!   $Id: 5458,v 27.1 1994/07/27 18:13:32 pepsa Exp $

coverpage:

  title_1:         EVOLUTION OF GALAXIES IN INTERMEDIATE REDSHIFT CLUSTERS : IMAGING
    title_2:       OF ABELL 665 : CYCLE 4 MEDIUM
    sci_cat:       GALAXIES & CLUSTERS
    sci_subcat:    EVOLUTION/COSMOLOGY
    proposal_for:  GO
    pi_fname:      MARIJN
    pi_lname:      FRANX
    pi_inst:       6830
    pi_country:    NETHERLANDS
    pi_phone:      (011) 31 50 634067
    hours_pri:     6.69
    num_pri:       2
    wf_pc:         Y
    off_fname:     PIET
    off_lname:     VAN DER KRUIT
    off_title:     CHAIRMAN
    off_inst:      6830
    off_addr_1:    KAPTEYN ASTRONOMICAL LABORATORY
    off_addr_2:    P. O. BOX 800
    off_city:      GRONINGEN
    off_zip:       9700 AV
    off_country:   NETHERLANDS
    off_phone:     (011) 31 50 634053
! end of coverpage

abstract:

    line_1:        One of the more fundamental problems in current astronomy is that of galaxy
    line_2:        evolution. We still do not have good constraints on how galaxy densities,
    line_3:        types, and luminosities evolve with redshift. Most studies until now have used
    line_4:        only photometric and spectrophotometric information to derive 'spectral'
    line_5:        classifications and luminosities.  Whereas these methods will remain essential
    line_6:        to understanding evolution, they are insufficient for a unique interpretation
    line_7:        of the data. I have started a ground-based program to measure dynamical
    line_8:        parameters of galaxies in intermediate redshift clusters.  I have successfully
    line_9:        measured velocity dispersions, and in some cases, rotational velocities.  These
    line_10:       dynamical data are a fundamental step forward towards quantifying the effects
    line_11:       of 'passive evolution', mergers, starburst, etc. The first results on
    line_12:       galaxies in Abell 665 at z=0.18 have demonstrated the value of these data
    line_13:       amply: one of the galaxies is an E+A galaxy, rotates rapidly, and lies far
    line_14:       off the Faber-Jackson relation measured for other cluster galaxies. This
    line_15:       is the first time that such detailed information has become available on such
    line_16:       a galaxy, and it provides insight into the mechanisms which cause the rapid
    line_17:       evolution of  galaxies in rich clusters (the Butcher--Oemler effect). Here it
    line_18:       is proposed to obtain 2 color WFPC images of this galaxy, and the other cluster
    line_19:       galaxies. This galaxy is ideally suited because of it brightness, rather low
    line_20:       redshift, and the detailed groundbased data.

!
! end of abstract

general_form_proposers:

  lname:           FRANX
    fname:         MARIJN
    inst:          6830
    country:       NETHERLANDS
    esa:           Y

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        I propose to take WFPC2 images of Abell 665, a well studied cluster at a
    line_2:        redshift of 0.18.  This cluster is one of the clusters for which the
    line_3:        Sunyaev-Zel'dovitch effect has been established(1), and a good dataset of
    line_4:        spectra and radial velocities are available(2,3).  I have already measured
    line_5:        internal velocity dispersions for a sample of galaxies (4).  Images will be
    line_6:        taken in two passbands (F606W and F814W). This will provide the detailed
    line_7:        morphological information on the galaxies,  and detailed color
    line_8:        information. The E+A galaxy is one of the best studied Butcher Oemler
    line_9:        galaxies, and the color information is going to be particularly interesting. As
    line_10:       an example, we can determine whether the starbust formed only a disk component,
    line_11:       or whether it contributed to both bulge and disk. We can also hope to determine
    line_12:       disk and bulge parameters separately, which will enable us to make an easy
    line_13:       comparison with galaxies in nearby clusters. The hope is to find the class of
    line_14:       galaxies into which these Butcher Oemler galaxies evolved.
    line_16:       Two fields will be studied, both in two colors. These two fields will include
    line_17:       all the galaxies for which kinematic data is available.  The integration time
    line_18:       in each passband will be two orbits. Experience with current deep cluster
    line_19:       imaging, and folding in the improved PSF, but lower quantum efficiency,
    line_20:       indicates that such integration times will produce images with the fine detail
    line_21:       necessary for morphological and color studies.
    line_23:       1 Birkinshaw, Hughes and Arnaud, 1991, Ap. J. in press.

!

  question:        3
    section:       2
    line_1:        2 Oegerle, Fitchett, Hill, Hintzen, 1991, preprint.
    line_2:        3 Birkinshaw, private communication.
    line_3:        4 Franx, 1993, ApJ L 407, 5.
    line_5:        Postscript: Note that the "blue" filter has been changed from F555W
    line_6:        to F606W. This is done because of the higher throughput of F606W,
    line_7:        which amounts to a factor of 2 more signal.
    line_9:        NOTE: THE PI HAS ALTERNATE SUGGESTIONS FOR TARGET POSITIONS, ORIENT ANGLES,
    line_10:       AND FOR POSSIBLE RELAXATION OF SOME CONSTRAINTS IN THE SPECIAL REQUIREMENTS
    line_11:       IF NEEDED FOR SCHEDULING. PLEASE CONTACT THE PI IF THERE ARE PROBLEMS OF THIS
    line_12:       SORT FOR WHICH HE MAY HAVE USEFUL SUGGESTIONS.

!

  question:        4
    section:       1
    line_1:        The need for HST images is obvious since there is no spherical aberration after
    line_2:        the repair mission.  It will provide us with 2D photometry comparable to the
    line_3:        ground-based data that can be achieved on Coma. Thus detailed structural
    line_4:        studies are possible.  It is obvious that no such detailed information is
    line_5:        available from the ground (see also Figure 5
    line_6:        ground based images can be improved by deconvolution, it is impossible to
    line_7:        retrieve the small scale color information that we plan to obtain through the
    line_8:        HST images. Especially for the E+A galaxy, such color information is essential
    line_9:        for a proper understanding of the underlying mechanisms.

!

  question:        5
    section:       1
    line_1:        THERE IS A BRIGHT STAR QUITE NEAR TO THE OBJECT. PLEASE READ SECTION
    line_2:        8 WHERE I  EXPLAIN MY STRATEGY TO AVOID BLEEDING AND SCATTERED LIGHT.
    line_5:        NOTE: THE PI HAS ALTERNATE SUGGESTIONS FOR TARGET POSITIONS, ORIENT ANGLES,
    line_6:        AND FOR POSSIBLE RELAXATION OF SOME CONSTRAINTS IN THE SPECIAL REQUIREMENTS
    line_7:        IF NEEDED FOR SCHEDULING. PLEASE CONTACT THE PI IF THERE ARE PROBLEMS OF THIS
    line_8:        SORT FOR WHICH HE MAY HAVE USEFUL SUGGESTIONS.

!

  question:        6
    section:       1
    line_1:

!


!

  question:        8
    section:       1
    line_1:        There is a bright star quite near to the most interesting object in the
    line_2:        field. To avoid bleeding and/or ghosts, it is important that the star
    line_3:        does NOT get onto the same Chip as the object. The star lies south of
    line_4:        the object. The position that I define in ABELL0665-POS1 is
    line_5:        in between the galaxy and the star. I define as the field of view
    line_6:        PC1-FIX, and then give a POS-TARG = -18.4, -18.4, so that the
    line_7:        apex of the pyramid falls exactly on the position ABELL0665-POS1.
    line_8:        There is a distance of about 16
    line_9:        arcsec in between the galaxy and the star. I then require that the
    line_10:       position angle of the telescope is such that the object falls on
    line_11:       one of the chips - this gives four positions angles to choose
    line_12:       from, plus some leeway. Note that observations could also be done at
    line_13:       other position angles, but I would have to select a different field
    line_14:       center, to avoid the bright star. PLEASE CONTACT ME DIRECTLY DURING THE
    line_15:       PLANNING OF THE OBSERVATIONS. I CAN AT ANY TIME DEFINE A NEW FIELD
    line_16:       CENTER AT ANY GIVEN POSITION ANGLE OF THE TELESCOPE . FEEL WELCOME
    line_17:       TO CALL ME OUT OF BED (BUT TRY AN EMAIL FIRST: FRANX@ASTRO.RUG.NL).
    line_18:       For field 2 (ABELL0665-POS2) a similar constraint applies. There
    line_19:       are some stars near the edge of the field, which I want to avoid.
    line_20:       The current field center allows 4 position angles. AGAIN,
    line_21:       I CAN ADAPT THE FIELD CENTER TO ACCOMODATE ANY POSITION ANGLE.

!

  question:        8
    section:       2
    line_1:        There is considerable freedom in changing the exposure times. The main
    line_2:        purpose is to get as high signal to noise as possible (so, the longest
    line_3:        integration time. It helps if each field/passband combination has
    line_4:        two exposures with identical exposure time, and this exposure time
    line_5:        should be above 1600 sec. Feel free to change things to these criteria,
    line_6:        and please contact me to make sure everything is OK. My email is
    line_7:        franx@astro.rug.nl. I am asking for 2 images with identical exposure
    line_8:        time to facilitate removal of cosmic ray events.

!

  question:        9
    section:       1
    line_1:
    line_2:        Approved Proposals on which I am PI:
    line_3:        Evolution of Galaxies in Intermediate Redshift Clusters: Imaging of
    line_4:        CL0024+16
    line_5:        Cycle 2 Archival proposal # 3503.
    line_7:        This archival proposal is related to the current proposal. The data has
    line_8:        just been released.
    line_10:       Co-I on the following proposals:
    line_12:       Ellipticals with Kinematically Distinct Nuclei # 3441 Cycle 2.
    line_13:       First paper is being written. No direct relation to the current proposal.
    line_15:       Nearby Nuclei Snapshot survey # 4664 Cycle 3.
    line_16:       The data is just coming in.

!

  question:        10
    section:       1
    line_1:        I am a full professor at the University of Groningen, and have full
    line_2:        access to all research facilities, which includes computing, library,
    line_3:        preprint services, etc. Students, travel money, etc. are available.

!
!end of general form text

general_form_address:

  lname:           FRANX
    fname:         MARIJN
    category:      PI
    inst:          6830
    addr_1:        KAPTEYN ASTRONOMICAL LABORATORY
    addr_2:        P. O. BOX 800
    city:          GRONINGEN
    zip:           9700 AV
    country:       NETHERLANDS
    phone:         (011) 31 50 634067
    telex:         FRANX@ASTRO.RUG.NL

!

  lname:
    category:      CON

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        ABELL0665-POS1
    descr_1:       F,404
    pos_1:         RA= 08H26M09.77S +/-0.1S,
    pos_2:         DEC= +66D00'31.2" +/- 0.1"
    equinox:       B1950
    comment_1:     PLEASE READ SECTION 8
    comment_2:     ABOUT THE POSITIONING.
    comment_3:     WHEN CENTERED ON THIS POSI-
    comment_4:     TION, BRIGHT STAR IN
    comment_5:     SOUTHERN FIELD, WHICH WILL
    comment_6:     SATURATE CCD
    fluxnum_1:     1
    fluxval_1:     SURF-BKG(R) = 19 +/- 1.0

!

    targnum:       2
    name_1:        ABELL0665-POS2
    descr_1:       F,404
    pos_1:         RA= 08H26M29.85S +/-0.1S,
    pos_2:         DEC= +66D00'11.1" +/- 0.1"
    equinox:       B1950
    comment_1:     PLEASE READ SECTION 8
    comment_2:     ABOUT THE POSITIONING.
    comment_3:     THIS FIELD DOES NOT CONTAIN
    comment_4:     THE BRIGHT STAR.
    fluxnum_1:     1
    fluxval_1:     SURF-BKG(R) = 19 +/- 1.0
!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    targname:      ABELL0665-POS2
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F606W
    num_exp:       2
    time_per_exp:  2200S
    fluxnum_1:     1
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         CYCLE 4 / 1-4;
    req_2:         ORIENT 276D +/- 6D;
    req_3:         POS TARG -18.4, -18.4
    comment_1:     ORIENTATIONS 96 +-6, 186 +- 6 AND
    comment_2:     276 +- 6 ALSO ALLOWED. PLEASE READ
    comment_3:     GF QUESTION 8 ABOUT THE ORIENTA-
    comment_4:     TIONS. POS2 OBS TO BE DONE BEFORE
    comment_5:     POS1 OBS. 

!

    linenum:       2.000
    targname:      ABELL0665-POS2
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F814W
    num_exp:       2
    time_per_exp:  2200S
    fluxnum_1:     1
    priority:      1
    param_1:       CR-SPLIT=NO
    req_2:         SAME POS FOR 2 AS 1;
    req_4:         GROUP 1-2 NO GAP
    comment_3:     ALL OBS OF POS2 SHOULD BE
    comment_4:     REASONABLY CLOSE TO EACH OTHER
    comment_5:     IN TIME, BUT WE MAY RELAX THIS
    comment_6:     CONSTRAINT. CONTACT PI IF NEEDED.

!

    linenum:       3.000
    targname:      ABELL0665-POS1
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F606W
    num_exp:       3
    time_per_exp:  1700S
    fluxnum_1:     1
    priority:      1
    param_1:       CR-SPLIT=NO
    req_1:         AFTER 2;
    req_3:         SAME ORIENT FOR 3-4 AS 1;
    req_4:         POS TARG -18.4, -18.4
    comment_1:     DO NOT USE WFC WITHIN A
    comment_2:     HALF HOUR AFTER LAST EXPOSURE.
    comment_4:     DO AFTER LOG LINE 2. ALL OBS OF POS1
    comment_5:     SHOULD BE CLOSE TOGETHER IN TIME, BUT
    comment_6:     CONSTRAINT MAY BE RELAXED. CALL PI.

!

    linenum:       4.000
    targname:      ABELL0665-POS1
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1-FIX
    sp_element:    F814W
    num_exp:       3
    time_per_exp:  1600S
    fluxnum_1:     1
    priority:      1
    param_1:       CR-SPLIT=NO
    req_3:         SAME POS FOR 4 AS 3;
    req_4:         GROUP 3-4 NO GAP
    comment_3:     SAME POSITION AND ORIENT AS
    comment_4:     EXP LOG LINE 3. 
!
! end of exposure logsheet

! No scan data records found