!  File:  4250C.PROP
!  Database:  PEPDB
!  Date:  20-FEB-1994:19:02:25

coverpage:

  title_1:         MASSIVE STARS IN STARBURST GALAXIES-FOS EXPOSURES(PART2)
    sci_cat:       STELLAR POPULATIONS
    sci_subcat:    MASSIVE STARS/BURSTS
    proposal_for:  GO
    cont_id:       3591
    pi_fname:      TIMOTHY
    pi_mi:         M.
    pi_lname:      HECKMAN
    pi_inst:       STSCI
    pi_country:    USA
    pi_phone:      301-338-7369
    hours_pri:     24.83
    num_pri:       13
    foc:           Y
    fos:           Y
    funds_amount:  268922
    funds_length:  12
    off_fname:     HERVEY
    off_mi:        S.
    off_lname:     STOCKMAN
    off_title:     DEPUTY DIRECTOR
    off_inst:      SPACE TELESCOPE SCIENCE INSTITUTE
    off_addr_1:    3700 SAN MARTIN DRIVE
    off_city:      BALTIMORE
    off_state:     MD
    off_zip:       21218
    off_country:   USA
    off_phone:     301-338-4700
! end of coverpage

abstract:

    line_1:        Starburst galaxies are ideal laboratories to study both the
    line_2:        physics of massive stars and processes important in galaxy
    line_3:        formation and evolution. Observations of these galaxies at
    line_4:        ultraviolet wavelengths are crucial to our understanding of the
    line_5:        starburst phenomenon, because only in this spectral regime can we
    line_6:        directly observe the spectroscopic signatures of the hot, massive
    line_7:        stars that power the emission at other wavebands. Indeed, we
    line_8:        believe that the investigation of the UV properties of starburst
    line_9:        galaxies is one of the most valuable tasks to be undertaken with
    line_10:       HST. We have identified what we believe to be an optimal sample of
    line_11:       the UV-brightest starburst galaxies in the local universe. These
    line_12:       span as broad a range as possible in metal abundance and starburst
    line_13:       luminosity. We describe an HST program designed to both give us a
    line_14:       broad overview of the UV properties and stellar content of
    line_15:       starbursts and to answer some important specific questions about
    line_16:       starbursts. We anticipate that observations like these will be the
    line_17:       prelude to a decade of fundamental and exciting HST research on
    line_18:       massive stars and starburst galaxies.

!
! end of abstract

general_form_proposers:

  lname:           HECKMAN
    fname:         TIMOTHY
    title:         PI
    mi:            M.
    inst:          STSCI
    country:       USA

!

  lname:           GARNETT
    fname:         DON
    inst:          STSCI
    country:       USA

!

  lname:           KINNEY
    fname:         ANNE
    inst:          STSCI
    country:       USA

!

  lname:           LEITHERER
    fname:         CLAUS
    inst:          STSCI
    country:       USA
    esa:           Y

!

  lname:           ROBERT
    fname:         CARMELLE
    inst:          STSCI
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        2
    section:       1
    line_1:

!

  question:        3
    section:       1
    line_1:        We will obtain an image of the UV continuum of each of the 9 galaxies.
    line_2:        We will use the FOC in the f/48 mode with the F140W filter, combined
    line_3:        with the F130LP to block geocoronal Ly-Alpha. These images will have
    line_4:        scientific value on their own, and will be used to select targets
    line_5:        for the FOS spectroscopy based on adequate surface brightness in a
    line_6:        1x1 arcsec region and a structure that will not confuse the FOS
    line_7:        peak-up algorthm. After inspecting the FOC images we will select a
    line_8:        subset of the sample for FOS spectroscopy. For each selected galaxy
    line_9:        we will obtain two spectra with the blue detector through the 1x1
    line_10:       arcsec aperture, using the G130H and G190H gratings respectively.
    line_11:       We will use the FOC images to set exposure times for the FOS spectra
    line_12:       that are adequate to produce a SNR of 25 to 1 per diode. The G130H
    line_13:       will be primarily used to measure the CIV1550 and SiIV1400 lines,
    line_14:       which are the strongest lines seen in IUE spectra of starbursts.
    line_15:       The G190H spectrum covers the HeII1640 and NIV1720 lines, which are
    line_16:       crucial diagnostics of highly evolved stars, like Wolf-Rayets. The
    line_17:       spectral resolution of about 500 km/sec will be adequate to meet
    line_18:       our scientific objectives.

!

  question:        4
    section:       1
    line_1:        The space-UV is the spectral region in which the hot, massive stars
    line_2:        that power starburst galaxies can be best directly observed. IUE
    line_3:        has too little collecting area and too poor spectral resolution
    line_4:        to discriminate between an interstellar, photospheric, or stellar
    line_5:        wind origin for the UV absorption lines seen in starbursts.

!

  question:        5
    section:       1
    line_1:        We need the FOC images to be taken in advance of the final scheduling
    line_2:        of the FOS spectral observations. The UV structures of these starbursts
    line_3:        are unknown on arcsec-scales, and we presently have only UV fluxes
    line_4:        obtained through a 10x20 arcsec aperture with IUE. In order to select
    line_5:        the optimum targets for FOS observations, and in order to calculate
    line_6:        the FOS exposure times needed to achieve our desired SNR of 25 to 1 per
    line_7:        diode through the 1x1 arcsec FOS aperture, we need to inspect the FOC
    line_8:        images prior to submitting the final exposure logsheets for the FOS.

!

  question:        6
    section:       1
    line_1:        We have no special requirements.

!

  question:        7
    section:       1
    line_1:        The FOC images will be inspected in order to select those galaxies
    line_2:        with regions of high enough surface brightness within a 1x1 arcsec
    line_3:        area to make FOS spectroscopy feasible. The derived UV fluxes in
    line_4:        these regions will be used to calculate FOS exposure times needed
    line_5:        to obtain an SNR of 25 to 1 per diode. We also plan to deconvolve the
    line_6:        FOC images. The radial velocity, equivalent width, width, and flux
    line_7:        will be measured for all detectable stellar and interstellar absorption
    line_8:        and nebular emission lines in the FOS data. The broad profiles of the
    line_9:        stellar wind lines will be compared to model profiles produced by
    line_10:       Leitherer and Robert.

!

  question:        8
    section:       1
    line_1:        We have measured coordinates for all our galaxies using GASP.
    line_2:        Comparison of these positions to radio positions available for
    line_3:        some of our galaxies indicates typical uncertainties of +/- 1 arcsec.
    line_4:        These uncertainties must arise in part because the central parts of
    line_5:        these galaxies are burned out on the POSS plates. The positions now
    line_6:        in hand are adequate to place the region of interest safely within the
    line_7:        22x22 arcsec field of the FOC. For the FOS acquisitions, we plan to
    line_8:        use the peak-up algorithm, initially within the 1.4x4.3 arcsec
    line_9:        aperture, followed by a peak-up using the 1.0 arcsec aperture. This
    line_10:       means that we need positions that are good to better
    line_11:       than +/- 0.3 arcsec. Our plan is to use ground-based CCD images
    line_12:       to locate the nuclei of these galaxies with respect to the Guide Star
    line_13:       coordinate system by measuring positions of many field stars in each
    line_14:       CCD and GASP frame. The CCD images are in hand for all but three of
    line_15:       the nine targets, and we plan to get images of the other three targets
    line_16:       within the next three months.

!

  question:        9
    section:       1
    line_1:        Program 2644 "The Environments of Starburst Galaxies" C.A. Norman (PI),
    line_2:        J.C. Blades, L. Danly, and T. Heckman (coI's). No observations for
    line_3:        this program have been obtained yet.

!

  question:        10
    section:       1
    line_1:        The data reduction and analysis will be undertaken at STScI
    line_2:        and at JHU. The extensive computer software and FOS and FOC
    line_3:        expertise available at these two institutions will be utilized (see
    line_4:        above). We will use the SDA ('Science Data Analyst') pool at STScI
    line_5:        to assist us in the data reduction and analysis. STScI will pay 25 percent
    line_6:        of the salary of this person. In addition, at least one JHU graduate
    line_7:        student (supported by other contract funds) will be involved in the
    line_8:        portion of the project dealing with interstellar absorption lines.

!
!end of general form text

general_form_address:

  lname:           HECKMAN
    fname:         TIMOTHY
    mi:            M.
    category:      PI
    inst:          STSCI
    addr_1:        3700 SAN MARTIN DRIVE
    city:          BALTIMORE
    state:         MD
    zip:           21218
    country:       USA
    phone:         301-338-7369

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        NGC1705
    descr_1:       E,318,928
    pos_1:         RA=04H 54M 13.4S +/- 0.1S,
    pos_2:         DEC=-53D 21' 38.9" +/-1.0"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxval_1:     F(1500)=1.5 E-14,
    fluxval_2:     F(3000)=3.7 E-15

!

    targnum:       2
    name_1:        NGC3690
    descr_1:       E,318,928
    pos_1:         RA=11H 28M 30.8S +/- 0.1S,
    pos_2:         DEC=+58D 33' 43.0" +/-1.0"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxval_1:     F(1500)=1.8 E-15,
    fluxval_2:     F(3000)=8.0 E-16

!

    targnum:       3
    name_1:        NGC4670
    descr_1:       E,318,928
    pos_1:         RA=12H 45M 17.2S +/- 0.1S,
    pos_2:         DEC=+27D 07' 32.2" +/-1.0"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxval_1:     F(1500)=5.5 E-15,
    fluxval_2:     F(3000)=2.0 E-15

!

    targnum:       4
    name_1:        NGC7552
    descr_1:       E,318,928
    pos_1:         RA=23H 16M 10.8S +/- 0.1S,
    pos_2:         DEC=-42D 35' 03.2" +/-1.0"
    equinox:       2000
    pos_epoch_bj:  J
    pos_epoch_yr:  1990.00
    acqpr_1:       EXT
    fluxval_1:     F(1500)=3.0 E-15,
    fluxval_2:     F(3000)=4.0 E-15

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       100.000
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    sp_element:    MIRROR
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    param_4:       SCAN-STEP-Y=1.4
    req_1:         CYCLE 2;
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!

    linenum:       101.000
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!

    linenum:       102.000
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!

    linenum:       103.000
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    req_4:         SEQ 100-105 NO GAP;

!

    linenum:       104.000
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!

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!

    linenum:       200.000
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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!

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!
! end of exposure logsheet

! No scan data records found