!  File:  5197C.PROP
!  Database:  PEPDB
!  Date:  24-FEB-1994:00:38:45

coverpage:

  title_1:         DYNAMICS OF PLANETARY UPPER ATMOSPHERES - HOPR# 131
    sci_cat:       SOLAR SYSTEM
    proposal_for:  RPT/HSP
    cont_id:       4257
    pi_fname:      ROBERT
    pi_mi:         C.
    pi_lname:      BLESS
    pi_inst:       WISCONSIN, UNIVERSITY OF
    pi_country:    USA
    pi_phone:      608-262-1715
    keywords_1:    PLANETARY ATMOSPHERES, JOVIAN PLANETS, MARS, UPPER
    keywords_2:    OCCULTATIONS, TEMPERATURE PROFILES
    hours_pri:     4.80
    num_pri:       1
    hsp:           Y
    realtime:      N
    time_crit:     Y
! end of coverpage

abstract:

    line_1:        Observations of planetary upper atmospheres through
    line_2:        stellar occultations are of interest because they
    line_3:        provide information about the radiative and
    line_4:        dynamical processes at work in these rarefied
    line_5:        regions (number density range: 10super13 - 10super15
    line_6:        cmsuper-3), which could be otherwise measured only
    line_7:        through direct atmospheric probe launched from a
    line_8:        spacecraft. One of the problems with interpretation
    line_9:        of the temperature profiles obtained from
    line_10:       ground-based occultation observations has been that
    line_11:       the numerical inversion of the data is highly
    line_12:       sensitive to photometric errors--especially in
    line_13:       obtaining the mean temperature of the atmosphere.
    line_14:       The much greater stability of photometry that is
    line_15:       possible with the ST will allow us to obtain more
    line_16:       accurate temperature profiles and permit a
    line_17:       comparison of the atmospheric structures of the
    line_18:       Jovian planets with much greater precision than has
    line_19:       been possible in the past. We propose a series of
    line_20:       three occultation observations for each Jovian

!
! end of abstract

general_form_proposers:

  lname:           ROBINSON
    fname:         EDWARD
    mi:            L.
    inst:          TEXAS, UNIVERSITY OF
    country:       USA

!

  lname:           BLESS
    fname:         ROBERT
    mi:            C.
    inst:          WISCONSIN, UNIVERSITY OF
    country:       USA

!

  lname:           VAN CITTERS
    fname:         G.
    mi:            W.
    inst:          NATIONAL SCIENCE FOUNDATION
    country:       USA

!

  lname:           DOLAN
    fname:         JOSEPH
    mi:            F.
    inst:          NASA, GODDARD SPACE FLIGHT CENTER
    country:       USA

!

  lname:           WHITE
    fname:         RICHARD
    mi:            L.
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       USA

!

  lname:           ELLIOT
    fname:         JAMES
    mi:            L.
    inst:          MASSACHUSETTS INSTITUTE OF TECHNOLOGY
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        This proposal contains repeats of backscan
    line_2:        observations which had failed in 4257.  The
    line_3:        observation proceeds as follows: 1) Acquire
    line_4:        center of Uranus using onboard acquisition.
    line_5:        2) Offset to starting point indicated (along
    line_6:        path occulted star took).  3) Scan along path
    line_7:        in zigzag pattern indicated, mapping the scattered
    line_8:        light from Uranus.  These data will be used to
    line_9:        determine the contribution of Uranus scattered
    line_10:       light to the occultation profile obtained in
    line_11:       4257.  Note:  backscan specifications here assume
    line_12:       the NEW COMMANDING.  That is, they do not take into
    line_13:       account instrumental overheads.

!

  question:        4
    section:       1
    line_1:        We can achieve a much better signal-to-noise ratio
    line_2:        for the temperature profiles than has been possible
    line_3:        from the ground for the following reasons: (i) the
    line_4:        greatly improved photometric stability of ST
    line_5:        photometry, which will substantially reduce the
    line_6:        errors in the numerical inversion of the data that
    line_7:        is necessary to obtain the temperature profiles;
    line_8:        (ii) our ability to reject background light from the
    line_9:        planetary limb by employing small focal plane
    line_10:       apertures; and (iii) the absence of scintillation
    line_11:       noise, which has strong components at frequencies
    line_12:       comparable to the occultation timescale.

!

  question:        6
    section:       1
    line_1:        A prior scan over 10 arc-seconds is needed to map
    line_2:        the scattered light field, which is needed for the
    line_3:        data reduction.

!

  question:        7
    section:       1
    line_1:        Data will be reduced and analyzed at MIT with the
    line_2:        DEC 5000 belonging to the planetary astronomy
    line_3:        group.

!

  question:        10
    section:       1
    line_1:        Data reduction and analysis will be supported on
    line_2:        computer facilities at MIT.

!

  question:        13
    section:       1
    line_1:        Observations of the upper atmospheres of Mars and
    line_2:        the Jovian planets with HSP through stellar
    line_3:        occultations will provide infromation about the
    line_4:        radiative and dynamical processes in this region.
    line_5:        The temperature profiles obtained will allow testing
    line_6:        of the various transfer models for each planet.

!
!end of general form text

general_form_address:

  lname:           BLESS
    fname:         ROBERT
    mi:            C.
    category:      PI
    inst:          UNIVERSITY OF WISCONSIN
    addr_1:        DEPARTMENT OF ASTRONOMY
    city:          MADISON
    state:         WI
    zip:           53706
    country:       USA

!

  lname:           ELLIOT
    fname:         JAMES
    mi:            L.
    category:      CON
    inst:          MASSACHUSETTS INSTITUTE OF TECHNOLOGY
    addr_1:        BLDG. 54-422
    city:          CAMBRIDGE
    state:         MA
    zip:           02139
    country:       USA
    phone:         617-253-6308
    telex:         921473 MIT CAM

!
! end of general_form_address records

! No fixed target records found

solar_system_targets:

  targnum:         21
    name_1:        URANUS-CENTER
    descr_1:       PLANET URANUS
    lev1_1:        STD = URANUS, ACQ = 0.1
    comment_1:     ACQUISITION TARGET FOR
    comment_2:     BACKGROUND SCANS
    fluxnum_1:     1
    fluxval_1:     V = 5.5 +/- 0.5

!

  targnum:         24
    name_1:        U111-BACKGROUND
    descr_1:       OFFSET URANUS
    lev1_1:        STD = URANUS
    lev2_1:        TYPE = POS_ANGLE,
    lev2_2:        RAD = 10.0,
    lev2_3:        ANG = 81.25,
    lev2_4:        REF = NORTH
    comment_1:     FOR USE IN A SCAN OF
    comment_2:     BACKGROUND LEVELS ALONG
    comment_3:     THE PATH OF THE OCCULTED STAR.
    comment_4:     THESE START POSITIONS DO NOT
    comment_5:     TAKE INSTRUMENTAL OVERHEAD
    comment_6:     INTO ACCOUNT; ASSUMES NEW
    comment_7:     COMMANDING.

!
! end of solar system targets

! No generic target records found

exposure_logsheet:

    linenum:       4.000
    sequence_1:    DEFINE
    sequence_2:    ONBRD-ACQ
    targname:      #
    config:        HSP/VIS
    opmode:        ACQ
    num_exp:       1
    time_per_exp:  1S
    fluxnum_1:     1
    priority:      1

!

    linenum:       6.000
    sequence_1:    DEFINE
    sequence_2:    BACK-SCAN
    targname:      #
    config:        HSP/PMT/VIS
    opmode:        SPLIT
    aperture:      1.0
    sp_element:    F750W/F320N
    num_exp:       1
    time_per_exp:  1S
    fluxnum_1:     1
    priority:      1
    param_1:       #
    req_1:         SPATIAL SCAN;

!

    linenum:       40.000
    sequence_1:    USE
    sequence_2:    ONBRD-ACQ
    targname:      URANUS-CENTER
    time_per_exp:  X1
    req_1:         ONBOARD ACQ FOR 40.01 - 40.05;
    req_2:         SEQ 40.00 - 40.01 NO GAP;

!

    linenum:       40.010
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,
    req_1:         SEQ 40.01 - 40.05;
    req_2:         CYCLE 3/40.00 - 40.30;

!

    linenum:       40.020
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!

    linenum:       40.030
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!

    linenum:       40.040
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!

    linenum:       40.050
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!

    linenum:       40.250
    sequence_1:    USE
    sequence_2:    ONBRD-ACQ
    targname:      URANUS-CENTER
    time_per_exp:  X1
    req_1:         ONBOARD ACQ FOR 40.26 - 40.30;
    req_2:         SEQ 40.25 - 40.30 NO GAP;

!

    linenum:       40.260
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,
    req_1:         SEQ 40.26 - 40.30;

!

    linenum:       40.270
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!

    linenum:       40.280
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!

    linenum:       40.290
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!

    linenum:       40.300
    sequence_1:    USE
    sequence_2:    BACK-SCAN
    targname:      U111-BACKGROUND
    time_per_exp:  X250
    param_1:       SAMPLE-TIME = 0.01,
    param_2:       DATA-FORMAT = ALL,
    param_3:       PMT-ANALOG = 10000,
    param_4:       VIS-ANALOG = 1000,

!
! end of exposure logsheet

scan_data:

    line_list:     40.01, 40.03, 40.05, 40.26, 40.28, 40.30
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     18.7500
    sides_angle:    90.0000
    number_lines:  1
    scan_rate:       0.0750
    first_line_pa: 263.5000
    scan_frame:    CEL
    len_offset:    0.
    wid_offset:    0.

!

    line_list:     40.02, 40.27
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     18.7500
    sides_angle:    90.0000
    number_lines:  1
    scan_rate:       0.0750
    first_line_pa: 263.5000
    scan_frame:    CEL
    len_offset:    0.
    wid_offset:    0.5

!

    line_list:     40.04, 40.29
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     18.7500
    sides_angle:    90.0000
    number_lines:  1
    scan_rate:       0.0750
    first_line_pa: 263.5000
    scan_frame:    CEL
    len_offset:    0.
    wid_offset:    -0.5

!
! end of scan data