Observation Objectives
Atmospheric Working Group

1.0 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?

2.0 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 Atmospheres Working Group observations where possible.

3.0 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.

4.0 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 in section 5.0. Following that section, Figure 1 graphically depicts each of the observations on the disk of Jupiter. A summary of the observations is shown in the spreadsheet entitled "Preliminary UVS/AWG/OPG Observations" which outlines the observation time and bits-to-the-ground for each of the observations during the tour. The tour is then graphically described by figures showing each orbit's geometry, the location of the UVS/AWG observations, and other useful orbit information. Finally, the observations are summarized in the attached OAPel forms.

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 in section 5.0.

4.1 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.

4.2 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.

4.3 Airglow observations are generally grouped into the complementary observation 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, H 2 , 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. 4.4 Auroral observations are generally grouped into the complementary observation 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.

4.5 Calibration is done early and late in the mission with star calibrations on previously observed targets using the STRCAL observation. The star k-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.

4.6 Targets of opportunity may exist and will be identified on a case- by- case basis.

4.7 Additional data is required through AACS-provided pointing information, cooperative images on some observations, and the use of science turns to achieve some measurements. Each of these are listed within the specific observation below.

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 and tape track allocations. The realtime observations include the highest priority UVS activities (designed to minimize bits-to-ground and tape track allocation resources) and will use realtime bits-to-ground during the encounter period in TBD realtime formats.

4 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
9D) FIXTMD - realtime
9B) FIXTMB - realtime and recorded
10) FIXLON - realtime
11a) EWMAPS - recorded
11b) NEWSMP - recorded
12) STRCAL - realtime

DESCRIPTIONS OF MEASUREMENT SET ELEMENTS

RECORDED:
JA/J0 1) RADMON
Objective: radiation environment characterization during Jupiter approach;
Strategy: G-N channel recorded 1 RIM for each of 5 R j distances; target to the NEP (North Ecliptic Pole);
Location: 100, 50, 25, 15 and 9 R j ; geometry constrained;
AWG priorities: 16;
Bits-to-ground: 1 RIM x (60.67 sec/RIM) x 1008 bps = 0.061152 x 10 6 bits; AACS = 144 bps x (60.667 sec x 1 RIMs) = 0.008736 x 10 6 bits. TOTAL observation bits = 0.069888 x 10 6 bits [5 observations/J0 = 0.349440 x 10 6 bits].
Tracks: (14.2203 tics/RIM 1 RIM)/6977 tics/track = 0.002 tracks.
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 in TARGET;
Location: 90o phase angle; geometry constrained;
AWG priorities: 3, 6A/B, 9, 13, 14A/B;
Bits-to-ground: 3 observations x (1092 words/summation buffer x 16 bits/word) = 0.052416 x 10 6 bits. TOTAL observation bits = 0.052416 x 10 6 bits.
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 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 90o SITURN); geometry constrained;
AWG priorities: 1, 12, 13, 15;
Bits-to- ground: 6 RIMs x (60.67 sec/RIM) x 1008 bps = 0.366912 x 10 6 bits; AACS = 144 bps x (60.667 sec x 6 RIMs) = 0.052416 x 10 6 bits. TOTAL observation bits = 0.419328 x 10 6 bits [3 observations/orbit = 1.257984 x 10 6 bits].
Tracks: (14.2203 tics/RIM x 6 RIMs)/6977 tics/track = 0.012 tracks [3 observations = 0.037 tracks.]
JA/J0 2) FUVPES
Objective: FUV feature track campaign (reflectance map) of the Probe Entry Site (PES) for three emission angles near 60o 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;
AWG priorities: 1, 12, 13, 15;
Bits-to-ground: 6 RIMs x (60.67 sec/RIM) x 1008 bps = 0.366912 x 10 6 bits; AACS = 144 bps x (60.667 sec x 6 RIMs) = 0.052416 x 10 6 bits. TOTAL observation bits = 0.419328 x 10 6 bits [3 observations/orbit = 1.257984 x 10 6 bits].
Tracks: (14.2203 tics/RIM x 6 RIMs)/6977 tics/track = 0.012 tracks [3 observations = 0.037 tracks.]
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; 45o 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: 10o phase angle and 14-15 Rj; geometry critical; first orbits (G1 or G2);
AWG priorities: 1, 3, 10, 12, 13;
Bits-to-ground: {[30 RIMs x (60.67 sec/RIM) x 1008 bps = 1.83456 x 10 6 bits] + [AACS 144 bps x (60.667 sec x 30 RIMs) = 0.26208 x 10 6 bits]} = 2.09664 x 10 6 bits}. TOTAL observation bits = 2.09664 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 30 RIMs)/6977 tics/track = 0.061 tracks.
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 H 2 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;
AWG priorities: 1, 2, 5, 6A, 12, 13, 14A, 15;
Bits-to-ground: {1.553 hr x 3600 sec/hr x 1008 bps = 5.635526 x 10 6 bits} + {AACS = 144 bps x (3600 sec x 1.553) = 0.805075 x 10 6 bits} = 6.440601 x 10 6 bits. TOTAL observation bits = 6.440601 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 93 RIM)/6977 tics/track = 0.190 tracks.
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;
AWG priorities: 1, 6A/B, 12, 13, 14A/B;
Bits-to-ground: 30 minutes x 60 sec/min x (1008 bps) = 1.814400 x 10 6 bits. AACS = 144 bps x 1800 sec = 0.259200 x 10 6 bits. TOTAL observation bits = 2.073600 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 30 RIM)/6977 tics/track = 0.061 tracks.
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;
AWG priorities: 1, 3, 10, 12, 13;
Bits-to-ground: {5 observations (1092 words/summation buffer x 16 bits/word) = 0.08736 x 10 6 bits} + {5 RIMs x (60.67 sec/RIM) x 1008 bps = 0.30576 x 10 6 bits} = 0.39312 x 10 6 bits. TOTAL observation bits = 0.39312 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 5 RIMs)/6977 tics/track = 0.010 tracks.
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;
AWG priorities: 2, 3, 5, 9, 10, 13;
Bits-to-ground: {9 observations x (1092 words/summation buffer x 16 bits/word) = 0.157248 x 10 6 bits} + {9 RIMs x (60.67 sec/RIM) x 1008 bps = 0.550368 x 10 6 bits} = 0.707616 x 10 6 bits. TOTAL observation bits = 0.707616 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 9 RIM)/6977 tics/track = 0.018 tracks.
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);
Location: where darkside viewing is possible early in mission (farther out global coverage) and later in the mission (closer in zonal coverage); geometry constrained;
AWG priorities: 2, 3, 5, 6A, 9, 10, 12, 13, 14A;<BR> Bits-to-ground: 3 scans x (1092 words/summation buffer x 16 bits/word) = 0.052416 x 106 bits. TOTAL observation bits = 0.052416 x 10 6 bits.
DRKMAP OBSERVING STRATEGY
EARLY LATE
CLOSE (zonal) E4, E6 G7, G8, C9, C10
FAR (global) G1, G2, C3 E11
9D) 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 90o as well as the closest location as possible to Jupiter (G7-E11 when darkside is most visible);
AWG priorities: 2, 6A/B, 9, 10, 13, 14A/B;
Bits-to- ground: 20 summation buffers x (1092 words/buffer x 16 bits/word) = 0.349440 x 10 6 bits. TOTAL observation bits = 0.349440 x 10 6 bits.
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 90o as well as the closest location as possible to Jupiter (G1-E6 when brightside is most visible);
AWG priorities: 2, 6A/B, 9, 10, 13, 14A/B;
Bits-to-ground: {20 summation buffers (10 hours G channel) x (1092 words/buffer x 16 bits/word) = 0.349440 x 10 6 bits} + {10 RIMs x (60.67 sec/RIM) x 1008 bps = 0.61152 x 10 6 bits} = 0.96096 x 10 6 bits. TOTAL observation bits = 0.96096 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 10 RIM)/6977 tics/track = 0.020 tracks.
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; ge-ometry constrained;
AWG priorities: 2, 3, 6A/B, 9, 10, 13, 14A/B;
Bits-to-ground: 10 summation buffers x (1092 words/buffer x 16 bits/word) = 0.174720 x 10 6 bits. TOTAL observation bits = 0.174720 x 10 6 bits.
FIXLON OBSERVING STRATEGY
BRIGHTBRIGHT DARKDARK
Early Late Early Late
CLOSE (zonal)
early G1, G2, C3 - (E6) -
late - C9 - G8, C10
FAR (global)
early E4 - (E6) -
late - G7 - E11
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 45o-60o;
AWG priorities: 3, 5, 10, 12, 13;
Bits-to-ground: 30 minutes x 60 sec/min x (1008 bps) = 1.814400 x 10 6 bits. AACS = 144 bps x 1800 sec = 0.259200 x 10 6 bits. Coop image (OPNAV) = 0.012656 x 10 6 bits. TOTAL observation bits = 2.086256 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 30 RIMs)/6977 tics/track = 0.061 tracks.
11b) NEWSMP
Objective: Dayglow/electroglow study using north-east-west-south swaths to determine limb-darkening curves of Lyman-alpha and global H 2 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 45o-60o early and late in mission (G2 and C10);
AWG priorities: 3, 5, 10, 12, 13;
Bits-to-ground: {0.93 hours x 3600 sec/hr x (1008 bps) = 3.374784 x 10 6 bits} + {AACS = 144 bps x 3348 sec = 0.482112 x 10 6 bits} + {Coop image (OPNAV) = 0.012656 x 10 6 bits} = 3.869552 x 10 6 bits. TOTAL observation bits = 3.869552 x 10 6 bits.
Tracks: (14.2203 tics/RIM x 56 RIMs)/6977 tics/track = 0.114 tracks.
REALTIME:
12) STRCAL
Objective: Instrument calibration twice during mission (early and late) on previously calibrated star; alpha-Eri not suitable due to variability while k-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;
AWG priority: 16;
Bits-to-ground: 3 observations (1092 words/summation buffer x 16 bits/word) = 0.052416 x 10 6 bits. Cooperative image (SSI cut-out windows) = 0.050432 x 10 6 bits. TOTAL observation bits = 0.102848 x 10 6 bits.
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 datastream are not costed to science bits.
Cooperative images
SSI frame uncompressed : 5.05 x 10 6 bits (defined as: 1 FFE). Can estimate 100:1 compression (0.05 x 10 6 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 10 6 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 90o off Earth point; use for solar occultation, ammonia/ acetylene map, and high phase feature campaign; AWG priorities = 1, 2, 5, 6A, 12, 13, 14A, 15.
6.0 JA/J0 ACTIVITY PLANS
  1. RADMON100: 0.0699 x 10 6 BTG; UVS radiation monitor (G-N); 1 RIM; 139 bytes; 95-333/20:30 at 100 Rj .
  2. RADMON050: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1 RIM; 139 bytes; 95-338/16:30 at 50 R j .
  3. RADMON025: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1 RIM; 139 bytes; 95-340/14:30 at 25 Rj .
  4. RADMON015: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1 RIM; 139 bytes; 95-341/05:30 at 15 Rj .
  5. RADMON009: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1 RIM; 139 bytes; 95-341/13:30 at 9 Rj .
  6. FUVPES1: 0.4193 x 10 6 BTG; UVS FUV PES ridealong; 6 RIMs; 0 bytes; 95-340/20:00 at 20 Rj .
  7. FUVPES2: 0.4193 x 10 6 BTG; UVS FUV PES ridealong; 6 RIMs; 0 bytes; 95-340/20:00 at 20 Rj .
  8. FUVPES3: 0.4193 x 10 6 BTG; UVS FUV PES ridealong; 6 RIMs; 0 bytes; 95-340/20:00 at 20 Rj .
Eight observations' total = 1.607 x 10 6 BTG with total tape tracks = 0.0468779 and total tics = 327.07.

Provided by Kent Tobiska, Galileo UVS Team at JPL

Last Updated Jan 30, 1997


These observation descriptions are indicative of those carried out throughout the mission. A complete mission list is available in the "EDR dataset" document for each instrument.