!  File:  3944C.PROP
!  Database:  PEPDB
!  Date:  20-FEB-1994:01:04:36

coverpage:

  title_1:         IMAGERY AND UV SPECTROSCOPY OF GALAXIES WITH STARBURST NUCLEI
    sci_cat:       GALAXIES & CLUSTERS
    proposal_for:  GTO/HRS
    pi_title:      DR.
    pi_fname:      DENNIS
    pi_mi:         C.
    pi_lname:      EBBETS
    pi_inst:       BALL AEROSPACE CORPORATION
    pi_country:    USA
    pi_phone:      (303) 939-5964
    keywords_1:    EMISSION LINE GALAXY, NUCLEUS, INTERACTING GALAXIES,
    keywords_2:    EXTRAGALACTIC HII REGION
    hours_pri:     3.96
    num_pri:       3
    pi_position:   PRIN MEM TECH STAFF
! end of coverpage

abstract:

    line_1:        Galaxies with starburst nuclei show evidence for large populations of massive
    line_2:        hot stars existing in a small volume in the nucleus. This phenomenon may be a
    line_3:        precursor to more dramatic activity powered by the evolutionary endproducts of
    line_4:        thousands of high mass stars. Multiband images obtained with the Wide Field
    line_5:        Camera will be used to invesitgate the location, size, structure, colors and
    line_6:        luminosity of the starburst region. Ultraviolet spectroscopy with the High
    line_7:        Resolution Spectrograph will provide direct insight into the nature of the hot
    line_8:        stars.
    line_11:       cycle 2 revisions prepared and submitted May 21, 1991

!
! end of abstract

general_form_proposers:

  lname:           BALZANO
    fname:         VICKI
    inst:          COMPUTER SCIENCE CORPORATION
    country:       USA

!

  lname:           EBBETS
    fname:         DENNIS
    mi:            C.
    inst:          BALL AEROSPACE CORPORATION
    country:       USA

!

  lname:           SHARA
    fname:         MIKE
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        WFC images in four filters will be taken for each galaxy. Filter
    line_2:        F336W will show the locations of hot stars, without confusion
    line_3:        with cooler stars and gas in the galaxy. F569W is close to a
    line_4:        V band. F675W is a wide red band, which includes both continuum
    line_5:        and nebular emission lines. F664N is a narrow red filter which
    line_6:        will pass hydrogen alpha and nitrogen II at the redshift of the
    line_7:        galaxy. Two exposures with each filter allow censoring of cosmic
    line_8:        ray hits, and increases the dynamic range of the image. Together
    line_9:        the images will show the overall morphology of the galaxy,the
    line_10:       location and size of the hot star populations, and the distribution
    line_11:       of gas. The GHRS spectra will cover the wavelength interval
    line_12:       1220 A to 1785A. This will provide high quality profiles of the
    line_13:       most important tracers of massive stars, including N V, Si IV,
    line_14:       C IV, He II and N IV. The exposures have been designed to
    line_15:       minimize problems with thermal and magnetic drift, and to allow
    line_16:       a S/N of at least 25 in the continuum.

!

  question:        4
    section:       1
    line_1:        We have obtained and studied IUE spectra of 13 starburst galaxies, including
    line_2:        several included in this proposal. UV fluxes have been measured to assist with
    line_3:        exposure time estimates. The galaxies are near the limit of feasibility with
    line_4:        IUE, and the spectral line features, both stellar and interstellar, while
    line_5:        clearly present, are difficult to interpret in detail. GHRS will provide vastly
    line_6:        improved resolution and signal to noise ratio in a fraction of the IUE
    line_7:        observing time. We have also obtained CCD images from Kitt Peak and Mauna Kea.
    line_8:        Although we have many images, both observing runs were hampered by medicore
    line_9:        sky conditions. The spatial resolution and photometric precision expected from
    line_10:       WFC images will allow much more confident analysis of the size, morphlogy,
    line_11:       colors and luminosity of the starburst regions.

!

  question:        5
    section:       1
    line_1:        We request that the GHRS spectra be scheduled at least 60 days
    line_2:        after the WFC images that include the F336W exposures. This is
    line_3:        to allow us to examine the "U" band images and select the best
    line_4:        region on which to center the GHRS aperture. The GHRS target
    line_5:        acquisitions are specified as INT ACQs to allow observer selection
    line_6:        of the precise centering of the starburst in the aperture.
    line_7:        Although these knots appear to be point like in ground based
    line_8:        images, they may be extended and show structure with HST spatial
    line_9:        resolution. Such structure could cause the GHRS onboard acq
    line_10:       flight software to center up in a less than optimum way.

!

  question:        7
    section:       1
    line_1:        The WFC images will be calibrated and reduced using standard RSDP and SDAS
    line_2:        procedure.
    line_3:        The starburst regions will be analyzed in terms of location in
    line_4:        the galaxy, size, colors, luminosity, morphology and interaction with other
    line_5:        regions (neighboring galaxies?). The broad band R and narrow band H Alpha
    line_6:        images will be scaled and differenced to highlight nebular regions emitting
    line_7:        strongly in emission lines. These will serve as tracers of the ionized gas.
    line_8:        The ultraviolet images will directly show the location of hot stars.
    line_12:       The GHRS spectra will be analyzed at IDT facilities. Continuum
    line_13:       fluxes, ultraviolet luminosity, and stellar emission and absorption lines will
    line_14:       be studied. Photospheric and stellar wind line will be used as diagnostics of
    line_15:       the population of hot stars.

!

  question:        13
    section:       1
    line_1:        The star formation regions in galaxies with starburst nuclei will be studied
    line_2:        with narrow band imagery obtained with the Wide Field Camera, and ultraviolet
    line_3:        spectroscoy observed with the High Resolution Spectrograph. Images will be
    line_4:        obtained in "U", "V" and "R" band passes, and through an
    line_5:        appropriate H Alpha filter. Spectroscopy with a resolving power near 2000 and
    line_6:        signal to noise ratio of 25 will be obtained in the 1200 to 1800A region. The
    line_7:        size, morphology, environment, stellar content and luminosity of the starburst
    line_8:        regions will be studied.

!
!end of general form text

general_form_address:

  lname:           SHARA
    fname:         MIKE
    category:      CON
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    addr_1:        3700 SAN MARTIN DRIVE
    addr_2:        HOMEWOOD CAMPUS
    city:          BALTIMORE
    state:         MD
    zip:           21218
    country:       USA
    phone:         (301) 338-4743
    telex:         6849101

!

  lname:           EBBETS
    fname:         DENNIS
    mi:            C.
    title:         DR.
    category:      PI
    inst:          BALL AEROSPACE CORPORATION
    addr_1:        GHRS PROJECT AR1
    addr_2:        P.O. BOX 1062
    city:          BOULDER
    state:         CO
    zip:           80306
    country:       USA
    phone:         (303) 939-5964

!

  lname:           BALZANO
    fname:         VICKI
    category:      CON
    inst:          COMPUTER SCIENCE CORPORATION
    addr_1:        SPACE TELESCOPE SCIENCE INSTITUTE
    addr_2:        3700 SAN MARTIN DRIVE
    addr_3:        HOMEWOOD CAMPUS
    city:          BALTIMORE
    state:         MD
    zip:           21218
    country:       USA
    phone:         (301) 338-4736
    telex:         6849101

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        MK799NUC
    name_2:        NGC5430
    descr_1:       NUCLEUS OF BARRED SPIRAL
    pos_1:         RA = 14H 00M 45.904S+/-0.1",
    pos_2:         DEC = +59D 19' 40.77"+/-0.1"
    equinox:       J2000
    pm_or_par:     NO
    rv_or_z:       Z=.011
    fluxnum_1:     1
    fluxval_1:     B=15.8 +/- 0.2
    fluxnum_2:     2
    fluxval_2:     F(1500)=2 +/- 0.5 E-14

!

    targnum:       2
    name_1:        MK799HII
    descr_1:       HII REGION AT END OF BAR
    pos_1:         RA = 14H 00M 47.109S+/-0.1",
    pos_2:         DEC = +59D 19' 27.43"+/-0.1"
    equinox:       J2000
    pm_or_par:     NO
    rv_or_z:       Z=0.011
    fluxnum_1:     1
    fluxval_1:     F(1500)=2 +/- 0.5 E-14

!

    targnum:       3
    name_1:        NGC7714
    descr_1:       SPIRAL GALAXY
    pos_1:         RA = 23H 36M 14.303S+/-0.1",
    pos_2:         DEC = +02D 09' 17.38"+/-0.1"
    equinox:       J2000
    pm_or_par:     NO
    rv_or_z:       Z=.0096
    comment_1:     ALL COORDINATES MEASURED BY
    comment_2:     ARCHIE WARNOCK USING GASP
    fluxnum_1:     1
    fluxval_1:     V=13.1 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     F(1500)=4 E-14

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       10.000
    sequence_1:    DEFINE
    sequence_2:    WFCIMG
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F336W
    num_exp:       1
    time_per_exp:  20S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       20.000
    sequence_1:    DEFINE
    sequence_2:    WFCIMG
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F336W
    num_exp:       1
    time_per_exp:  100S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       30.000
    sequence_1:    DEFINE
    sequence_2:    WFCIMG
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F569W
    num_exp:       1
    time_per_exp:  1S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       40.000
    sequence_1:    DEFINE
    sequence_2:    WFCIMG
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F569W
    num_exp:       1
    time_per_exp:  5S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       50.000
    sequence_1:    DEFINE
    sequence_2:    WFCRED
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F675W
    num_exp:       1
    time_per_exp:  5S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       60.000
    sequence_1:    DEFINE
    sequence_2:    WFCRED
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F675W
    num_exp:       1
    time_per_exp:  25S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       70.000
    sequence_1:    DEFINE
    sequence_2:    WFCRED
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F664N
    num_exp:       1
    time_per_exp:  20S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       80.000
    sequence_1:    DEFINE
    sequence_2:    WFCRED
    targname:      #
    config:        WFC
    opmode:        IMAGE
    aperture:      ALL
    sp_element:    F664N
    num_exp:       1
    time_per_exp:  100S
    s_to_n:        100
    fluxnum_1:     #
    priority:      #
    param_1:       CR-SPLIT=NO,
    param_2:       PRE-FLASH=YES,

!

    linenum:       100.000
    sequence_1:    USE
    sequence_2:    WFCRED
    targname:      NGC7714
    time_per_exp:  X1.5
    fluxnum_1:     1
    priority:      3
    req_1:         CYCLE 2

!

    linenum:       200.000
    sequence_1:    USE
    sequence_2:    WFCIMG
    targname:      MK799NUC
    time_per_exp:  X5
    fluxnum_1:     1
    priority:      3
    req_1:         CYCLE 2 / 200-210;
    req_2:         EARLY ACQ FOR 400;
    req_3:         COND IF TAC OK;

!

    linenum:       210.000
    sequence_1:    USE
    sequence_2:    WFCRED
    targname:      MK799NUC
    time_per_exp:  X5
    fluxnum_1:     1
    priority:      3
    req_1:         COND IF TAC OK;

!

    linenum:       400.000
    targname:      MK799HII
    config:        HRS
    opmode:        ACQ
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  25.0S
    fluxnum_1:     1
    priority:      1
    param_1:       FAINT=100,
    param_2:       SEARCH-SIZE=5,
    req_1:         ONBOARD ACQ FOR 405-440;
    req_2:         CYCLE 2 / 400-440;
    req_3:         COND IF TAC OK;

!

    linenum:       405.000
    targname:      MK799HII
    config:        HRS
    opmode:        ACQ/PEAKUP
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  46S
    fluxnum_1:     1
    priority:      1
    req_1:         COND IF TAC OK;

!

    linenum:       410.000
    targname:      MK799HII
    config:        HRS
    opmode:        IMAGE
    aperture:      2.0
    sp_element:    MIRROR-N2
    num_exp:       1
    time_per_exp:  256S
    s_to_n:        5
    fluxnum_1:     1
    priority:      3
    param_1:       NX=16,
    param_2:       NY=16,
    req_1:         COND IF TAC OK;

!

    linenum:       420.000
    targname:      MK799HII
    config:        HRS
    opmode:        IMAGE
    aperture:      2.0
    sp_element:    MIRROR-N1
    num_exp:       1
    time_per_exp:  512S
    s_to_n:        5
    fluxnum_1:     1
    priority:      3
    param_1:       NX=16,
    param_2:       NY=16,
    req_1:         COND IF TAC OK;

!

    linenum:       430.000
    targname:      MK799HII
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G140L
    wavelength:    1362.5
    num_exp:       2
    time_per_exp:  1203.2S
    s_to_n:        25
    fluxnum_1:     1
    priority:      3
    param_1:       STEP-PATT=2,
    param_2:       FP-SPLIT=STD,
    req_1:         COND IF TAC OK;

!

    linenum:       440.000
    targname:      MK799HII
    config:        HRS
    opmode:        ACCUM
    aperture:      2.0
    sp_element:    G140L
    wavelength:    1642.5
    num_exp:       2
    time_per_exp:  1203.2S
    s_to_n:        25
    fluxnum_1:     1
    priority:      3
    param_1:       STEP-PATT=2,
    param_2:       FP-SPLIT=STD,
    req_1:         COND IF TAC OK;

!
! end of exposure logsheet

! No scan data records found