!  File:  4531C.PROP
!  Database:  PEPDB
!  Date:  22-FEB-1994:16:28:33

coverpage:

  title_1:         THE STELLAR CONTENT OF WOLF-RAYET GALAXIES
    title_2:       CYC3 SUPPLEMENTAL
    sci_cat:       STELLAR POPULATIONS
    sci_subcat:    YOUNG FIELD STARS
    proposal_for:  GO
    pi_title:      DR.
    pi_fname:      PETER
    pi_mi:         S.
    pi_lname:      CONTI
    pi_inst:       JILA
    pi_country:    USA
    pi_phone:      (303) 492-8497
    keywords_1:    LBV'S, WOLF-RAYET STARS, STARBURSTS
    hours_pri:     7.50
    num_pri:       18
    wf_pc:         Y
    fos:           Y
    pi_position:   ASTRONOMER
    off_fname:     LAURENCE
    off_mi:        D.
    off_lname:     NELSON
    off_title:     DIR/OCG
    off_inst:      THE REGENTS OF THE UNIVERSITY OF COLORADO
    off_addr_1:    BOX 19
    off_addr_2:    UNIVERSITY OF COLORADO
    off_city:      BOULDER
    off_state:     CO
    off_zip:       803090019
    off_country:   USA
    off_phone:     (303) 492-6221
! end of coverpage

abstract:

    line_1:        We propose to observe a comprehensive sample of Wolf-Rayet (W-R) galaxies
    line_2:        --- starburst galaxies in which broad 4686 He II emission of stellar
    line_3:        origin has been detected. These galaxies generally contain far more W-R
    line_4:        stars than the Milky Way, M31, and other normal galaxies. The
    line_5:        WFPC images and FOS spectra will be combined with optical and infrared
    line_6:        data as part of a large effort to perform a broad, systematic analysis
    line_7:        of the properties of W-R galaxies. The UV data obtained with HST will
    line_8:        provide crucial constraints on the hot star (O and W-R) populations, and
    line_9:        will lead to a better understanding of the physical conditions, initial
    line_10:       mass functions, and starburst parameters of these galaxies. The overall
    line_11:       continuum will be analyzed within the framework of evolutionary and
    line_12:       spectral synthesis models that we are developing. Quantitative
    line_13:       spectroscopy of UV resonance lines will allow us to study the hot star
    line_14:       populations in detail, and to directly measure the number of OB stars
    line_15:       within these galaxies. Our main goal is to determine which physical
    line_16:       properties of W-R galaxies (e.g., IMF slope, chemical composition, age,
    line_17:       strength and duration of the starburst) have led to the production of
    line_18:       large numbers of W-R stars. The results of this study will have
    line_19:       important implications for our understanding of W-R galaxies, and also
    line_20:       of starburst and emission-line galaxies in general.

!
! end of abstract

general_form_proposers:

  lname:           CONTI
    fname:         PETER
    title:         PI
    mi:            S.
    inst:          UNIVERSITY OF COLORADO
    country:       USA

!

  lname:           FILIPPENKO
    fname:         ALEXEI
    mi:            V.
    inst:          UNIVERSITY OF CALIFORNIA, BERKELEY
    country:       USA

!

  lname:           LEITHERER
    fname:         CLAUS
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       USA

!

  lname:           ROBERT
    fname:         CARMELLE
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       USA

!

  lname:           SARGENT
    fname:         WALLACE
    mi:            L.
    inst:          CALIFORNIA INSTITUTE OF TECHNOLOGY
    country:       USA

!

  lname:           VACCA
    fname:         WILLIAM
    mi:            D.
    inst:          UNIVERSITY OF CALIFORNIA, BERKELEY
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        We would like to obtain WFPC images of ALL of our W-R galaxies.
    line_2:        We anticipate that many if not most of our systems will contain multiple
    line_3:        knots of hot stars which will readily stand out against the overall
    line_4:        galaxy background in these wavelengths. Ground-based observations
    line_5:        suggest typical knot-sizes of approximately 3". The WFPC
    line_6:        set-up meets the following requirements: (i) large FOV; (ii) image scale
    line_7:        small enough to maximize count-rate; (iii) sampling large enough to
    line_8:        study spatial morphology; (iv) no significant red leak. The data
    line_9:        serve a threefold purpose: (i) morphology; (ii) flux measurement for
    line_10:       FOS; (iii) check for potential difficulties in the FOS target
    line_11:       acquisition.
    line_12:       We would also like to obtain FOS spectra of the brightest knots of
    line_13:       some W-R galaxies. The objects will be selected on the basis of the FOC
    line_14:       data. The scientific goal can be best achieved with the FOS and gratings
    line_15:       G130H and G190H. We intend to use the blue-side detector for both
    line_16:       gratings. The positions and the exposure times of the candidates for
    line_17:       FOS spectroscopy will be updated in order to ensure successful target
    line_18:       acquisition. A peak-up technique is used for the TA.

!

  question:        4
    section:       1
    line_1:
    line_3:        It is the combination of the superior resolution (IUE: 6A; FOS: 3A for
    line_4:        a knot of 2-3") and vastly better S/N (IUE: typically 10; FOS: 35 for
    line_5:        our proposed observations) of HST data which provide a dramatic
    line_6:        improvement. STRONG lines (like C IV) can be modeled quantitatively
    line_7:        with HST, and WEAKER lines (like N IV 1718, which is an important
    line_8:        signature of hot EVOLVED stars) can only be detected with HST, in
    line_9:        contrast to IUE.

!

  question:        5
    section:       1
    line_1:        None.

!

  question:        6
    section:       1
    line_1:        No special calibrations are requested.

!

  question:        7
    section:       1
    line_1:        The general management of the observations (including the ground
    line_2:        observations) and the data reduction and interpretation will be
    line_3:        coordinated by Peter Conti.
    line_4:        Reduction of the images with deconvolution techniques will be done
    line_5:        under P. Conti's supervision at JILA utilizing a graduate student RA.
    line_6:        FOS deconvolution will be carried out by Claus Leitherer. P. Conti is
    line_7:        also in charge of the pre-analysis of the HST observations (line
    line_8:        identification, interstellar extinction...). Other observations from
    line_9:        the ground are to be acquired, reduced and analysed by A. Filippenko,
    line_10:       Sargent and W. Vacca.
    line_11:       The population synthesis models will be done at STScI by Carmelle
    line_12:       Robert and Claus Leitherer. All co-Is will be intimately involved with
    line_13:       data analysis and interpretation.

!

  question:        8
    section:       1
    line_1:        The HST observations are supported by ground-based observations. There
    line_2:        is no need for simultaneous observations.

!
!end of general form text

general_form_address:

  lname:           CONTI
    fname:         PETER
    mi:            S
    title:         DR.
    category:      PI
    inst:          JILA/UNIV. OF COLORADO
    addr_1:        CAMPUS BOX 440
    city:          BOULDER
    state:         CO
    zip:           80309
    country:       USA
    phone:         (303) 492-8497
    telex:         755842 JILA

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        NGC1614
    descr_1:       E,318,928
    pos_1:         RA=4H 33M 59.6S +/- 0.1S,
    pos_2:         DEC=-8D 34' 46.2" +/-1"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxnum_1:     1
    fluxval_1:     V=14.0 +/- 1.0

!

    targnum:       2
    name_1:        MRK1087
    descr_1:       E,318,928
    pos_1:         RA=4H 49M 44.4S +/- 0.1S,
    pos_2:         DEC=+3D 20' 02.5" +/-1"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxnum_1:     1
    fluxval_1:     V=15.0 +/- 1.0

!

    targnum:       3
    name_1:        NGC1741
    descr_1:       E,318,928
    pos_1:         RA=5H 01M 37.7S +/- 0.1S,
    pos_2:         DEC=-4D 15' 31.4" +/-1"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxnum_1:     1
    fluxval_1:     V=14.0 +/- 1.0

!

    targnum:       7
    name_1:        HE2-10
    descr_1:       E,318,928
    pos_1:         RA=8H 36M 15.1S +/- 0.1S,
    pos_2:         DEC=-26D 24' 34.1" +/-1"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxnum_1:     1
    fluxval_1:     F(2200)= 2.5 E-15

!

    targnum:       8
    name_1:        MRK1236
    descr_1:       E,318,928
    pos_1:         RA=9H 49M 54.1S +/- 0.1S,
    pos_2:         DEC=+00D 36' 58.1" +/-1"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxnum_1:     1
    fluxval_1:     V=14.0 +/- 1.0

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       100.000
    targname:      HE2-10
    config:        FOS/BL
    opmode:        ACQ/PEAK
    aperture:      4.3
    sp_element:    MIRROR
    num_exp:       1
    time_per_exp:  1.0S
    priority:      1
    param_1:       TYPE=UP
    param_2:       SEARCH-SIZE-X=1
    param_3:       SEARCH-SIZE-Y=3
    param_4:       SCAN-STEP-Y=1.4
    req_1:         CYCLE 3;
    req_4:         ONBOARD ACQ FOR 101;

!

    linenum:       101.000
    targname:      HE2-10
    config:        FOS/BL
    opmode:        ACQ/PEAK
    aperture:      1.0
    sp_element:    MIRROR
    num_exp:       1
    time_per_exp:  2.0S
    priority:      1
    param_1:       TYPE=UP
    param_2:       SEARCH-SIZE-X=6
    param_3:       SEARCH-SIZE-Y=2
    param_4:       SCAN-STEP-X=0.7
    param_5:       SCAN-STEP-Y=0.7
    req_1:         CYCLE 3;
    req_4:         ONBOARD ACQ FOR 102

!

    linenum:       102.000
    targname:      HE2-10
    config:        FOS/BL
    opmode:        ACQ/PEAK
    aperture:      0.5
    sp_element:    MIRROR
    num_exp:       1
    time_per_exp:  4.0S
    priority:      1
    param_1:       TYPE=UP
    param_2:       SEARCH-SIZE-X=3
    param_3:       SEARCH-SIZE-Y=3
    param_4:       SCAN-STEP-X=0.35
    param_5:       SCAN-STEP-Y=0.35
    req_1:         CYCLE 3;
    req_4:         ONBOARD ACQ FOR 103-105;

!

    linenum:       103.000
    targname:      HE2-10
    config:        FOS/BL
    opmode:        ACCUM
    aperture:      1.0
    sp_element:    G130H
    num_exp:       1
    time_per_exp:  9300S
    priority:      1
    req_1:         CYCLE 3;
    req_4:         SEQ 100-105 NO GAP;

!

    linenum:       104.000
    targname:      HE2-10
    config:        FOS/BL
    opmode:        ACCUM
    aperture:      1.0
    sp_element:    G190H
    num_exp:       1
    time_per_exp:  4000S
    priority:      1
    req_1:         CYCLE 3;

!

    linenum:       105.000
    targname:      HE2-10
    config:        FOS/BL
    opmode:        ACQ
    aperture:      4.3
    sp_element:    MIRROR
    num_exp:       1
    time_per_exp:  300S
    priority:      1
    req_1:         CYCLE 3;
    comment_4:     IMAGE TO LOCATE THE APERTURE;

!

    linenum:       200.000
    targname:      NGC1614
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F439W
    num_exp:       1
    time_per_exp:  20M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SEQ 200-202 NO GAP

!

    linenum:       201.000
    targname:      NGC1614
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F555W
    num_exp:       1
    time_per_exp:  15M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;

!

    linenum:       202.000
    targname:      NGC1614
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F785LP
    num_exp:       1
    time_per_exp:  10M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SAME ORIENT FOR 201,202 AS 200;

!

    linenum:       300.000
    targname:      NGC1741
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F439W
    num_exp:       1
    time_per_exp:  20M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SEQ 300-302 NO GAP

!

    linenum:       301.000
    targname:      NGC1741
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F555W
    num_exp:       1
    time_per_exp:  15M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;

!

    linenum:       302.000
    targname:      NGC1741
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F785LP
    num_exp:       1
    time_per_exp:  10M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SAME ORIENT FOR 301,302 AS 300;

!

    linenum:       400.000
    targname:      HE2-10
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F439W
    num_exp:       1
    time_per_exp:  20M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SEQ 400-402 NO GAP

!

    linenum:       401.000
    targname:      HE2-10
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F555W
    num_exp:       1
    time_per_exp:  15M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;

!

    linenum:       402.000
    targname:      HE2-10
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F785LP
    num_exp:       1
    time_per_exp:  10M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SAME ORIENT FOR 401,402 AS 400;

!

    linenum:       500.000
    targname:      MRK1236
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F439W
    num_exp:       1
    time_per_exp:  20M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SEQ 500-502 NO GAP

!

    linenum:       501.000
    targname:      MRK1236
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F555W
    num_exp:       1
    time_per_exp:  15M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;

!

    linenum:       502.000
    targname:      MRK1236
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F785LP
    num_exp:       1
    time_per_exp:  10M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SAME ORIENT FOR 501,502 AS 500;

!

    linenum:       600.000
    targname:      MRK1087
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F439W
    num_exp:       1
    time_per_exp:  20M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SEQ 600-602 NO GAP

!

    linenum:       601.000
    targname:      MRK1087
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F555W
    num_exp:       1
    time_per_exp:  15M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;

!

    linenum:       602.000
    targname:      MRK1087
    config:        PC
    opmode:        IMAGE
    aperture:      PCALL
    sp_element:    F785LP
    num_exp:       1
    time_per_exp:  10M
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 3;
    req_2:         SAME ORIENT FOR 601,602 AS 600;

!
! end of exposure logsheet

! No scan data records found