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:
- 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?
- 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?
- 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?
- 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
| BRIGHT | BRIGHT | DARK | DARK |
| 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
- RADMON100: 0.0699 x 10 6 BTG; UVS radiation monitor (G-N); 1
RIM; 139 bytes; 95-333/20:30 at 100 Rj .
- RADMON050: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1 RIM; 139 bytes; 95-338/16:30 at 50 R j .
- RADMON025: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1
RIM; 139 bytes; 95-340/14:30 at 25 Rj .
- RADMON015: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1
RIM; 139 bytes; 95-341/05:30 at 15 Rj .
- RADMON009: 0.07 x 10 6 BTG; UVS radiation monitor (G-N); 1
RIM; 139 bytes; 95-341/13:30 at 9 Rj .
- FUVPES1: 0.4193 x 10 6 BTG; UVS FUV PES ridealong; 6 RIMs; 0 bytes; 95-340/20:00 at 20 Rj .
- FUVPES2: 0.4193 x 10 6 BTG; UVS FUV PES ridealong; 6 RIMs; 0
bytes; 95-340/20:00 at 20 Rj .
- 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.