were observed between the V1 and V2 flybys, and major changes also occurred between the Pioneer and Voyager missions, five years apart. The chief thrust of the GLL EUV/UVS torus observations is to measure and characterize the hot and cold torus densities, composition, and temperatures on time scales varying from the shortest achievable in the light of signal-to- noise considerations (nominally 30 mins) to the length of the orbital mission (about 2 years). EUV/UVS MEASUREMENTS Emission lines suitable for observations are those that are diagnostic of composition and/or temperature and that produce adequately strong signals. Table 1 shows, for selected lines, the expected brightness and signal-to- noise for 1-hour observations. The EUV S/N values take account of the spin-scan nature of these observations, and the UVS values assume a fixed inertial 'stare' at an ansa. The noise levels are estimated from Voyager UVS data. See the OPG document for additional figures and tables. TABLE 1 - TORUS EMISSION LINES AND S/N VALUES Line Wavelength Brightness Signal S/N for 60 min. obs (A) (Rayleigh) cts/s @ 65 Rj @ 40 Rj S III 685 360 13.6 8.7 5.7 O II 834 250 7.8 5.6 3.4 S III 1194 53 7.1 20. 11. S II 1259 34 7.0 20. 11. S IV 1406 8 1.2 3.6 1.9 O III 1666 6* O II 2471 48 2.0 5.9 3.1 O II 3728 270 189 310 230 S II 4070 76 46 110 67 * No confirmed detection; estimated intensity at V1 encounter according to model partitioning calculations. Estimated intensity at V2 encounter is ~1 R. The relevance of the above emissions to the scientific goals can be summarized as follows: a) To monitor the energy radiated by the torus, the EUV spectrum, which carries about 80% of the total, must be measured. b) The most abundant ion in the torus is O II, followed by S III and S II. Measurements of the 3728A and 4070A emissions will establish the S II/O II ratio. Measurements of the 1259A and 1194A emissions will establish the S III/S II ratio. c) Measurements of ratio of the S II features at 4070A and 1259A will establish the effective electron temperature. d) The densities of the minor ions S IV and O III are diagnostic of the presence of hot electrons. Its emission at 1406A will be monitored to establish S IV population. The species most sensitive to the hot component of the electron population is O III. It is therefore expected to be the most unstable component, and a very sensitive measure of energy input by the hot electron population. Measurements of the upper limit to the 1666A line therefore constitute an important limitation on energy source mechanisms. e) In addition to the above, the excellent S/N in the O II emission at 3728A makes it possible to 'map' the extent of the torus beyond 7 Rj in Io's orbital plane and beyond 1 Rj above and below it. A typical estimate of the ion composition has O II, O III, S II, S III, and S IV present with partition fractions .62, .01, .175, .180, and .02 respectively. The S/N values at 65 Rj allow variations in these partition fractions, and therefore in the total ion density also, to be detected at or below the 1% level. The ratio of the S II line at 1259A to that at 4070A varies almost linearly with electron temperature, and at 65 Rj the S/N in the two lines allows the temperature to be measured to +- 5%, or +- 3000 deg. OBSERVING PLAN Opportunities to make the above measurements are subject to several constraints. The EUV instrument looks at a S/C cone angle of 90 deg; its observing times are determined by orbital parameters and by the pointing of the S/C spin axis. The UVS is on the scan platform, so the above measurements require the dual-spin S/C mode. UVS measurements must be made at S/C cone angles not less than 90 deg, and for the N channel the 'sun cone' angle must also be not less than 90 deg. In addition, both instruments are subject to radiation noise, and measurements will not be made within specific distances from Jupiter, currently set at 25 Rj for the EUV and 15 Rj for the UVS. Figure 2 shows the times on each orbit at which each of these constraints can be met. Five 'events' on each orbit are shown for each cone constraint, to wit: the midnight and noon ansae of Io's orbit, Jupiter itself, and the midnight and noon 'ansae' of Europa's orbit at which the EUV measurements are begun and ended. The noise constraints are also shown; these override any other constraint. The observing strategy is as follows: During the EUV observing window, the UVS will observe at a S/C cone of 90 deg to provide simultaneous coverage with the EUV. UVS measurements will be of O II at 3728A, S II at 4070A and 1259A, and S III at 1194A, to satisfy the scientific goals (a), (b), and (c) above. After the end of the EUV measurements, and before the UVS reaches its noise limit, the UVS can observe the dawn-side ansa of the torus. On some orbits, the dusk-side ansa can also be observed after Jupiter closest approach (C/A). During these opportunities, the UVS will measure O II at 3728A, S II at 4070A and at 1259A, and S III at 1194A, to further goals (a), (b), and (c). It will also look for S IV at 1406A, to fulfill goal (d). Finally, it will look for O II at 3728A and S II at 4070A above and below Io's orbit plane to satisfy goal (e). The EUV utilizes an instrument memory buffer configured in a wavelength by sky-sector matrix to accumulate Phase 2 RTS data. This buffer configuration is controlled by the Fixed Pattern Noise Table (FPNT); the FPNT is uplinked via the sequence whenever the instrument is powered on. There are three standard FPNTs: the Torus table, the Aurora table, and a General table. If EUV is to make Aurora observations, for example as the spacecraft causes the EUV FOV to pass over Jupiter, then the Torus table is replaced by the Aurora table for the duration of that observation. The Torus table would then reconfigure the buffer matrix for the remaining Torus observations. Generally, these tables determine the wavelength resolution by summing over the specified detector pixels; line features and background criteria determine the construction of these tables so that the optimum resolution may be obtained for the science in consideration. Which table is in effect is given in the data file label. The three FPNT tables are described in the EUV instrument label file. Table 2 give a skeleton timeline for EUV/UVS torus measurements. TABLE 2 - INSTRUMENT ON/OFF AND TARGET TIMELINE orb inst begin end pointing G1 EUV 176/21:40-182/11:47 @ 90 deg S/C cone UVS 176/21:20-182/11:47 @ 90 deg S/C cone UVS 182/11:47-186/10:04 torus a.m. ansa G2 EUV 238/15:19-244/23:22 @ 90 deg S/C cone UVS 238/15:19-244/23:22 @ 90 deg S/C cone UVS 244/23:22-250/19:00 torus a.m. ansa C3 EUV 301/22:37-307/04:15 @ 90 deg S/C cone UVS 301/22:37-307/04:15 @ 90 deg S/C cone UVS 307/04:15-310/17:17 torus a.m. ansa E4 EUV 346/20:07-351/08:40 @ 90 deg S/C cone UVS 346/20:07-351/08:40 @ 90 deg S/C cone UVS 351/08:40-353/07:17 torus a.m. ansa E6 EUV 048/04:07-049/23:29 @ 90 deg S/C cone UVS 048/04:07-050/23:28 @ 90 deg S/C cone UVS 050/23:28-051/00:49 torus a.m. ansa G7 EUV 091/12:30-092/14:30 @ 90 deg S/C cone UVS 091/12:30-093/14:52 @ 90 deg S/C cone (post-perijove) UVS 095/04:50-096/16:00 torus p.m. ansa G8 EUV 125/05:23-126/15:11 @ 90 deg S/C cone UVS 125/05:23-127/15:56 @ 90 deg S/C cone (post-perijove) UVS 129/05:10-129/16:00 torus p.m. ansa C9 EUV 176/11:38-176/16:51 @ 90 deg S/C cone UVS 176/11:38-177/17:46 @ 90 deg S/C cone (post-perijove) UVS 179/03:20-180/16:00 torus p.m. ansa C10 EUV 259/11:17-260/03:23 @ 90 deg S/C cone UVS 259/11:17-261/03:20 @ 90 deg S/C cone (post-perijove) UVS 262/16:50-263/16:00 torus p.m. ansa E11 EUV 308/11:42-309/04:57 @ 90 deg S/C cone UVS 308/11:42-310/04:52 @ 90 deg S/C cone (post-perijove) UVS 311/18:43-313/16:00 torus p.m. ansa MWG MEASUREMENT SETS The UVS and EUV measurement sets are listed by acronym and fully described above. There are no recorded observations. The realtime observations include high priority EUV and UVS activities and will use realtime BTG. EUV file names are coordinated with UVS OAPEL observation names so that time periods of simultaneous observations have like file names. Orbits JA/J0-E11: UVS observation names MANSxx - Midnight Ansa, cone = 90 deg NANSxx - Noon Ansa, cone = 90 deg MPROxx - Midnight Profile, cone > 90 deg NPROxx - Noon Profile, cone > 90 deg CROSSCAL, XCALxx - UVS/EUV cross-calibration EUV observation names MANSxx - Midnight Ansa NANSxx - Noon Ansa MPROxx - Midnight Profile NPROxx - Noon Profile AURAxx - Jupiter Aurora (UVS aurora observations are listed under AWG) CROSSCAL, XCALxx - UVS/EUV cross-calibration ++++++++++++++++++++++++++++++++++++++ SWG SCIENCE AND OBSERVATION OBJECTIVES ++++++++++++++++++++++++++++++++++++++ KEY QUESTIONS The UVS and EUV satellite observations during the Jupiter tour will answer several key questions related to the state of evolution and the surface composition of the Jovian satellites. The observational goals and strategies detailed below, combined with the Galileo's capabilities based upon the Phase II flight software, will permit observations which can answer these questions. The UVS and EUV satellite observations will determine the composition, or upper limits to the number density, of the neutral atmosphere of the Galilean satellites and the Io neutral cloud. The UVS observations will also determine the excitation mechanisms and escape rates of the satellite atmospheres. In addition, the UV albedo, when combined with the visible and infrared spectra, will determine surface composition and particle size. OBSERVATION GOALS The UVS and EUV satellite observations will be conducted during each Jovian orbit with the exception of the non-targeted fifth orbit (J5). The principal goal of these observations will be to answer these key scientific questions as well as to support the Satellite Working Group observations where possible. OBSERVATION STRATEGY Observations which will address the science questions are based upon the detailed observation descriptions below. UVS and EUV observations can be grouped into two general science area categories. These are 1) Volatile Escape; and 2) Surface Albedo and Composition observations. The categories are described below where the capitalized acronyms are the six-character observation names. 1) Volatile Escape observations will search for atomic spectral lines (H,O,C,N), molecular bands (OH,CO,CO2+), and neutral clouds (SO2,SO,O,S,K,Na) to determine the altitude near the Jovian satellites. These measurements will enable an understanding of the excitation mechanisms and the escape rates to determine the state of evolution of the Jovian satellites. The measurement set used to obtain this information consists of the BRTLMB, DRKLMB, ECLIPS, NRLCLD and SPNSCN observations. 2) Surface Albedo and composition observations will extend the surface scattering property measurements into the ultraviolet (1600A-3200A) and extreme ultraviolet (500A-1300A) wavelengths. The data retrieved will provide information about particle size and absorption properties of the surface materials at resolutions and phase angles which cannot be obtained from Earth. The data will also be used to supplement and complement the NIMS surface property measurements. The measurement set used to obtain this information consists of the GLOBAL, MAPPNG, PHASE and SPNSCN observations. 3) Additional data are required through AACS-provided pointing information for all realtime and recorded observations. These data are provided through the realtime science formats and the recorded low-rate science ancillary data packets. SWG MEASUREMENT SET PRIORITIES The UVS and EUV measurment sets are listed by acronym and fully described below. The recorded observations reflect the agreements made between discipline working groups as to the bits-to-ground and tape track allocations. The realtime observations include high priority UVS activities (designed to minimize the bits-to-ground and tape track allocation resources) and will use realtime bits-to-ground during the encounter period. Orbit JA/J0: No UVS or EUV satellite observations are planned. Orbits G1-E11: BRTLMB - UVS Satellite Bright Limb Drift Observations DRKLMB - UVS Satellite Dark Limb Drift Observations ECLIPS - UVS Satellite Eclipse Observations GLOBAL - UVS Satellite Global Observations (ride-along with NIMS team) MAPPNG - UVS Satellite Mapping Observations (ride-along with NIMS team) NRLCLD - UVS Io Neutral Cloud Observations PHASE - UVS Satellite Phase Coverage Observations SPNSCN - EUV Callisto Spin Scan Image Observations Note: The NIMS team often uses observation names based on the surface feature; when UVS rides-along with their observation, the same name is used. Recorded: 1) BRTLMB Objective: Measure the altitude distribution of the volatiles near the sub-solar point to determine the escape rates from the Jovian satellites when the atmosphere is in full solar illumination. Strategy: Near the satellite closest-approach, position the UVS field-of-view (FOV) approximately 1 satellite-radius off the satellite sub-solar point and allow the spacecraft motion to carry the FOV onto the body surface. Once this has completed, reposition the UVS FOV to ~1000 km off the satellite sub-solar point and allow the spacecraft motion to carry the FOV onto the body surface. Orbits: Ganymede - G1, G2; Callisto - C3, C10; Europa - E11. 2) DRKLMB Objective: Measure the altitude distribution of volatiles off the dark limb to determine the particle impact excitation emission rates from the Jovian satellites. Strategy: Near the satellite closest-approach, position the UVS field-of-view (FOV) on the surface of the dark limb and allow the spacecraft motion to carry the FOV to approximately 1 satellite radius off the satellite surface. Orbits: Ganymede - G1, G2; Callisto - C3, C10; Europa - E11. 3) GLOBAL Objective: Extend the surface scattering property measurements into the UV (1600A - 3200A) in concert with the NIMS measurements to infer information about particle size, and refractive and absorption properties of the surface materials. Strategy: Ride-along with the NIMS Ganymede and Callisto global observations. Cover the satellite surface at the highest resolution available within the allocated downlink bits and tape. Orbits: Ganymede - G1, G7; Callisto - C3, C9, C10. 4) MAPPNG Objective: Extend the surface scattering property measurements into the UV (1600A - 3200A) in concert with the NIMS measurements to infer information about particle size, and refractive and absorption properties of the surface materials. Strategy: Ride-along with several NIMS Ganymede and Callisto high resolution observations. Cover the satellite surface at the highest resolution available within the allocated downlink bits and tape. Orbits: Ganymede - G1, G8; Callisto - C9. 5) SPNSCN Objective: Characterize Callisto's surface and aeronomic properties by measuring the EUV surface albedo (He,O2,H) and local atmospheric resonance line wavelengths (H,He,O,Ar,S,C). Strategy: Record EUV data for approximately 15 RIMS centered on the time when Callisto will cross the EUV FOV at 90 deg. cone. Orbits: Callisto - C3, C10. Realtime 6) ECLIPS Objective: Characterize the change in the lower atmospheric UV airglow emissions as Io and Europa enter and exit eclipse. Determine if the source of the change is due to: 1) a change in the lower atmospheric composition as it cools (ie. SO2 condensation); or 2) a potential change in the excitation mechanism if solar excitation is dominant over particle impact. Strategy: Monitor the satellite for one hour prior to ingress, one hour after ingress, one hour before egress, and one hour after egress utilizing the UVS 10bps realtime capacity. Orbits: Io - all, Europa - all. 7) NRLCLD Objective: Determine the composition and time variation of the ionized Io neutral cloud (SO2,SO,O,S,K,Na) to assist in the modeling of the Io plasma torus and Io's atmosphere. Strategy: Monitor the emissions from Io at various distances from the satellite for a total of four hours per orbit. Orbits: Io - all. 8) PHASE Objective: Observe Io and Europa in the 1600A to 3200A wavelength regions at phase angles not obtainable from the Earth to supplement and complement the NIMS surface property measurements. Strategy: Observe Io and Europa at various phase angles throughout the tour utilizing the UVS 10bps realtime capability. Orbits: Io - all, Europa - all. +++++++++++++++++++++++++++++++++++++ As of August 1997 the planned UVS GEM Mission Jupiter Observations are: E12 *Satellites Europa tenuous atmosphere Io atmosphere *Magnetosphere None in this orbit *Jovian Atmosphere Upper atmosphere energy budget E14 *Satellites Europa tenuous atmosphere and surface composition Io atmosphere *Magnetosphere Io plasma torus energetics *Jovian Atmosphere North polar aurora energetics E15 *Satellites Europa and Io tenuous atmosphere and surface comp. *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Upper atmosphere energy budget E16 *Satellites Europa surface composition *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Stratosphere composition and upper atmosphere energy budget E17 *Satellites Europa tenuous atmosphere and surface composition *Magnetosphere Io plasma torus energetics *Jovian Atmosphere South polar aurora energetics E18 *Satellites Europa tenuous atmosphere and surface composition *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Upper atmosphere energy budget E19 *Satellites Europa tenuous atmosphere and surface composition *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Stratosphere composition and upper atmosphere/aurora energy budget C20 *Satellites Io surface composition *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Stratosphere composition and upper atmosphere/aurora energy budget C21 *Satellites Callisto and Io surface composition *Magnetosphere None *Jovian Atmosphere None C22 *Satellites None *Magnetosphere Io plasma torus energetics *Jovian Atmosphere Stratosphere composition and aurora energy budget C23 *Satellites None *Magnetosphere Io plasma torus energetics *Jovian Atmosphere North polar aurora energetics I24 *Satellites Io surface composition *Magnetosphere None *Jovian Atmosphere None I25 *Satellites Io surface composition *Magnetosphere None *Jovian Atmosphere None These GEM observations will complete the correlated set of observations needed to answer the science questions given above. Parameters ========== The Playback data represent the highest time resolution data. The detector is read out every 0.688 seconds for 528 values over 4.0 seconds for each recorded spectra of 4.333 seconds. The instrument operation may vary for each observation. Read the file label and the associated orbit command sequence for explicit details. The Real-Time-Science (RTS) data format integrates pairs of spectra in a 16-bit on-board CDS (Command and Data System) buffer. After the specified summation period, the RTS buffer is sent to the ground in real time packets. Files of RTS UVS spectra are formatted to contain one summation buffer with its associated (time tags) header. The duration of the summation period varies, as does the instrument configuration, within and across Observation classes. The file label and command sequence must be used to verify the observation criteria. Data ==== AWG OBSERVATIONAL RESULTS As of Aug 27, 1997, the following observation data have been obtained. STRATOSPHERIC AEROSOLS and HYDROCARBONS Feature tracks: Great Red Spot & vortices G1, C9 Acetylene distribution G2 belt-zone boundary C3 5 micron hot spot E4 white oval E6 brown barge G7 southern polar haze G8 plume C9 hi phase crescent C9 AURORAE EUV G1, C3, E4, E6, G7 (G) FUV G1, G2, C3, E4, E6, G7, G8, C9 (F) MUV G1, C3, E4, E6, G7, C9 (N) NUV (none) IMAGE/SPECTRA C3, G7, C9 AIRGLOW Lyman-alpha distribution G1, G2, C3, E4, E6, G7, G8, C9 Lyman-alpha limb curve G1, G2, G8 EUV H2 dayglow J0CD, G2, C3 FUV H2 dayglow G2, E4, E6, G7, G8 Hydrogen corona G8 The following EDR data files are available as of 1 September 1998. The files are grouped with the descriptions of AWG, SWG and MWG observation objectives for the orbit. The descriptions originate with the planning package. Some described observations may have been lost during downlink. They are included for completeness of the science concepts and designs. All available data files are shown. Orbit J0CD/G1 * G1 AWG The G1 UVS Jovian atmosphere observations focus on 4 types of activities: 1) GRS Feature Track Campaign: 6 observations. G1JUFTKR2E12,13,22,23,32,33 observe the GRS in conjunction with the AWG GRS campaign. The UVS objective is to supplement the campaign with measurements of the spectral (i.e., compositional) features of the GRS and its vicinity. (RTS only) 2) Auroral studies: 3 observations investigate Jovian auroral processes. a) G1JUEWMAPS01 is a recorded, 1/2 hour observation of the southern auroral region, including the footprint of the Io fluxtube. Precipitating electron energies, as they impact the upper atmosphere hydrogen, will be derived. This observation is planned in collaboration with near-simultaneous HST Jovian auroral observations by John Clarke of Univ. of Michigan. b) G1JUAURMAP01, also in a campaign with HST observations, will observe the southern auroral region asymmetries between dayside and nightside aurorae. (RTS only) c) G1JUFIXTMD01 will observe northern auroral activity in a unique look at precipitating electron energies as they vary with longitude during 1 full Jupiter day (10 hours). (RTS only) 3) Upper atmosphere and global energy studies: 2 observations. G1JUFIXLON01 and G1JUDRKMAP01 both measure the characteristics of the upper atmosphere hydrogen on the darkside of the planet (i.e., without the effects of solar illumination) in order to develop a global map of equatorial hydrogen distribution during the mission for global energy budget studies. (RTS only) 4) calibration: 2 observations: a) G1HUSTRCAL01 will perform a UVS calibration on the star delta-Scorpii as one of two calibrations during the mission (also to be observed in C9). (RTS only) b) G1JURADMON01 is an LPW recorded, 1 RIM observation that will perform a radiation monitor test at 11 Rj. These data will be compared to data collected from the sky background just off the star in G1HUSTRCAL01 to quantify radiation effects upon the instrument far and close to Jupiter. * MWG - The standard Torus ansa (MANSxx, NANSxx) and Profile measurements (MPROxx, NPROxx) were obtained. * G1 SWG In this orbit, the priority UVS satellite observations will be the recorded bright and dark limb tenuous atmosphere measurements of Ganymede (BRTLMB and DRKLMB). These observations are designed to uniquely measure the altitudinal distribution of volatiles from their spectral signatures in the UV (O: 130.4 nm) and FUV (H: Lyman-alpha) and in the UV (OH:301.9 to 311.4 nm) for the two Bright Limb observations and in the UV (OH:301.9 to 311.4 nm) for the one Dark Limb. Five full spectrum MUV recorded ridealong observations with NIMS will observe surface scattering properties of the Memphis Facula (MEMPIS01), the AMON Crater (AMON__01), Isis and Ptah area (PTAH__01), Nippur Sulcus (NIPPUR01) and the Ganymede Global map (GLOBAL01). Realtime Io eclipse full spectral FUV/MUV observations (IECLPS) will characterize airglow emissions as Io enters and exits eclipse. Analysis of these data will provide the morphology of Io's atmosphere in the presence and absence of direct sunlight. An Io neutral cloud realtime observation (G1NTRC01) will provide information on the composition and time variation of neutral constituents that produce this cloud to assist in modeling the Io plasma torus and Io atmosphere. J0CD_URT_G1AURA02.DAT;2 J0CD_URT_G1AURA03.DAT;2 J0CD_URT_G1AURA11.DAT;2 J0CD_URT_G1AURA12.DAT;3 J0CD_URT_G1MANS02.DAT;2 J0CD_URT_G1MANS03.DAT;2 J0CD_URT_G1MANS11.DAT;2 J0CD_URT_G1MANS12.DAT;2 J0CD_URT_G1MPRO01.DAT;2 J0CD_URT_G1MPRO02.DAT;2 J0CD_URT_G1MPRO03.DAT;3 J0CD_URT_G1MPRO04.DAT;2 J0CD_URT_G1MPRO05.DAT;2 J0CD_URT_G1MPRO06.DAT;2 J0CD_URT_G1NANS01.DAT;3 J0CD_URT_G1NANS02.DAT;4 J0CD_URT_G1NANS31.DAT;2 J0CD_URT_G1NANS32.DAT;2 J0CD_URT_G1NANS33.DAT;2 J0CD_URT_G1NANS34.DAT;2 G01A_UPB_AMON__01.DAT;1 G01A_UPB_BRTLMB01.DAT;2 G01A_UPB_BRTLMB02.DAT;1 G01A_UPB_DRKLMB01.DAT;1 G01A_UPB_EWMAPS01.DAT;1 G01A_UPB_GLOBAL01.DAT;1 G01A_UPB_MEMPIS01.DAT;1 G01A_UPB_NIPPUR01.DAT;1 G01A_UPB_PTAH__01.DAT;1 G01A_UPB_RADMON01.DAT;1 G01A_URT_AURMAP01.DAT;2 G01A_URT_DRKMAP01.DAT;2 G01A_URT_EECLPS01.DAT;3 G01A_URT_EECLPS02.DAT;2 G01A_URT_EECLPS03.DAT;2 G01A_URT_EECLPS04.DAT;2 G01A_URT_FIXLON01.DAT;2 G01A_URT_FIXTMD01.DAT;3 G01A_URT_FTKR2E12.DAT;5 G01A_URT_FTKR2E13.DAT;3 G01A_URT_FTKR2E22.DAT;2 G01A_URT_FTKR2E23.DAT;2 G01A_URT_FTKR2E32.DAT;2 G01A_URT_FTKR2E33.DAT;3 G01A_URT_G1MPRO04.DAT;5 G01A_URT_G1MPRO05.DAT;2 G01A_URT_G1MPRO06.DAT;2 G01A_URT_G1NPRO01.DAT;2 G01A_URT_G1NPRO02.DAT;2 G01A_URT_G1NPRO03.DAT;2 G01A_URT_G1NPRO41.DAT;2 G01A_URT_G1NPRO42.DAT;2 G01A_URT_G1NPRO62.DAT;3 G01A_URT_G1NTRC01.DAT;1 G01A_URT_IECLPS01.DAT;2 G01A_URT_IECLPS02.DAT;2 G01A_URT_IECLPS03.DAT;2 G01A_URT_IECLPS04.DAT;2 G01A_URT_STRCAL01.DAT;2 G01C_URT_RECOVERY.DAT;1 G1_FIXED_TIME_MAP.DAT;2 G1_FIXTIM_MAP_INT.DAT;2 Orbit G2 * G2 AWG The top priority UVS Jupiter atmospheric observation during this orbit is a recorded far- and mid-ultraviolet (FUV/MUV: 115-320 nm) acetylene- ammonia map (ACELAT). In order to obtain latitudinal resolution better than that which is possible from Earth, the UVS slit is reoriented using a 23 degree science turn. Analysis of the data will result in a unique, seminal data set of stratospheric meridional circulation. Additional atmospheric observations will provide global UV energy budget measurements that are important for energy transfer modeling. Both the darkside/bright- side recorded NEWSMP and the realtime BRTMAP observations will provide FUV and MUV full spectral mapping to be used as the baseline for realtime- only observations in other orbits. A recorded ridealong observation with NIMS (GLOMOS) will provide complementary hydrogen (H) Lyman-alpha FUV measurements for brightside global energy mapping and will be compared with infrared measurements. Hydrogen bulge (Lyman-alpha) mapping will continue in this orbit with realtime observations focusing on time variability of specific longitudes (FIXLON) and on longitudinal asymmetries (DRKMAP). Realtime southern auroral full spectral FUV observations will provide longitudinal coverage during one Jupiter rotation. Analysis of the ratios between different spectral lines (color ratios) will yield energies of the electrons precipitating into the auroral zones. * G2 MWG The highest priority UVS magnetospheric observations during this orbit will be those in conjunction with the EUV instrument for the observations of the Io torus. There are two general segments of these observations, one set for the G2 inbound torus measurements at the beginning of the G2A encounter period and the second set for the C3 inbound measurements at the end of the G2C cruise period. Both sets of realtime measurements (G2NANS/G2MPRO, C3NANS/C3MPRO/C3NPRO) will map the torus ansae simultaneously with the EUV in S and O emission lines using the FUV/MUV wavelengths. Ratios of the emission lines will determine electron temperatures. The profile measurements, in particular, will characterize the torus ansae as a function of longitude, time and radius. Additionally, in conjunction with the MWG's magnetospheric survey, the UVS will conduct magnetonebula measurements (MAGNEB) during the G2B,C outbound cruise period. These long duration realtime measurements of FUV S I and O I emission lines looking down the magnetonebula axis (antisun direction) will integrate the flux in 24-hour segments. * G2 SWG In this orbit, the priority UVS satellite observations will be the recorded bright and dark limb tenuous atmosphere measurements of Ganymede (BRTLMB and DRKLMB). These observations are designed to uniquely measure the altitudinal distribution of volatiles from their spectral signatures in the UV (OH: 301-312 nm) and FUV (H: Lyman-alpha), respectively. Two full spectrum MUV recorded ridealong observations with NIMS will observe surface scattering properties of the Tammuz Crater (TAMMUZ) and the Ganymede north pole (NRPOLE). Realtime Europa full spectral FUV phase angle observations (EUPHAS), not obtainable from Earth (phases 79, 60, 43, and 58 degrees), will complement NIMS surface property measurements. Realtime Io eclipse full spectral FUV/MUV observations (IECLPS) will characterize airglow emissions as Io enters and exits eclipse. Analysis of these data will provide the morphology of Io's atmosphere in the presence and absence of direct sunlight. An Io neutral cloud realtime observation (NTRCLD) will provide information on the composition and time variation of neutral constituents that produce this cloud to assist in modeling the Io plasma torus and Io atmosphere. G02A_UPB_ACELAT01.DAT;2 G02A_UPB_BRTLMB01.DAT;2 G02A_UPB_DRKLMB01.DAT;1 G02A_UPB_FIXLON01.DAT;1 G02A_UPB_GLOMOS01.DAT;1 G02A_UPB_NEWSMP01.DAT;2 G02A_UPB_NRPOLE01.DAT;1 G02A_UPB_SIPPAR01.DAT;1 G02A_UPB_TAMMUZ01.DAT;2 G02A_URT_AURMAP01.DAT;1 G02A_URT_BRTMAP01.DAT;1 G02A_URT_DRKMAP01.DAT;2 G02A_URT_EUPHAS43.DAT;1 G02A_URT_EUPHAS58.DAT;3 G02A_URT_EUPHAS60.DAT;3 G02A_URT_EUPHAS79.DAT;3 G02A_URT_FIXLON01.DAT;1 G02A_URT_FIXTMD01.DAT;3 G02A_URT_G2NANS04.DAT;1 G02A_URT_G2NPRO01.DAT;1 G02A_URT_G2NPRO02.DAT;1 G02A_URT_G2NPRO03.DAT;1 G02A_URT_IECLPS01.DAT;1 G02A_URT_IECLPS02.DAT;1 G02A_URT_IECLPS03.DAT;1 G02A_URT_IECLPS04.DAT;1 G02A_URT_NTRCLD01.DAT;2 G02B_URT_GRATNG04.DAT;1 G02B_URT_UVSREC62.DAT;1 G02C_URT_C3AURA01.DAT;2 G02C_URT_C3AURA02.DAT;2 G02C_URT_C3AURA03.DAT;1 G02C_URT_C3MANS01.DAT;2 G02C_URT_C3MANS02.DAT;2 G02C_URT_C3MANS03.DAT;2 G02C_URT_C3MPRO02.DAT;2 G02C_URT_C3MPRO03.DAT;1 G02C_URT_C3MPRO04.DAT;1 G02C_URT_C3MPRO05.DAT;1 G02C_URT_C3MPRO06.DAT;1 G02C_URT_C3NANS01.DAT;2 G02C_URT_C3NANS02.DAT;3 G02C_URT_C3NANS31.DAT;2 G02C_URT_C3NANS32.DAT;1 G02C_URT_C3NPRO01.DAT;1 G02C_URT_C3NPRO02.DAT;1 G02C_URT_CROSSCAL.DAT;2 Orbit C3 * C3 AWG The top priority UVS Jupiter atmospheric observation during this orbit will be a recorded ultraviolet (115-410 nm) darkside map (DRKNEW) which is not possible to obtain from Earth. This observation during solar occultation will measure the planetary distribution of hydrogen (Balmer series and H2 continuum emissions) to distinguish hemispheric and longitudinal asymmetries with high spatial resolution. Analysis of the data will provide unique information on the energetics of the upper atmosphere without direct solar illumination. A major series of investigations will be the FUV/MUV (115-320 nm) contribution to the AWG feature track campaign. A white oval will be observed at two solar phase angles and three emission angles in realtime mode (FTKR1A/FTKR2A). The northern auroral zone (FTKR2B) will also be observed in the FUV/MUV almost coincident in time with MWG magnetospheric observations of field lines and particles connecting to the auroral region to be studied. Other realtime atmospheric observations will provide darkside equatorial hydrogen bulge (Lyman-alpha emission) mapping (FIXLON/DRKMAP), and a star calibration on Spica (DRKMAP). Realtime southern auroral full spectral FUV observations (AURMAP) will provide dayside/nightside asymmetries for an analysis of color ratios. These ratios will provide the energies of the electrons precipitating into the auroral zone. A realtime, fixed local time FUV map of the equatorial brightside (FIXTMB) during one Jupiter rotation will provide information on local time variability of the upper atmosphere as well as long-term variability when combined with observations in other orbits. * C3 MWG The highest priority UVS magnetospheric observations during this orbit will be those in conjunction with the EUV instrument for the observations of the Io torus and Jupiter aurora. There are two general segments of the torus observations, one set for the C3 inbound torus measurements at the beginning of the C3A encounter period and the second set for the E4 inbound measurements at the end of the C3C cruise period. Both sets of realtime torus measurements (C3NPRO and E4MANS/E4MPRO/E4NANS) will map the torus ansae simultaneously with the EUV in S and O ion emission lines using the FUV/MUV wavelengths. Ratios of the emission lines will determine electron temperatures. The profile measurements, in particular, will characterize the torus ansae as a function of longitude, time, and radius. The realtime auroral measurements (E4AURA) will map the aurora and electroglow simultaneously with the EUV in the H2 bands. The integrated intensities will characterize the global energy output and the latitudinal and time variation of energetic particles input into the atmosphere. * C3 SWG In this orbit, the highest priority UVS satellite observations will be the recorded bright and dark limb tenuous atmosphere measurements of Callisto (BRTLMB and DRKLMB). These observations are designed to uniquely measure the altitudinal distribution of volatiles from their spectral signatures in the UV (OH: 301-312 nm) and FUV (H: Lyman-alpha), respectively. Two full spectrum MUV recorded ridealong observations with NIMS will observe surface scattering properties of the Asgard Crater (ASGARD) and the Asgard Ring structures (ARINGS). Realtime Europa and Ganymede full spectral FUV phase angle observations (EUPHAS and GUPHAS), not obtainable from Earth (Europa phases 68 and 40 degrees, Ganymede phase 80 degrees), will complement NIMS surface property measurements. Realtime Io and Europa eclipse full spectral FUV/MUV observations (IECLPS and EECLPS) will characterize airglow emissions as Io and Europa enter and exit eclipse. Analysis of these data will provide the morphology of Io's and Europa's atmospheres in the presence and absence of direct sunlight. An Io neutral cloud realtime observation (NTRCLD) will provide information on the composition and time variation of neutral constituents that produce this cloud to assist in modeling the Io plasma torus and Io atmosphere. C03A_UPB_ARINGS01.DAT;1 C03A_UPB_ASGARD01.DAT;3 C03A_UPB_BRTLMB01.DAT;1 C03A_UPB_BRTLMB02.DAT;1 C03A_UPB_DRKLMB01.DAT;2 C03A_UPB_DRKNEW01.DAT;2 C03A_UPB_FTKR2B11.DAT;1 C03A_UPB_GLOBAL01.DAT;4 C03A_URT_AURMAP01.DAT;2 C03A_URT_C3NPRO01.DAT;2 C03A_URT_C3NPRO02.DAT;2 C03A_URT_DRKMAP01.DAT;1 C03A_URT_DRKNEW01.DAT;1 C03A_URT_EUPHAS40.DAT;2 C03A_URT_EUPHAS41.DAT;2 C03A_URT_EUPHAS57.DAT;2 C03A_URT_EUPHAS68.DAT;2 C03A_URT_FIXLON01.DAT;2 C03A_URT_FIXLON02.DAT;2 C03A_URT_FTKR1A21.DAT;2 C03A_URT_FTKR1A22.DAT;1 C03A_URT_FTKR2A11.DAT;4 C03A_URT_FTKR2A12.DAT;1 C03A_URT_FTKR2A21.DAT;3 C03A_URT_FTKR2A22.DAT;1 C03A_URT_FTKR2A31.DAT;3 C03A_URT_FTKR2A32.DAT;1 C03A_URT_FTKR2B11.DAT;1 C03A_URT_GUPHAS80.DAT;2 C03A_URT_NTRCLD01.DAT;1 C03B_URT_GRATNG02.DAT;1 C03C_URT_CROSSCAL.DAT;1 C03C_URT_E4AURA01.DAT;2 C03C_URT_E4AURA02.DAT;2 C03C_URT_E4AURA03.DAT;2 C03C_URT_E4MANS02.DAT;1 C03C_URT_E4MANS03.DAT;1 C03C_URT_E4MANS11.DAT;1 C03C_URT_E4MANS12.DAT;2 C03C_URT_E4MPRO01.DAT;1 C03C_URT_E4MPRO02.DAT;1 C03C_URT_E4MPRO03.DAT;1 C03C_URT_E4MPRO04.DAT;1 C03C_URT_E4MPRO05.DAT;1 C03C_URT_E4MPRO06.DAT;1 C03C_URT_E4NANS01.DAT;1 C03C_URT_E4NANS02.DAT;2 C03C_URT_E4NANS31.DAT;1 C03C_URT_E4NANS32.DAT;1 C03C_URT_E4UCAL01.DAT;2 Orbit E4 * E4 AWG The top priority UVS Jupiter atmospheric observation during this orbit is a realtime far- and mid-ultraviolet (FUV/MUV: 115-320 nm) high solar phase angle (148 to 160 deg) hot spot feature track observation (FTKH1E). In order to obtain this observation unattainable from Earth, the AWG executes an 80 degree science turn. Analysis of the data will result in a unique data set of stratospheric aerosol scattering properties at high solar phase angles. Additional hot spot feature track realtime observations (3 emission angles at 55 deg solar phase angle - FTKR1E) will be performed in conjunction with other AWG instruments. Independent UVS atmospheric observations will provide a realtime fixed local time map for global FUV spectral coverage and energy budget measurements during 1 Jovian rotation on the equatorial brightside (FIXTMB). Realtime global mapping of equatorial H Lyman-alpha on the darkside will continue as in previous orbits to obtain hydrogen distribution maps without the influence of direct solar radiation (FIXLON). Realtime southern auroral full spectral FUV observations will provide longitudinal coverage during part of a Jupiter rotation on both the dayside and nightside (AURMAP). Analysis of the ratios between different spectral lines (color ratios) will yield energies of the electrons that are precipitating into the auroral zones. * E4 MWG The highest priority UVS magnetospheric observations during this orbit will be those of the Io torus in conjunction with the EUV instrument (both pointed perpendicular to the spacecraft). This 10-hour set of E4-inbound torus measurements at the beginning of the E4A encounter period (E4NANS) completes the Io torus observations begun during C3C, and will map the torus noon ansa in S and O emission lines using UVS FUV and MUV wavelengths simultaneously with the EUV. Ratios of emission lines will determine electron temperatures. There are no UVS or EUV science observations during E4 cruise, only UVS grating movement commands to comply with a Flight Rule. * E4 SWG The E4 orbit includes several realtime UVS satellite eclipse and phase observations done at resolutions and phase angles not obtainable from the earth. The phase angle observation set includes two Io Phase observations (E4IUPHAS67 & E4IUCHEMIS), one Ganymede Phase observation (E4GUPHAS45), two Callisto Phase observations (E4CUPHAS45 & E4CUGLOBAL), and one Himalia Phase observations (E4SUHIML25). The data obtained from these phase angle observations will be used to supplement and complement the NIMS surface property measurements. In addition, Io eclipse full spectral FUV/MUV observations (E4IUIECLPS) will characterize the airglow emissions as Io enters and exits eclipse. Analysis of these data will provide the morphology of Io's atmosphere in the presence and absence of direct sunlight. UVS will also ride along with four NIMS observations of Europa. One, E4ENASTERI01 will return 4 integrated RIMs of data sampling four distinct latitudes roughly centered on 270 degrees longitude. The other ride-along observations will be with the three Surface Composition observations (E4ENSUCOMP) for which data will be recorded and 6 RIMs of data returned. These will be the first high spatial resolution observations of Europa by the UVS instrument. E04A_UPB_SUCOMP01.DAT;1 E04A_UPB_SUCOMP02.DAT;1 E04A_UPB_SUCOMP03.DAT;1 E04A_URT_ASTERI01.DAT;1 E04A_URT_AURMAP01.DAT;2 E04A_URT_CHEMIS01.DAT;1 E04A_URT_CUPHAS45.DAT;1 E04A_URT_E4NANS04.DAT;2 E04A_URT_FIXLON01.DAT;1 E04A_URT_FIXTMB01.DAT;1 E04A_URT_FTKH1E11.DAT;1 E04A_URT_FTKH1E12.DAT;1 E04A_URT_FTKH1E21.DAT;1 E04A_URT_FTKH1E22.DAT;1 E04A_URT_FTKR1E11.DAT;1 E04A_URT_FTKR1E12.DAT;1 E04A_URT_FTKR1E13.DAT;1 E04A_URT_FTKR1E14.DAT;1 E04A_URT_FTKR1E21.DAT;1 E04A_URT_FTKR1E22.DAT;1 E04A_URT_FTKR1E23.DAT;1 E04A_URT_FTKR1E24.DAT;1 E04A_URT_FTKR1E31.DAT;1 E04A_URT_FTKR1E32.DAT;1 E04A_URT_FTKR1E33.DAT;1 E04A_URT_FTKR1E34.DAT;1 E04A_URT_GUPHAS87.DAT;1 E04A_URT_HIML2501.DAT;1 E04A_URT_IECLPS03.DAT;1 E04A_URT_IECLPS04.DAT;1 E04A_URT_IECLPS05.DAT;1 E04A_URT_IECLPS06.DAT;1 E04A_URT_IUPHAS67.DAT;1 Orbit E5 was the navigation 'transfer orbit'; no science data. Orbit E6 * E6 AWG The top priority UVS Jupiter atmospheric observation during this orbit is a realtime far- and mid-ultraviolet (FUV/MUV: 115-320nm) moderate solar phase angle (48 deg) white oval feature track observation (FTKR2E). Analysis of the data will result in a unique data set of stratospheric aerosol scattering properties at a moderate solar phase angle and three emission angles. These data follow SSI images. An additional white oval feature track observation (1 emission angle at 64 deg solar phase angle) (FTKR1E) is performed also in conjunction with SSI. In order to obtain hydrogen distribution maps without the influence of direct solar radiation, independent UVS atmospheric observations will provide a realtime darkside global mapping of equatorial H Lyman-alpha using a fixed local time map (FIXTMD) and a darkside map (DRKMAP). Combined with similar measurements in previous orbits, this orbit's mapping nearly completes the first full global map of H Lyman-alpha distribution on the Jovian darkside at all system III longitudes. Global H distribution maps help determine upper atmosphere energy transfer and dynamics processes. Realtime southern auroral full spectral FUV observations will provide new longitudinal coverage on both the dayside and nightside (AURMAP). Analysis of the ratios between different spectral lines (color ratios) in these data will yield energies of the electrons precipitating into the auroral zones. A central meridian brightside map (BRTMAP) using FUV spectral coverage of the equatorial region provides dayglow at 1260-1333 and 1447-1521 A. One ridealong observation with SSI Io Pele monitoring will measure MUV/FUV irradiances coincident with imaged volcanic activity (PLUMON24). Enhancements are expected in Io's SO2 and S emissions. * E6 MWG The highest priority UVS magnetospheric observations during E6 will be realtime encounter measurements of the Io torus and Jupiter aurora at approximately 90 degree cone angle in conjunction with the EUV instrument. Io torus midnight ansa maps (E6MANS01-03) will consist of spectra centered on ionized S and O emission lines using the UVS FUV and MUV wavelengths simultaneously with the EUV. Ratios of emission line strengths will determine electron temperatures. E6MANS04 will map the inner, colder part of the Io torus at FUV wavelengths that also cover hydrogen Lyman alpha emission lines; the last 4 hours of this observation are designed to cross-calibrate the EUV with the UVS since Lyman alpha is observed by both instruments. Jupiter dark-side aurora measurements in this orbit (E6AURA01-03) focus on northern hemisphere hydrogen emissions at FUV and MUV wavelengths. Brief dark-side equatorial electroglow and southern aurora observations are also made. Integrated intensities will help to characterize the global energy output and the latitudinal and time variation of energetic particle input into the atmosphere. Inside the EUV 25 Rj radiation limit, the UVS will map the Io torus noon ansa at FUV and MUV wavelengths corresponding to ionized S and O emissions. During E6 cruise, the UVS instrument will make its first measurements of neutral O and S emissions in the anti-solar direction of the Jovian magnetosphere. These magnetonebula observations (MAGNEB01-05) will be 2 to 5 days in duration, with UVS readouts occurring every 24 hours. Finally, at the end of E6C, UVS is performing a first-time search for neutral H and O emissions in the orbits of Ganymede and Callisto. 18-hour observations centered on the ansa of each orbit (GTORUS and CTORUS) allow for the possible detection of a neutral torus of material associated with the surfaces and atmospheres of the two Galilean satellites. In GTORUS, the UVS will look at 70 degree cone angle through the spacecraft booms, demonstrating whether such measurements are feasible. * E6 SWG Ride-alongs with NIMS continue in E6 with E6ENTERINC01 (Terra Incognita), and E6SUCOMP01 and 02 (surface composition). The two surface composition observations will be recorded, while 4 separate RIMS of data varying in latitude will be returned in real-time from the Terra Incognita observation. The UVS SWG E6 orbit includes a set of Io eclipse full-spectral FUV/MUV observations. E6IUIECLPS03 & 04 are observations of Io just before and just after it exits eclipse (egress). Analysis of the eclipse data sets will be used with similar observations from previous and later orbits to provide the morphology of Io's atmosphere in the presence and absence of direct sunlight. In addition to the UVS FUV/MUV eclipse observations, the E6 orbit includes a full-spectral UVS N-channel (2818A - 4319A) observation of Io while it is in eclipse. This will be the first full-spectral N-channel data returned of Io during the tour. Similar observations of each of the Galilean satellites are planned in later orbits. An Io Neutral Cloud observation is also included in the E6 orbit. It consists of staring at 7 targets for collecting 12 RIMS of Lyman alpha (1215A) data at each. The targets are at varying distances from Io in the plane of its orbit. The data returned will be used with similar observations from previous and later orbits to determine the composition and time variation of the Io Neutral Cloud and to assist in the modelling of the Io plasma torus and Io's atmosphere. E06A_UPB_PLUMON24.DAT;1 E06A_UPB_SUCOMP01.DAT;1 E06A_UPB_SUCOMP02.DAT;5 E06A_URT_AURMAP01.DAT;1 E06A_URT_BRTMAP01.DAT;1 E06A_URT_CROSSCAL.DAT;1 E06A_URT_DRKMAP01.DAT;1 E06A_URT_E6AURA01.DAT;1 E06A_URT_E6AURA02.DAT;1 E06A_URT_E6AURA03.DAT;1 E06A_URT_E6MANS01.DAT;1 E06A_URT_E6MANS02.DAT;1 E06A_URT_E6MANS03.DAT;1 E06A_URT_E6MANS04.DAT;3 E06A_URT_E6NANS01.DAT;1 E06A_URT_E6NANS02.DAT;1 E06A_URT_E6NANS31.DAT;1 E06A_URT_E6NANS32.DAT;1 E06A_URT_FIXTMD01.DAT;1 E06A_URT_FTKR1E21.DAT;1 E06A_URT_FTKR1E22.DAT;1 E06A_URT_FTKR2E11.DAT;1 E06A_URT_FTKR2E12.DAT;1 E06A_URT_FTKR2E21.DAT;1 E06A_URT_FTKR2E22.DAT;1 E06A_URT_FTKR2E23.DAT;1 E06A_URT_FTKR2E31.DAT;1 E06A_URT_FTKR2E32.DAT;1 E06A_URT_IECLPS03.DAT;1 E06A_URT_IECLPS04.DAT;1 E06A_URT_IODARK01.DAT;1 E06A_URT_NTRLCL01.DAT;1 E06A_URT_TERINC01.DAT;1 E06B_URT_MAGNEB01.DAT;1 E06B_URT_MAGNEB21.DAT;1 E06C_URT_CTORUS01.DAT;1 E06C_URT_GTORUS01.DAT;1 E06C_URT_MAGNEB03.DAT;1 E06C_URT_MAGNEB04.DAT;1 E06C_URT_MAGNEB05.DAT;1 E06C_URT_MAGNEB22.DAT;3 Orbit G7 * G7 AWG The top priority UVS Jupiter atmospheric observation during this orbit is a realtime far- and mid-ultraviolet (FUV/MUV: 115-320 nm) moderate solar phase angle (75 deg) brown barge feature track observation (FTKR1E). Analysis of the data will result in a unique data set of stratospheric aerosol scattering properties at a moderate solar phase angle and three emission angles performed in conjunction with other AWG instruments. Realtime data in the MUV will be retrieved from the observations immediately following the SSI frames. Additional UVS atmospheric observations will provide a realtime fixed local time map for northern and southern auroral FUV spectral coverage and precipitating electron energy (color ratio) measurements (FIXTMD01). This observation is slightly different from previous FIXTMD observations in that the UVS will drift at cone 90 deg from the darkside onto the dayside. This observation will benefit from a NIMS ridealong for looking at H3+ and from EUV realtime observations occurring during this time. Additional realtime coverage of the southern and northern auroral darkside and brightside asymmetries (AURMAP01) will occur immediately following FIXTMD01 and will benefit from SSI, NIMS, and EUV ridealongs. Analysis of the ratios between different spectral lines (color ratios) will yield energies of the electrons precipitating into the auroral zones. Global mapping of equatorial H Lyman-alpha on the darkside will continue as in previous orbits to obtain hydrogen distribution maps without the influence of direct solar radiation (DRKMAP01 and FIXLON01). Finally, a realtime equatorial brightside map (BRTMAP01) will occur to obtain the dayglow UV spectrum. * G7 MWG At the beginning of G7A, UVS will observe the Callisto and Ganymede orbit ansae (CTORUS02 and GTORUS02), continuing measurements begun in E6C and designed to search for neutral H and O emissions. The highest priority UVS magnetospheric observations during the G7 orbit will be those in conjunction with the EUV instrument for observations of the Io torus midnight ansa and Jupiter aurora. This set of realtime torus measurements (G7MANS01-03) will map the torus ansa simultaneously with the EUV in S and O ion emission lines using FUV and near-ultraviolet (NUV: ~400 nm) wavelengths. Ratios of emission line intensities will determine electron temperatures. A UVS-only midnight ansa profile will also be taken (G7MPRO01), using the scan platform to target at greater than 90 deg cone angle, while EUV continues to observe the colder portion of the inner torus. Realtime auroral measurements (G7AURA01-03) will map the aurora and electroglow simultaneously with the EUV in the FUV hydrogen bands. AURA03 is EUV-only, and occurs at the same time as UVS-AWG, NIMS, SSI, and HST observations of the aurora. Integrated intensities will characterize the global energy output and the latitudinal and time variation of energetic particle input into the atmosphere. Inside 23 Rj, the UVS alone will map the Io torus noon ansa (G7NANS02-03) in S and O ion emission lines. Again, a UVS-only noon ansa profile will also be taken (G7NPRO01). The noon and midnight ansa observations will help characterize the torus ansae as a function of longitude, time, and radial distance. During cruise, several UVS magnetonebula observations are planned. These observations are long-duration measurements of FUV neutral H and O emissions along the axis of the magnetonebula in the antisun direction. * G7 SWG UVS-SWG activities in G7 feature recorded observations of each of the Galilean satellites, mostly conducted as ridealongs with NIMS investigations. For Ganymede, there are NHILAT01 (two scans across high northern latitudes) and BRITRL01 (bright material on the trailing hemisphere). The G7 orbit allows for another in the UVS instrument's series of limb observations, BRTLMB01. Following the trend established in E4, surface observations of Europa continue with the NIMS ride-alongs, FLEXUS01 and TYREMA01. One Callisto measurement is planned, a ridealong with the NIMS global observation, GLOBAL01. Three very short recorded observations of Io occur, CHEMIS01 and CHEMIS02 (Io dayside) and THRMAL02 (Io nightside). All of the recorded UVS measurements occur at FUV and MUV wavelengths, with the UVS G- and F-channels. Realtime data will be obtained during an eclipse of Europa (EECLPS01-04). This eclipse observation includes UVS N-channel sampling of Europa during midumbra (EURDRK01). Io also will be observed in realtime during mid- eclipse with the N-channel (IODARK01). G07A_UPB_AURMAP01.DAT;1 G07A_UPB_BRITRL01.DAT;2 G07A_UPB_BRTLMB01.DAT;1 G07A_UPB_CHEMIS01.DAT;2 G07A_UPB_CHEMIS02.DAT;3 G07A_UPB_FLEXUS01.DAT;1 G07A_UPB_GLOBAL01.DAT;1 G07A_UPB_NHILAT01.DAT;2 G07A_UPB_THRMAL02.DAT;2 G07A_UPB_TYREMA01.DAT;1 G07A_URT_AURMAP01.DAT;1 G07A_URT_BRTMAP01.DAT;1 G07A_URT_CTORUS02.DAT;2 G07A_URT_DRKMAP01.DAT;1 G07A_URT_EECLPS01.DAT;1 G07A_URT_EECLPS02.DAT;1 G07A_URT_EECLPS03.DAT;1 G07A_URT_EECLPS04.DAT;1 G07A_URT_EURDRK01.DAT;1 G07A_URT_FIXLON01.DAT;1 G07A_URT_FIXTMD01.DAT;1 G07A_URT_FTKR1E11.DAT;1 G07A_URT_FTKR1E12.DAT;1 G07A_URT_FTKR1E21.DAT;1 G07A_URT_FTKR1E22.DAT;1 G07A_URT_FTKR1E31.DAT;1 G07A_URT_FTKR1E32.DAT;1 G07A_URT_G7AURA01.DAT;1 G07A_URT_G7AURA02.DAT;1 G07A_URT_G7MANS01.DAT;1 G07A_URT_G7MANS02.DAT;1 G07A_URT_G7MANS03.DAT;1 G07A_URT_G7MPRO01.DAT;1 G07A_URT_G7NANS02.DAT;1 G07A_URT_G7NANS03.DAT;1 G07A_URT_G7NPRO01.DAT;1 G07A_URT_GTORUS02.DAT;1 G07A_URT_IODARK01.DAT;1 G07B_URT_MAGNEB01.DAT;1 G07B_URT_MAGNEB02.DAT;3 G07B_URT_MAGNEB03.DAT;1 G07B_URT_MAGNEB04.DAT;1 G07B_URT_MAGNEB05.DAT;1 G07B_URT_MAGNEB06.DAT;1 G07B_URT_MAGNEB07.DAT;1 Orbit G8 * G8 AWG The highest priority UVS Jupiter atmospheric observations during G8 are a set of four real-time far- and mid-ultraviolet (FUV and MUV, UVS G and F channels, 115-320 nm), moderate solar phase angle (66 deg) southern-region feature track observations (FTKR2Exx). Analysis of the data will result in a unique data set of polar haze scattering properties at moderate solar phase angles and two emission angles, performed in conjunction with other AWG instruments. Real-time data in the MUV will be retrieved from those observations that follow SSI images. Real-time global mapping of equatorial H Lyman-alpha on the Jupiter dark- side (DRKMAP and FIXLON) will continue as in previous orbits, to obtain hydrogen distribution maps without the effect of direct solar radiation. Real-time coverage of northern auroral darkside-brightside asymmetries (AURMAP) will also continue in G8. In addition, southern auroral morphology and variability (AURVAR) will be recorded on a short timescale using H2 color ratios at fixed longitude during the MWG quarter-rotation observation. Darkside/dayside H Lyman-alpha emissions will be recorded (EWMAPS) to determine limb-brightening and hydrogen corona extent. Real- time mapping of central meridian brightside hydrocarbons (CENMAP) will also be performed for long-term variation studies. * G8 MWG The highest priority UVS magnetospheric observations during G8 are a set of four real-time Io torus midnight ansa measurements performed inbound to Jupiter C/A, in conjunction with EUV, when both are pointed at 90 deg cone angle. These G8MANS observations are designed to obtain S and O ion emission line strengths at EUV as well as FUV and NUV (UVS N channel, 280-430 nm) wavelengths. Ratios of intensities will determine electron temperatures, while the integrated intensity characterizes the torus energy output for energy budget considerations. Although not simultaneous with EUV (inside EUV 25 Rj radiation limit), two real-time FUV auroral measurements are also a high priority during G8. These G8AURA observations will be outbound from Jupiter C/A, and will map the aurora and electroglow at H2 band wavelengths. To help characterize the torus midnight ansa as a function of longitude, time, and radius, UVS will also obtain four profiles centered on the torus ribbon, three of which will be performed inbound to Jupiter C/A, and all with the scan platform at >90 deg cone angle. There are no torus noon ansa observations planned during G8. However, UVS will observe the midnight ansa of Ganymede and Callisto's orbits (GTORUS and CTORUS) twice each in G8. These observations are intended to search for FUV emissions from H, O, and S in hypothetical neutral clouds in the vicinity of each satellite. These observations and one aurora measurement will be made at <90 deg cone angle. Finally, a set of ten UVS magnetonebula observations are planned during the cruise portions of G8. These MAGNEB observations will be long-duration measurements (36 days total) of FUV emissions looking along the axis of the magnetonebula in the spacecraft antisun direction. * G8 SWG The UVS Galilean satellite observations during G8 include a set of four high-resolution observations of Ganymede in the MUV (160-320 nm) at solar phase angles not obtainable from Earth, and one MUV Ganymede phase angle observation at low resolution. The four high-resolution observations are recorded ridealongs with NIMS and are designed to supplement and complement NIMS surface property measurements. URUK views Uruk Sulcus, LIDARK views light/dark material, TRANSI views transition boundary material, and OSIRIS views Osiris Crater. The fifth Ganymede observation is an independent real-time UVS view, PHAS68 at 68 deg solar phase angle. It will be used with complementary observations obtained in other orbits to measure satellite albedos and emissions at different phase angles. In addition, a set of six MUV Callisto observations during the non-targeted encounter, again at solar phase angles not reachable from Earth, will be obtained in G8. As with Ganymede, five are recorded NIMS ridealongs. ADLIND views Adlinda Crater, BURI views Buri Crater, SPOLE_ views the south polar region, and there are two GLOBAL views of Callisto. The sixth Callisto observation is an independent real-time UVS view, PHAS78 at 78 deg solar phase angle. Two real-time MUV Europa observations in G8 are planned, PHAS65 and PHAS07 at 65 and 7 deg solar phase angle. A set of three real-time Io eclipse full-spectral (FUV/MUV) observations (IECLPS) are also included in G8. Analysis of the eclipse data will be used with similar observations from other orbits during eclipse ingress and egress to provide the morphology of Io's atmosphere in the presence and absence of direct sunlight. Finally, there will be realtime Io neutral cloud (NTRCLD) and 73 deg solar phase angle (PHAS73) observations. G08A_UPB_ADLIND01.DAT;3 G08A_UPB_AURVAR01.DAT;4 G08A_UPB_BURI__01.DAT;3 G08A_UPB_EWMAPS01.DAT;4 G08A_UPB_GLOBAL01.DAT;3 G08A_UPB_LIDARK01.DAT;1 G08A_UPB_OSIRIS01.DAT;2 G08A_UPB_SPOLE_01.DAT;3 G08A_UPB_TRANSI01.DAT;1 G08A_UPB_URUK__01.DAT;1 G08A_URT_AURMAP01.DAT;1 G08A_URT_CENMAP01.DAT;2 G08A_URT_CROSSCAL.DAT;1 G08A_URT_CTORUS01.DAT;1 G08A_URT_CUPHAS78.DAT;1 G08A_URT_DRKMAP01.DAT;1 G08A_URT_EUPHAS07.DAT;1 G08A_URT_EUPHAS65.DAT;1 G08A_URT_FIXLON01.DAT;1 G08A_URT_FTKR2E11.DAT;1 G08A_URT_FTKR2E12.DAT;1 G08A_URT_FTKR2E21.DAT;1 G08A_URT_G8AURA04.DAT;1 G08A_URT_G8AURA05.DAT;1 G08A_URT_G8MANS02.DAT;1 G08A_URT_G8MANS03.DAT;1 G08A_URT_G8MANS11.DAT;1 G08A_URT_G8MANS12.DAT;1 G08A_URT_G8MPRO01.DAT;1 G08A_URT_G8MPRO02.DAT;2 G08A_URT_G8MPRO03.DAT;3 G08A_URT_GTORUS01.DAT;1 G08A_URT_GTORUS02.DAT;1 G08A_URT_GUPHAS68.DAT;1 G08A_URT_IECLPS02.DAT;1 G08A_URT_IECLPS03.DAT;1 G08A_URT_IECLPS04.DAT;1 G08A_URT_IUPHAS73.DAT;1 G08A_URT_NTRCLD01.DAT;1 G08B_URT_CTORUS02.DAT;2 G08B_URT_MAGNEB01.DAT;1 G08B_URT_MAGNEB02.DAT;1 G08B_URT_MAGNEB03.DAT;1 G08B_URT_MAGNEB04.DAT;1 G08B_URT_MAGNEB05.DAT;1 G08B_URT_MAGNEB06.DAT;2 G08B_URT_MAGNEB07.DAT;1 G08B_URT_MAGNEB08.DAT;1 G08B_URT_MAGNEB09.DAT;1 G08B_URT_MAGNEB10.DAT;1 Orbit C9 * C9 AWG The highest priority UVS Jupiter atmospheric observations during C9 are a set of real-time far- and mid-ultra-violet (FUV and MUV, UVS G and F channels, 115-320 nm), high solar phase angle (70 deg) observations of the GRS trailing vortices (FTKR2Exx). Combined with this is a set of FUV plume observations 1/2 rotation earlier, also at high solar phase angle (80 deg) (FTKR1Exx). There will be two additional high solar phase angle observations (157 and 140 deg) obtained in the FUV/MUV as ridealong observations (FTK15701 and FTK14001) with SSI during two science turns inbound to C10. Analysis of the data will result in a unique data set of stratospheric aerosol scattering properties at high solar phase angles and two emission angles, simultaneous with SSI two-color images. In FTK15701 we also obtain dark-limb ring data in the MUV as a ridealong with NIMS. Real-time global mapping of equatorial H Lyman-alpha on the Jupiter darkside (DRKMAP) will continue as in previous orbits, to obtain hydrogen distribution maps without the effect of direct solar radiation. Southern aurora will be mapped from 260 to 360 deg longitude; H2 band color ratios will be observed to determine precipitating particle energies (AURMAP01- 02). Northern aurora will be mapped on the dayside at 170 deg longitude with a similar objective (FIXLON). Of unique importance are two outbound auroral observations. AURMAP04 observes southern dusk aurora with objectives similar to AURMAP01-02. AURVAR is coincident with the Fields and Particles Campaign A observation and will record southern aurora short time-scale variability as well as spatial characteristics of the Io fluxtube footprint at H Lyman-alpha wavelengths. There will also be the second of two UVS star calibrations in the mission during the cruise portion of the orbit on the same star as viewed during G1 (Delta Scorpii). * C9 MWG The highest priority UVS magnetospheric observation during C9 is a set of realtime Io torus midnight ansa measurements performed outbound from Jupiter C/A, in conjunction with EUV, when both are pointed at 90 deg cone angle. This C9MANS04 observation is designed to obtain S and O ion emission line strengths at EUV as well as FUV and NUV (UVS N channel, 280-430 nm) wavelengths. Ratios of intensities will determine electron temperatures, and the integrated intensity characterizes the torus energy output for energy budget considerations. Although not simultaneous with EUV, two sets of realtime FUV and NUV torus ansa observations are also a high priority during C9. C9MPROxx (inbound at >90 deg cone angle) and C9NANSxx (outbound, at 90 deg) are torus ansa profiles obtained while the UVS drifts over the midnight and noon ansa ribbons, respectively. Two independent real-time EUV observations also occur after the instrument is turned on 19 Rj outbound from Jupiter C/A, an aurora map (C9AURA) and a map of the extension of the Io torus midnight ansa beyond Europa's orbit (C9FANS). UVS will also observe the midnight ansa of Callisto and Ganymede's orbits (CTORUS and GTORUS) in C9. These observations are intended to search for FUV emissions from H, O, and S in hypothetical neutral clouds in the vicinity of each satellite, and will be made at <90 deg cone angle. Finally, a set of seventeen UVS magnetonebula observations are planned during the cruise portions of C9. Six of these MAGNEB observations will be long-duration measurements (18 days total) of FUV emissions looking along the axis of the magnetonebula in the spacecraft antisun direction, and eleven will be 3-hour observations designed to monitor the performance of the UVS grating. * C9 SWG The UVS Galilean satellite observations during C9 include four high- resolution observations of Ganymede in the MUV (160-320 nm), and one MUV Ganymede phase angle observation at low resolution at a solar phase angle not obtainable from Earth. The four high-resolution observations are recorded ridealongs with NIMS and are designed to supplement and complement NIMS surface property measurements. In addition to two GLOBAL views, DRKLIT observes the transition between dark and light material in Galileo Regio, and BRILED observes the bright endmember on the leading hemisphere. The other Ganymede observation is an independent real-time UVS view, PHAS78 at 78 deg solar phase angle. It will be used with complementary observations obtained in other orbits to measure satellite albedos and emissions at different phase angles. In addition, a set of seven MUV Callisto observations will be obtained during the targeted satellite encounter in C9. Most are recorded NIMS ridealongs in the MUV: ANARR and SKULD view high-albedo craters, NOLAT obtains northern latitude coverage, VALHAL and VALSPC observe Valhalla's palimpsest and ring structure, and there is one GLOBAL view of Callisto. A seventh recorded Callisto observation is an independent UVS measurement in the FUV of volatile distribution with altitude off the bright limb of the satellite. Five real-time MUV Europa observations are planned in C9, PHAS81, 77, 05, and 03 at solar phase angles from 81 to 3 deg, plus one eclipse observat- ion, DARK. A set of four real-time Io eclipse full-spectral (FUV/MUV) observations (IECLPS) also occur in C9. Comparison with eclipse ingress and egress observations from other orbits will provide the morphology of Io's atmosphere in the presence and absence of direct sunlight. Finally, there is a real-time Io neutral cloud (NTRCLD) observation. C09A_UPB_ANARR_01.DAT;1 C09A_UPB_AURVAR01.DAT;2 C09A_UPB_BRILED01.DAT;1 C09A_UPB_BRTLMB01.DAT;1 C09A_UPB_CGLOBAL01.DAT;1 C09A_UPB_DRKLIT01.DAT;3 C09A_UPB_GGLOBAL01.DAT;1 C09A_UPB_GGLOBAL02.DAT;1 C09A_UPB_NOLAT01.DAT;2 C09A_UPB_SKULD_01.DAT;1 C09A_UPB_VALHAL01.DAT;2 C09A_UPB_VALSPC01.DAT;2 C09A_URT_AURMAP01.DAT;1 C09A_URT_AURMAP03.DAT;1 C09A_URT_AURMAP04.DAT;2 C09A_URT_C9MANS04.DAT;1 C09A_URT_C9MPRO02.DAT;1 C09A_URT_C9MPRO31.DAT;1 C09A_URT_C9MPRO32.DAT;2 C09A_URT_C9NANS21.DAT;1 C09A_URT_C9NANS22.DAT;1 C09A_URT_C9NANS23.DAT;2 C09A_URT_CTORUS01.DAT;1 C09A_URT_DRKMAP01.DAT;1 C09A_URT_EUDARK01.DAT;1 C09A_URT_EUPHAS03.DAT;1 C09A_URT_EUPHAS05.DAT;1 C09A_URT_EUPHAS77.DAT;1 C09A_URT_EUPHAS81.DAT;1 C09A_URT_FIXLON01.DAT;1 C09A_URT_FTKR1E11.DAT;1 C09A_URT_FTKR1E12.DAT;1 C09A_URT_FTKR1E21.DAT;1 C09A_URT_FTKR1E22.DAT;1 C09A_URT_FTKR2E11.DAT;1 C09A_URT_FTKR2E12.DAT;1 C09A_URT_FTKR2E21.DAT;1 C09A_URT_FTKR2E22.DAT;1 C09A_URT_GTORUS01.DAT;1 C09A_URT_GUPHAS78.DAT;1 C09A_URT_IECLPS01.DAT;1 C09A_URT_IECLPS02.DAT;1 C09A_URT_IECLPS03.DAT;1 C09A_URT_IECLPS04.DAT;1 C09A_URT_NTRCLD01.DAT;1 C09B_URT_MAGNEB01.DAT;1 C09B_URT_MAGNEB02.DAT;1 C09B_URT_MAGNEB03.DAT;1 C09B_URT_MAGNEB04.DAT;1 C09B_URT_MAGNEB05.DAT;1 C09B_URT_MAGNEB06.DAT;1 C09B_URT_MAGNEB07.DAT;2 C09B_URT_STRCAL01.DAT;1 C09C_UPB_FTK15701.DAT;1 C09C_URT_FTK14001.DAT;1 C09C_URT_FTK15701.DAT;1 C09C_URT_MAGNEB08.DAT;1 C09C_URT_MAGNEB09.DAT;1 C09C_URT_MAGNEB10.DAT;1 C09C_URT_MAGNEB11.DAT;1 C09C_URT_MAGNEB12.DAT;1 C09C_URT_MAGNEB13.DAT;1 C09C_URT_MAGNEB14.DAT;1 C09C_URT_MAGNEB15.DAT;1 C09C_URT_MAGNEB16.DAT;1 C09C_URT_MAGNEB17.DAT;1 ORBIT C10 * C10 AWG The top priority UVS Jupiter atmospheric observation during C10 is a half- hour recorded far and near-ultraviolet (FUV 115-192 nm, and NUV 280-430 nm) high solar phase angle (180 deg in solar occultation) observation of the southern aurora (AURMAP02). With this observation using the N- channel, UVS will obtain the first near-UV spectra of the Jovian aurora from the darkside containing Balmer series hydrogen emission and providing information on energetics and absorbers in the polar regions. Other unique, high-priority observations include those of H limb brightening/ darkening and H corona to be obtained in an equatorial Lyman-alpha scan (NEWSMP01), and of the variable Lyman-alpha southern aurora, including the Io fluxtube footprint, with high time and spatial resolution (AURVAR01). Along with these recorded observations are FUV northern polar haze observations for two rotations of the feature track campaign (FTKRzExx), taken immediately after SSI multi-color images. Analysis of these data will result in a unique data set of high-latitude stratospheric aerosol scattering properties for several emission angles. Global mapping of darkside equatorial H Lyman-alpha will continue as in previous orbits to obtain hydrogen distribution maps without the influence of direct sunlight (DRKMAP01 and 02). Northern and southern aurora will be mapped with H2 band color ratios to determine precipitating particle energies (AURMAP01). Hydrocarbon maps at four latitude bands (BRTMAP01 and 02) will be part of a study of long-term changes in stratospheric absorbers. * C10 MWG The highest priority UVS magnetospheric observations in C10 are realtime Io torus noon and midnight ansa measurements. A far-midnight ansa observation (10FANS01), is performed inbound to Jupiter C/A, observing the torus outside of the orbit of Europa in conjunction with EUV, when both are pointed at 90 deg cone angle. It is designed to obtain S and O ion emission line strengths at EUV as well as FUV and NUV wavelengths. Intensity ratios will determine electron temperatures, and integrated intensity characterizes the torus energy output for energy budget considerations. Although not simultaneous with EUV, two real-time FUV and NUV torus ansa observations are also a high priority during C10. 10NPRO01 (inbound at >90 deg cone angle) and 10MPRO01 (outbound at >90 deg) are profiles obtained while the UVS drifts over the noon and midnight ansa ribbons, respectively. A UVS FUV observation of the Jupiter southern aurora (10AURA01) also occurs on C10 inbound. Finally, a search (CTORUS01) for FUV neutral emissions from H and O in the vicinity of the Callisto orbit ansa, is made at > 90 deg cone angle. In C10 cruise, there are seven UVS magnetonebula observations (MAGNEBxx), two of which will be long-duration measurements of FUV oxygen emissions looking along the axis of the magnetonebula in the spacecraft antisun direction, and five of which will be 3-hour observations designed to monitor the performance of the UVS grating. A UVS-EUV cross-calibration at Lyman-alpha wavelengths will also occur inbound to E11 (11XCAL01). * C10 SWG In C10, UVS will continue to observe Europa, Ganymede and Io at various phase angles and longitudes. Along with complementary measurements of satellite albedos and emission obtained in other orbits, these observations contribute to the UV phase function curves for the Galilean satellites. Europa is observed at the following longitudes (and phase angles): 104 deg (93 deg), 131 deg (92 deg), 165 deg (95 deg), 287 deg (103 deg), 294 deg (96 deg), 300 deg (82 deg), and 303 deg (64 deg). IUPHAS55 observes Io at 45 deg longitude (55 deg), and GUPHAS77 observes Ganymede at 30 deg longitude (77 deg). Continuing its eclipse campaign, UVS observes Europa and Io in EUEURDRK and IUIODARK. Analysis of eclipse data sets will be used with similar observations in other orbits to provide the morphology of the Europa and Io atmospheres in the presence and absence of direct sunlight. Europa is viewed twice near the center of the eclipse umbra, looking for OH- with the N-channel (306 nm) and for neutral H and O with the G-channel (121.6 and 130.4 nm). Oxygen is viewed on Io near the center of the eclipse umbra with the G-channel (130.4 and 147.9 nm). A unique EUV satellite observation (CVSPNSCN) before Callisto closest approach will search for extreme UV (60-130 nm) absorptions and emissions. UVS will observe Callisto three times at high resolution. CUBRTLMB01 and CUBRTLMB02 examine the Callisto limb in sunlight to determine the morphology of the Callisto atmosphere. CUNOLAT observes Callisto at 60 deg north latitude. In addition, CUNTRLCL observes the Callisto neutral cloud (of atomic H and O) with the G-channel (121.6 and 130.4 nm). These measurements will be used to determine the morphology of the Callisto extended atmosphere and will complement the CUBRTLMB observations. Finally, UVS plans ridealong observations performed in conjunction with NIMS in order to supplement and complement NIMS satellite surface property measurements. CUGLOBAL01, CUGLOBAL02, CUASGARD (Asgard crater), CUPALIMP (palimpsest), CUSMTHPL (smooth pole), CUVALHAL (Valhalla crater), and CUCATENA (Catena crater) are high-resolution Callisto observations at 160 to 320 nm. UVS will also perform NIMS ridealong measurements of Io (IUCHEMIS03, IUHRSPEC01, and IUVOLCAN03) in the same wavelength region. C10A_UPB_ASGARD01.DAT;1 C10A_UPB_AURVAR01.DAT;2 C10A_UPB_BRTLMB01.DAT;3 C10A_UPB_BRTLMB02.DAT;2 C10A_UPB_CATENA01.DAT;4 C10A_UPB_CHEMIS03.DAT;1 C10A_UPB_GLOBAL01.DAT;3 C10A_UPB_GLOBAL02.DAT;4 C10A_UPB_HRSPEC01.DAT;2 C10A_UPB_NEWSMP01.DAT;2 C10A_UPB_NOLAT_01.DAT;2 C10A_UPB_PALIMP01.DAT;2 C10A_UPB_SMTHPL01.DAT;3 C10A_UPB_VALHAL01.DAT;5 C10A_UPB_VOLCAN03.DAT;2 C10A_URT_10AURA01.DAT;1 C10A_URT_10FANS01.DAT;1 C10A_URT_10MPRO01.DAT;1 C10A_URT_10NPRO01.DAT;1 C10A_URT_AURMAP01.DAT;1 C10A_URT_BRTMAP01.DAT;1 C10A_URT_BRTMAP02.DAT;1 C10A_URT_CTORUS01.DAT;1 C10A_URT_DRKMAP01.DAT;1 C10A_URT_DRKMAP02.DAT;1 C10A_URT_EULON250.DAT;1 C10A_URT_EULON270.DAT;1 C10A_URT_EULON290.DAT;1 C10A_URT_EULON300.DAT;1 C10A_URT_EULON_10.DAT;1 C10A_URT_EUPHAS93.DAT;1 C10A_URT_EUPHAS95.DAT;1 C10A_URT_EURDRK01.DAT;1 C10A_URT_EURDRK02.DAT;1 C10A_URT_FTKR1E11.DAT;1 C10A_URT_FTKR1E12.DAT;1 C10A_URT_FTKR1E21.DAT;1 C10A_URT_FTKR1E22.DAT;1 C10A_URT_FTKR2E11.DAT;1 C10A_URT_GUPHAS77.DAT;1 C10A_URT_IODARK01.DAT;1 C10A_URT_IUPHAS55.DAT;1 C10A_URT_NTRLCL01.DAT;2 C10B_UPB_AURMAP02.DAT;1 C10B_URT_11XCAL01.DAT;1 C10B_URT_MAGNEB01.DAT;1 C10B_URT_MAGNEB03.DAT;1 C10B_URT_MAGNEB04.DAT;1 C10B_URT_MAGNEB05.DAT;1 C10B_URT_MAGNEB06.DAT;1 C10B_URT_MAGNEB07.DAT;1 Orbit E11 * E11 AWG The top priority UVS Jupiter atmospheric observation during E11 is a recorded and realtime far-ultraviolet Lyman-alpha (121 nm) observation of the northern aurora (AURVAR01,02,03). With this observation using the G-detector, we will obtain the best spatial and temporal detail in Lyman- alpha of the Jovian aurora from the darkside during the mission. SSI will observe near the 180 longitude immediately before and after this observation which covers the same longitude region for the UVS. NIMS rides along with UVS for this observation. We expect to observe the footprint of the Io fluxtube and any potential emission from a Europa fluxtube footprint if it exists above the limits of our detectability. Another unique, high priority recorded observation is the H limb brightening/ darkening and H corona to be obtained in an equatorial region Lyman-alpha scan (EWMAPS01). This observation is similar to one done in C10 and should provide a second dataset to definitively map the H corona. A FUV brown barge observation set will be obtained in the feature track campaign (FTKR1Exx) for one rotation at 3 emission angles. Analysis of these data will result in a unique data set of stratospheric aerosol scattering properties surrounding this feature over different emission angles. The brown barge data will be taken immediately following the SSI multi-color images as well as coincident with the NIMS data. Global mapping of equatorial H Lyman-alpha on the darkside will continue as in previous orbits to obtain hydrogen distribution maps without the influence of direct solar radiation (DRKMAP01-02). The southern aurora will be mapped by the color ratios for H2 bands which help determine precipitating particle energies (AURMAP01). Finally, the mapping of hydrocarbons at four latitude bands will occur (BRTMAP01) to compare with previous observations as part of the study of long-term changes to stratospheric absorbers. * E11 MWG The highest priority UVS magnetospheric observations in E11 are realtime Io torus midnight ansa measurements (11MANS01-02-03) performed inbound to Jupiter in conjunction with EUV, when both are pointed at 90 deg cone angle. They are designed to obtain S and O ion emission line strengths at EUV as well as FUV (115-320 nm) and NUV (280-430 nm) wavelengths. Intensity ratios will determine electron temperatures, and integrated intensity characterizes the torus energy output for energy budget considerations. Other simultaneous UVS/EUV goals include two midnight ansa profiles (11MPRO01-02: UVS observes ansa at >90 deg cone angle, while EUV views the cold inner torus) and two Jupiter northern aurora observations (11AURA01-02: UVS at ~90 deg). A final observation of the cold torus occurs with EUV (11MPRO04) before it is shut off at 17.0 Rj (closest operation in the prime mission, although it is intended to be operated to 17 Rj in GEM). Although not simultaneous with EUV, UVS observations of the noon ansa of the Io torus (11NANS11-12-02-03) are also performed inbound to Jupiter. In addition, a search (CTORUS01) for FUV neutral emissions from H and O in the vicinity of the Callisto orbit ansa, is made early in E11A at >90 deg cone angle. Finally, two 3-hour observations (GRATNG01-02) of interplanetary Lyman-alpha emissions occur in E11B; they are designed to monitor the performance of the UVS grating. * E11 SWG In E11, UVS will continue to observe Europa, Ganymede, Callisto and Io at various phase angles and longitudes. Along with complementary measurements of satellite albedos and emission obtained in other orbits, these observations contribute to the UV phase function curves for the Galilean satellites. UVS observes Callisto (CUPHASxx) at the following phase angles (and longitudes): 89 deg (100 deg), 70 deg (100 deg), and 61 deg (90 deg). EUPHAS65 and EUPHAS64 observe Europa at 65 deg phase (135 deg) and 64 deg phase (139 deg), respectively. Ganymede is observed at 21 deg phase (350 deg) in GUPHAS21 and 0 deg phase (342 deg) in GUPHAS00. IUPHAS113 observes Io at 113 deg phase (112 deg). Continuing its eclipse campaign, UVS observes each Galilean satellite in eclipse (ccDARK). Analysis of eclipse data sets will be used with similar observations in other orbits to provide the morphology of the satellite's atmospheres in the presence and absence of direct sunlight. UVS observes Callisto twice near the eclipse umbra, once looking for the OH- with the N-channel (309.0 nm) and again with the G-channel to look for oxygen (135.6 nm). Europa is viewed twice near the eclipse umbra, both observations looking for oxygen (135.6 nm) and sulfur (147.9 nm) with the G-channel. Ganymede is observed twice near eclipse umbra, the first observation looking for OH- (309.0 nm) with the F-channel and the second observation looking for oxygen (135.6 nm). UVS also observes Io near eclipse umbra, looking for oxygen (135.6 nm) and sulfur (147.9 nm) with the G-channel. UVS has two Europa closest approach observations planned. EUEUDISK targets Europa at 12 locations with F-channel full scans to determine high spatial resolution albedos. EULEAD observes Europa's leading hemisphere's albedo at four latitudes (60 deg N, 30 deg N, 0 deg, 30 deg S) with F-channel full scans. Finally, UVS plans ridealong observations performed in conjunction with NIMS in order to supplement and complement NIMS satellite surface property measurements. EUM20HR (20 hours from closest approach), EUP17HR (17 hours from closest approach), EUM15HR (15 hours from closest approach), EUDRKLIT (dark mosaic of crater), EURORT (realtime), EUCYCLOD (cyclodal) are high-resolution Europa observations at 160 to 320 nm. UVS will also perform NIMS ridealong measurements of Io in IUHRSPEC in the same wavelength region. E11A_UPB_AURVAR01.DAT;1 E11A_UPB_AURVAR02.DAT;1 E11A_UPB_CYCLOD01.DAT;1 E11A_UPB_DRKLIT01.DAT;1 E11A_UPB_EWMAPS01.DAT;1 E11A_UPB_FTKR1E31.DAT;1 E11A_UPB_FTKR1E32.DAT;2 E11A_UPB_HRSPEC01.DAT;3 E11A_UPB_M15HR_01.DAT;2 E11A_UPB_M20HR_01.DAT;2 E11A_UPB_P17HR_01.DAT;2 E11A_URT_11AURA01.DAT;1 E11A_URT_11AURA02.DAT;1 E11A_URT_11MANS01.DAT;1 E11A_URT_11MANS02.DAT;1 E11A_URT_11MANS03.DAT;1 E11A_URT_11MPRO01.DAT;1 E11A_URT_11MPRO02.DAT;1 E11A_URT_11NANS02.DAT;1 E11A_URT_11NANS11.DAT;1 E11A_URT_11NANS12.DAT;1 E11A_URT_AURMAP01.DAT;1 E11A_URT_AURVAR03.DAT;1 E11A_URT_CALDRK01.DAT;1 E11A_URT_CALDRK02.DAT;1 E11A_URT_CTORUS01.DAT;1 E11A_URT_CUPHAS61.DAT;1 E11A_URT_CUPHAS89.DAT;1 E11A_URT_DRKMAP01.DAT;1 E11A_URT_DRKMAP02.DAT;2 E11A_URT_EUDARK01.DAT;1 E11A_URT_EUDARK02.DAT;1 E11A_URT_EUDISK01.DAT;1 E11A_URT_EULEAD01.DAT;1 E11A_URT_EUPHAS64.DAT;1 E11A_URT_EUPHAS65.DAT;1 E11A_URT_EURORT01.DAT;1 E11A_URT_FTKR1E11.DAT;1 E11A_URT_FTKR1E12.DAT;2 E11A_URT_FTKR1E21.DAT;1 E11A_URT_FTKR1E31.DAT;1 E11A_URT_FTKR1E32.DAT;1 E11A_URT_GADARK01.DAT;1 E11A_URT_GADARK02.DAT;1 E11A_URT_GUPHAS00.DAT;1 E11A_URT_IODARK01.DAT;1 E11A_URT_IPHAS113.DAT;1 E11A_URT_STRCAL01.DAT;1 E11B_URT_GRATING01.DAT;1 E11B_URT_GRATING02.DAT;1 Ancillary Data ============== These are raw UVS data sets. For analysis, geometry parameters are obtained from the SPICE kernels for the time period of analysis. The Galileo SEF (Sequence of Events) file may be needed to verify the UVS configuration during the observation. Calibration files are available from the PDS UVS Instrument sets. Analysis techniques for various data classes are described in the published papers. A publication list is also available from PDS. The Galileo Project archives the SEF and ASRUN sequence products as well as some observation design materials. These may be used to help understand each observation. The UVS/EUV team retains some design materials as well. The team visualization tool, called GGGS, can be used to review the observation geometry, based on SEF and SPICE products. Coordinate System ================= Time tags are given in spacecraft clock (SCET), UTC as well as ground receipt time (ERT), UTC. Specific timing details are given in the file labels. Any value not recovered by the ground system is assigned a value of -1. Zero is a legitimate UVS EDR value. Software ======== UVS EDR data files are written with IDL (Interactive Data Language, a product of Research Systems, Inc. of Boulder, Colorado.) The files are created on a Digital Equipment Vax computer. No special software is necessary to read the simple array structures. Media/Format ============ The standard distribution format for the data is electronic transfer. ..............................................." CONFIDENCE_LEVEL_NOTE = " Confidence Level Overview ========================= All EDR data are exactly as recovered from the ground system. Ground system data recovery flags are included in the EDR headers. Resultant reliability and accuracy of the raw data is 100% described. Completeness can be derived from the data file header information. Pointing accuracy in the supplemental (SPICE) data kernels may be the largest uncertainty in analyzing the data. Reduced downlink capacity caused less raw pointing information to be downlinked. Particularly when the spacecraft was not on gyros, and Target Motion Compensation (TMC), the scan platform may not have been pointing where it was commanded to point. Subsequently, there can be difficulty in coordinating the UVS data with pointing knowledge. Gyros are only used during Encounter sequence load periods; raw pointing knowledge is on 5 RIM centers in Cruise loads and 10 minor frame centers during Encounter loads. Recent Publications =================== Galileo Ultraviolet Spectrometer Observations of Atomic Hydrogen in the Atmosphere of Ganymede, C.A.Barth, C.W.Hord, A.I.F.Stewart, W.R.Pryor, K.E.Simmons, W.E.McClintock, J.M.Ajello, K.L.Naviaux, J.J.Aiello, GRL, Vol.24, No.17, pp 2147-2150, September 1, 1997. Simultaneous Extreme Ultraviolet and Far Ultraviolet Observations of Jupiter Aurora From The Galileo Orbiter, Ajello, J., D. Shemansky, W. Pryor, K. Tobiska, C. Hord, S. Stephens, I. Stewart, J. Clarke, K. Simmons, W. McClintock, C. Barth, J. Gebben, D. Miller and B. Sandel, submitted to GRL, June 1, 1997. Europa: Disk-Resolved Ultraviolet Measurements using the Galileo Ultraviolet Spectrometer, Hendrix, A.R., C.A. Barth, A.L. Lane, submitted to Icarus, September 1997. Galileo Ultraviolet Spectrometer Observations of Jupiter's Auroral Spectrum from 1600-3200A, Pryor, Wayne R., Joseph M. Ajello, W. Kent Tobiska, Donald E. Shemansky, Geoffrey K. James, Charles W. Hord, Stuart K. Stephens, Robert A. West, A. Ian F. Stewart, William E. McClintock, Karen E. Simmons, Amanda R. Hendrix, Deborah A. Miller, JGR, Vol. 103, No. E9, pp 20,149- 20,158, August 30, 1998. Data Coverage and Quality ========================= Any value not recovered by the ground system is assigned a value of -1. Zero is a legitimate UVS EDR value. The UVS instrument puts out 8-bit values of range 0-277 (octal). The PB data are in this range. The RTS data are accumulated in an on-board 16-bit, roll-over buffer. Zero is a legitimate value; values greater that 2^15 roll-over to zero and continue accumulating. Limitations =========== Sequenced science observations may not necessarily have been recovered to the ground. All available EDR UVS data sets will be archived in PDS. As of Orbit 17, the only known UVS instrument operation question regards the actual versus commanded grating position. The EDR file data information accurately describes where the grating was at the time of the data acquisition. A UVS 'status' file is archived for each orbit which compares the commanded versus actual grating position. ................................................." END_OBJECT = DATA_SET_INFORMATION OBJECT = DATA_SET_TARGET TARGET_NAME = JUPITER END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_TARGET TARGET_NAME = IO END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_TARGET TARGET_NAME = EUROPA END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_TARGET TARGET_NAME = GANYMEDE END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_TARGET TARGET_NAME = CALLISTO END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_TARGET TARGET_NAME = HIMALIA END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_TARGET TARGET_NAME = "IO TORUS" END_OBJECT = DATA_SET_TARGET OBJECT = DATA_SET_HOST INSTRUMENT_HOST_ID = "GO" INSTRUMENT_ID = "UVS" END_OBJECT = DATA_SET_HOST OBJECT = DATA_SET_REFERENCE_INFORMATION REFERENCE_KEY_ID = "to be completed" END_OBJECT = DATA_SET_REFERENCE_INFORMATION END_OBJECT = DATA_SET END