!   $Id: 5368,v 5.1 1994/07/27 17:10:10 pepsa Exp $
COVERPAGE:
  TITLE_1:  HST SPECTROSCOPY OF CYGNUS A -I. EARLY ACQ IMAGING
  SCI_CAT:  QUASARS & AGN
  SCI_SUBCAT:           RADIO GALAXIES
  PROPOSAL_FOR:         GO
  PI_FNAME:             NEAL
  PI_MI:
  PI_LNAME:             JACKSON
  PI_INST:              LEIDEN OBSERVATORY
  PI_COUNTRY:           NETHERLANDS
  PI_PHONE:             31-71-275851
  HOURS_PRI:            9.83
  NUM_PRI:              1
  WF_PC:  Y
  FOS:                  Y
  OFF_FNAME:            HARM
  OFF_LNAME:            HABING
  OFF_TITLE:            DIRECTOR, LEIDEN
  OFF_INST:             6870
  OFF_ADDR_1:           STERREWACHT LEIDEN
  OFF_ADDR_2:           POSTBUS 9513
  OFF_ADDR_3:           2300RA LEIDEN
  OFF_CITY:
  OFF_STATE:
  OFF_ZIP:
  OFF_COUNTRY:          NETHERLANDS
  OFF_PHONE:
ABSTRACT:
LINE_1:We propose to obtain spectroscopy of the nucleus and extended line emitting
LINE_2:knot of the prototypical high-power radio galaxy Cygnus A. Ground based
LINE_3:images and spectra have so far failed to provide convincing explanations for
LINE_4:the ionization structure of the line emission or proof for the model in
LINE_5:which the continuum light is due to scattering of a hidden quasar nucleus.
LINE_6:By using the HST resolution to exclude contaminating continuum-emitting
LINE_7:components we will be able to do two things. First, we will be able to
LINE_8:search for a broad Balmer line in the central sources, which would be proof
LINE_9:of the existence of a hidden quasar nucleus: only marginal evidence of this
LINE_10:broad component exists from ground-based spectra. Second, we will be able
LINE_11:to select out the high surface brightness condensation in the northwest
LINE_12:line-emitting component. This will be examined to clarify the kinematics,
LINE_13:find out if it is the location of the narrow line "moving component" and
LINE_14:examine the excitation mechanism of the emission lines in a clearly
LINE_15:defined region rather than the average over the whole source typically
LINE_16:seen in ground based images.
GENERAL_FORM_PROPOSERS:
  LNAME:                JACKSON
  FNAME:                NEAL
  MI:
  INST:                 6870
  COUNTRY:              NETHERLANDS
  LNAME:                SPARKS
  FNAME:                WILLIAM
  MI:                   B.
  INST:                 3470
  COUNTRY:              USA
  ESA:   Y
  LNAME:                MILEY
  FNAME:                GEORGE
  MI:                 K.
  INST:                 6870
  COUNTRY:              NETHERLANDS
  LNAME:                TADHUNTER
  FNAME:                CLIVE
  MI:                   N.
  INST:                 UNIVERSITY OF SHEFFIELD
  COUNTRY:              ENGLAND
  LNAME:                MACCHETTO
  FNAME:                F
  MI:
  INST:                 3470
  COUNTRY:              USA
GENERAL_FORM_ADDRESS:
  LNAME:                JACKSON
  FNAME:                NEAL
  MI:
  CATEGORY:      PI
  INST:                 6870
  ADDR_1:               STERREWACHT LEIDEN
  ADDR_2:               POSTBUS 9513
  ADDR_3:  2300RA LEIDEN
  CITY:
  STATE:
  ZIP:
  COUNTRY:  NETHERLANDS
  PHONE:                31-71-275851
  TELEX:                jackson@strw.LeidenUniv.nl
  LNAME:
  FNAME:
  MI:
  CATEGORY:      CON
  INST:
  ADDR_1:
  ADDR_2:
  ADDR_3:
  CITY:
  STATE:
  ZIP:
  COUNTRY:
  PHONE:
  TELEX:
GENERAL_FORM_TEXT:
 QUESTION:  3
  SECTION:  1
LINE_1: Our aim is to obtain spectra of two small regions within the
LINE_2: radio galaxy Cygnus A. The first region is very close to the
LINE_3: radio core of the object and the second in the northwest
LINE_4: optical condensation. Both regions are embedded in complex
LINE_5: emission line regions.
LINE_6: A WFPC2 exposure is required for accurate location of these
LINE_7: two regions and we therefore propose to obtain a 2x25 min
LINE_8: early acquisition exposure. Since both regions are strong
LINE_9: line emitters we propose to use the F555W filter for maximum
LINE_10: efficiency in their location (this includes the very strong
LINE_11: redshifted [OIII] 5007 line).
LINE_12: The subsequent FOS exposures will be taken using both the
LINE_13: G570H and G780H, to cover all important optical lines out to
LINE_14: redshifted H alpha/[SII] and to locate blueshifted narrow line
LINE_15: components.
LINE_16: THIS FILE CONTAINS THE EARLY ACQUISITION EXPOSURES ONLY
 QUESTION:  4
  SECTION:  1
LINE_1:We have made extensive spectroscopic and spectropolarimetric
LINE_2:observations from the ground. These observations cannot give us
LINE_3:the spectrum of the near-nuclear region alone, and cannot
LINE_4:give uncontaminated spectral information about the major line-
LINE_5:emitting component and thus provide a handle on its kinematics and
LINE_6:ionization state. In both cases this is because of the degradation
LINE_7:by ground-based seeing which allows light unconnected with the
LINE_8:regions under study to enter the science aperture.
 QUESTION:  5
  SECTION:  1
LINE_1: An Early Acquisition WFPC2 exposure is needed as the target regions
LINE_2: lie in a complex area of extended emission at the core of the galaxy.
LINE_3: THIS FILE CONTAINS THE EARLY ACQUISITION EXPOSURES ONLY.
LINE_4:
LINE_5:
LINE_6:
LINE_7:
LINE_8:
LINE_9:
LINE_10:
LINE_11:
LINE_12:
LINE_13:
LINE_14:
LINE_15:
 QUESTION:  6
  SECTION:  1
LINE_1:
LINE_2:
LINE_3:
LINE_4:
LINE_5:
LINE_6:
LINE_7:
LINE_8:
 QUESTION:  8
  SECTION:  1
LINE_1:
LINE_2:
LINE_3:
LINE_4:
LINE_5:
 QUESTION:  9
  SECTION:  1
LINE_1: As part of the GTO program we obtained HST FOC images of the
LINE_2: central region, both in the [OII] line and in the nearby continuum.
LINE_3: This shows a "channel" of lower surface brightness emission along
LINE_4: the inner part of the radio jet which appears to bisect the NW
LINE_5: component and possibly also the SE component, which would indicate
LINE_6: the influence of a counterjet. The line emission appears conentrated
LINE_7: in two relatively small regions: the core component (which may
LINE_8: be part of the nucleus according to some authors) and a region
LINE_9: in the NW component to the north of the radio jet.
LINE_10:
LINE_11:
LINE_12:
LINE_13:
LINE_14:
LINE_15:
LINE_16:
LINE_17:
LINE_18:
LINE_19:
 QUESTION:  10
  SECTION:  1
LINE_1: The reduction will take place at Leiden and STScI.
LINE_2: SDAS/IRAF runs at both Leiden and STScI and there is an ample supply of
LINE_3: workstation at both institutes.
LINE_4:
LINE_5:
LINE_6:
LINE_7:
FIXED_TARGETS:
    targnum:       1
    name_1:        3C405
    name_2:        CYGNUS-A
    descr_1:       E,315
    pos_1:         RA= 19H 57M 44.443S +/- 0.03S,
    pos_2:         DEC=+40D 35' 46.37" +/- 0.3"
    equinox:       1950
    rv_or_z:       Z=0.0567
    fluxnum_1:     1
    fluxval_1:     SURF(V)=19.0+/-0.2
    fluxnum_2:     2
    fluxval_2:     E(B-V)=0.7+/-0.1
    fluxnum_3:     3
    fluxval_3:
    comment_1:V SURFACE BRIGHTNESS BASED ON
    comment_2:12.2 ARCSEC**2 APERTURE OF VAN
    comment_3:DEN BERGH, APJ 210 L63. DISTRN
    comment_4:OF E(B-V) COMPLEX AND VARIES
    comment_5:OVER SOURCE.
    comment_6:
    comment_7:
    comment_8:
    targnum:       2
    name_1:        3C405-OFFSET
    name_2:        CYGNUS-A-OFFSET
    descr_1:       A,132
    pos_1: TBD-EARLY,RA= 19H 57M 43.455S +/- 0.06S,
    pos_2: TBD-EARLY,DEC=+40D 35' 37.71" +/- 0.6"
    equinox:       1950
    rv_or_z:       Z=0.0567
    fluxnum_1: 1
    fluxval_1: V=16.0+/-0.5
    fluxnum_2:
    fluxval_2:
    fluxnum_3:
    fluxval_3:
    comment_1: EXACT OFFSET STAR TBD
    comment_2: AFTER EARLY ACQ PC
    comment_3: OBSERVATION
    comment_4:
    comment_5:
    comment_6:
    comment_7:
    comment_8:
    comment_9:
    comment_10:
    targnum:       3
    name_1:        3C405-NUC
    name_2:        CYGNUS-A-NUC
    descr_1:       E,315
    pos_1:TBD-EARLY,RA= 19H 57M 44.443S +/- 0.06S,
    pos_2:TBD-EARLY,DEC=+40D 35' 46.37" +/- 0.6"
    equinox:       1950
    rv_or_z:       Z=0.0567
    fluxnum_1:     1
    fluxval_1:     SURF(V)=20.3 +/- 0.2
    fluxnum_2:     2
    fluxval_2:     SURF(R)=19.1 +/- 0.2
    fluxnum_3:     3
    fluxval_3:     F-LINE(3727)=6 +/- 1 E-15
    comment_1: SURFACE BRIGHTNESSES BASED ON
    comment_2: VESTERGAARD & BARTHEL AJ 105 456
    comment_3: 3727 FLUX IS IN CENTRAL KNOT
    comment_4: VISIBLE IN OUR FOC OBSERVATION
    comment_5: 5007 LINE SHOULD BE AT LEAST 3X
    comment_6: AS BRIGHT AS OII
    comment_7:
    targnum:       4
    name_1:        3C405-NW
    name_2:        CYGNUS-A-NW
    descr_1:       E,315
    pos_1:TBD-EARLY,RA= 19H 57M 44.353S +/- 0.06S,
    pos_2:TBD-EARLY,DEC=+40D 35' 47.00" +/- 0.6"
    equinox:       1950
    rv_or_z:       Z=0.0567
    fluxnum_1:     1
    fluxval_1:     SURF(V) = 19.8 +/- 0.4
    fluxnum_2:     2
    fluxval_2:     SURF(R) = 18.6 +/- 0.4
    fluxnum_3:     3
    fluxval_3:     F-LINE(3727) = 8+/-3E-15
    comment_1: V AND R BRIGHTNESSES ARE
    comment_2: EXTRAPOLATIONS FROM VESTERGAARD
    comment_3: & BARTHEL USING FLUX RATIOS FROM
    comment_4: FOC IMAGE: LINE FLUX IS DERIVED
    comment_5: FROM OUR FOC IMAGE
    comment_6: TOTAL FLUX FROM OII 3727 LINE FROM
    comment_7: ALL CPTS OF OUR FOC IMAGE AGREES
    comment_8: WITH OSTERBROCK'S ESTIMATE
    comment_9: (APJ 197 535) TO FACTOR OF ~2.
    comment_10:
EXPOSURE_LOGSHEET:
  LINENUM:  1.0
  SEQUENCE_1:
  SEQUENCE_2:
  TARGNAME:  3C405
  CONFIG:               WFPC2
  OPMODE:               IMAGE
  APERTURE:             PC1
  SP_ELEMENT:           F555W
  WAVELENGTH:
  PARAM_1:             CR-SPLIT=NO
  NUM_EXP:              1
  TIME_PER_EXP:         2S
  S_TO_N:
  S_TO_N_TIME:
  FLUXNUM_1:            1
  FLUXNUM_2:
  FLUXNUM_3:
  FLUXNUM_4:
  PRIORITY:           1
  REQ_1:       CYCLE 4;
  REQ_2:       ORIENT 120D +/- 60D;
  REQ_3:
  REQ_4:
  REQ_5:
  REQ_6:
  REQ_7:
  REQ_8:
  REQ_9:
  REQ_10:
  COMMENT_1:ORIENT+180 OK TOO.
  COMMENT_2:NB THESE ARE EARLY
  COMMENT_3:ACQ EXPOSURES FOR
  COMMENT_4:LATER FOS/RD
  COMMENT_5:SPECTROSCOPY. S:N
  COMMENT_6:IS CNTR PIXELS.
  LINENUM:  2.0
  SEQUENCE_1:
  SEQUENCE_2:
  TARGNAME:  3C405
  CONFIG:               WFPC2
  OPMODE:               IMAGE
  APERTURE:             PC1
  SP_ELEMENT:           F555W
  WAVELENGTH:
  PARAM_1:             CR-SPLIT=NO
  NUM_EXP:              1
  TIME_PER_EXP:         30S
  S_TO_N:
  S_TO_N_TIME:
  FLUXNUM_1:            1
  FLUXNUM_2:
  FLUXNUM_3:
  FLUXNUM_4:
  PRIORITY:           1
  REQ_1:       CYCLE 4;
  REQ_2:       ORIENT 120D +/- 60D;
  REQ_3:
  REQ_4:
  REQ_5:
  REQ_6:
  REQ_7:
  REQ_8:
  REQ_9:
  REQ_10:
  COMMENT_1:ORIENT+180 OK TOO.
  COMMENT_2:NB THESE ARE EARLY
  COMMENT_3:ACQ EXPOSURES FOR
  COMMENT_4:LATER FOS/RD
  COMMENT_5:SPECTROSCOPY. S:N
  COMMENT_6:IS CNTR PIXELS.
  LINENUM:  3.0
  SEQUENCE_1:
  SEQUENCE_2:
  TARGNAME:  3C405
  CONFIG:               WFPC2
  OPMODE:               IMAGE
  APERTURE:             PC1
  SP_ELEMENT:           F555W
  WAVELENGTH:
  PARAM_1:             CR-SPLIT=NO
  NUM_EXP:              3
  TIME_PER_EXP:         900S
  S_TO_N:              20
  S_TO_N_TIME:
  FLUXNUM_1:            1
  FLUXNUM_2:
  FLUXNUM_3:
  FLUXNUM_4:
  PRIORITY:           1
  REQ_1:       CYCLE 4;
  REQ_2:       ORIENT 120D +/- 60D;
  REQ_3:
  REQ_4:
  REQ_5:
  REQ_6:
  REQ_7:
  REQ_8:
  REQ_9:
  REQ_10:
  COMMENT_1:ORIENT+180 OK TOO.
  COMMENT_2:NB THESE ARE EARLY
  COMMENT_3:ACQ EXPOSURES FOR
  COMMENT_4:LATER FOS/RD
  COMMENT_5:SPECTROSCOPY. S:N
  COMMENT_6:IS CNTR PIXELS.
!~~~RPSS~~~,JACKSON,phase2new.,24-JAN-1994 15:17

!