!  File:  4056C.PROP
!  Database:  PEPDB
!  Date:  20-FEB-1994:06:49:49

coverpage:

  title_1:         BINARIES IN GLOBULAR CLUSTERS AUGMENTATION: CYCLE 2 OBSERVATIONS
    sci_cat:       STELLAR ASTROPHYSICS
    proposal_for:  AUG/FOS
    cont_id:       3651
    pi_title:      PROF.
    pi_fname:      BRUCE
    pi_lname:      MARGON
    pi_inst:       WASHINGTON, UNIVERSITY OF
    pi_country:    USA
    pi_phone:      206-543-0089
    hours_pri:     2.68
    num_pri:       1
    fos:           Y
! end of coverpage

abstract:

    line_1:        The pre-launch FOS GTO program proposed a systematic study of degenerate stars
    line_2:        in binary systems, both in the field and in globular clusters, plus a handful
    line_3:        of related objects. For the isolated field systems, the emphasis is on spectro-
    line_4:        photometry (in many cases time-resolved over a pulse or orbital period) and
    line_5:        spectropolarimetry, to observe the effects of the intense ionizing flux emitted
    line_6:        by the compact object on the nearby normal star and/or accretion disk. While
    line_7:        some such effects are seen from the ground, they should be far more spectacular
    line_8:        in the UV. The GTO program for the globular cluster systems typically proposes
    line_9:        WF/PC or FOC images to locate candidates for cluster X-ray sources, followed by
    line_10:       confirming FOS spectroscopy. Our published FOC observations of M14 show that
    line_11:       even with the primary's spherical aberration, it is possible to reach flux
    line_12:       levels relevant to these problems with angular resolution far better than
    line_13:       achievable from the ground. Even one or two new close binaries identified
    line_14:       through this program will be extremely important, as these systems are thought
    line_15:       to dominate the kinetic energy budget of globular clusters, yet virtually none
    line_16:       are currently known. Also proposed for augmentation are two related programs:
    line_17:       FOS observations of the Crab pulsar and a study of UV-bright objects in
    line_18:       globular cluster cores. The increased FOS integration times caused by the
    line_19:       spherical aberration have drastically disrupted the original intended
    line_20:       scientific program; augmentation proposed here partially restores these efforts.

!
! end of abstract

general_form_proposers:

  lname:           MARGON
    fname:         BRUCE
    inst:          UNIVERSITY OF WASHINGTON
    country:       USA

!

  lname:           HARMS
    fname:         RICHARD
    title:         PI
    mi:            J.
    inst:          APPLIED RESEARCH CORPORATION
    country:       USA

!

  lname:           BOHLIN
    fname:         RALPH
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       USA

!

  lname:           ANGEL
    fname:         J. ROGER
    mi:            P.
    inst:          UNIVERSITY OF ARIZONA
    country:       USA

!

  lname:           BARTKO
    fname:         FRANK
    inst:          UNIVERSITY OF CALIFORNIA, SAN DIEGO
    country:       USA

!

  lname:           BEAVER
    fname:         EDWARD
    inst:          UNIVERSITY OF CALIFORNIA, SAN DIEGO
    country:       USA

!

  lname:           BURBIDGE
    fname:         E. MARGARET
    inst:          UNIVERSITY OF CALIFORNIA, SAN DIEGO
    country:       USA

!

  lname:           DAVIDSEN
    fname:         ARTHUR
    mi:            F.
    inst:          JOHNS HOPKINS UNIVERSITY
    country:       USA

!

  lname:           FORD
    fname:         HOLLAND
    mi:            C.
    inst:          JOHNS HOPKINS UNIVERSITY
    country:       USA

!

  lname:           HARTIG
    fname:         GEORGE
    mi:            F.
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       USA

!

  lname:           ANDERSON
    fname:         SCOTT
    mi:            F.
    inst:          UNIVERSITY OF WASHINGTON
    country:       USA

!

  lname:           DOWNES
    fname:         RONALD
    mi:            A.
    inst:          NASA GODDARD SPACE FLIGHT CENTER
    country:       USA

!

  lname:           ALLEN
    fname:         RICHARD
    mi:            P.
    inst:          UNIVERSITY OF ARIZONA
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        2
    section:       1
    line_1:

!

  question:        3
    section:       1
    line_1:        WF/PC images of globular cluster interacting binaries will
    line_2:        be obtained as acquistions for follow-up FOS spectra in
    line_3:        cycle 3. If no interesting candidates are found, no
    line_4:        followup spectra will be taken. If an interesting looking
    line_5:        candidate is found, then follow-up spectra will be obtained
    line_6:        in a later cycle, with the specific gratings to be used
    line_7:        determined by the quality of the candidate.

!

  question:        4
    section:       1
    line_1:        For this program, it is the high angular resolution of the
    line_2:        HST which is most essential, although the UV capability is
    line_3:        also exploited. The PC images will be used to search
    line_4:        relatively crowded regions of Omega-Cen with the aim of
    line_5:        optically selecting (via UV excess) a candidate for the
    line_6:        globular cluster X-ray source. Follow-up FOS spectroscopy
    line_7:        will be done in a later cycle if a suitable candidate is found.

!

  question:        5
    section:       1
    line_1:        The images must be obtained NON-INT to avoid unecessary
    line_2:        readout noise in these low S/N data

!

  question:        7
    section:       1
    line_1:        Data reduction will be performed at the ST ScI, and the analysis will be
    line_2:        performed using FOS IDT computer facilities. As a quick-look analysis,
    line_3:        the PC multicolor images will simply be displayed and blinked to provide
    line_4:        an initial search for candidates of unusual color. A more detailed
    line_5:        examination of the images will come from DAOPHOT and DoPHOT (plus aperture)
    line_6:        photometry of all of the stars.

!

  question:        8
    section:       1
    line_1:        The PC images will be measured for precise target coordinates, so that the
    line_2:        later FOS observations can be done as blind offsets from a nearby isolated
    line_3:        star.

!

  question:        9
    section:       1
    line_1:        Partial data from about a dozen different FOS/GTO programs (and many
    line_2:        OV and SV proposals) have been obtained to date. This proposal includes
    line_3:        augmentation time related to the following FOS/GTO and SAO proposals
    line_4:        1053, 3002, 3003, 3198, 3282 (Binaries in Globular Clusters);
    line_5:        Among these related programs, data have been taken for SAO
    line_6:        observations of M14 (proposals 3002 and 3003), and NGC6712 (proposal
    line_7:        1053). One relevant refereed paper has been published in ApJ Let.

!

  question:        10
    section:       1
    line_1:        Data analysis, research assistant support, and funding will be provided under
    line_2:        NASA's FOS GTO contract(s). The FOS IDT support includes a total of roughly
    line_3:        30 Ph.D. astronomers and graduate students at 5 different institutions. At
    line_4:        each institution one or more workstations (typically Sparc 2's or the
    line_5:        equivalent), plus one or more Microvaxes (or equivalent) are essentially
    line_6:        devoted to processing of HST data.

!

  question:        13
    section:       1
    line_1:        Multicolor WF/PC images will be used to search for the optical counterparts of
    line_2:        both central and noncentral X-ray sources. Objects identified through unusual
    line_3:        colors will be observed with the FOS.

!
!end of general form text

general_form_address:

  lname:           MARGON
    fname:         BRUCE
    category:      PI
    inst:          UNIVERSITY OF WASHINGTON
    addr_1:        ASTRONOMY DEPARTMENT, FM-20
    city:          SEATTLE
    state:         WA
    zip:           98195
    country:       USA
    phone:         206 543-0089
    telex:         4740096

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        NGC5139
    name_2:        OMEGA-CEN
    descr_1:       C,201,I,605
    pos_1:         RA =13H 26M 15.3S+/-0.1S,
    pos_2:         DEC = -47D 06' 58" +/-1"
    equinox:       1950
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 16.7 +/-0.5

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    sequence_1:    DEFINE
    sequence_2:    PC
    targname:      #
    config:        PC
    opmode:        IMAGE
    aperture:      PC8-FIX
    sp_element:    F336W
    wavelength:    3363
    num_exp:       1
    time_per_exp:  2000S
    fluxnum_1:     1
    priority:      1
    param_1:       PRE-FLASH=YES,
    param_2:       CR-SPLIT=NO
    req_1:         SEQ 1-3 NO GAP;
    req_2:         NON-INT / 1-3;
    req_3:         POS TARG -5.4,+5.4  / 1-3;
    comment_1:     PC PICTURES FOR SOURCE IDENTIFICATION.

!

    linenum:       2.000
    sequence_1:    DEFINE
    sequence_2:    PC
    targname:      #
    config:        PC
    opmode:        IMAGE
    aperture:      PC8-FIX
    sp_element:    F439W
    wavelength:    4385
    num_exp:       1
    time_per_exp:  2000S
    fluxnum_1:     1
    priority:      1
    param_1:       PRE-FLASH=YES,
    param_2:       CR-SPLIT=0.1

!

    linenum:       3.000
    sequence_1:    DEFINE
    sequence_2:    PC
    targname:      #
    config:        PC
    opmode:        IMAGE
    aperture:      PC8-FIX
    sp_element:    F336W
    wavelength:    3363
    num_exp:       1
    time_per_exp:  2000S
    fluxnum_1:     1
    priority:      1
    param_1:       PRE-FLASH=YES,
    param_2:       CR-SPLIT=NO

!

    linenum:       4.000
    sequence_1:    USE
    sequence_2:    PC
    targname:      NGC5139
    req_2:         CYCLE 2/ 1-4;

!
! end of exposure logsheet

! No scan data records found