!  File:  4810C.PROP
!  Database:  PEPDB
!  Date:  23-FEB-1994:04:32:18

coverpage:

  title_1:         CONSTRAINTS ON CONTINUUM MODELS OF ACTIVE NUCLEI: FAST ULTRAVIOLET
    title_2:       VARIATIONS
    sci_cat:       QUASARS & AGN
    proposal_for:  GO
    pi_title:      DR.
    pi_fname:      M.
    pi_mi:         J.
    pi_lname:      WARD
    pi_inst:       OXFORD, UNIVERSITY OF
    pi_country:    UK
    pi_phone:      44-865-273303
    keywords_1:    ACTIVE NUCLEII/RAPID CONTINUUM VARIABILITY
    hours_pri:     5.00
    num_pri:       2
    hsp:           X
    pi_position:   MRS.
    off_fname:     P.
    off_lname:     BAND
    off_title:     SECRETARY
    off_inst:      ASTROPHYSICS
    off_addr_1:    KEBLE ROAD
    off_city:      OXFORD
    off_zip:       OX1 3RH
    off_country:   UK
    off_phone:     44-865-273303
    off_telex:     83295 NUCLOX G
! end of coverpage

abstract:

    line_1:        We propose to use the Fast Photometer to observe fast-timescale ultraviolet
    line_2:        continuum variations in Active Nuclei. The two objects selected have the
    line_3:        fastest observed X-ray variations down to 100 seconds, an observational limit
    line_4:        set by the satellite sensitivity. Importantly, the Fourier Power-Spectrum of
    line_5:        the X-ray data shows no sign that we have yet sampled the fastest variations.
    line_6:        The large contribution of starlight, even through the smallest apertures, means
    line_7:        that no ground-based experiment can approach the sensitivity to short
    line_8:        timescales variations that the HSP can potentially observe. The proposed
    line_9:        ultraviolet observations can be made near-simultaneously through two
    line_10:       ultraviolet filters, giving crude two color spectral information that will help
    line_11:       define the characteristics of the variable component. Using the HSP we can
    line_12:       improve the time resolution by an order of magnitude, thus setting strong
    line_13:       constraints of models of compact source energy generation.

!
! end of abstract

general_form_proposers:

  lname:           DONE
    fname:         C.
    title:         DR.
    inst:          GODDARD
    country:       USA

!

  lname:           FABIAN
    fname:         A.
    title:         DR.
    mi:            C.
    inst:          CAMBRIDGE, UNIVERSITY OF
    country:       UK
    esa:           X

!

  lname:           WARD
    fname:         M.
    title:         P.I.
    mi:            J.
    inst:          OXFORD, UNIVERSITY OF
    country:       UK
    esa:           X

!

  lname:           ELVIS
    fname:         MARTIN
    title:         DR.
    mi:            S.
    inst:          CFA
    country:       USA

!

  lname:           LAWRENCE
    fname:         A.
    title:         DR.
    inst:          QUEEN MARY WESTFIELD COLLEGE, LONDON
    country:       UK
    esa:           X

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        All exposures are Cycle 1 exposures

!

  question:        13
    section:       1
    line_1:        We propose to use the Fast Photometer to observe fast-timescale ultraviolet
    line_2:        continuum variations in Active Nuclei. The two objects selected have the
    line_3:        fastest observed X-ray variations down to 100 seconds, an observational limit
    line_4:        set by the satellite sensitivity. Importantly, the Fourier Power-Spectrum of
    line_5:        the X-ray data shows no sign that we have yet sampled the fastest variations.
    line_6:        The large contribution of starlight, even through the smallest apertures, means
    line_7:        that no ground-based experiment can approach the sensitivity to short
    line_8:        timescales variations that the HSP can potentially observe. The proposed
    line_9:        ultraviolet observations can be made near-simultaneously through two
    line_10:       ultraviolet filters, giving crude two color spectral information that will help
    line_11:       define the characteristics of the variable component. Using the HSP we can
    line_12:       improve the time resolution by an order of magnitude, thus setting strong
    line_13:       constraints of models of compact source energy generation.

!
!end of general form text

general_form_address:

  lname:           WARD
    fname:         M.
    mi:            J.
    title:         DR.
    category:      PI
    inst:          ASTROPHYSICS
    addr_1:        KEBLE ROAD
    city:          OXFORD OX1 3RH
    country:       U.K.
    phone:         44-865-273303
    telex:         83295 NUCLOX G

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        NGC4051
    descr_1:       SEYFERT GALAXY
    pos_1:         RA=12H 03M 09.67S +/- 0.04S,
    pos_2:         DEC=+44D 31' 52.3" +/- 0.4"
    equinox:       2000
    pm_or_par:     N
    rv_or_z:       Z=0.002
    plate_req:     N
    plate_avail:   Y
    fluxnum_1:     1
    fluxval_1:     V=15.0 +/- 0.5

!

    targnum:       2
    name_1:        NGC6814
    descr_1:       ^
    pos_1:         RA=19H 42M 40.70S +/- 0.08S,
    pos_2:         DEC=-10D 19' 25.5" +/- 1.2"
    equinox:       ^
    pm_or_par:     ^
    rv_or_z:       Z=0.005
    plate_req:     N
    plate_avail:   Y
    fluxnum_1:     1
    fluxval_1:     V=15.5 +/- 0.5

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.500
    targname:      NGC4051
    config:        HSP/UV1
    opmode:        ACQ
    num_exp:       1
    time_per_exp:  1M
    fluxnum_1:     1
    priority:      1
    req_1:         ONBOARD ACQ FOR 2;
    req_3:         CYCLE 2 / 1.5-4;

!

    linenum:       2.000
    targname:      NGC4051
    config:        HSP/UV1
    opmode:        SINGLE
    aperture:      1.0
    sp_element:    F240W
    num_exp:       1
    time_per_exp:  125M
    fluxnum_1:     1
    priority:      1
    param_1:       SAMPLE-TIME=0.2

!

    linenum:       3.500
    targname:      NGC6814
    config:        HSP/UV1
    opmode:        ACQ
    num_exp:       1
    time_per_exp:  1M
    fluxnum_1:     1
    priority:      1
    req_1:         ONBOARD ACQ FOR 4;

!

    linenum:       4.000
    targname:      NGC6814
    config:        HSP/UV1
    opmode:        SINGLE
    aperture:      1.0
    sp_element:    F240W
    num_exp:       1
    time_per_exp:  125M
    fluxnum_1:     1
    priority:      1
    param_1:       SAMPLE-TIME=0.2

!
! end of exposure logsheet

! No scan data records found