!  File:  2340C.PROP
!  Database:  PEPDB
!  Date:  17-FEB-1994:05:08:43

coverpage:

  title_1:         IMAGING AND SPECTROSCOPY IN THE CRAB NEBULA
    sci_cat:       INTERSTELLAR MEDIUM
    sci_subcat:    SN & SNR
    proposal_for:  GO
    pi_title:      DR.
    pi_fname:      KRIS
    pi_lname:      DAVIDSON
    pi_inst:       MINNESOTA, UNIVERSITY OF
    pi_country:    USA
    pi_phone:      612-624-5711
    keywords_1:    SUPERNOVA, SUPERNOVA REMNANT, CRAB NEBULA, ABUNDANCE,
    keywords_2:    NUCLEOSYNTHESIS, MORPHOLOGY
    hours_pri:     12.40
    num_pri:       9
    wf_pc:         Y
    foc:           Y
    funds_amount:  140000
    funds_length:  12
    funds_date:    JAN-91
    pi_position:   DR.
    off_fname:     MERLIN
    off_lname:     GARLID
    off_title:     ASSISTANT DIRECTOR
    off_inst:      UNIVERSITY OF MINNESOTA
    off_addr_1:    1919 UNIVERSITY AVENUE - 5TH FLOOR
    off_addr_2:    OFFICE OF RESEARCH ADMINISTRATION
    off_city:      ST. PAUL
    off_state:     MN
    off_zip:       55104
    off_country:   USA
    off_phone:     612-624-0288
! end of coverpage

abstract:

    line_1:        The Crab Nebula is the only young SNR (i.e., composed mainly of SN
    line_2:        ejecta) whose condensations are resolvable by ST while also being
    line_3:        "easily" observable in the UV. Moreover,it is now thought to represent
    line_4:        an important SN mass range, and at the same time the Crab's chemical
    line_5:        composition is poorly understood. V spectral data is essential for
    line_6:        understanding the Crab, while high-spatial-resolution studies of its
    line_7:        condensations will also be useful for producing more reliable
    line_8:        ionization models in order to study it composition and its dynamics.
    line_10:       We propose a detailed set of observations with the WFC, and FOC,
    line_11:       partly to obtain useful data soon and partly to enable planning of
    line_12:       future, more sophisticated UV spectroscopy. The WFC is to study
    line_13:       density gradients and local structure in the condensations and also to
    line_14:       provide accurate positions for possible future FOS work. The FOC is to
    line_15:       make images of UV emission lines, for composition with visual-
    line_16:       wavelength structure and also for possible future planning.

!
! end of abstract

general_form_proposers:

  lname:           KAFATOS
    fname:         MINAS
    title:         DR.
    inst:          GEORGE MASON UNIVERSITY
    country:       USA

!

  lname:           MACALPINE
    fname:         GORDON
    title:         DR.
    mi:            M
    inst:          MICHIGAN, UNIVERSITY OF
    country:       USA

!

  lname:           UOMOTO
    fname:         ALAN
    title:         DR.
    inst:          JOHNS HOPKINS UNIVERSITY
    country:       USA

!

  lname:           WILSON
    fname:         ANDREW
    title:         DR.
    mi:            S
    inst:          MARYLAND, UNIVERSITY OF
    country:       USA

!

  lname:           DAVIDSON
    fname:         KRIS
    title:         P.I.
    inst:          MINNESOTA, UNIVERSITY OF
    country:       USA

!

  lname:           HENRY
    fname:         RICHARD
    title:         DR.
    mi:            BC
    inst:          OKLAHOMA, UNIVERSITY OF
    country:       USA

!

  lname:           FESEN
    fname:         ROBERT
    title:         DR.
    mi:            A
    inst:          DARTMOUTH COLLEGE
    country:       USA

!

  lname:           KIRSHNER
    fname:         ROBERT
    title:         DR.
    mi:            P
    inst:          CFA
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        WFC: We will image the OIII, H-alpha, NII, and SII emission lines in 2
    line_2:        WFC fields in the Crab using narrow filters and about 20 m per
    line_3:        exposure.  We also plan continuum exposures in two of the fields to
    line_4:        assess the degree of non-thermal structure associated with the thermal
    line_5:        filaments.  A third intermediate field will be done with one filter
    line_6:        for additional coverage and astrometry.  We have optimized the fields
    line_7:        to have maximum expectation of excluding the 3 brightest stars in the
    line_8:        region without any special requirement on ST orientation, but this
    line_9:        detail is not critical to the project.
    line_11:       FOC/48, 44" field: This is essential for imaging the brightest UV
    line_12:       emission lines in selected parts of the Crab. (WFC readout noise is
    line_13:       too large for this low UV surface brightness object.)  The 3 most
    line_14:       promising filamentary regions have been selected for this purpose.  We
    line_15:       will use filter F175W to detect CIII] 1908 emission and F150W to
    line_16:       detect the sum of CIII] 1908 plus CIV 1549 and HeII 1640. (F195W is
    line_17:       unsuitable because its visual-wavelength transmission is too high.)
    line_18:       The exposure times are about 30 minutes each.  A shorter exposure with
    line_19:       F275W will be used to determine UV continuum for subtraction.

!

  question:        4
    section:       1
    line_1:        WFC: Models suggest characteristic size scales of 0.1 to 0.4 arcsec
    line_2:        for the thermal-gas structure, and ground-based images appear
    line_3:        consistent with this idea. The Crab obviously cannot be done by
    line_4:        speckle techniques. Therefore, only HST can provide images to
    line_5:        resolve the ionization and gas-dynamical structure. Excellent
    line_6:        measures of the filament proper motions are also attainable from the
    line_7:        WFC images.
    line_8:        FOC/48: We know that major spatial variations in spectra occur in the
    line_9:        Crab, probably due to composition gradients. Bright spots in the UV
    line_10:       carbon lines are expected to occur, and if they do occur then we need
    line_11:       to see the UV in order to detect them for future UV and
    line_12:       visual-wavelength spectroscopy.  The FOC is the only instrument that
    line_13:       can detect the carbon UV lines at the expected surface brightnesses.
    line_14:       (WFC won't work for this;  readout noise makes it impossible.)

!

  question:        5
    section:       1
    line_1:        Since surface brightnesses of emission lines in the Crab Nebula span a
    line_2:        very large range, S/N ratios depend on location.  In general, the
    line_3:        surface brightness is low enough to be difficult for both the WFC and
    line_4:        the FOC.  We have adjusted our exposure times to give excellent S/N
    line_5:        and high spatial resolution on the few brightest condensations, and
    line_6:        useful S/N on a reasonably large fraction of the Crab filaments.
    line_7:        Spatial resolution will be S/N limited for the fainter filaments in
    line_8:        the WFC images and for all structure in the FOC images.  Refs. to
    line_9:        fluxes in the Crab are given in (e.g.) Ann.Revs.Astron.Ap. 23, 119,
    line_10:       Ap.J. 228, 179 (visual-wavelength) and Ap.J. 253, 696 (UV).
    line_11:       WFC: Fairly bright filaments have apparent intensities of the order of
    line_12:       1.E-14 erg cm-2 s-1 arcsec-2 in each of the brightest
    line_13:       visual-wavelength emission lines. The peak QT-factors for appropriate
    line_14:       WFC filters are slightly less than 0.1, implying somewhat more than
    line_15:       100 cts/pixel in 20-minutes, for S/N = about 7.  For fainter filaments
    line_16:       the S/N-limited resolution may be degraded to 0.2 arcsec.  Since we
    line_17:       must sample several physically different emission lines, 20 minutes
    line_18:       per field is appropriate for exploratory purposes.

!

  question:        5
    section:       2
    line_1:        FOC: IUE data suggest that we can expect about 1.E-14 erg cm-2 s-1
    line_2:        arcsec-2 in the CIII] 1908 line (e.g.) in a bright condensation.  With
    line_3:        F175W, of the order of 360 cts per arcsec2 will be obtained in a
    line_4:        30-minute exposure.  But the non-thermal continuum background will be
    line_5:        comparable; therefore the S/N ratio in one arcsec2 would be 10-15 if
    line_6:        continuum subtraction (based on F275W exposure) were perfect.  So a
    line_7:        realistic S/N in the net CIII]-emission image is between 5 and 10 for
    line_8:        1 arcsec2, which will therefore be the effective resolution for the
    line_9:        assumed emission brightness.  A few condensations may be considerably
    line_10:       brighter.

!

  question:        7
    section:       1
    line_1:        A WFC image of the Crab will contain structure across most of the WFC
    line_2:        field, and is more complicated than an image even of a cluster of
    line_3:        localized objects. Moreover, the intersection of radial velocities in
    line_4:        the Crab within the available WFC narrow emission-line filter bands
    line_5:        will create additional complexity in the data analysis. Image
    line_6:        resolution will be position-dependent (because it is S/N-limited in
    line_7:        some of the filaments). The FOC images will not be quite as
    line_8:        complicated, but will have to be linearly combined in order to produce
    line_9:        separate CIII], (CIV+HeII), and UV-continuum maps of the localized FOC
    line_10:       fields.
    line_11:       Davidson, Uomoto, Fesen, and Wilson will concentrate on data
    line_12:       reduction.  Using the WFC images, emission-line surface brightnesses
    line_13:       will be measured at high resolution, leading to estimates of local
    line_14:       column thickness and densities of ions as functions of location within
    line_15:       individual condensations.  Astrometry will be done on stars in the WFC
    line_16:       fields and precise locations of gaseous condensations will be
    line_17:       determined -- both for future spectroscopy and also to measure the
    line_18:       nebular expansion rate.

!

  question:        7
    section:       2
    line_1:        The FOC ultraviolet images will allow maps of (CIV + HeII) and CIII]
    line_2:        emission-line brightnesses to be made.  These will be compared with
    line_3:        ground-based visual-wavelength spectroscopy of the same regions.  If
    line_4:        UV-bright spots are discovered in the FOC images, ground-based spectra
    line_5:        of those locations will be obtained using, for example, the
    line_6:        McGraw-Hill 2.4-m telescope.
    line_8:        Henry, MacAlpine, Kafatos and Kirshner will concentrate on the
    line_9:        spectroscopic implications of the FOC data.  MacAlpine's
    line_10:       photoionization codes will be used to produce realistic models of
    line_11:       thermal condensations, taking local morphology indicated in the WFC
    line_12:       images into account.

!
!end of general form text

general_form_address:

  lname:           DAVIDSON
    fname:         KRIS
    title:         DR.
    category:      PI
    inst:          UNIVERSITY OF MINNESOTA
    addr_1:        116 CHRUCH ST. S.E.
    city:          MINNEAPOLIS
    state:         MN
    zip:           55455
    country:       USA

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        NGC1952-WFCC1
    name_2:        CRAB-NEBULA
    name_3:        M1
    descr_1:       INTERSTELLAR MEDIUM; SUPERNOVA REMNANT;
    descr_2:       CENTRAL FIELD
    pos_1:         RA= 05H 34M 32.72S +/- 0.07S,
    pos_2:         DEC=+22D 01' 04.00" +/- 1"
    equinox:       2000
    rv_or_z:       V=0
    comment_1:     EMISSION LINES SPAN +/- 1500 KM/S
    comment_2:     IN RADIAL VELOCITY IN EACH PART
    comment_3:     OF FIELD. SURFACE BRIGHTNESS
    comment_4:     SPANS A LARGE RANGE OF VALUES.
    comment_5:     FLUXES QUOTED HERE REFER
    comment_6:     TO A TYPICAL MODERATE FILAMENT.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 21 +/- 2
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(5007) = 1.0 +/- 1.0 E-14
    fluxnum_3:     3
    fluxval_3:     SURF-LINE(6563) = 1.0 +/- 1.0 E-14
    fluxnum_4:     4
    fluxval_4:     SURF-LINE(6583) = 1.0 +/- 1.0 E-15
    fluxnum_5:     5
    fluxval_5:     SURF-LINE(6724) = 0.7 +/- 0.7 E-15
    fluxnum_6:     6
    fluxval_6:     SURF-LINE(3727) = 5.0 +/- 5.0 E-15
    fluxnum_7:     7
    fluxval_7:     W-LINE(5007) = 1.0 +/- 0.0
    fluxnum_8:     8
    fluxval_8:     W-LINE(6563) = 1.0 +/- 0.0
    fluxnum_9:     9
    fluxval_9:     W-LINE(6583) = 1.0 +/- 0.0
    fluxnum_10:    10
    fluxval_10:    W-LINE(6724) = 1.0 +/- 0.0

!

    targnum:       2
    name_1:        NGC1952-WFCS1
    name_2:        CRAB-NEBULA
    name_3:        M1
    descr_1:       INTERSTELLAR MEDIUM; SUPERNOVA REMNANT;
    descr_2:       SOUTH-1 FIELD
    pos_1:         RA= 05H 34M 33.44S +/- 0.07S,
    pos_2:         DEC=+22D 00' 12.00" +/- 1"
    equinox:       2000
    rv_or_z:       V=0
    comment_1:     EMISSION LINES SPAN +/- 1500 KM/S
    comment_2:     IN RADIAL VELOCITY IN EACH PART
    comment_3:     OF FIELD. SURFACE BRIGHTNESS
    comment_4:     SPANS A LARGE RANGE OF VALUES.
    comment_5:     FLUXES QUOTED HERE REFER
    comment_6:     TO A TYPICAL MODERATE FILAMENT.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 21 +/- 2
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(5007) = 1.0 +/- 1.0 E-14
    fluxnum_3:     3
    fluxval_3:     SURF-LINE(6563) = 1.0 +/- 1.0 E-14
    fluxnum_4:     4
    fluxval_4:     SURF-LINE(6583) = 1.0 +/- 1.0 E-15
    fluxnum_5:     5
    fluxval_5:     SURF-LINE(6724) = 0.7 +/- 0.7 E-15
    fluxnum_6:     6
    fluxval_6:     SURF-LINE(3727) = 5.0 +/- 5.0 E-15
    fluxnum_7:     7
    fluxval_7:     W-LINE(5007) = 1.0 +/- 0.0
    fluxnum_8:     8
    fluxval_8:     W-LINE(6563) = 1.0 +/- 0.0
    fluxnum_9:     9
    fluxval_9:     W-LINE(6583) = 1.0 +/- 0.0
    fluxnum_10:    10
    fluxval_10:    W-LINE(6724) = 1.0 +/- 0.0

!

    targnum:       3
    name_1:        NGC1952-WFCN1
    name_2:        CRAB-NEBULA
    name_3:        M1
    descr_1:       INTERSTELLAR MEDIUM; SUPERNOVA REMNANT;
    descr_2:       NORTH-1 FIELD
    pos_1:         RA= 05H 34M 28.84S +/- 0.07S,
    pos_2:         DEC=+22D 02' 44.00" +/- 1"
    equinox:       2000
    rv_or_z:       V=0
    comment_1:     EMISSION LINES SPAN +/- 1500 KM/S
    comment_2:     IN RADIAL VELOCITY IN EACH PART
    comment_3:     OF FIELD. SURFACE BRIGHTNESS
    comment_4:     SPANS A LARGE RANGE OF VALUES.
    comment_5:     FLUXES QUOTED HERE REFER
    comment_6:     TO A TYPICAL MODERATE FILAMENT.
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 21 +/- 2
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(5007) = 1.0 +/- 1.0 E-14
    fluxnum_3:     3
    fluxval_3:     SURF-LINE(6563) = 1.0 +/- 1.0 E-14
    fluxnum_4:     4
    fluxval_4:     SURF-LINE(6583) = 1.0 +/- 1.0 E-15
    fluxnum_5:     5
    fluxval_5:     SURF-LINE(6724) = 0.7 +/- 0.7 E-15
    fluxnum_6:     6
    fluxval_6:     SURF-LINE(3727) = 5.0 +/- 5.0 E-15
    fluxnum_7:     7
    fluxval_7:     W-LINE(5007) = 1.0 +/- 0.0
    fluxnum_8:     8
    fluxval_8:     W-LINE(6563) = 1.0 +/- 0.0
    fluxnum_9:     9
    fluxval_9:     W-LINE(6583) = 1.0 +/- 0.0
    fluxnum_10:    10
    fluxval_10:    W-LINE(6724) = 1.0 +/- 0.0

!

    targnum:       4
    name_1:        NGC1952-FOC01
    name_2:        CRAB-NEBULA
    name_3:        M1
    descr_1:       INTERSTELLAR MEDIUM; SUPERNOVA REMNANT;
    descr_2:       NORTH LOOP
    pos_1:         RA= 05H 34M 32.80S +/- 0.07S,
    pos_2:         DEC=+22D 02' 11.00" +/- 1"
    equinox:       2000
    rv_or_z:       V=0
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 21.1 +/- 0.8
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(1908) = 1.0 +/- 0.8 E-14
    fluxnum_3:     3
    fluxval_3:     SURF-LINE(1548) = 1.0 +/- 0.8 E-14
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1800) = 0.6 +/- 0.3 E-17
    fluxnum_5:     5
    fluxval_5:     W-LINE(1908) = 1.0 +/- 0.0
    fluxnum_6:     6
    fluxval_6:     W-LINE(1548) = 1.0 +/- 0.0

!

    targnum:       5
    name_1:        NGC1952-FOC02
    name_2:        CRAB-NEBULA
    name_3:        M1
    descr_1:       INTERSTELLAR MEDIUM; SUPERNOVA REMNANT;
    descr_2:       BRIGHT FILAMENT WSW
    pos_1:         RA= 05H 34M 29.70S +/- 0.07S,
    pos_2:         DEC=+22D 00' 35.00" +/- 1"
    equinox:       2000
    rv_or_z:       V=0
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 19.8 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(1908) = 1.0 +/- 0.8 E-14
    fluxnum_3:     3
    fluxval_3:     SURF-LINE(1548) = 1.0 +/- 0.8 E-14
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1800) = 2.0 +/- 0.8 E-17
    fluxnum_5:     5
    fluxval_5:     W-LINE(1908) = 1.0 +/- 0.0
    fluxnum_6:     6
    fluxval_6:     W-LINE(1548) = 1.0 +/- 0.0

!

    targnum:       6
    name_1:        NGC1952-FOC03
    name_2:        CRAB-NEBULA
    name_3:        M1
    descr_1:       INTERSTELLAR MEDIUM; SUPERNOVA REMNANT;
    descr_2:       BRIGHT FILAMENT SE
    pos_1:         RA= 05H 34M 34.20S +/- 0.07S,
    pos_2:         DEC=+21D 59' 50.00" +/- 1"
    equinox:       2000
    rv_or_z:       V=0
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 20.5 +/- 0.6
    fluxnum_2:     2
    fluxval_2:     SURF-LINE(1908) = 1.0 +/- 0.8 E-14
    fluxnum_3:     3
    fluxval_3:     SURF-LINE(1548) = 1.0 +/- 0.8 E-14
    fluxnum_4:     4
    fluxval_4:     SURF-CONT(1800) = 1.1 +/- 0.5 E-17
    fluxnum_5:     5
    fluxval_5:     W-LINE(1908) = 1.0 +/- 0.0
    fluxnum_6:     6
    fluxval_6:     W-LINE(1548) = 1.0 +/- 0.0

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       11.000
    sequence_1:    DEFINE
    sequence_2:    WFCC1
    targname:      NGC1952-WFCC1
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    #
    num_exp:       1
    time_per_exp:  1M
    s_to_n:        #
    fluxnum_1:     #
    priority:      #
    param_1:       PRE-FLASH=YES,
    param_2:       CR-SPLIT=NO
    req_1:         POS TARG 0,0

!

    linenum:       12.000
    sequence_1:    DEFINE
    sequence_2:    WFCS1
    targname:      NGC1952-WFCS1
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    #
    num_exp:       1
    time_per_exp:  1M
    s_to_n:        #
    fluxnum_1:     #
    priority:      #
    param_1:       PRE-FLASH=YES,
    param_2:       CR-SPLIT=NO
    req_1:         POS TARG 0,0

!

    linenum:       13.000
    sequence_1:    DEFINE
    sequence_2:    WFCN1
    targname:      NGC1952-WFCN1
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    #
    num_exp:       1
    time_per_exp:  1M
    s_to_n:        #
    fluxnum_1:     #
    priority:      #
    param_1:       PRE-FLASH=YES,
    param_2:       CR-SPLIT=NO
    req_1:         POS TARG 0,0

!

    linenum:       14.000
    sequence_1:    DEFINE
    sequence_2:    FOC01
    targname:      NGC1952-FOC01
    config:        FOC/48
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    #
    num_exp:       1
    time_per_exp:  1M
    s_to_n:        #
    fluxnum_1:     #
    priority:      #
    param_1:       PIXEL=50X25

!

    linenum:       15.000
    sequence_1:    DEFINE
    sequence_2:    FOC02
    targname:      NGC1952-FOC02
    config:        FOC/48
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    #
    num_exp:       1
    time_per_exp:  1M
    s_to_n:        #
    fluxnum_1:     #
    priority:      #
    param_1:       PIXEL=50X25

!

    linenum:       16.000
    sequence_1:    DEFINE
    sequence_2:    FOC03
    targname:      NGC1952-FOC03
    config:        FOC/48
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    #
    num_exp:       1
    time_per_exp:  1M
    s_to_n:        #
    fluxnum_1:     #
    priority:      #
    param_1:       PIXEL=50X25

!

    linenum:       111.000
    sequence_1:    USE WFCC1
    sp_element:    F664N
    time_per_exp:  X15
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4,
    fluxnum_3:     5
    priority:      3

!

    linenum:       112.000
    sequence_1:    USE WFCC1
    sp_element:    F656N
    time_per_exp:  X15
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4
    priority:      3

!

    linenum:       114.000
    sequence_1:    USE WFCC1
    sp_element:    F502N
    time_per_exp:  X15
    s_to_n:        7
    fluxnum_1:     2
    priority:      3

!

    linenum:       121.000
    sequence_1:    USE WFCS1
    sp_element:    F664N
    time_per_exp:  X30
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4,
    fluxnum_3:     5
    priority:      2

!

    linenum:       122.000
    sequence_1:    USE WFCS1
    sp_element:    F656N
    time_per_exp:  X24
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4
    priority:      2

!

    linenum:       123.000
    sequence_1:    USE WFCS1
    sp_element:    F547M
    time_per_exp:  X20
    s_to_n:        7
    fluxnum_1:     1
    priority:      2
    comment_1:     S/N IS FOR 1 PIXEL WITH
    comment_2:     SURF(V)=21, CRAB AVERAGE.
    comment_3:     CONTINUUM IS
    comment_4:     BRIGHTER THAN SURF(V)=21 IN
    comment_5:     PARTS OF FIELD.

!

    linenum:       124.000
    sequence_1:    USE WFCS1
    sp_element:    F502N
    time_per_exp:  X30
    s_to_n:        7
    fluxnum_1:     2
    priority:      2

!

    linenum:       125.000
    sequence_1:    USE WFCS1
    sp_element:    F658N
    time_per_exp:  X30
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4
    priority:      2

!

    linenum:       126.000
    sequence_1:    USE WFCS1
    sp_element:    F673N
    time_per_exp:  X30
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4,
    fluxnum_3:     5
    priority:      2

!

    linenum:       131.000
    sequence_1:    USE WFCN1
    sp_element:    F664N
    time_per_exp:  X20
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4,
    fluxnum_3:     5
    priority:      1

!

    linenum:       132.000
    sequence_1:    USE WFCN1
    sp_element:    F656N
    time_per_exp:  X20
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4
    priority:      1
    req_1:         SAME POS FOR 132-136 AS 131

!

    linenum:       133.000
    sequence_1:    USE WFCN1
    sp_element:    F547M
    time_per_exp:  X15
    s_to_n:        7
    fluxnum_1:     1
    priority:      2

!

    linenum:       134.000
    sequence_1:    USE WFCN1
    sp_element:    F502N
    time_per_exp:  X20
    s_to_n:        7
    fluxnum_1:     2
    priority:      1

!

    linenum:       135.000
    sequence_1:    USE WFCN1
    sp_element:    F658N
    time_per_exp:  X20
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4
    priority:      1

!

    linenum:       136.000
    sequence_1:    USE WFCN1
    sp_element:    F673N
    time_per_exp:  X20
    s_to_n:        7
    fluxnum_1:     3,
    fluxnum_2:     4,
    fluxnum_3:     5
    priority:      2

!

    linenum:       141.000
    sequence_1:    USE FOC01
    sp_element:    F175W
    time_per_exp:  X30
    s_to_n:        12
    fluxnum_1:     4
    priority:      3
    comment_1:     S/N IS PER SQ ARCSEC FOR
    comment_2:     EMISSION LINE IMAGE AFTER
    comment_3:     CONTINUUM SUBTRACTION.

!

    linenum:       142.000
    sequence_1:    USE FOC01
    sp_element:    F150W
    time_per_exp:  X30
    s_to_n:        12
    fluxnum_1:     3
    priority:      3
    comment_1:     S/N IS PER SQ ARCSEC FOR
    comment_2:     EMISSION LINE IMAGE AFTER
    comment_3:     CONTINUUM SUBTRACTION.

!

    linenum:       143.000
    sequence_1:    USE FOC01
    sp_element:    F275W
    time_per_exp:  X10
    s_to_n:        15
    fluxnum_1:     4
    priority:      3
    comment_1:     S/N IS FOR 1 SQ ARCSEC,
    comment_2:     NEEDED FOR SUBTRACTION IN
    comment_3:     LINE EMISSION IMAGES.

!

    linenum:       151.000
    sequence_1:    USE FOC02
    sp_element:    F175W
    time_per_exp:  X30
    s_to_n:        12
    fluxnum_1:     4
    priority:      2
    comment_1:     S/N IS PER SQ ARCSEC FOR
    comment_2:     EMISSION LINE IMAGE AFTER
    comment_3:     CONTINUUM SUBTRACTION.

!

    linenum:       152.000
    sequence_1:    USE FOC02
    sp_element:    F150W
    time_per_exp:  X30
    s_to_n:        12
    fluxnum_1:     3
    priority:      2
    comment_1:     S/N IS PER SQ ARCSEC FOR
    comment_2:     EMISSION LINE IMAGE AFTER
    comment_3:     CONTINUUM SUBTRACTION.

!

    linenum:       153.000
    sequence_1:    USE FOC02
    sp_element:    F275W
    time_per_exp:  X10
    s_to_n:        25
    fluxnum_1:     4
    priority:      2
    comment_1:     S/N IS FOR 1 SQ ARCSEC,
    comment_2:     NEEDED FOR SUBTRACTION IN
    comment_3:     LINE EMISSION IMAGES.

!

    linenum:       161.000
    sequence_1:    USE FOC03
    sp_element:    F175W
    time_per_exp:  X30
    s_to_n:        12
    fluxnum_1:     4
    priority:      1
    comment_1:     S/N IS PER SQ ARCSEC FOR
    comment_2:     EMISSION LINE IMAGE AFTER
    comment_3:     CONTINUUM SUBTRACTION.

!

    linenum:       162.000
    sequence_1:    USE FOC03
    sp_element:    F150W
    time_per_exp:  X30
    s_to_n:        12
    fluxnum_1:     3
    priority:      1
    comment_1:     S/N IS PER SQ ARCSEC FOR
    comment_2:     EMISSION LINE IMAGE AFTER
    comment_3:     CONTINUUM SUBTRACTION.

!

    linenum:       163.000
    sequence_1:    USE FOC03
    sp_element:    F275W
    time_per_exp:  X10
    s_to_n:        20
    fluxnum_1:     4
    priority:      1
    comment_1:     S/N IS FOR 1 SQ ARCSEC,
    comment_2:     NEEDED FOR SUBTRACTION IN
    comment_3:     LINE EMISSION IMAGES.

!
! end of exposure logsheet

! No scan data records found