!  File:  3790C.PROP
!  Database:  PEPDB
!  Date:  19-FEB-1994:19:34:07

coverpage:

  title_1:         POLARIZATION IMAGING OF RADIO GALAXIES
    sci_cat:       QUASARS & AGN
    sci_subcat:    RADIO GALAXIES
    proposal_for:  GO
    pi_fname:      ROBERT
    pi_mi:         R
    pi_lname:      ANTONUCCI
    pi_inst:       UNIV. OF CAL., SANTA BARBARA
    pi_country:    USA
    pi_phone:      805-893-4350
    hours_pri:     6.00
    num_pri:       6
    foc:           Y
    funds_amount:  73286
    funds_length:  12
    off_fname:     RAY
    off_lname:     SAWYER
    off_title:     CHAIR
    off_inst:      UCSB
    off_addr_1:    PHYSICS DEPT
    off_city:      SANTA BARBARA
    off_state:     CA
    off_zip:       93106
    off_country:   USA
    off_phone:     805-893-3495
! end of coverpage

abstract:

    line_1:        Spectropolarimetry of the narrow line radio galaxy 3C234 was used to show
    line_2:        in 1982 that there is a hidden broad line region occulted by an opaque
    line_3:        torus oriented perpendicular to the radio structure axis.  Given the luminosity
    line_4:        of the reflected light, it follows that 3C234 would be called a quasar if
    line_5:        its orientation with respect to the line of sight were different.  Since
    line_6:        then similar results were found for five Seyfert 2's.  If many NLRG's are
    line_7:        occulted quasars in the sky plane, several statistical anomalies in the
    line_8:        beam model for superluminal motion are understandable.  However, further
    line_9:        optical spectropolarimetry has been disappointing in this regard, at least
    line_10:       partially because of severe dilution of reflected light by starlight, sometimes
    line_11:       polarized, from the host galaxies.  We can solve this problem by observing
    line_12:       in the UV.  Furthermore, recent observations of two NLRGs have revealed OFF-
    line_13:       NUCLEAR dust clouds reflecting and strongly "bluening" nuclear light in two
    line_14:       NLRG's.  Such dust clouds, abundant in the merger debris surrounding many
    line_15:       luminous radio galaxies, should show up spectacularly in UV polarization
    line_16:       images, providing information on the beam pattern and time history of nuclear
    line_17:       emission.  We request FOC polarization images of a sample of radio galaxies.
    line_18:       We will also get for free and with high efficiency total flux images, suitable
    line_19:       for studying the nuclei and the anomalous young stellar populations seen
    line_20:       in merging radio galaxies from the ground.

!
! end of abstract

general_form_proposers:

  lname:           ANTONUCCI
    fname:         ROBERT
    title:         PI
    mi:            R
    inst:          UNIV. CALIF., SANTA BARBARA
    country:       USA

!

  lname:           COHEN
    fname:         ROSS
    mi:            D
    inst:          UNIV. OF CALIFORNIA, SANTA DIEGO
    country:       USA

!

  lname:           KINNEY
    fname:         ANNE
    mi:            L
    inst:          SPACE TELESCOPE SCI. INST.
    country:       USA

!

  lname:           KROLIK
    fname:         JULIAN
    mi:            H
    inst:          JOHNS HOPKINS UNIV.
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        2
    section:       0
    line_1:

!

  question:        3
    section:       1
    line_1:        For each object we will take the standard series of
    line_2:        polarization images using F/96 and F320W, taking
    line_3:        exposures with POL0, POL60, and POL120.

!

  question:        4
    section:       1
    line_1:        We have carried out a very extensive ground based pro-
    line_2:        gram of optical spectropolarimetry of radio galaxies.
    line_3:        As discussed in the Sci. Just., these obsns are often
    line_4:        thwarted by host galaxy light, often slightly polarized,
    line_5:        in the optical.  In the UV, the starlight contribution
    line_6:        is down drastically.  If hot stars are present in the
    line_7:        UV, and polaried by dust transmission, in that wave-
    line_8:        length range the ratio of reddening to interstellar poln
    line_9:        is so high that they cannot contribute significantly in
    line_10:       pol. flux. Also, ground-based obsns are limited severely
    line_11:       by sky-subtraction systematics.  Flatfielding the FOC
    line_12:       is not a porblem since we use quotient images.  (No room
    line_13:       for elaboration here, as in Phase I original.)

!

  question:        5
    section:       0
    line_1:

!

  question:        6
    section:       0
    line_1:

!

  question:        7
    section:       1
    line_1:        Data to be reduced at STSCI using STSDAS/IRAF, and ana-
    line_2:        lyzed at UCSB and Johns Hopkins.  Reducing polarization
    line_3:        imaging data is straightforward although complicated. We
    line_4:        construct Stokes Q and U images with linear combinations
    line_5:        of the data, and use them to make poln., pol. flux, and
    line_6:        position angle images.  Most likely, the off-nuclear
    line_7:        poln. will be circumferential due to reflected nuclear
    line_8:        light.  The azimuthal dependence (radial average) will
    line_9:        provide info. on the beam pattern, and the radial depen-
    line_10:       (azimuthal ave.) will provide some info. on the time
    line_11:       histroy of nuclear activity.  Also in the UV the nuclear
    line_12:       radiation will brightly illuminate the dust in any
    line_13:       merger debris, which can then be analyzed morphologi-
    line_14:       cally.
    line_15:       The images will also be combined and deconvolved for
    line_16:       total-flux images.  The "featureless continuum" will
    line_17:       be studied for spatial resolution (see Sci. Just), and
    line_18:       the host galaxies (and off-nuclear "blue patches") and
    line_19:       environments analyzed.

!

  question:        8
    section:       1
    line_1:        This section is lengthy and can be found in the Phase I
    line_2:        submission.

!

  question:        9
    section:       0
    line_1:

!

  question:        10
    section:       1
    line_1:        One Sun workstation supplied by UCSB has STSDAS/IRAF
    line_2:        installed.  Krolik has a Sun 3 and a Sparc 2 for analy-
    line_3:        sis and modeling.  Cohen has adequate facilities at the
    line_4:        UCSD Center for Astrophysics and Space Sciences.  It
    line_5:        would be very desirable to involve one or more graduate
    line_6:        student in this research if STScI funding is available.

!
!end of general form text

general_form_address:

  lname:           ANTONUCCI
    fname:         ROBERT
    mi:            R
    category:      PI
    inst:          UNIV. OF CAL., SANTA BARBARA
    addr_1:        PHYSICS DEPT.
    city:          SANTA BARBARA
    state:         CA
    zip:           93106
    country:       USA
    phone:         805-893-4350
    telex:         NONE

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        PKS1345+12
    descr_1:       E,315
    pos_1:         RA = 13H 45M 6.29S   +/- 1",
    pos_2:         DEC = 12D 32' 19.6"  +/- 1"
    equinox:       1950
    pm_or_par:     N
    rv_or_z:       Z = 0.0595
    fluxnum_1:     1
    fluxval_1:     U = 18.5 +/- 1.0

!

    targnum:       2
    name_1:        3C109
    descr_1:       E,315
    pos_1:         RA = 4H 10M 54.82S +/- 1",
    pos_2:         DEC = 11D 4' 41.2" +/- 1"
    equinox:       1950
    pm_or_par:     N
    rv_or_z:       Z = 0.3056
    fluxnum_1:     1
    fluxval_1:     U = 19.9 +/- 1.0

!

    targnum:       3
    name_1:        3C225B
    descr_1:       E,315
    pos_1:         RA = 9H 39M 32.2S +/- 1",
    pos_2:         DEC = 13D 59' 34" +/- 1"
    equinox:       1950
    pm_or_par:     N
    rv_or_z:       Z = 0.582
    fluxnum_1:     1
    fluxval_1:     U = 20 +/- 1

!

    targnum:       4
    name_1:        3C234
    descr_1:       E,315
    pos_1:         RA = 9H 58M 57.42S +/- 1",
    pos_2:         DEC = 29D 1' 37.4" +/- 1.0"
    equinox:       1950
    pm_or_par:     N
    rv_or_z:       Z = 0.1848
    fluxnum_1:     1
    fluxval_1:     U = 18.6 +/- 1.0

!

    targnum:       5
    name_1:        3C321
    descr_1:       E,315
    pos_1:         RA = 15H 29M 33.42S +/- 1",
    pos_2:         DEC = 24D 14' 26.2" +/- 1"
    equinox:       1950
    pm_or_par:     N
    rv_or_z:       Z = 0.096
    fluxnum_1:     1
    fluxval_1:     U = 18 +/- 1

!

    targnum:       6
    name_1:        3C405
    name_2:        CYG-A
    descr_1:       E,315
    pos_1:         RA = 19H 57M 44.43S +/- 1",
    pos_2:         DEC = 40D 35' 45.2" +/- 1"
    equinox:       1950
    pm_or_par:     N
    rv_or_z:       Z = 0.0565
    fluxnum_1:     1
    fluxval_1:     U = 19.5 +/- 1.0

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    targname:      PKS1345+12
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL0
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25
    req_1:         CYCLE 2 / 1-18;
    req_2:         SEQ 1-3 NO GAP;

!

    linenum:       2.000
    targname:      PKS1345+12
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL60
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       3.000
    targname:      PKS1345+12
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL120
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       4.000
    targname:      3C109
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL0
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25
    req_1:         SEQ 4-6 NO GAP;

!

    linenum:       5.000
    targname:      3C109
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL60
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       6.000
    targname:      3C109
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL120
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       7.000
    targname:      3C225B
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL0
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25
    req_1:         SEQ 7-9 NO GAP;

!

    linenum:       8.000
    targname:      3C225B
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL60
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       9.000
    targname:      3C225B
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL120
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       10.000
    targname:      3C234
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL0
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25
    req_1:         SEQ 10-12 NO GAP;

!

    linenum:       11.000
    targname:      3C234
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL60
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       12.000
    targname:      3C234
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL120
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       13.000
    targname:      3C321
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL0
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25
    req_1:         SEQ 13-15 NO GAP;

!

    linenum:       14.000
    targname:      3C321
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL60
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       15.000
    targname:      3C321
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL120
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       16.000
    targname:      3C405
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL0
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25
    req_1:         SEQ 16-18 NO GAP;

!

    linenum:       17.000
    targname:      3C405
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL60
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!

    linenum:       18.000
    targname:      3C405
    config:        FOC/96
    opmode:        IMAGE
    aperture:      512X1024
    sp_element:    F320W,POL120
    num_exp:       1
    time_per_exp:  606S
    s_to_n:        50
    s_to_n_time:   30M
    fluxnum_1:     1
    priority:      1
    param_1:       PIXEL = 50X25

!
! end of exposure logsheet

! No scan data records found