!   $Id: 5374,v 13.1 1995/01/25 20:31:33 pepsa Exp $


coverpage:

  title_1:         THE BRIGHT, MYSTERIOUS WHITE DWARF STAR PROCYON B CYCLE 4 MEDIUM
    sci_cat:       HOT STARS
    sci_subcat:    WHITE DWARFS
    proposal_for:  GO
    longterm:      1
    pi_fname:      HARRY
    pi_mi:         L
    pi_lname:      SHIPMAN
    pi_inst:       UNIVERSITY OF DELAWARE
    pi_country:    USA
    pi_phone:      302 831 2986
    hours_pri:     0.20
    num_pri:       1
    wf_pc:         Y
    off_fname:     THOMAS
    off_lname:     E
    off_title:     WHITE
    off_inst:      1840
    off_addr_1:    SPONSORED PROGRAMS ADMINISTRATION
    off_addr_2:    UNIVERSITY OF DELAWARE
    off_city:      NEWARK
    off_state:     DE
    off_zip:       19716
    off_country:   USA
    off_phone:     302 831-8001
! end of coverpage

abstract:

    line_1:        We request 1.5 hours of HST time in order to obtain images of
    line_2:        Procyon B in a variety of filters with the WF/PC-2.  These images
    line_3:        will allow us, for the first time, to determine the temperature,
    line_4:        radius, and spectral type of this star. The importance of Procyon
    line_5:        B is that it is one of a handful of white dwarf stars which are
    line_6:        in a visual binary system.  These data will allow us to place
    line_7:        Procyon B on the mass-radius relation, testing our concept of
    line_8:        relativistic degeneracy.  Furthermore, since the age of the system
    line_9:        is known, we can determine the mass of Procyon B's progenitor star
    line_10:       and thus provide an important fundamental datum to test theories
    line_11:       of stellar mass loss.

!
! end of abstract

general_form_proposers:

  lname:

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        Observations in various filters should permit us to determine how
    line_2:        bright Procyon B is, what its temperature is, and by using some
    line_3:        carefully selected filter combinations around H-alpha and H-beta,
    line_4:        determine whether it is a white dwarf of spectral type DA --
    line_5:        with hydrogen lines -- or type DZ -- without hydrogen lines.
    line_6:        Our observing strategy calls for a wide variety of filters and
    line_7:        exposure times.  We seek to replicate a series of Johnson UBVRI
    line_8:        observations, and make an observation in the ultraviolet, in
    line_9:        addition to our observations near the hydrogen lines.

!

  question:        3
    section:       2
    line_1:

!

  question:        4
    section:       1
    line_1:        As discussed in the "scientific justification" section, many observers
    line_2:        have tried and failed to obtain clean data on Procyon B from the
    line_3:        ground.  The spatial resolution is simply insufficient.

!

  question:        5
    section:       1
    line_1:        None.

!

  question:        6
    section:       1
    line_1:        None.

!


!

  question:        8
    section:       1
    line_1:

!

  question:        9
    section:       1
    line_1:        Shipman was PI and leader of a massive team of astronomers who
    line_2:        obtained time in cycles 1 and 2 for a comprehensive attack on a
    line_3:        variety of problems related to white dwarf stars.  This project,
    line_4:        under the title of "White Dwarf Stars," was allotted 17.5 hours
    line_5:        of spacecraft time in cycle 1 and 15 hours in cycle 2. Program
    line_6:        numbers were 2593 (cycle 1) and 3816 (cycle 2).
    line_8:        Most team members agreed with me in believing that obtaining some
    line_9:        data on Procyon B was one of the most important things to do with
    line_10:       our precious HST time.  We knew that obtaining clean data with
    line_11:       an optically defective telescope was chancy.  We have done all that
    line_12:       we can do with the cycle 1 data, postponing work on some important
    line_13:       spectra because Procyon B was more important.  We took a chance,
    line_14:       and did not succeed.  We wish to try again.
    line_16:       As for the remainder of our HST data, we have presented the spectra
    line_17:       at a conference in the summer of 1992 and at the Phoenix AAS meeting.
    line_18:       Three papers describing these results are in the final stages of
    line_19:       preparation.

!

  question:        10
    section:       1
    line_1:        The PI's and the co-I's are all faculty members at universities,
    line_2:        or equivalent, and the institutions are supporting this project by
    line_3:        providing us with the time and facilities to do the research.
    line_4:        The PI's institution will acquire a workstation which will be
    line_5:        used for the data reduction.

!
!end of general form text

general_form_address:

  lname:           Shipman
    fname:         Harry
    mi:            L
    category:      PI
    inst:          1840
    addr_1:        Department of Physics and Astronomy
    addr_2:        University of Delaware
    city:          Newark
    state:         DE
    zip:           19716
    country:       USA
    phone:         302 831 2986
    telex:         harrys@strauss.udel.edu

!

  lname:           Bond
    fname:         Howard
    inst:          3470
    country:       USA

!

  lname:           Liebert
    fname:         James
    inst:          1212
    country:       USA

!

  lname:
    category:      CON

!

  lname:           Roby
    fname:         Scott
    inst:          2986
    country:       USA

!

  lname:           Sion
    fname:         Ed
    inst:          3720
    country:       USA

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        ALPHA-C-MI-B
    name_2:        BD+5D1739
    descr_1:       A,136
    pos_1:         RA=07H 36M 39.01215S +/- 0.003S,
    pos_2:         DEC=+05D 20' 31.0195" +/- 0.02"
    equinox:       1950.0
    pm_or_par:     Y
    pos_epoch_bj:  B
    pos_epoch_yr:  1994.50
    ra_pm_val:     -0.047300
    dec_pm_val:    -1.0290
    an_prlx_val:   0.2850
    comment_1:     THE FLUX VALUE GIVEN ABOVE IS FOR
    comment_2:     THE SCIENTIFIC TARGET PROCYON B.
    comment_3:     THE POSITION IS FOR PROCYON A, THE
    comment_4:     ONE WHICH WE WANT AT THE OPTIMUM
    comment_5:     CENTER OF THE PC TO START.
    comment_6:     IN CASE YOU NEED TO KNOW, THE V
    comment_7:     MAGNITUDE OF PROCYON A IS 0.4.
    comment_8:     PROCYON B IS ABOUT 5 ARCSEC NORTH
    comment_9:     OF PROCYON A.
    fluxnum_1:     1
    fluxval_1:     V=10.7 +/- 0.1

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.010
    targname:      ALPHA-C-MI-B
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1
    sp_element:    F218W
    wavelength:    2159
    num_exp:       1
    time_per_exp:  0.11S
    fluxnum_1:     1
    priority:      1
    param_2:       ATD-GAIN=15
    req_1:         CYCLE 4 / 1.01-1.410;
    req_2:         ORIENT 69D +/-10D / 1.010-1.410;
    req_3:         SEQ 1.010-1.050 NON-INT

!
    linenum:       1.020
    targname:      ALPHA-C-MI-B
    config:        WFPC2
    opmode:        IMAGE
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    sp_element:    F218W
    wavelength:    2159
    num_exp:       1
    time_per_exp:  35S
    fluxnum_1:     1
    priority:      1
    param_1:       CLOCKS=YES,
    param_2:       ATD-GAIN=15

!
    linenum:       1.030
    targname:      ALPHA-C-MI-B
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    wavelength:    2159
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    time_per_exp:  160S
    fluxnum_1:     1
    priority:      1
    param_1:       CLOCKS=YES,
    param_2:       ATD-GAIN=15

!
    linenum:       1.040
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    opmode:        IMAGE
    aperture:      PC1
    sp_element:    F255W
    wavelength:    2159
    num_exp:       1
    time_per_exp:  0.11S
    fluxnum_1:     1
    priority:      1
    param_2:       ATD-GAIN=15

!
    linenum:       1.05
    targname:      ALPHA-C-MI-B
    config:        WFPC2
    opmode:        IMAGE
    aperture:      PC1
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    num_exp:       1
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    fluxnum_1:     1
    priority:      1
    param_1:       CLOCKS=YES,
    param_2:       ATD-GAIN=15

!

    linenum:       1.110
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    wavelength:    5623
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    fluxnum_1:     1
    priority:      1
    param_2:       ATD-GAIN=15
!

    linenum:       1.120
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    time_per_exp:  5S
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    param_2:       ATD-GAIN=15

!

    linenum:       1.130
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    param_2:       ATD-GAIN=15

!

    linenum:       1.140
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!

    linenum:       1.150
    targname:      ALPHA-C-MI-B
    config:        WFPC2
    opmode:        IMAGE
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    sp_element:    F791W
    wavelength:    7829
    num_exp:       1
    time_per_exp:  0.23S
    fluxnum_1:     1
    priority:      1
    param_2:       ATD-GAIN=15

!

    linenum:       1.200
    targname:      ALPHA-C-MI-B
    config:        WFPC2
    opmode:        IMAGE
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    fluxnum_1:     1
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    param_2:       ATD-GAIN=15

!

    linenum:       1.210
    targname:      ALPHA-C-MI-B
    config:        WFPC2
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    aperture:      PC1
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    param_2:       ATD-GAIN=15

!

    linenum:       1.220
    targname:      ALPHA-C-MI-B
    config:        WFPC2
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    param_2:       ATD-GAIN=15

!

    linenum:       1.300
    targname:      ALPHA-C-MI-B
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    opmode:        IMAGE
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    fluxnum_1:     1
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    param_1:       CLOCKS=YES,
    param_2:       ATD-GAIN=15

!

    linenum:       1.310
    targname:      ALPHA-C-MI-B
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    fluxnum_1:     1
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    param_1:       CLOCKS=YES,
    param_2:       ATD-GAIN=15

!

    linenum:       1.320
    targname:      ALPHA-C-MI-B
    config:        WFPC2
    opmode:        IMAGE
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    wavelength:    5013
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    fluxnum_1:     1
    priority:      1
    param_1:       CLOCKS=YES,
    param_2:       ATD-GAIN=15

!

    linenum:       1.410
    targname:      ALPHA-C-MI-B
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    time_per_exp:  600S
    fluxnum_1:     1
    priority:      1
    param_1:       CLOCKS=YES,
    param_2:       ATD-GAIN=15

!


! end of exposure logsheet

! No scan data records found