!  File:  4600C.PROP
!  Database:  PEPDB
!  Date:  22-FEB-1994:19:14:17

coverpage:

  title_1:         FUV SPECTROSCOPY OF IO'S SO2 ATMOSPHERE AND SURFACE -- CYCLE 3 HIGH
    sci_cat:       SOLAR SYSTEM
    proposal_for:  GO
    pi_title:      DR.
    pi_fname:      JOHN
    pi_mi:         T.
    pi_lname:      CLARKE
    pi_inst:       UNIVERSITY OF MICHIGAN
    pi_country:    USA
    pi_phone:      313-747-3540
    keywords_1:    PLANETARY SATELLITE, PLASMA TORUS
    hours_pri:     7.75
    num_pri:       1
    fos:           Y
    time_crit:     Y
    funds_length:  12
    funds_date:    JUN-93
    off_fname:     NEIL
    off_mi:        D.
    off_lname:     GERL
    off_title:     PROJECT REP., DRDA
    off_inst:      UNIVERSITY OF MICHIGAN
    off_addr_1:    475 E. JEFFERSON
    off_city:      ANN ARBOR
    off_state:     MI
    off_zip:       48109
    off_country:   USA
! end of coverpage

abstract:

    line_1:        Cycle 1 HST observations of Io have provided new insights into the
    line_2:        nature of Io's surface albedo, the distribution of the SO2 atmosphere,
    line_3:        and the extent and excitation of the FUV airglow emissions. FOC images
    line_4:        show an anti-correlation between the brightness at 4000 A and 2800 A,
    line_5:        due to either surface SO2 frost or SO2 gas absorption above the frost
    line_6:        at the shorter wavelength. FOS spectra of the albedo spectrum at high
    line_7:        signal to noise clearly show SO2 gas absorption bands near 1900-2000 A
    line_8:        and evidence up to 1000 times spatial variation in the SO2 gas column
    line_9:        from the 2300 A spectrum. The FOS and GHRS airglow spectra have for the
    line_10:       first time resolved the extent of the FUV emission lines (1.7 Io radii
    line_11:       in diameter), and found that these lines decrease by a factor of 4-5
    line_12:       within 15 minutes of Io's passing into eclipse.  This suggests that in
    line_13:       shadow either the SO2 atmosphere condenses onto the surface or the
    line_14:       ionosphere recombines rapidly: the difference between these two
    line_15:       possibilities is very significant.  In cycle 3 we propose to scan across
    line_16:       Io with a small FOS aperture to obtain spatially resolved spectra of the
    line_17:       known bright and dark regions to discriminate between gas absorption and
    line_18:       surface albedo changes.  We will also obtain FUV spectra of Io emerging
    line_19:       from eclipse to determine the time scale on which the FUV airglow
    line_20:       emission lines recover their intensity on return into sunlight.

!
! end of abstract

general_form_proposers:

  lname:           CLARKE
    fname:         JOHN
    title:         PI
    mi:            T.
    inst:          2660
    country:       USA

!

  lname:           MCGRATH
    fname:         MELISSA
    inst:          3470
    country:       USA

!

  lname:           AJELLO
    fname:         JOE
    inst:          2370
    country:       USA

!

  lname:           SCHNEIDER
    fname:         NICK
    inst:          1760
    country:       USA

!

  lname:           BALLESTER
    fname:         GILDA
    inst:          2660
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        2
    section:       1
    line_1:

!

  question:        3
    section:       1
    line_1:        We propose to obtain spectra of specific regions on Io with
    line_2:        FOS G190H and G270H using the 0.25 arc sec aperture with offsets
    line_3:        from the acquired center of Io.  These will be obtained near
    line_4:        times of Io western elongation, when the apparent
    line_5:        motion is small and corresponding to the existing FOC images at
    line_6:        2800 A.  We will center the aperture on known bright and dark
    line_7:        regions from the FOC images, and also perform a single spatial
    line_8:        scan N/S across the disk of Io to look for unexpected spectral
    line_9:        changes. We will also take a FOS G130H spectral time series of Io
    line_10:       emerging from eclipse behind Jupiter, with Io centered in the
    line_11:       4.3 arc sec aperture: this will complete the series of eclipse
    line_12:       observations begun in cycles 1 and 2.

!

  question:        4
    section:       1
    line_1:        The line emissions excited by the impact of magnetospheric plasma
    line_2:        at Io are radiated chiefly in the FUV, and require a space-based
    line_3:        instrument with high sensitivity and angular resolution to be detected.
    line_4:        Ground-based instruments today have great difficulty in detecting
    line_5:        atmospheric line emissions from Io.  Emissions from the extended
    line_6:        atmosphere of Io are just detectable with the IUE, but higher
    line_7:        sensitivity and angular resolution are required to determine the
    line_8:        source region and spatial distribution.  Only the HST is fast enough
    line_9:        to detect changes in emission brightness through the eclipse events.
    line_10:       The capability of the FOS for measuring the 1600-3300 A albedo of Io
    line_11:       has been demonstrated in cycle 1 in 2 separate programs, whereas IUE
    line_12:       spectra are much too noisy below roughly 2400 A due to the decreasing
    line_13:       flux. Even with the HST spherical aberration, the central 0.15 arc sec
    line_14:       peak is sufficient to sample regions on the 1 arc sec Io disk with the
    line_15:       0.25 arc sec aperture and compare the spectra of different regions of
    line_16:       known overall reflectivity from the FOC images.  Only the angular
    line_17:       resolution and large aperture of HST can provide the high signal
    line_18:       spatially resolved spectra proposed here.  After the insertion of
    line_19:       COSTAR the point spread function should be greatly improved, however
    line_20:       there will be a loss of sensitivity at the shorter wavelengths from
    line_21:       the added mirrors.  We prefer to do what we can now in the UV, and
    line_22:       after COSTAR we may propose additional observations at longer
    line_23:       wavelengths.

!

  question:        5
    section:       1
    line_1:        The FOS G190H and G270H spectra are to be scheduled near
    line_2:        western elongation of Io.  Io must be acquired and its center
    line_3:        determined to within roughly 0.10 arc sec: an offset will then be
    line_4:        made to position the FOS 0.25 arc sec aperture on the desired region(s)
    line_5:        of Io.  The FOS G130H observation of Io must be centered (+/- 15  min.)
    line_6:        on the time of eclipse re-appearance, and must occur at the time of
    line_7:        year when the orbital longitude of Jupiter is 250 to 300 degrees.
    line_8:        These constraints can be relaxed somewhat if necessary to allow
    line_9:        scheduling.

!

  question:        6
    section:       1
    line_1:        None.

!

  question:        7
    section:       1
    line_1:        The UV spectra of Io will be reduced using standard routines as
    line_2:        in cycle 1: both JC and MM have reduced their cycle 1 data using IDL
    line_3:        on Sun workstations, and both have complete software packages for
    line_4:        the reduction and analysis of HST data.  We have developed a
    line_5:        synthetic model program in IDL which predicts the albedo spectrum
    line_6:        of Io for assumed surface amounts of SO2 frost and a given column
    line_7:        of SO2 gas (see section 2). We are presently adapting the Ballester
    line_8:        et al (1990) IUE models for our cycle 1 HST FOS spectra which
    line_9:        accounts in more detail for spatial surface and atmospheric
    line_10:       structure.  We are also in the process of a quantitative model of
    line_11:       the grating scatter in FOS for the 3 high dispersion gratings: we
    line_12:       expect these results to be concluded within the next 6 months.  In
    line_13:       other words, we are ready to reduce, model, and interpret the new
    line_14:       albedo data.  J. Ajello and collaborators are performing laboratory
    line_15:       studies of electron excitation of SO2 gas, measuring the electron
    line_16:       impact induced fluorescence spectrum of SO2 in the UV (400-2000 A)
    line_17:       at 2.5 A resolution.  For the strongest features we have measured
    line_18:       excitation functions from 0-400 eV for  modeling the excitation rates
    line_19:       at Io.  This group also has a proposal in to measure the SO2 gas
    line_20:       photoabsorption cross sections over 1600-3300 A as a function of
    line_21:       pressure and temperature to address outstanding questions about line
    line_22:       saturation effects in the low density/low temperature lower
    line_23:       atmosphere of Io.

!

  question:        8
    section:       1
    line_1:        None.

!

  question:        9
    section:       1
    line_1:        1. GO 2602 - "The Excitation of the Atmospheres of Planetary Satellites", J.
    line_2:        Clarke PI, J. Ajello and N. Schneider Co-I's - directly related.
    line_3:        2. GO 2603 - "Parallel Observations of H Ly alpha Emission from the Local ISM",
    line_4:        J. Clarke PI - unrelated.
    line_5:        3. GO 2393 - "D/H Ratio of Venus and Mars from Lyman alpha Emission", J. Clarke
    line_6:        Co-I - unrelated.
    line_7:        4. GO 2625 - "Excitation Processes for the Outer Planet UV  Emissions", M.
    line_8:        McGrath and J. Clarke Co-I's - unrelated.
    line_9:        5. GO 2627 - "Io's Atmosphere and its Interaction with the Plasma Torus",
    line_10:       Co-I's: M. McGrath, G. Ballester - directly related.
    line_11:       6. GO 3511 - "H Ly alpha Dayglow Emission Line Profiles from the Outer Planets",
    line_12:       J. Clarke PI - unrelated.
    line_13:       7. GO 3616 - "Upper Atmospheres of Uranus and Neptune", M. McGrath PI, J. Clarke
    line_14:       Co-I - unrelated.
    line_15:       8. GO 3617 - "The UV Emissions of Titan", M. McGrath PI, unrelated.
    line_16:       9. GO 3618 - "Excitation Processes for the Outer Planet UV Emissions" - Cycle
    line_17:       2 Continuation - M. McGrath PI - unrelated.
    line_18:       10. GO 3862 - "The Excitation of the Atmospheres of Planetary Satellites", J.
    line_19:       Clarke PI,  - J. Ajello and N. Schneider Co-I's - directly related.

!

  question:        10
    section:       1
    line_1:        Complete computing facilities are in place and available within
    line_2:        the Space Physics Research Lab. at the University of Michigan for use
    line_3:        on this project.  Two Sparcstations, including a Sun IPX procured with
    line_4:        cycle 1 GO funding, and a VAX 8600 are available and connected via a
    line_5:        local area network, in addition to the Michigan network MERIT, SPAN,
    line_6:        and Internet.  All Co-I's also have complete computing facilities at
    line_7:        their institutions for use on this project.  In addition, the laboratory
    line_8:        work of J. Ajello and collaborators is proceeding with input from the
    line_9:        HST data and with independent funding.

!
!end of general form text

general_form_address:

  lname:           CLARKE
    fname:         JOHN
    mi:            T.
    title:         PROF.
    category:      PI
    inst:          UNIVERSITY OF MICHIGAN
    addr_1:        AOSS DEPT.
    city:          ANN ARBOR
    state:         MI
    zip:           481092143
    country:       USA

!
! end of general_form_address records

! No fixed target records found

solar_system_targets:

  targnum:         1
    name_1:        IO-ACQ-SPOTS
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    wind_1:        OLG OF IO BETWEEN 215-235,
    wind_2:        OLG OF JUPITER BETWEEN 300 60
    comment_1:     IO ACQUISITION IN 4.3 ARC SEC
    comment_2:     APERTURE: TAKE A SET OF 11 SPECTRA
    comment_3:     AT DIFFERENT Y-DEFLECTIONS TO
    comment_4:     DETERMINE CENTERING IN X AND Y
    comment_5:     (FROM OBSERVED WAVELENGTH) THEN
    comment_6:     UPLINK HST POINTING CORRECTION.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13

!

  targnum:         2
    name_1:        IO-W-BRIGHT
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    lev3_1:        TYPE = CARTO,
    lev3_2:        LONG = 222.0,
    lev3_3:        LAT = +5.0
    wind_1:        SEP OF EUROPA IO FROM EARTH GT 10",
    wind_2:        SEP OF GANYMEDE IO FROM EARTH GT 10",
    wind_3:        SEP OF CALLISTO IO FROM EARTH GT 10",
    wind_4:        OLG OF IO BETWEEN 230 265,
    wind_5:        OLG OF JUPITER BETWEEN 300 60
    comment_1:     OBSERVE BRIGHT REGION ON IO WHEN
    comment_2:     IO IS FROM ABOUT -30 TO -5 DEGREES
    comment_3:     FROM WESTERN ELONGATION, WHEN JUPITER
    comment_4:     IS WITHIN 60 DEGREES OF OPPOSITION.
    comment_5:     PLEASE NOTE THAT THE WINDOWS CAN BE
    comment_6:     EXPANDED IF NEEDED TO SCHEDULE.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1900) = 1.5 +/- 1 E-15

!

  targnum:         3
    name_1:        IO-W-PELE
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    lev3_1:        TYPE = CARTO,
    lev3_2:        LONG = 257.0,
    lev3_3:        LAT = -19.0
    wind_1:        SEP OF EUROPA IO FROM EARTH GT 10",
    wind_2:        SEP OF GANYMEDE IO FROM EARTH GT 10",
    wind_3:        SEP OF CALLISTO IO FROM EARTH GT 10",
    wind_4:        OLG OF IO BETWEEN 240 280,
    wind_5:        OLG OF JUPITER BETWEEN 300 60
    comment_1:     OBSERVE PELE VOLCANO ON IO WHEN
    comment_2:     IO IS FROM ABOUT -30 TO +10 DEGREES
    comment_3:     FROM WESTERN ELONGATION, WHEN JUPITER
    comment_4:     IS WITHIN 60 DEGREES OF OPPOSITION.
    comment_5:     PLEASE NOTE THAT THE WINDOWS CAN BE
    comment_6:     EXPANDED IF NEEDED TO SCHEDULE.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1900) = 1.5 +/- 1 E-15

!

  targnum:         4
    name_1:        IO-W-DARK
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    lev3_1:        TYPE = CARTO,
    lev3_2:        LONG = 288.0,
    lev3_3:        LAT = -15.0
    wind_1:        SEP OF EUROPA IO FROM EARTH GT 10",
    wind_2:        SEP OF GANYMEDE IO FROM EARTH GT 10",
    wind_3:        SEP OF CALLISTO IO FROM EARTH GT 10",
    wind_4:        OLG OF IO BETWEEN 265 295,
    wind_5:        OLG OF JUPITER BETWEEN 300 60
    comment_1:     OBSERVE DARK REGION ON IO WHEN
    comment_2:     IO IS FROM ABOUT -5 TO +25 DEGREES
    comment_3:     FROM WESTERN ELONGATION, WHEN JUPITER
    comment_4:     IS WITHIN 60 DEGREES OF OPPOSITION.
    comment_5:     PLEASE NOTE THAT THE WINDOWS CAN BE
    comment_6:     EXPANDED IF NEEDED TO SCHEDULE.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1900) = 1.5 +/- 1 E-15

!

  targnum:         5
    name_1:        IO-W-LOKI
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    lev3_1:        TYPE = CARTO,
    lev3_2:        LONG = 304.0,
    lev3_3:        LAT = +20.0
    wind_1:        SEP OF EUROPA IO FROM EARTH GT 10",
    wind_2:        SEP OF GANYMEDE IO FROM EARTH GT 10",
    wind_3:        SEP OF CALLISTO IO FROM EARTH GT 10",
    wind_4:        OLG OF IO BETWEEN 280 325,
    wind_5:        OLG OF JUPITER BETWEEN 300 60
    comment_1:     OBSERVE LOKI VOLCANO ON IO WHEN
    comment_2:     IO IS FROM ABOUT +10 TO +55 DEGREES
    comment_3:     FROM WESTERN ELONGATION, WHEN JUPITER
    comment_4:     IS WITHIN 60 DEGREES OF OPPOSITION.
    comment_5:     PLEASE NOTE THAT THE WINDOWS CAN BE
    comment_6:     EXPANDED IF NEEDED TO SCHEDULE.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1900) = 1.5 +/- 1 E-15

!

  targnum:         6
    name_1:        IO-ACQ-SCAN
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    comment_1:     IO ACQUISITION IN 4.3 ARC SEC
    comment_2:     APERTURE: TAKE A SET OF 5 SPECTRA
    comment_3:     AT DIFFERENT Y-DEFLECTIONS TO
    comment_4:     DETERMINE CENTERING IN X AND Y
    comment_5:     (FROM OBSERVED WAVELENGTH) THEN
    comment_6:     UPLINK HST POINTING CORRECTION.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13

!

  targnum:         7
    name_1:        IO-W-SCAN
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    wind_1:        SEP OF EUROPA IO FROM EARTH GT 10",
    wind_2:        SEP OF GANYMEDE IO FROM EARTH GT 10",
    wind_3:        SEP OF CALLISTO IO FROM EARTH GT 10",
    wind_4:        OLG OF IO BETWEEN 250 290,
    wind_5:        OLG OF JUPITER BETWEEN 300 60
    comment_1:     OBSERVE IO WITHIN +/- 20 DEGREES
    comment_2:     OF WESTERN ELONGATION WHEN JUPITER
    comment_3:     IS WITHIN 60 DEGREES OF OPPOSITION.
    comment_4:     PLEASE NOTE THAT THE WINDOWS CAN
    comment_5:     BE EXPANDED IF NEEDED TO SCHEDULE.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1900) = 1.5 +/- 1 E-15

!

  targnum:         8
    name_1:        IO-ACQ-SHADOW
    descr_1:       OFFSET EUROPA
    lev1_1:        STD = JUPITER
    lev2_1:        STD = EUROPA
    comment_1:     STRATEGY IS TO ACQUIRE EUROPA
    comment_2:     AND THEN BLIND OFFSET TO IO, BOTH
    comment_3:     IN 4.3 APERTURE. TO ACQUIRE EUROPA
    comment_4:     WITH FOS, TAKE A SET OF 5 SPECTRA
    comment_5:     AT DIFFERENT Y-DEFLECTIONS TO
    comment_6:     DETERMINE CENTERING IN X AND Y
    comment_7:     (FROM OBSERVED WAVELENGTH) THEN
    comment_8:     UPLINK HST POINTING CORRECTION.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.3 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 0.9  +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13

!

  targnum:         9
    name_1:        IO-EGRESS
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    wind_1:        OLG OF JUPITER BETWEEN 250 300,
    wind_2:        ECL U OF IO BY JUPITER,
    wind_3:        SEP OF EUROPA IO FROM EARTH GT 10",
    wind_4:        SEP OF GANYMEDE IO FROM EARTH GT 10",
    wind_5:        SEP OF CALLISTO IO FROM EARTH GT 10",
    wind_6:        SEP OF EUROPA IO FROM EARTH LT 2'
    comment_1:     OBSERVE IO COMING OUT OF ECLIPSE
    comment_2:     BEHIND JUPITER; BEGIN FOS EXPOSURE
    comment_3:     15-20 MINUTES BEFORE IO ECLIPSE
    comment_4:     REAPPEARANCE AND SCHEDULE
    comment_5:     WHEN ORBITAL LONGITUDE OF JUPITER
    comment_6:     IS 250 TO 300 DEGREES.
    comment_7:     PLEASE NOTE THAT THE WINDOWS CAN
    comment_8:     BE EXPANDED IF NEEDED TO SCHEDULE.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13

!

  targnum:         10
    name_1:        IO-ACQ-IMAGE
    descr_1:       SATELLITE IO
    lev1_1:        STD = JUPITER
    lev2_1:        STD = IO
    comment_1:     ACQUISITION IMAGE OF IO IN 4.3
    comment_2:     FOS APERTURE FOR POST-UPLINK
    comment_3:     POINTING INFORMATION.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 5.0 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SIZE = 1.0 +/- .2
    fluxnum_3:     3
    fluxval_3:     SURF-CONT(2700) = 2 +/- 1 E-13

!
! end of solar system targets

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    targname:      IO-ACQ-SPOTS
    config:        FOS/BL
    opmode:        IMAGE
    aperture:      4.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  660 S
    fluxnum_1:     3
    priority:      1
    param_1:       Y-SIZE = 5,
    param_2:       Y-SPACE = 64,
    param_3:       COMB = YES,
    param_4:       SUB-STEP = 4
    req_1:         CYCLE 3 / 1-16;
    req_2:         SEQ 1-10 NOGAP;
    req_3:         INT ACQ FOR 2;
    comment_1:     SPECTRA OF IO FOR INTERACTIVE
    comment_2:     ACQUISITION: REQUIRES REAL-TIME
    comment_3:     UPLINK FOR S/C MOTIONS IN X AND
    comment_4:     Y DURING EARTH OCCULTATION.

!

    linenum:       2.000
    targname:      IO-ACQ-SPOTS
    config:        FOS/BL
    opmode:        IMAGE
    aperture:      4.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  4.0 S
    fluxnum_1:     3
    priority:      2
    param_1:       STEP-TIME=1.0,
    param_2:       SUB-STEP=1,
    param_3:       Y-SIZE=4,
    param_4:       Y-SPACE=64,
    param_5:       COMB=NO
    comment_1:     IMAGE OF 4.3 APERTURE
    comment_2:     FOR POST-UPLINK POINTING
    comment_3:     INFORMATION.  NEXT,
    comment_4:     OFFSET TO 0.3 APERTURE
    comment_5:     FOR SPECTRA IN LINENUM 3.

!

    linenum:       3.000
    targname:      IO-W-BRIGHT
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  9 M
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G270H SPECTRA OF BRIGHT SPOT
    comment_2:     OF IO AT LONG,LAT = 222,+5.

!

    linenum:       4.000
    targname:      IO-W-BRIGHT
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G190H
    num_exp:       1
    time_per_exp:  33 M
    fluxnum_1:     4
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G190H SPECTRA OF BRIGHT SPOT
    comment_2:     OF IO AT LONG,LAT = 222,+5.

!

    linenum:       5.000
    targname:      IO-W-PELE
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  10 M
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G270H SPECTRA OF PELE VOLCANO
    comment_2:     OF IO AT LONG,LAT = 257,-19.

!

    linenum:       6.000
    targname:      IO-W-PELE
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G190H
    num_exp:       1
    time_per_exp:  31 M
    fluxnum_1:     4
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G270H SPECTRA OF PELE VOLCANO
    comment_2:     OF IO AT LONG,LAT = 257,-19.

!

    linenum:       7.000
    targname:      IO-W-DARK
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  10 M
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G270H SPECTRA OF DARK SPOT
    comment_2:     OF IO AT LONG,LAT = 288,-15.

!

    linenum:       8.000
    targname:      IO-W-DARK
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G190H
    num_exp:       1
    time_per_exp:  38 M
    fluxnum_1:     4
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G270H SPECTRA OF DARK SPOT
    comment_2:     OF IO AT LONG,LAT = 288,-15.

!

    linenum:       9.000
    targname:      IO-W-LOKI
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  10 M
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G270H SPECTRA OF LOKI VOLCANO
    comment_2:     OF IO AT LONG,LAT = 304,+20.

!

    linenum:       10.000
    targname:      IO-W-LOKI
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G190H
    num_exp:       1
    time_per_exp:  31 M
    fluxnum_1:     4
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       READ-TIME=60
    comment_1:     G270H SPECTRA OF LOKI VOLCANO
    comment_2:     OF IO AT LONG,LAT = 304,+20.

!

    linenum:       11.000
    targname:      IO-ACQ-SCAN
    config:        FOS/BL
    opmode:        IMAGE
    aperture:      4.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  300 S
    fluxnum_1:     3
    priority:      1
    param_1:       Y-SIZE = 5,
    param_2:       Y-SPACE = 128,
    param_3:       COMB = YES,
    param_4:       SUB-STEP = 4
    req_1:         SEQ 11-13 NOGAP;
    req_2:         INT ACQ FOR 12;
    comment_1:     SPECTRA OF IO FOR INTERACTIVE
    comment_2:     ACQUISITION: REQUIRES REAL-TIME
    comment_3:     UPLINK FOR S/C MOTIONS IN X AND
    comment_4:     Y DURING EARTH OCCULTATION.
    comment_5:     NEXT, OFFSET TO 0.3 APERTURE
    comment_6:     FOR SPECTRA IN LINENUM 12.

!

    linenum:       12.000
    targname:      IO-W-SCAN
    config:        FOS/BL
    opmode:        RAPID
    aperture:      0.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  24 M
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=SINGLE
    param_2:       COMB = YES,
    param_3:       READ-TIME=60.0
    req_1:         SPATIAL SCAN ;
    req_2:         REQ UPLINK;
    comment_1:     VERY SLOW SPATIAL SCAN
    comment_2:     N/S ACROSS DISK OF IO.
    comment_3:     REQUIRES REVIEW BY STSCI.

!

    linenum:       13.000
    targname:      IO-ACQ-IMAGE
    config:        FOS/BL
    opmode:        IMAGE
    aperture:      4.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  4.0 S
    fluxnum_1:     3
    priority:      2
    param_1:       STEP-TIME=1.0,
    param_2:       SUB-STEP=1,
    param_3:       Y-SIZE=4,
    param_4:       Y-SPACE=64,
    param_5:       COMB=NO
    comment_1:     IMAGE OF 4.3 APERTURE
    comment_2:     FOR POST-UPLINK POINTING
    comment_3:     INFORMATION.

!

    linenum:       14.000
    targname:      IO-ACQ-SHADOW
    config:        FOS/BL
    opmode:        IMAGE
    aperture:      4.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  300 S
    fluxnum_1:     3
    priority:      1
    param_1:       Y-SIZE = 5,
    param_2:       Y-SPACE = 128,
    param_3:       COMB = YES,
    param_4:       SUB-STEP = 4
    req_1:         SEQ 14-16 NOGAP;
    req_2:         INT ACQ FOR 15;
    comment_1:     SPECTRA OF EUROPA FOR INT. ACQ.
    comment_2:     REQUIRES REAL-TIME UPLINK FOR
    comment_3:     S/C MOTIONS IN X AND Y DURING
    comment_4:     EARTH OCCULTATION.  AFTER
    comment_5:     CENTERING ON EUROPA, OFFSET TO
    comment_6:     IO, WHICH IS IN SHADOW.

!

    linenum:       15.000
    targname:      IO-EGRESS
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    num_exp:       1
    time_per_exp:  25 M
    fluxnum_1:     3
    priority:      1
    param_1:       STEP-PATT=DEF,
    param_2:       READ-TIME=60.
    req_1:         DARK TIME;
    req_2:         REQ UPLINK;
    comment_1:     G130H SPECTRA OF IO: BEGIN
    comment_2:     15-20 MINUTES BEFORE IO
    comment_3:     REAPPEARS IN SUNLIGHT FROM
    comment_4:     ECLIPSE.  SCHEDULE IN DARK TIME
    comment_5:     DUE TO 1304 OXYGEN AIRGLOW.

!

    linenum:       16.000
    targname:      IO-ACQ-IMAGE
    config:        FOS/BL
    opmode:        IMAGE
    aperture:      4.3
    sp_element:    G270H
    num_exp:       1
    time_per_exp:  4.0 S
    fluxnum_1:     3
    priority:      2
    param_1:       STEP-TIME=1.0,
    param_2:       SUB-STEP=1,
    param_3:       Y-SIZE=4,
    param_4:       Y-SPACE=64,
    param_5:       COMB=NO
    comment_1:     IMAGE OF 4.3 APERTURE
    comment_2:     FOR POST-UPLINK POINTING
    comment_3:     INFORMATION, PERFORMED
    comment_4:     WHEN IO IS IN SUNLIGHT.

!
! end of exposure logsheet

scan_data:

    line_list:     12.00
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:      1.2600
    sides_angle:    90.0000
    number_lines:  1
    scan_rate:       0.0009
    first_line_pa:  25.0000
    scan_frame:    CEL
    len_offset:    0.6300
    wid_offset:    0.0000

!
! end of scan data