!  File:  2123C.PROP
!  Database:  PEPDB
!  Date:  17-FEB-1994:01:11:07

coverpage:

  title_1:         POLARIZATION AND BROAD ABSORPTION LINES IN QUASARS
    sci_cat:       QUASARS & AGN
    sci_subcat:    QUASAR EMISSION
    proposal_for:  GO
    pi_fname:      ROBERT
    pi_lname:      ANTONUCCI
    pi_inst:       UCSB
    pi_country:    USA
    pi_phone:      805-893-4350
    keywords_1:    QUASAR
    hours_pri:     1.40
    num_pri:       1
    fos:           X
    funds_amount:  15181
    funds_length:  12
    funds_date:    JUL-91
    pi_position:   PROF.
    off_fname:     RAY
    off_lname:     SAWYER
! end of coverpage

abstract:

    line_1:        OI 287 is a unique extragalactic source. It appears to take one property
    line_2:        from each class of object. It is either some kind of missing link, or a new
    line_3:        type of activity. Because of the high optical polarization, OI 287 has been
    line_4:        classified with the blazars. However, every other blazar is variable in optical
    line_5:        flux, polarization, and polarization angle., while OI 287 is constant at V=17,
    line_6:        P=8%, and theta=145 degrees. Also, every other blazar has a radio source
    line_7:        dominated by an intense flat-spectrum core, while OI 287 has an upper limit of
    line_8:        2% of the total 20cm flux in the core.
    line_10:       The only group of quasars which ever shows even moderate (2-5%) constant
    line_11:       optical polarization is the broad absorption line (BAL) objects, e.g. PHL 5200
    line_12:       and H1413+113. Among the BAL quasars, PHL 5200 and H1413+113 have exceptionally
    line_13:       smooth deep, attached absorption lines, and also the highest polarization. We
    line_14:       want to know whether OI 287 is a BAL quasar. It would be the first definite
    line_15:       radio loud example. If it is a BAL quasar then the high polarization is really
    line_16:       related to (and perhaps the key to) the BAL phenomenon, and we can use the
    line_17:       techniques of spectropolarimetry to help unlock the BAL geometry. The UV
    line_18:       spectral shape would also provide help determining the cause of polarization.

!
! end of abstract

general_form_proposers:

  lname:           ULVESTAD
    fname:         J.
    mi:            S.
    inst:          JET PROPULSION LABORATORY
    country:       USA

!

  lname:           ANTONUCCI
    fname:         ROBERT
    title:         PROF.
    inst:          UCSB
    country:       USA

!

  lname:           KINNEY
    fname:         A.
    mi:            L.
    inst:          STSCI
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        Our observing plan is very simple. We would like 69 min. with the FOS, Red Tube
    line_2:        G190H Grating. Our target, OI 287, has Fnu(1.5mu) = 0.22 m Jy (V = 18) and
    line_3:        Fnu is proportional to nu**(-1.5). Our main goal is to search for broad
    line_4:        absorption blueward of the Si IV lambda 1397 and CIV lambda 1549 emission
    line_5:        lines, which actually appear at 2020 Angstroms and 2240 Angstroms,
    line_6:        respectively. Our other goal is to measure the spectrum slope to help determine
    line_7:        the cause of the high polarization.
    line_9:        The FOS simulator program shows that we can expect SNR 12/diode, which is good
    line_10:       for our purpose. This is our simulation of a featureless power law of
    line_11:       appropriate amplitude and slope:
    line_13:       FIGURE IS SHOWN

!

  question:        4
    section:       1
    line_1:        The resonance lines normally seen in absorption in BAL quasars appear in the
    line_2:        UV, and this target (V=18, F proportional to nu**(-1.5)) is much too faint
    line_3:        for IUE. Broad absorption rarely appears at MgII lambda 2800, and existing
    line_4:        ground based spectra rule this out for OI 287.

!

  question:        7
    section:       1
    line_1:
    line_2:        SDAS and IRAF programs. We have all the necessary programs for measuring the
    line_3:        data, e.g. determining spectral slopes, line flux and equivalent widths, etc.

!

  question:        9
    section:       1
    line_1:        a.
    line_2:        We've worked for the FOS IDT.

!

  question:        10
    section:       1
    line_1:        STScI will provide the data analysis packages and computer hardware that we
    line_2:        need.

!
!end of general form text

general_form_address:

  lname:           ANTONUCCI
    fname:         ROBERT
    category:      PI
    inst:          U. C., SANTA BARBARA
    addr_1:        PHYSICS DEPARTMENT
    city:          SANTA BARBARA
    state:         CA
    zip:           93106
    country:       USA

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        OI-287
    descr_1:       GALAXY; QUASAR
    pos_1:         PLATE-ID=02UF,
    pos_2:         RA=7H 52M 37.051S +/- 0.5",
    pos_3:         DEC=25D 42' 38.59" +/- 0.5"
    equinox:       2000
    pm_or_par:     NO
    rv_or_z:       Z=0.446
    fluxnum_1:     1
    fluxval_1:     F(2100) = 3.8 +/- 1.0E-16

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    targname:      OI-287
    config:        FOS/RD
    opmode:        ACQ/BINARY
    aperture:      4.3
    sp_element:    MIRROR
    time_per_exp:  20S
    fluxnum_1:     1
    priority:      1
    req_1:         CYCLE 1;
    req_2:         ONBOARD ACQ FOR 2

!

    linenum:       2.000
    targname:      OI-287
    config:        FOS/RD
    opmode:        ACCUM
    aperture:      4.3
    sp_element:    G190H
    wavelength:    1900
    num_exp:       1
    time_per_exp:  3700S
    s_to_n:        12
    fluxnum_1:     1
    priority:      1
    req_1:         CYCLE 1

!
! end of exposure logsheet

! No scan data records found