!   $Id: 5465,v 15.1 1994/07/27 18:18:42 pepsa Exp $

coverpage:

  title_1:         WFPC 2 IMAGING OF TWO GALAXY CLUSTERS AT Z=1.2
    sci_cat:       GALAXIES & CLUSTERS
    sci_subcat:    CLUSTERS/LENSES
    proposal_for:  GO
    pi_fname:      MARK
    pi_lname:      DICKINSON
    pi_inst:       3470
    pi_country:    USA
    pi_phone:      510 642 6110
    hours_pri:     17.50
    num_pri:       1
    wf_pc:         Y
    off_fname:     HERVEY
    off_lname:     STOCKMAN
    off_title:     DEPUTY DIRECTOR
    off_inst:      3470
    off_addr_1:    SPACE TELESCOPE SCIENCE INSTITUTE
    off_addr_2:    3700 SAN MARTIN DR.
    off_city:      BALTIMORE
    off_state:     MD
    off_zip:       21218
    off_country:   USA
    off_phone:     410 338 4730
! end of coverpage

abstract:

    line_1:        Using deep optical and infrared images taken at the KPNO 4m, we have
    line_2:        identified two rich galaxy clusters around 3CR radio galaxies at z=1.2
    line_3:        These are perhaps the most distant clusters yet observed.
    line_4:        The clusters appear to have a large population of extremely red members,
    line_5:        contrary to naive expectations from an extrapolation of the
    line_6:        Butcher-Oemler effect to large redshift.  Both clusters apparently include
    line_7:        galaxies as red as present day (z=0) ellipticals redshifted out to z=1.2.
    line_8:        We propose to obtain deep HST images with WFPC 2 in order to examine the
    line_9:        morphological types of these very red galaxies, and to study the
    line_10:       properties of cluster galaxies in general at very large cosmic lookback
    line_11:       times.  We hope to investigate: whether the red galaxies are in fact
    line_12:       relatively "unevolved" ellipticals; how their structural parameters compare
    line_13:       to elliptical galaxies today; whether S0 galaxies exist at z=1.2; the
    line_14:       frequency of interactions and mergers in very high redshift clusters;
    line_15:       and the morphologies of cluster galaxies bluer than the "red envelope"
    line_16:       galaxies.  By imaging the radio galaxies themselves with the PC camera,
    line_17:       we will obtain extremely deep images of these giant, morphologically
    line_18:       peculiar objects.  Finally, we will look for evidence of
    line_19:       gravitational lensing of faint, extremely distant background sources by
    line_20:       these high redshift clusters.

!
! end of abstract

general_form_proposers:

  lname:           DICKINSON
    fname:         MARK
    inst:          3470
    country:       USA

!

  lname:           SPINRAD
    fname:         HYRON
    inst:          1500
    country:       USA

!

  lname:           EISENHARDT
    fname:         PETER
    inst:          2370
    country:       USA

!

  lname:           STANFORD
    fname:         S. ADAM
    inst:          2370
    country:       USA

!

  lname:           DJORGOVSKI
    fname:         STANISLAV
    inst:          1590
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        Deep WFPC2 imaging of the z=1.2 radio galaxy 3C324 and the extremely faint
    line_2:        cluster companions in the surrounding field will be obtained through the
    line_3:        F702W filter.  The radio galaxy itself (whose coordinates are those specified
    line_4:        in the target information section) will be placed onto the PC1 planetary
    line_5:        camera CCD to obtain high spatial resolution images.  We request a
    line_6:        particular orientation with the ORIENT parameter to optimally position the
    line_7:        other galaxies of interest from the surrounding cluster onto the other WFPC2
    line_8:        CCDs, and to keep them away from the interstices between the CCDs as much as
    line_9:        is possible in order to avoid possible image degradation and light loss.
    line_10:       The galaxies in the cluster are distributed out to the limits of the WFPC2
    line_11:       field of view.  Thus the ORIENT angle we specify and the range of acceptable
    line_12:       angles around it is fairly tightly constrained.  An alternative ORIENT angle
    line_13:       (approx. ORIENT=155D) is possible if the one we have specified proves to be
    line_14:       too difficult to schedule;  please contact the P.I. if this becomes necessary,
    line_15:       as it may also require revisions to the POS TARG parameters.  We have
    line_16:       divided our total exposure time into many individual 2200s exposures,
    line_17:       i.e. approximately the unocculted period of one orbit after allowing
    line_18:       overhead time for guide star re-acquisition.  We wish to maximize the per
    line_19:       orbit exposure time in order to minimize the effects of readout noise;  if
    line_20:       during scheduling it becomes possible to increase this amount over 2200s,
    line_21:       we would like to do so.  Similarly, we hope that it will not be necessary to
    line_22:       reduce the per orbit exposure time below approx. 2000s.  We set CR-SPLIT=NO
    line_23:       because many separate exposures will be obtained at each telescope

!

  question:        3
    section:       2
    line_1:        pointing, facilitating cosmic ray removal without the need for CR-SPLIT.
    line_2:        We have divided our observation into 4 groups of 7 exposures each.  Within
    line_3:        each group of 7, we will maintain the same FGS lock position. The telescope
    line_4:        pointing is then offset between one group and the next by a small amount
    line_5:        using a POS TARG command.  This will result in the observations being taken
    line_6:        in a small, square raster pattern in order to expose the objects to
    line_7:        several portions of the WFPC2 CCDs and thus minimize the impact of any
    line_8:        defects in the arrays.  We request the same ORIENT angle for all of the
    line_9:        exposures.  Finally, we have included an "extra" 1400s exposure as
    line_10:       LINENUM=5.0 in the exposure log sheet in order to fill out the allocated
    line_11:       21 hours of spacecraft time.

!

  question:        4
    section:       1
    line_1:        As for most WFPC-2 programs, the primary justification for observing with
    line_2:        HST is its high angular resolution.  At z=1.2, the linear scale corresponding
    line_3:        to 1 arcsecond is 8.5 kpc for q0=0.5 and 12 kpc for q0=0  (H0=50 km/s/Mpc).
    line_4:        It is essentially impossible to obtain useful morphological information with
    line_5:        even the best ground-based seeing for any galaxies at this redshift except
    line_6:        the giant radio galaxies.   Without HST imaging, we can only measure global
    line_7:        spectrophotometric properties for these galaxies.  Their morphological types,
    line_8:        the details of their structure, and their close interactions with other
    line_9:        galaxies remain invisible from the ground.
    line_11:       HST imaging of clusters at z=0.4 has provided a remarkably dynamic picture
    line_12:       of activity:  observations of spiral structure of many blue cluster members,
    line_13:       evidence for frequent galaxy-galaxy interactions, and morphological/color
    line_14:       correlations are permitting a thorough analysis of the evolutionary state of
    line_15:       galaxies in clusters at modest lookback times.  With the corrected optics of
    line_16:       WFPC-2 we can now extend this work out to z > 1, where our ground--based images
    line_17:       barely provide evidence for spatial extent, and give no clues as to the Hubble
    line_18:       types of cluster members.  In our two target clusters, the very red colors
    line_19:       we observe for some of the galaxies lead us to infer that they are
    line_20:       early type systems:  HST will let us study their strucure at resolutions
    line_21:       comparable to those achieved in ground--based observations the Coma Cluster.

!

  question:        5
    section:       1
    line_1:

!

  question:        6
    section:       1
    line_1:

!


!


!

  question:        8
    section:       1
    line_1:

!

  question:        9
    section:       1
    line_1:        The PI has worked on reduction and analysis of WFPC-1 images of
    line_2:        faint galaxies taken during HST Cycle 2.  All of the co-investigators
    line_3:        have been involved in other previous HST programs, and Stanford
    line_4:        and Djorgovski in particular have been extensively involved in
    line_5:        data reduction and analysis of HST imaging.   Several papers have
    line_6:        been published based on that work.

!

  question:        10
    section:       1
    line_1:        The PI will be a fellowship postdoc at STScI for two to three years beginning
    line_2:        this fall;  this should provide an excellent opportunity for direct access to
    line_3:        the expert human resources most important for processing, analyzing, and
    line_4:        understanding HST data, as well as software and computing support.  Two of the
    line_5:        co-Is (Spinrad and Djorgovski) will have regular access to the Keck 10m
    line_6:        telescope, now beginning scientific operation in Hawaii.  Its merits are
    line_7:        self-evident for ground-based followup observations.  In particularly,
    line_8:        spectroscopy of these cluster galaxies is only feasible with very large
    line_9:        aperture telescopes such as Keck.   We also hope to obtain very deep infrared
    line_10:       imaging observations in with the best angular resolution that Mauna Kea can
    line_11:       offer.  Dickinson will receive year-round salary support from STScI, and thus
    line_12:       is not requesting funds for that purpose.  Academic year salaries for Spinrad
    line_13:       and Djorgovski are provided by their respective institutions, and partial salary
    line_14:       support is provided for Stanford and Eisenhardt by other grants to JPL.
    line_15:       As this research program will be a primary occupation for Stanford during
    line_16:       the period of the grant, we request several months of salary support for that
    line_17:       purpose.
    line_19:       In general, all of our institutions provide excellent computing resources,
    line_20:       facilities, and administrative support.  UC Berkeley and CalTech have excellent
    line_21:       graduate students available for research assistance, and it is anticipated that
    line_22:       one or more students will be invited to participate in data reduction and
    line_23:       analysis at those institutions.

!
!end of general form text

general_form_address:

  lname:           Dickinson
    fname:         Mark
    category:      PI

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        3C324
    descr_1:       F,404,406,409,
    descr_2:       E,303,309,315,325
    pos_1:         RA = 15H 47M 37.2S +/- 0.1S,
    pos_2:         DEC = +21D 34' 41.0" +/- 1.0"
    equinox:       1950
    rv_or_z:       Z = 1.206
    comment_1:     OBJECTS OF INTEREST ARE VERY FAINT
    comment_2:     (21 < R < 25) GALAXIES IN A HIGH
    comment_3:     REDSHIFT CLUSTER.  THE PRECISE
    comment_4:     SURFACE BRIGHTNESSES ARE UNKNOWN
    comment_5:     AND DEPEND ON GALAXY MORPHOLOGIES.
    comment_6:     SURF(R)=25 IS GIVEN AS A CHARAC-
    comment_7:     TERISTIC VALUE FOR USE IN THE
    comment_8:     S_TO_N CALCULATIONS BELOW IN THE
    comment_9:     EXPOSURE LOGSHEET; SPECIFIED S/N
    comment_10:    IS PER PC PIXEL AT SURF(R)=25.
    fluxnum_1:     1
    fluxval_1:     V=21.5 +/- 0.5
    fluxnum_2:     2
    fluxval_2:     SURF(R)=25

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.100
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   15400S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         ORIENT 173D +/- 1D;
    req_3:         POS TARG -11.25,-11.00;
    req_4:         SEQ 1.1-1.2 NO GAP;
    req_5:         SAME ORIENT FOR 1.2-4.4 AS 1.1;
    req_6:         GROUP 1.1-1.4 WITHIN 5D
    comment_1:     FIRST OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       1.200
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   15400S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 1.2 AS 1.1
    comment_1:     FIRST OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       1.300
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   15400S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         POS TARG -11.25,-11.00;
    req_3:         SEQ 1.3-1.4 NO GAP
    comment_1:     FIRST OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       1.400
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   15400S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 1.4 AS 1.3
    comment_1:     FIRST OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       2.100
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         POS TARG -11.00,-10.50;
    req_3:         SEQ 2.1-2.2 NO GAP;
    req_4:         GROUP 2.1-2.4 WITHIN 5D
    comment_1:     SECOND OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       2.200
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 2.2 AS 2.1
    comment_1:     SECOND OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       2.300
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         POS TARG -11.00,-10.50;
    req_3:         SEQ 2.3-2.4 NO GAP
    comment_1:     SECOND OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       2.400
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 2.4 AS 2.3
    comment_1:     SECOND OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       3.100
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         POS TARG -10.50,-10.75;
    req_3:         SEQ 3.1-3.2 NO GAP;
    req_4:         GROUP 3.1-3.4 WITHIN 5D
    comment_1:     THIRD OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       3.200
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 3.2 AS 3.1
    comment_1:     THIRD OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       3.300
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         POS TARG -10.50,-10.75;
    req_3:         SEQ 3.3-3.4 NO GAP
    comment_1:     THIRD OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       3.400
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 3.4 AS 3.3
    comment_1:     THIRD OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!


    linenum:       4.100
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         POS TARG -10.75,-11.25;
    req_3:         SEQ 4.1-4.2 NO GAP;
    req_4:         GROUP 4.1-4.4 WITHIN 5D
    comment_1:     FOURTH OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       4.200
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 4.2 AS 4.1
    comment_1:     FOURTH OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES
!

    linenum:       4.300
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       1
    time_per_exp:  1800S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         POS TARG -10.75,-11.25;
    req_3:         SEQ 4.3-4.4 NO GAP
    comment_1:     FOURTH OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES

!

    linenum:       4.400
    targname:      3C324
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F702W
    num_exp:       3
    time_per_exp:  2100S
    s_to_n:        1
    s_to_n_time:   13200S
    fluxnum_1:     2
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4;
    req_2:         SAME POS FOR 4.4 AS 4.3
    comment_1:     FOURTH OF 4 POINTINGS SEPARATED BY
    comment_2:     SMALL POS TARG SHIFTS.  THE ORIENT IS
    comment_3:     CHOSEN TO POSITION FAINT CLUSTER
    comment_4:     GALAXIES AWAY FROM CCD BORDERS.
    comment_5:     USE SAME ORIENT FOR ALL EXPOSURES
!

! end of exposure logsheet

! No scan data records found