!  File:  4171C.PROP
!  Database:  PEPDB
!  Date:  20-FEB-1994:12:01:02

coverpage:

  title_1:         GLOBULAR CLUSTER CORES, WFPC GTO AUGMENTATION,
    title_2:       CYCLE 3
    sci_cat:       STELLAR POPULATIONS
    proposal_for:  AUG/WFC
    cont_id:       3640
    pi_title:      PROF.
    pi_fname:      JAMES
    pi_mi:         A.
    pi_lname:      WESTPHAL
    pi_inst:       CALTECH
    pi_country:    USA
    pi_phone:      (818) 356-4900
    keywords_1:    GLOBULAR CLUSTERS
    hours_pri:     13.76
    num_pri:       5
    pi_position:   PROF. PLANETARY SCI.
! end of coverpage

abstract:

    line_1:        Stellar Populations Part III: Globular Cluster Cores.  The cores
    line_2:        of 4 globular clusters will be imaged in U to study core properties
    line_3:        and search for collapsed cusps.  The clusters are relatively nearby
    line_4:        and span the range from very regular to very cusplike.

!
! end of abstract

general_form_proposers:

  lname:           WESTPHAL
    fname:         JAMES
    mi:            A.
    inst:          CALTECH
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        All observations of the four globular clusters will consist of
    line_2:        F336W exposures, each split into two equal-length exposures to
    line_3:        facilitate the removal of cosmic rays.
    line_5:        For each of the four clusters, three 2200 second C-R split observa-
    line_6:        tions will be taken at each of two slightly different pointings.
    line_7:        The slightly different pointings will provide the data necessary to
    line_8:        compensate for anticipated calibration problems with the data.
    line_9:        For three of the four clusters (all except M15), one 800 second C-R
    line_10:       split observation will be taken to safeguard against the possibility
    line_11:       of an unusually bright star saturating the Planetary Camera.
    line_12:       For each cluster, all useful data will be combined to improve the
    line_13:       signal-to-noise ratio of the data.

!

  question:        4
    section:       1
    line_1:        Many groundbased observations of galactic globular cluster cores
    line_2:        have been taken during the past few decades.  Atmospheric seeing has
    line_3:        limited the resolution of the detailed nature of these cluster cores.
    line_4:        By being outside the bulk of the Earth's atmosphere, the HST can
    line_5:        produce observations that have finer resolution than is routinely
    line_6:        obtainable at groundbased observatories.  The scientific yield of
    line_7:        this finer resolution has been demonstrated by the analysis of the
    line_8:        SAO observations of the center of the glactic globular cluster M15
    line_9:        (see section 8a, 8b, and 8c of this proposal).

!

  question:        7
    section:       1
    line_1:        The following analysis will be performed individual image, after
    line_2:        having removed the cosmic rays indicated by comparison of all images.
    line_3:        This analysis will also be performed on the registered and
    line_4:        summed image.
    line_6:        1) Construct an observationally determined point-spread-function (PSF)
    line_7:        from isolated stars in the field.  2) Locate the bright resolved
    line_8:        stars near the cluster center, map their locations, determine their
    line_9:        distribution, fit a scaled PSF model to them and remove them from
    line_10:       the image.  3) Use the PSF to deconvolve the difference image (i.e.
    line_11:       with the bright stars near the center removed) and fit a power-law
    line_12:       model to the core.  4) Use the result of the above fit as a starting
    line_13:       point for iteratively fitting a convolved power-law model to the
    line_14:       original (i.e. not deconvolved) residual core image.  5)  Determine
    line_15:       the center of the cluster in terms of the center of the bright
    line_16:       resolved star component, the residual core component, and the total
    line_17:       light distribution.  6) Note the morphology and coincidence of the
    line_18:       above centers.  7) Compare WFPC data with groundbased data.
    line_19:       Finally, look for comparable trends between clusters.

!

  question:        8
    section:       1
    line_1:        All of the 2200s exposures given in the GC800 and GC2000
    line_2:        sequences may be adjusted by +/- 20 percent in order to
    line_3:        fit within one orbit.  However, the CR-split level must
    line_4:        remain equal when adjusting times as needed.

!
!end of general form text

general_form_address:

  lname:           O'NEIL
    fname:         EARL
    mi:            J.
    category:      CON
    inst:          NOAO/KPNO
    addr_1:        950 N. CHERRY
    addr_2:        P.O. BOX 26732
    city:          TUCSON
    state:         AZ
    zip:           85726
    country:       USA
    phone:         (602) 327-5511

!

  lname:           WESTPHAL
    fname:         JAMES
    mi:            A.
    title:         PROF.
    category:      PI
    inst:          CALTECH
    addr_1:        M/S 170-25
    addr_2:        DIVISION OF GEOLOGICAL
    addr_3:        & PLANETARY SCIENCES
    city:          PASADENA
    state:         CA
    zip:           91125
    country:       USA
    phone:         (818) 356-4900

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        NGC5272-M3
    descr_1:       C, 201
    pos_1:         RA= 13H39M52.9S +/-0.1S,
    pos_2:         DEC= +28D37'38" +/-1"
    equinox:       1950.0
    fluxnum_1:     1
    fluxval_1:     SURF(V)=16.3

!

    targnum:       2
    name_1:        NGC5272-OFF
    descr_1:       C, 201
    pos_1:         RA= 13H39M52.9S +/-0.1S,
    pos_2:         DEC= +28D37'28" +/-1"
    equinox:       1950.0
    fluxnum_1:     1
    fluxval_1:     SURF(V)=16.3

!

    targnum:       3
    name_1:        NGC6752
    descr_1:       C, 201
    pos_1:         RA= 19H06M27.3S +/-0.1S,
    pos_2:         DEC= -60D03'50" +/-1"
    equinox:       1950.0
    comment_1:     B-V=0.68 ALSO FOR FLUX DATA
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 16.2

!

    targnum:       4
    name_1:        NGC6752-OFF
    descr_1:       C, 201
    pos_1:         RA= 19H06M27.3S +/-0.1S,
    pos_2:         DEC= -60D03'40" +/-1"
    equinox:       1950.0
    comment_1:     B-V=0.68 ALSO FOR FLUX DATA
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 16.2

!

    targnum:       5
    name_1:        NGC7078-M15
    descr_1:       C, 201
    pos_1:         RA= 21H27M33.3S +/-0.1S,
    pos_2:         DEC= +11D56'49" +/-1"
    equinox:       1950.0
    comment_1:     B-V=0.68 ALSO FOR FLUX DATA
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 13.5

!

    targnum:       6
    name_1:        NGC7078-OFF
    descr_1:       C, 201
    pos_1:         RA= 21H27M33.3S +/-0.1S,
    pos_2:         DEC= +11D56'39" +/-1"
    equinox:       1950.0
    comment_1:     B-V=0.68 ALSO FOR FLUX DATA
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 13.5

!

    targnum:       7
    name_1:        NGC6341-M92
    descr_1:       C, 201
    pos_1:         RA= 17H15M35.0S +/-0.1S,
    pos_2:         DEC= +43D11'21" +/-1"
    equinox:       1950.0
    comment_1:     B-V=0.68 ALSO FOR FLUX DATA
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 15.4

!

    targnum:       8
    name_1:        NGC6341-OFF
    descr_1:       C, 201
    pos_1:         RA= 17H15M35.0S +/-0.1S,
    pos_2:         DEC= +43D11'11" +/-1"
    equinox:       1950.0
    comment_1:     B-V=0.68 ALSO FOR FLUX DATA
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 15.4

!

    targnum:       9
    name_1:        BD+75D325
    descr_1:       A, 105, 704
    pos_1:         RA = 08H 10M 49.31S +/- 1S,
    pos_2:         DEC = +74D 57' 57.5" +/- 1",
    equinox:       2000
    comment_1:     UV STANDARD; SP.TYPE = O5P;
    comment_2:     FOR USE WITH NGC 5272 OBS
    fluxnum_1:     1
    fluxval_1:     V = 9.54

!

    targnum:       10
    name_1:        BD+28D4211
    descr_1:       A, 105, 704
    pos_1:         RA = 21H 51M 11.07S +/- 1S,
    pos_2:         DEC = +28D 51' 51.8" +/- 1",
    equinox:       2000
    comment_1:     UV STANDARD; SP.TYPE = OP;
    comment_2:     FOR USE WITH NGC 7078 OBS
    fluxnum_1:     1
    fluxval_1:     V = 10.51

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    sequence_1:    DEFINE
    sequence_2:    GC800
    targname:      #
    config:        PC
    opmode:        IMAGE
    aperture:      PC6
    sp_element:    F336W
    num_exp:       1
    time_per_exp:  800S
    priority:      #
    param_1:       CR-SPLIT=0.5,
    param_2:       CR-TOLERANCE=0.0,
    param_3:       PRE-FLASH=YES
    req_1:         NON-INT / 1-2;
    req_2:         GROUP 1-2 WITHIN 1D;
    req_3:         PCS MODE C / 1-2
    comment_1:     GTO AUGMENTATION, CYCLE 3
    comment_2:     EJO/RML  3/18/92

!

    linenum:       2.000
    sequence_1:    ^
    targname:      #
    config:        PC
    opmode:        IMAGE
    aperture:      PC6
    sp_element:    F336W
    num_exp:       3
    time_per_exp:  2200S
    priority:      #
    param_1:       CR-SPLIT=0.5,
    param_2:       CR-TOLERANCE=0.0,
    param_3:       PRE-FLASH=YES
    req_1:         SAME POS FOR 2 AS 1;
    req_2:         SAME ORIENT FOR 2 AS 1
    comment_1:     EACH OF 3 EXP INTENDED TO FIT WITHIN
    comment_2:     ONE ORBIT. MODIFY THE 2200S EXP TIME
    comment_3:     +/- 20 PERCENT TO ACCOMPLISH THIS,
    comment_4:     BUT RESPECT THE EQUAL CR SPLIT.

!

    linenum:       5.000
    sequence_1:    DEFINE
    sequence_2:    GC2200
    targname:      #
    config:        PC
    opmode:        IMAGE
    aperture:      PC6
    sp_element:    F336W
    num_exp:       1
    time_per_exp:  2200S
    priority:      #
    param_1:       CR-SPLIT=0.5,
    param_2:       CR-TOLERANCE=0.0,
    param_3:       PRE-FLASH=YES
    req_1:         NON-INT;
    req_2:         PCS MODE C
    comment_1:     THIS EXPOSURE INTENDED TO FIT WITHIN
    comment_2:     ONE ORBIT. MODIFY THE 2200S EXP TIME
    comment_3:     +/- 20 PERCENT TO ACCOMPLISH THIS,
    comment_4:     BUT RESPECT THE EQUAL CR SPLIT.

!

    linenum:       21.000
    sequence_1:    USE
    sequence_2:    GC800
    targname:      NGC7078-M15
    priority:      1
    req_1:         GROUP 21-23 WITHIN 3D;
    req_2:         CYCLE 3 / 21-25

!

    linenum:       21.500
    sequence_1:    USE
    sequence_2:    GC2200
    targname:      NGC7078-M15
    priority:      1
    req_1:         SAME ORIENT FOR 21.5-22 AS 21

!

    linenum:       22.000
    sequence_1:    USE
    sequence_2:    GC800
    targname:      NGC7078-OFF
    priority:      1

!

    linenum:       23.000
    targname:      BD+28D4211
    config:        PC
    opmode:        IMAGE
    aperture:      PC6
    sp_element:    F336W
    num_exp:       2
    time_per_exp:  10S
    priority:      1
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES
    req_1:         PCS MODE C
    comment_1:     PSF STAR FOR M15 OBSERVATION;
    comment_2:     TO BE GROUPED WITH CLUSTER OBS

!

    linenum:       24.000
    sequence_1:    USE
    sequence_2:    GC800
    targname:      NGC6341-M92
    priority:      1
    req_1:         GROUP 24-25 WITHIN 1D

!

    linenum:       25.000
    sequence_1:    USE
    sequence_2:    GC800
    targname:      NGC6341-OFF
    priority:      1
    req_1:         SAME ORIENT FOR 25 AS 24

!
! end of exposure logsheet

! No scan data records found