!    $Id: 5222,v 11.1 1994/10/31 21:40:14 pepsa Exp $
COVERPAGE:
    TITLE_1: High-resolution Imaging of Nuclear Stellar Clusters in AGN
    TITLE_2: N1365
    SCI_CAT: Quasars and AGN
    SCI_SUBCAT: Host Galaxies
    PROPOSAL_FOR: GTO/WF2
    LARGE_PROJ:
    KEY_PROJ:
    TARG_OF_OPP:
    HOURS_PRI: 3.84
    HOURS_PAR: 0
    NUM_PRI: 1
    NUM_PAR: 0
    WF_PC: y
    REALTIME:  n
    TIME_CRIT: n
    SC_TIME: 3.75
    PGM_EFF: 48.
    PI_FNAME: John
    PI_MI: T
    PI_LNAME: Trauger
    PI_INST: 2370
    PI_COUNTRY: USA
    OFF_FNAME:
    OFF_MI:
    OFF_LNAME:
    OFF_TITLE:
    OFF_INST:
    OFF_ADDR_1:
    OFF_ADDR_2:
    OFF_ADDR_3:
    OFF_CITY:
    OFF_STATE:
    OFF_ZIP:
    OFF_COUNTRY:
    OFF_PHONE:
ABSTRACT:
LINE_1: We plan to use the high-resolution available to the PC-II to investigate the
LINE_2: central arcsec of a number of nearby AGN.  This study is motivated by
LINE_3: suggestions of connections between dense stellar clusters formed in starbursts
LINE_4: and conventional active galactic nuclei.  We shall image the nuclei of the
LINE_5: sample in the UV, and in U, V, and I in a manner that will allow us to
LINE_6: adequately remove scattered light from the central source and determine the
LINE_7: structure of extended emission in the surrounding regions.  By examining the
LINE_8: radial distribution of starlight from the nucleus we will be able to place
LINE_9: astrophysically useful limits on the magnitude and dimensions of the putative
LINE_10: central star cluster.  In particular, we will determine if the origin of the
LINE_11: `big blue bump' is hot stars in the cluster rather than the central engine,
LINE_12: look for extended UV emission from `warmers', and examine the structure of
LINE_13: the extended OIII emission-line region.
GENERAL_FORM_ADDRESS:
    LNAME:                   Trauger
    FNAME:                   John
    MI:                      T
    CATEGORY:                PI
    INST:                    2370
    ADDR_1:                  JPL
    ADDR_2:                  4800 Oak Grove Drive
    ADDR_3:
    CITY:                    Pasadena
    STATE:                   CA
    ZIP:                     91109
    COUNTRY:                 USA
    PHONE:                   818 354 9594
    E_MAIL:                  terry@wfpc2.jpl.nasa.gov
GENERAL_FORM_PROPOSERS:
    LNAME:                   Trauger
    FNAME:                   John
    MI:                      T
    INST:                    JPL
    COUNTRY:       USA
  LNAME:           BURROWS
    FNAME:         CHRIS
    INST:          STSCI
    COUNTRY:       USA
  LNAME:           CLARKE
    FNAME:         JOHN
    INST:          UNIV. OF MICHIGAN
    COUNTRY:       USA
  LNAME:           CRISP
    FNAME:         DAVID
    INST:          JPL
    COUNTRY:       USA
  LNAME:           GALLAGHER
    FNAME:         JAY
    INST:          UNIV. OF WISCONSIN
    COUNTRY:       USA
  LNAME:           GRIFFITHS
    FNAME:         RICHARD
    INST:          JOHNS HOPKINS UNIV
    COUNTRY:       USA
  LNAME:           HESTER
    FNAME:         JEFF
    INST:          ARIZONA STATE UNIV.
    COUNTRY:       USA
  LNAME:           HOESSEL
    FNAME:         JOHN
    INST:          UNIV. OF WISCONSIN
    COUNTRY:       USA
  LNAME:           HOLTZMAN
    FNAME:         JOHN
    INST:          LOWELL OBSERVATORY
    COUNTRY:       USA
  LNAME:           MOULD
    FNAME:         JEREMY
    INST:          CALTECH
    COUNTRY:       USA
  LNAME:           WESTPHAL
    FNAME:         JAMES
    INST:          CALTECH
    COUNTRY:       USA
GENERAL_FORM_TEXT:
QUESTION: 3
SECTION: 1
LINE_1: We plan to observe all of the sample in the UV, in U, V, and I, and
LINE_2: in OIII emission where appropriate.
LINE_3: The PC-II has a limited dynamic range, so to provide adequate S/N to
LINE_4: enable scattered light from the central source to be removed, we
LINE_5: require exposures of three different durations.  The shortest should
LINE_6: remain within the dynamic range of the ADC but provide good S/N at the
LINE_7: peak of the PSF; the longest should provide good S/N in the wings of
LINE_8: the PSF whilst minimizing bleeding from the central pixels; the
LINE_9: intermediate exposure will be used to bridge these exposures together.
LINE_10:
LINE_11: We shall split each exposure in two to allow cosmic ray events to be
LINE_12: detected.
LINE_13:
LINE_14: All of these exposures will be read with a gain of 15 electrons/ADU.
QUESTION: 4
SECTION: 1
LINE_1: Ground-based telescopes simply cannot provide the resolution required
LINE_2: for this programme.  In addition, we require the UV capabilities of
LINE_3: HST.
LINE_4:
LINE_5: We expect the limiting factor in these observations will be our
LINE_6: ability to accurately subtract light from the central bright source.
LINE_7: The OTA handbook predicts that the surface brightness of scattered
LINE_8: light at about 1 arcsec is about 0.001 of the peak surface brightness
LINE_9: at 2000A, 0.005 at 4000A, and 0.06 at 8000A.  In the UV, the dominant
LINE_10: effect is thought to be micro-structure in the primary, whereas in the
LINE_11: red Airy diffraction dominates.  The dynamic range of the PC-II is
LINE_12: 4096; with a gain of 15 the ADC will saturate at about 60k counts.  We
LINE_13: expect the chips will physically saturate and begin to bleed shortly
LINE_14: after this.  We expect that the fraction of the total counts in the
LINE_15: central PC-II pixel will be about 0.2.  We shall allow a safety margin
LINE_16: of a factor of 2, as the perils of over exposure are worse than
LINE_17: (moderate) under exposure.
LINE_18:
QUESTION: 13
SECTION: 1
LINE_1: This proposal forms an important part of the `Star Formation in
LINE_2: Galaxies' section of the WFPC-2 GTO program.
FIXED_TARGETS:
  TARGNUM: 1
    NAME_1: NGC1365
    DESCR_1: E,301,909,910,915,919
    POS_1: RA  =  03h 31m 41.33s +/- 1" ,
    POS_2: DEC = -36d 18' 25.1"   +/- 1"
    EQUINOX: 1950
    RV_OR_Z: V = +1639
    FLUXNUM_1: 1
    FLUXVAL_1: SURF(V) = 17.5
EXPOSURE_LOGSHEET:
    LINENUM: 1
    SEQUENCE_1: DEFINE
    SEQUENCE_2: WF-7
    TARGNAME: #
    CONFIG: WFPC2
    OPMODE: IMAGE
    APERTURE: WFALL
    SP_ELEMENT: #
    PRIORITY: 1
    NUM_EXP: #
    TIME_PER_EXP: 1s
    PARAM_1: CR-SPLIT = NO
    PARAM_2: ATD-GAIN = 7
  LINENUM: 2
    SEQUENCE_1: DEFINE
    SEQUENCE_2: PC-15
    TARGNAME: #
    CONFIG: WFPC2
    OPMODE: IMAGE
    APERTURE: PC1
    SP_ELEMENT: #
    PRIORITY: 1
    NUM_EXP: #
    TIME_PER_EXP: 1s
    PARAM_1: CR-SPLIT = NO
    PARAM_2: ATD-GAIN = 15
  LINENUM: 3
    SEQUENCE_1: DEFINE
    SEQUENCE_2: PC-7
    TARGNAME: #
    CONFIG: WFPC2
    OPMODE: IMAGE
    APERTURE: PC1
    SP_ELEMENT: #
    PRIORITY: 1
    NUM_EXP: #
    TIME_PER_EXP: 1s
    PARAM_1: CR-SPLIT = NO
    PARAM_2: ATD-GAIN = 7
  LINENUM: 4
    SEQUENCE_1: USE
    SEQUENCE_2: PC-7
    TARGNAME: NGC1365
    SP_ELEMENT: F160BW
    TIME_PER_EXP: x100
    NUM_EXP: 3
    REQ_1: CYCLE 4 / 4-16;
    REQ_2: SEQ 4-16 NO GAP;
    REQ_3: PCS MODE F / 4-16
  LINENUM: 5
    SEQUENCE_1: USE
    SEQUENCE_2: PC-7
    TARGNAME: NGC1365
    SP_ELEMENT: F160BW
    TIME_PER_EXP: x1000
    NUM_EXP: 3
    REQ_4: SAME ORIENT FOR 5-16 AS 4
  LINENUM: 6
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F336W
    TIME_PER_EXP: x10
    NUM_EXP: 3
  LINENUM: 7
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F336W
    TIME_PER_EXP: x100
    NUM_EXP: 3
  LINENUM: 8
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F555W
    TIME_PER_EXP: x1
    NUM_EXP: 3
  LINENUM: 9
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F555W
    TIME_PER_EXP: x10
    NUM_EXP: 3
  LINENUM: 10
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F555W
    TIME_PER_EXP: x100
    NUM_EXP: 3
  LINENUM: 11
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F814W
    TIME_PER_EXP: x1
    NUM_EXP: 3
  LINENUM: 12
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F814W
    TIME_PER_EXP: x10
    NUM_EXP: 3
  LINENUM: 13
    SEQUENCE_1: USE
    SEQUENCE_2: PC-15
    TARGNAME: NGC1365
    SP_ELEMENT: F814W
    TIME_PER_EXP: x100
    NUM_EXP: 3
  LINENUM: 15
    SEQUENCE_1: USE
    SEQUENCE_2: WF-7
    TARGNAME: NGC1365
    SP_ELEMENT: F547M
    TIME_PER_EXP: x10
    NUM_EXP: 2
  LINENUM: 16
    SEQUENCE_1: USE
    SEQUENCE_2: WF-7
    TARGNAME: NGC1365
    SP_ELEMENT: F547M
    TIME_PER_EXP: x100
    NUM_EXP: 2
!~~~RPSS~~~,WFPC2,n1365.prop, 3-MAR-1994 13:02