!  File:  4661C.PROP
!  Database:  PEPDB
!  Date:  22-FEB-1994:21:35:07

coverpage:

  title_1:         ULTRAVIOLET ECLIPSE MAPPING OF THE ACCRETION FLOW IN THE ECLIPSING
    title_2:       INTERMEDIATE POLAR, EX HYA: CYCLE3 HIGH
    sci_cat:       HOT STARS
    sci_subcat:    ERUPTIVE BINARIES
    proposal_for:  GO
    pi_fname:      SIMON
    pi_mi:         R
    pi_lname:      ROSEN
    pi_inst:       UNIVERSITY OF LEICESTER
    pi_country:    U.K.
    hours_pri:     7.00
    num_pri:       1
    fos:           Y
    time_crit:     Y
    off_fname:     KEN
    off_lname:     POUNDS
    off_title:     HEAD OF DEPT.
    off_inst:      8042
    off_addr_1:    DEPT. OF PHYSICS
    off_addr_2:    UNIVERSITY OF LEICESTER
    off_addr_3:    UNIVERSITY RD.
    off_city:      LEICESTER
    off_country:   U.K.
    off_phone:     UK-533-523509
! end of coverpage

abstract:

    line_1:        EX Hya offers a unique opportunity to study the accretion flow onto the white
    line_2:        dwarf in an Intermediate Polar binary, being the only member of its class in
    line_3:        which the environs of that star are eclipsed by its companion. We propose to
    line_4:        exploit the unique ability of HST FOS to secure good S/N, highly time-resolved
    line_5:        UV spectra to perform the first detailed UV eclipse mapping study of EX Hya.
    line_6:        The detailed form of the accretion flow onto the white dwarf in these systems
    line_7:        remains unresolved. It may occur as a funnelled flow along magnetic field lines
    line_8:        from a truncated disk or it may be primarily in the form of an inhomogenous
    line_9:        stream of material that penetrates the magnetosphere. UV observations are
    line_10:       critical because much of the radiation output from this high energy environment
    line_11:       emerges in this band. We aim to use FOS to a) study the line profile changes
    line_12:       through the narrow eclipse to dissect the UV emitting accretion flow near the
    line_13:       white dwarf, b) compare eclipse properties in different lines to search for
    line_14:       ionization structure, c) monitor the evolution of the lines through the broader
    line_15:       eclipse wings to map the putative inner `disk' flow and d) record the motion
    line_16:       and broadening of the line wings as the white dwarf rotates to formulate an
    line_17:       overall dynamical picture.

!
! end of abstract

general_form_proposers:

  lname:           ROSEN
    fname:         SIMON
    title:         PI
    mi:            R
    inst:          UNIVERSITY OF LEICESTER
    country:       UNITED KINGDOM
    esa:           Y

!

  lname:           MUKAI
    fname:         KOJI
    inst:          NASA GODDARD SPACE FLIGHT CENTER
    country:       USA
    esa:           N

!

  lname:           WATSON
    fname:         MIKE
    mi:            G
    inst:          UNIVERSITY OF LEICESTER
    country:       UNITED KINGDOM
    esa:           Y

!

  lname:           MASON
    fname:         KEITH
    mi:            O
    inst:          MULLARD SPACE SCIENCE LABORATORY
    country:       UNITED KINGDOM
    esa:           Y

!

  lname:           OSBORNE
    fname:         JULIAN
    mi:            P
    inst:          UNIVERSITY OF LEICESTER
    country:       UNITED KINGDOM
    esa:           Y

!

  lname:           KING
    fname:         ANDREW
    mi:            R
    inst:          UNIVERSITY OF LEICESTER
    country:       UNITED KINGDOM
    esa:           Y

!

  lname:           PRINJA
    fname:         RAMAN
    mi:            K
    inst:          UNIVERSITY COLLEGE LONDON
    country:       UNITED KINGDOM
    esa:           Y

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        We will use the FOS/BL with the G130H grating to measure the
    line_2:        1150A-1606A range, covering the important lines of N V 1240A,
    line_3:        Si IV 1400A and especially C IV 1550A. We will use the 4.3 arc
    line_4:        second aperture to maximise throughput. Spectra will be recorded
    line_5:        repetitively with 15s exposures using FOS RAPID mode, providing
    line_6:        around >8 spectra through the narrow (2-3 minute) orbital eclipse
    line_7:        and many more through the broader `eclipse effect' either side of
    line_8:        it. We are requesting time-critical obervations so that we can
    line_9:        monitor the eclipses in EX Hya that repeat every 98 mins (2 mins
    line_10:       different from the HST orbital period); we are specifying an
    line_11:       eclipse ephemeris so that observations can be centred near the
    line_12:       eclipses. Since the eclipse drifts by 2 minutes relative to the
    line_13:       HST orbital window every HST orbit, we seek a scheduling of two
    line_14:       blocks of 7 contiguous HST orbits to keep the eclipse within
    line_15:       +/- 10 mins of the center of the HST orbital window (first
    line_16:       eclipse in each block should occur towards -10 mins from centre).
    line_17:       This arrangement will also maximise our ability to monitor
    line_18:       the effects of the white dwarf's rotation on the line profiles
    line_19:       outside the eclipses (using data before and after eclipse).

!

  question:        4
    section:       1
    line_1:        The hot (10000<T<40000K) accretion flow near the white dwarf
    line_2:        radiates predominantly at UV wavelengths, hence the need for
    line_3:        space-borne telescopes. Previous attempts with IUE to sample the
    line_4:        eclipse in EX Hya demonstrate that IUE is incapable of providing
    line_5:        the S/N or temporal and spectral resolutions necessary to study the
    line_6:        UV eclipses in detail. To make any significant headway with UV
    line_8:        eclipse mapping, we require spectra with a time resolution of
    line_9:        10-20 seconds and a S/N of around 10 per spectral resolution
    line_10:       element which only HST can provide. Exposures of 15s will
    line_11:       providing a S/N of around 10 in the C IV line per spectrum.
    line_12:       The improved spectral resolution with FOS will provide about
    line_13:       20 spectral bins across the line compared to 5 with IUE.
    line_14:       Using the observed IUE fluxes, we expect around 6, 18 and 120
    line_15:       cts/diode at 1200A, NV(1240) and CIV(1550) respectively per 15s
    line_16:       spectrum. The S/N ~10 at CIV is sufficient to monitor profile
    line_17:       changes through eclipse. Phase binning, especially for studies of
    line_18:       the line properties on the 67 minute white dwarf rotation cycle
    line_19:       (outside eclipse), will signifiantly enhance the S/N.

!

  question:        5
    section:       1
    line_1:        Our primary objective is to obtain detailed, time-resolved UV
    line_2:        spectroscopy through the eclipse in EX Hya. The eclipse lasts
    line_3:        for 2-3 minutes (with an additional maximum of 14 minutes either
    line_4:        side of the main eclipse if the eclipse of the accretion disk
    line_5:        is also considered) and occurs every 98 minutes. We will specify
    line_6:        our constraints via an eclipse ephemeris, requesting observations
    line_7:        throughout the HST (unblocked) orbital window containing the
    line_8:        eclipse (with the eclipse roughly centred in that window). We are
    line_9:        requesting two blocks of 7 contiguous HST orbits so that the
    line_10:       eclipses can be reasonably centred (it drifts by 2 minutes
    line_11:       relative to the window with every HST orbit). This approach will
    line_12:       probably also sample eclipses at a greater range of 67 minute
    line_13:       spin cycle phases.

!

  question:        6
    section:       1
    line_1:        Routine FOS calibration data will be sufficient for our purposes.

!

  question:        7
    section:       1
    line_1:        Time-resolved spectroscopy is a commonly used technique throughout
    line_2:        CV astronomy. The short spectral integrations enable rapid
    line_3:        variability of line profiles to be monitored. This is especially
    line_4:        important for eclipse mapping studies. We will employ a number of
    line_5:        techniques such as line fitting and V/R ratio techniques to
    line_6:        monitor line profile changes: from these results, we can begin to
    line_7:        reconstruct the accretion flow. Dynamical simulations will be used
    line_8:        to try to test and distinguish between the competing accretion
    line_9:        models. We will also attempt to exploit established Doppler
    line_10:       tomography techniques. Our analysis may also address ionisation
    line_11:       structure if present in the inner accretion flow. Data analysis
    line_12:       on the basic spectra will be performed at the Leicester University
    line_13:       and MSSL where substantial computing facilities are available.

!

  question:        8
    section:       1
    line_1:        We will be endeavouring to obtain contemporaneous optical
    line_2:        spectroscopy of EX Hya with the HST observations to compare the
    line_3:        behaviour of the UV and optical lines. This may be particularly
    line_4:        useful with regard to searching for ionization structure. However,
    line_5:        we stress that we will arrange these observations to conform to
    line_6:        the HST schedule, i.e. we do NOT need to impose additional
    line_7:        constraints on the HST scheduling. We will apply for observing
    line_8:        time at the 3.9m Anglo Australian telescope or Mount Stromlo
    line_9:        observatory and/or we will arrange observations with collaborators
    line_10:       (D. Buckley, B. Warner) at the South African Astronomical
    line_11:       Observatory. Such arrangements have been very productive in
    line_12:       previous satellite/ground-based simultaneous observations.

!

  question:        9
    section:       1
    line_1:        GO-3578    Line eclipse mapping of an accretion disk wind
    line_2:        GO-3579    The UV orbital lightcurve of the X-ray binary X1822-371
    line_3:        Neither of these programmes are related to this project.

!

  question:        10
    section:       1
    line_1:        The analysis of our HST data will be undertaken by the PI and the
    line_2:        Co-I's. All proposers have access to DEC Vax machines or SUN
    line_3:        stations which are dedicated to astronomical research.

!
!end of general form text

general_form_address:

  lname:           ROSEN
    fname:         SIMON
    mi:            R
    category:      PI
    inst:          University of Leicester
    addr_1:        Dept. of Physics,
    addr_3:        University Rd.,
    city:          Leicester
    country:       UNITED KINGDOM
    phone:         0533 552077

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        EX-HYA
    descr_1:       A, 154
    pos_1:         RA = 12H 52M 24.40S +/- 0.03S,
    pos_2:         DEC = -29D 14' 56.7" +/- 0.4",
    pos_3:         PLATE-ID = 02C8
    equinox:       J2000
    comment_1:     MAGNITUDE ERROR IS THE TYPICAL
    comment_2:     VARIATION ABOUT THE MEAN OVER THE
    comment_3:     67 MINUTE CYCLE. DURING 2 MINUTE
    comment_4:     ECLIPSE, MAGNITUDE MAY REACH ABOUT
    comment_5:     14. UV FLUXES ARE FROM IUE
    comment_6:     SPECTRA. S/N NEEDED IS AROUND
    comment_7:     10/PIXEL/SPECTRUM AT C IV PEAK.
    fluxnum_1:     1
    fluxval_1:     V = 13.0 +/- 0.4
    fluxnum_2:     2
    fluxval_2:     B-V = 0.1 +/- 0.2
    fluxnum_3:     3
    fluxval_3:     E(B-V) = 0.0 +/- 0.1
    fluxnum_4:     4
    fluxval_4:     F-CONT(1200) = 2.0 +/- 0.7 E-13
    fluxnum_5:     5
    fluxval_5:     F-CONT(1550) = 1.8 +/- 0.7 E-13
    fluxnum_6:     6
    fluxval_6:     F-LINE(1550) = 5.0 +/- 1.5 E-13
    fluxnum_7:     7
    fluxval_7:     W-LINE(1550) = 10 +/- 3

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        ACQ/PEAK
    aperture:      4.3
    sp_element:    G400H
    num_exp:       1
    time_per_exp:  1S
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     1
    fluxnum_2:     3
    priority:      1
    req_1:         ONBOARD ACQ FOR 1.5;
    req_2:         GROUP 1-8 WITH 12H;
    req_3:         CYCLE 3;
    req_4:         SPATIAL SCAN;
    comment_1:     STAR VARIES BY AS MUCH AS 0.4
    comment_2:     MAGNITUDES  ABOUT ITS MEAN
    comment_3:     OF 13.0. IN ECLIPSE (2-3 MINS
    comment_4:     OUT OF THE 98 MIN ORBITAL
    comment_5:     PERIOD) THE STAR MAY DROP TO
    comment_6:     ABOUT MAGNITUDE 14.

!

    linenum:       1.500
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        ACQ/PEAK
    aperture:      1.0
    sp_element:    G400H
    num_exp:       1
    time_per_exp:  1S
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     1
    fluxnum_2:     3
    priority:      1
    req_1:         ONBOARD ACQ FOR 2-8;
    req_2:         CYCLE 3;
    req_3:         SPATIAL SCAN;
    comment_1:     STAR VARIES BY AS MUCH AS 0.4
    comment_2:     MAGNITUDES  ABOUT ITS MEAN
    comment_3:     OF 13.0. IN ECLIPSE (2-3 MINS
    comment_4:     OUT OF THE 98 MIN ORBITAL
    comment_5:     PERIOD) THE STAR MAY DROP TO
    comment_6:     ABOUT MAGNITUDE 14.

!

    linenum:       2.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PERIOD 0.068233846D +/- 0.000000005D;
    req_3:         ZERO-PHASE JD2437699.9414 +/- 0.0005D;
    req_4:         PHASE  0.9 +/- 0.06;
    req_5:         CYCLE 3/2-16
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF THE UNBLOCKED
    comment_4:     HST ORBITAL WINDOWS, HENCE USE OF
    comment_5:     TWO BLOCKS OF 7 CONTIGUOUS HST
    comment_6:     ORBITS (2-8, 10-16). SEE Q3.

!

    linenum:       3.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       4.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       5.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       6.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       7.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       8.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       9.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        ACQ/PEAK
    aperture:      4.3
    sp_element:    G400H
    num_exp:       1
    time_per_exp:  1S
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     1
    fluxnum_2:     3
    priority:      1
    req_1:         ONBOARD ACQ FOR 9.5;
    req_2:         GROUP 9-16 WITHIN 12H;
    req_3:         SPATIAL SCAN;
    comment_1:     STAR VARIES BY AS MUCH AS 0.4
    comment_2:     MAGNITUDES  ABOUT ITS MEAN
    comment_3:     OF 13.0. IN ECLIPSE (2-3 MINS
    comment_4:     OUT OF THE 98 MIN ORBITAL
    comment_5:     PERIOD) THE STAR MAY DROP TO
    comment_6:     ABOUT MAGNITUDE 14.

!

    linenum:       9.500
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        ACQ/PEAK
    aperture:      1.0
    sp_element:    G400H
    num_exp:       1
    time_per_exp:  1S
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     1
    fluxnum_2:     3
    priority:      1
    req_1:         ONBOARD ACQ FOR 10-16;
    req_2:         SPATIAL SCAN;
    comment_1:     STAR VARIES BY AS MUCH AS 0.4
    comment_2:     MAGNITUDES  ABOUT ITS MEAN
    comment_3:     OF 13.0. IN ECLIPSE (2-3 MINS
    comment_4:     OUT OF THE 98 MIN ORBITAL
    comment_5:     PERIOD) THE STAR MAY DROP TO
    comment_6:     ABOUT MAGNITUDE 14.

!

    linenum:       10.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF THE UNBLOCKED
    comment_4:     HST ORBITAL WINDOWS, HENCE USE OF
    comment_5:     TWO BLOCKS OF 7 CONTIGUOUS HST
    comment_6:     ORBITS (2-8, 10-16). SEE Q3.

!

    linenum:       11.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       12.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       13.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       14.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       15.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!

    linenum:       16.000
    targname:      EX-HYA
    config:        FOS/BL
    opmode:        RAPID
    aperture:      4.3
    sp_element:    G130H
    wavelength:    1380
    num_exp:       1
    time_per_exp:  30M
    s_to_n:        10
    s_to_n_time:   15S
    fluxnum_1:     6
    priority:      1
    param_1:       COMB=YES
    param_2:       READ-TIME=15
    req_1:         NON-INT;
    req_2:         PHASE  0.9 +/- 0.06 OF REF2;
    comment_1:     WE SEEK A SCHEDULING THAT PLACES
    comment_2:     ECLIPSES WITHIN +/- 10 MINUTES OF
    comment_3:     THE MID-POINT OF EACH OF THE
    comment_4:     UNBLOCKED HST ORBITAL WINDOWS.

!
! end of exposure logsheet

scan_data:

    line_list:     1, 9
    fgs_scan:
    cont_dwell:    D
    dwell_pnts:    3
    dwell_secs:       1.00
    scan_width:       0.0000
    scan_length:      2.8000
    sides_angle:    90.0000
    number_lines:  1
    scan_rate:       0.0000
    first_line_pa:   0.0000
    scan_frame:    S/C
    len_offset:    1.4
    wid_offset:    0.0

!

    line_list:     1.5, 9.5
    fgs_scan:
    cont_dwell:    D
    dwell_pnts:    6
    dwell_secs:       1.00
    scan_width:       0.7000
    scan_length:      3.5000
    sides_angle:    90.0000
    number_lines:  2
    scan_rate:       0.0000
    first_line_pa:  90.0000
    scan_frame:    S/C
    len_offset:    1.75
    wid_offset:    0.35

!
! end of scan data