!  File:  1084C.PROP
!  Database:  PEPDB
!  Date:  16-FEB-1994:01:04:18

coverpage:

  title_1:         LUNAR OCCULTATIONS WITH THE SPACE TELESCOPE
    sci_cat:       SOLAR SYSTEM
    proposal_for:  GTO/HSP
    pi_fname:      ROBERT
    pi_mi:         C.
    pi_lname:      BLESS
    pi_inst:       WISCONSIN, UNIVERSITY OF
    pi_country:    USA
    pi_phone:      608-262-1715
    keywords_1:    LUNAR OCCULTATIONS, BRIGHTNESS DISTRIBUTIONS, LIMB
    keywords_2:    DARKENING, SOLAR SYSTEM OBJECTS, EXTRA-SOLAR SYSTEM OBJECTS
    hours_pri:     3.00
    num_pri:       9
    realtime:      X
    time_crit:     Y
! end of coverpage

abstract:

    line_1:        In order to obtain their angular diameters, limb darkening and/or strip
    line_2:        brightness distributions, we propose to observe lunar occultations of Seyfert
    line_3:        galaxies, X-ray sources, white dwarfs, early stars, quasars, planetary nebulae,
    line_4:        late stars, asteroids, and satellites. For certain occultations, much greater
    line_5:        signal-to-noise ratio can be achieved with the HSP on the ST than has been
    line_6:        possible from the ground because of its orbital geometry, the greatly reduced
    line_7:        scattered light from the moon, and the absence of scintillation noise.
    line_8:        Revision History: Received on RPS 9/1/89;  Added to SCCS 9/5/89
    line_9:        Updated to V2 prop. instr.; RPSS V7.2 local & remote - SALM 9/5/89
    line_10:       Updated to pass RPSS;  asb@MIT 7May90;  Specified cycle 2 - SALM 6/21/90;
    line_11:       Fixed small logic errors--BJW 7/10/90;

!
! 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:        We plan to use the ST orbit parameters and catalogs of the objects of interest
    line_2:        to identify those occultations of sufficient signal-to-noise ratio to achieve
    line_3:        the goals outlined in Section 2. Each observation will require a scan of about
    line_4:        ten arc-seconds along the track that the object will follow relative to the
    line_5:        moon and a time series run on the object with whatever filter aperture
    line_6:        combination that is chosen for the observation. For some occultations to be
    line_7:        observed in the far UV, prior multi-filter photometry of the object will be
    line_8:        necessary in order to determine the most appropriate filter to use for the
    line_9:        occultation. For now, we shall assume that the calibration and observation
    line_10:       time will average about 15 minutes per lunar occultation observed.
    line_12:       After cycle 1.

!

  question:        4
    section:       1
    line_1:        We can achieve a much better signal-to-noise ratio for certain lunar
    line_2:        occultations than would be possible from the ground for the following reasons.
    line_3:        Twice each orbit, the ST will reach a point when the lunar limb will appear
    line_4:        nearly stationary with respect to the celestial sphere. (Due to the relative
    line_5:        inclinations of the lunar and ST orbits, however, there may be some residual
    line_6:        motion parallel to the lunar limb). At these stationary points, we can achieve
    line_7:        a high signal-to-noise ratio for lunar occultations because (i) the occultation
    line_8:        diffracted light pattern is scanned at low velocity; (ii) the lower level of
    line_9:        background scattered light from the moon seen by the ST; (iii) our ability to
    line_10:       reject background lunar light by employing small focal plane apertures; and (iv)
    line_11:       the absence of scintillation noise, which has strong components at frequencies
    line_12:       comparable to the occultation timescale. For example, if an occultation of
    line_13:       3C273 (v = +1.8) were to occur within 2' of a stationary point, we could
    line_14:       measure its diameter (assuming it would be resolved) with a precision of 0.005
    line_15:       arc-seconds--the diffraction limit of a 20-meter telescope.

!

  question:        5
    section:       1
    line_1:        Acquisition of the object near the moon may be difficult.

!

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

!

  question:        7
    section:       1
    line_1:        Data will be reduced and analyzed at MIT with the VAX 11-750 belonging to the
    line_2:        planetary astronomy group.

!

  question:        10
    section:       1
    line_1:        TBD

!

  question:        13
    section:       1
    line_1:        Observations of lunar occultations by the HSP of several different classes of
    line_2:        objects will give information about their angular diameters. Brightness
    line_3:        distributions of Seyfert galaxies and lower limits on quasar emission as well
    line_4:        as the physical size of some objects can be obtained in this manner.

!
!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
    phone:         608-262-1715

!

  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

! No solar system records found

generic_targets:

  targnum_1:       1
    name_1:        SEYFERT-OCC
    descr_1:       SEYFERT GALAXIES
    criteria_1:    SEYFERTS OCCULTED BY THE MOON NEAR STATIONARY PT.
    acqpr_1:       BKG
    comment_1:     THE FLUX FOR THE OCCULTED OBJECTS
    comment_2:     THAT WILL YIELD USEFUL LUNAR
    comment_3:     OCCULTATIONS WILL DEPEND
    comment_4:     CRITICALLY ON THE SCATTERED LIGHT
    comment_5:     PROPERTIES OF THE HST AND THE PART
    comment_6:     OF THE ST ORBIT AT WHICH THE
    comment_7:     OBJECT IS OCCULTED. ALL OBJECTS
    comment_8:     WILL BE SELECTED BY GTO.

!

  targnum_1:       2
    name_1:        X-RAY-SOURCES
    descr_1:       OPTICAL COUNTERPARTS OF X-RAY SOURCES
    criteria_1:    X-RAY SOURCES OCCULTED BY THE MOON NEAR STATIONARY POINT
    acqpr_1:       ^

!

  targnum_1:       3
    name_1:        DWARF-OCC
    descr_1:       WHITE DWARFS
    criteria_1:    WHITE DWARFS OCCULTED BY THE MOON NEAR STATIONARY POINT
    acqpr_1:       ^
    plate_req:     N
    plate_avail:   N

!

  targnum_1:       4
    name_1:        EARLY-OCC
    descr_1:       EARLY STARS
    criteria_1:    EARLY STARS OCCULTED BY THE MOON NEAR STATIONARY PT.
    acqpr_1:       ^
    plate_req:     N
    plate_avail:   N

!

  targnum_1:       5
    name_1:        QUAS-OCC
    descr_1:       QUASARS
    criteria_1:    QUASARS OCCULTED BY THE MOON NEAR STATIONARY PT.
    plate_req:     N
    plate_avail:   N

!

  targnum_1:       6
    name_1:        PLAN-NEB-OCC
    descr_1:       PLANETARY NEBULAE
    criteria_1:    PLAN. NEB. OCCULTED BY THE MOON NEAR STATIONARY PT.
    acqpr_1:       ^
    plate_req:     N
    plate_avail:   N

!

  targnum_1:       7
    name_1:        LATE-OCC
    descr_1:       LATE STARS
    criteria_1:    LATE STARS OCCULTED BY THE MOON NEAR STATIONARY PT.
    acqpr_1:       ^
    plate_req:     N
    plate_avail:   N

!

  targnum_1:       8
    name_1:        ASTER-OCC
    descr_1:       ASTEROIDS
    criteria_1:    ASTEROIDS OCCULTED BY THE MOON NEAR STATIONARY PT.
    acqpr_1:       ^
    plate_req:     N
    plate_avail:   N

!

  targnum_1:       9
    name_1:        SATELLITES
    descr_1:       SATELLITES
    criteria_1:    OBJECTS OCCULTED BY THE MOON NEAR STATIONARY PT.
    acqpr_1:       ^
    plate_req:     N
    plate_avail:   N

!
! end of generic targets

exposure_logsheet:

    linenum:       1.000
    sequence_1:    DEFINE
    sequence_2:    HSP-OCC
    targname:      #
    config:        HSP/VIS
    opmode:        ACQ
    num_exp:       1
    time_per_exp:  5M
    s_to_n:        10
    priority:      #
    req_1:         EARLY ACQ FOR 2-3;
    req_2:         SAME ORIENT FOR 2-3 AS 1;

!

    linenum:       2.000
    sequence_1:    ^
    targname:      #
    config:        HSP/PMT/VIS
    opmode:        SPLIT
    aperture:      1.0
    sp_element:    F750W/F320N
    num_exp:       1
    time_per_exp:  5M
    s_to_n:        5
    s_to_n_time:   1S
    priority:      #
    param_1:       SAMPLE-TIME=0.01,
    req_1:         CRIT OBS / 2-3;
    req_2:         SEQ 2-3 NO GAP;

!

    linenum:       3.000
    sequence_1:    ^
    targname:      #
    config:        ^
    opmode:        ^
    aperture:      ^
    sp_element:    ^
    num_exp:       1
    time_per_exp:  5M
    priority:      #
    param_1:       ^
    req_1:         SPATIAL SCAN SINGLE-EXP;

!

    linenum:       4.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      SEYFERT-OCC
    priority:      1
    req_1:         CYCLE 2 / 4-6;
    req_2:         SELECT 4 OF 4-6 OR 14-16 OR
    req_3:         24-26 OR 34-36 OR 44-46 OR
    req_4:         54-56 OR 64-66 OR 74-76 OR
    req_5:         84-86; COND IF OCCULTATION
    req_6:         GEOMETRY FAVORABLE / 4-6,
    req_7:         14-16, 24-26, 34-36, 44-46,
    req_8:         54-56, 64-66, 74-76, 84-86;

!

    linenum:       5.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       6.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       14.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      X-RAY-SOURCES
    priority:      1
    req_1:         CYCLE 2 / 14-16;

!

    linenum:       15.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       16.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       24.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      DWARF-OCC
    priority:      1
    req_1:         CYCLE 2 / 24-26;

!

    linenum:       25.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       26.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       34.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      EARLY-OCC
    priority:      1
    req_1:         CYCLE 2 / 34-36;

!

    linenum:       35.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       36.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       44.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      QUAS-OCC
    priority:      1
    req_1:         CYCLE 2 / 44-46;

!

    linenum:       45.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       46.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       54.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      PLAN-NEB-OCC
    priority:      1
    req_1:         CYCLE 2 / 54-56;

!

    linenum:       55.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      PLAN-NEB-OCC
    priority:      2

!

    linenum:       56.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       64.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      LATE-OCC
    priority:      1
    req_1:         CYCLE 2 / 64-66;

!

    linenum:       65.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       66.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       74.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      ASTER-OCC
    priority:      1
    req_1:         CYCLE 2 / 74-76;

!

    linenum:       75.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       76.000
    sequence_1:    ^
    targname:      ^
    priority:      3

!

    linenum:       84.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      SATELLITES
    priority:      1
    req_1:         CYCLE 2 / 84-86;

!

    linenum:       85.000
    sequence_1:    ^
    targname:      ^
    priority:      2

!

    linenum:       86.000
    sequence_1:    USE
    sequence_2:    HSP-OCC
    targname:      SATELLITES
    priority:      3

!
! end of exposure logsheet

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!

    line_list:     66.0
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     10.0000
    sides_angle:     0.0000
    number_lines:  1
    scan_rate:       0.2000
    first_line_pa:  90.0000
    scan_frame:    CEL
    len_offset:    10.0000
    wid_offset:    0.0000

!

    line_list:     74.0
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     10.0000
    sides_angle:     0.0000
    number_lines:  1
    scan_rate:       0.2000
    first_line_pa:  90.0000
    scan_frame:    CEL
    len_offset:    10.0000
    wid_offset:    0.0000

!

    line_list:     75.0
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     10.0000
    sides_angle:     0.0000
    number_lines:  1
    scan_rate:       0.2000
    first_line_pa:  90.0000
    scan_frame:    CEL
    len_offset:    10.0000
    wid_offset:    0.0000

!

    line_list:     76.0
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     10.0000
    sides_angle:     0.0000
    number_lines:  1
    scan_rate:       0.2000
    first_line_pa:  90.0000
    scan_frame:    CEL
    len_offset:    10.0000
    wid_offset:    0.0000

!

    line_list:     84.0
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     10.0000
    sides_angle:     0.0000
    number_lines:  1
    scan_rate:       0.2000
    first_line_pa:  90.0000
    scan_frame:    CEL
    len_offset:    10.0000
    wid_offset:    0.0000

!

    line_list:     85.0
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     10.0000
    sides_angle:     0.0000
    number_lines:  1
    scan_rate:       0.2000
    first_line_pa:  90.0000
    scan_frame:    CEL
    len_offset:    10.0000
    wid_offset:    0.0000

!

    line_list:     86.0
    fgs_scan:
    cont_dwell:    C
    dwell_pnts:    0
    dwell_secs:       0.00
    scan_width:       0.0000
    scan_length:     10.0000
    sides_angle:     0.0000
    number_lines:  1
    scan_rate:       0.2000
    first_line_pa:  90.0000
    scan_frame:    CEL
    len_offset:    10.0000
    wid_offset:    0.0000

!
! end of scan data