!   $Id: 5482,v 5.1 1994/07/27 18:31:24 pepsa Exp $
!
! Adopted by the RPS2 I/O Definition Team for
! prototyping LMN 4 Apr 94
!
coverpage:

  title_1:         HIGH RESOLUTION IMAGERY OF THE
    title_2:       RECURRENT NOVA T PYX'S NEXT ERUPTION  CYCLE4MEDIUM
    sci_cat:       INTERSTELLAR MEDIUM
    sci_subcat:    NOVAE
    proposal_for:  GO
    targ_of_opp:   Y
    longterm:      3
    pi_fname:      MICHAEL
    pi_mi:         M
    pi_lname:      SHARA
    pi_inst:       SPACE TELESCOPE SCIENCE INSTITUTE
    pi_country:    USA
    pi_phone:      410-338-4700
    hours_pri:     22.00
    num_pri:       1
    wf_pc:         Y
    time_crit:     Y
    off_fname:     PETER
    off_lname:     STOCKMAN
    off_title:     DEPUTY DIRECTOR
    off_inst:      3470
    off_addr_1:    3700 SAN MARTIN DRIVE
    off_city:      BALTIMORE
    off_state:     MD
    off_zip:       21218
    off_country:   USA
    off_phone:     410-338-4730
! end of coverpage

abstract:

    line_1:        The recurrent nova T Pyxidis displays at least three concentric
    line_2:        shells from its most recent eruptions (1920, 1944, and 1966).
    line_3:        It is one of only a dozen novae with known shells, and the only
    line_4:        recurrent nova with clearly resolved circumstellar matter. A
    line_5:        unique and once-only opportunity will exist during T Pyxidis'
    line_6:        next eruption (now overdue) to determine
    line_7:        1) The uniformity and isotropy of material (both dust and
    line_8:        different chemical elements) ejected in previous eruptions,
    line_9:        and
    line_10:       2) The smallest structures formed in nova eruptions.
    line_11:       The Planetary Camera will be used to obtain narrowband Hydrogen,
    line_12:       Helium, Nitrogen and Oxygen images, as well as broadband images.
    line_13:       These will be used to search for fluorescence and reflection light
    line_14:       echoes from, and small-scale structure in the nova
    line_15:       circumstellar gas and dust ejecta.
    line_16:       We note that this proposal was granted HST time during cycle 1.
    line_17:       The time was rescinded after the spherical aberration problem
    line_18:       was discovered. The refurbished HST and WFPCII will be able to
    line_19:       carry out all the scientific goals of the original proposal.

!
! end of abstract

general_form_proposers:

  lname:           WILLIAMS
    fname:         ROBERT
    inst:          SPACE TELESCOPE SCIENCE INSTITUTE
    country:       USA
    esa:           N

!

  lname:           PRIALNIK
    fname:         DINA
    inst:          TEL-AVIV UNIVERSITY
    country:       ISRAEL
    esa:           N

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        We propose to use the Planetary Camera CCD to image the nova shell
    line_2:        in the brightest emission lines seen its spectra (Williams, ApJ 261, 170
    line_3:        (1982)) before, during and after eruption. Narrowband filters at Halpha,
    line_4:        HeII, [NII], [OII] and [OIII], as well as reference images in B and R will be
    line_5:        taken as soon as possible after HST refurbishment (hopefully before the
    line_6:        next eruption
    line_7:        and then about 4, 10, 20, 40, 100, 200, and 600 days after eruption.
    line_8:        The light sphere from the nova flash expands at
    line_9:        the rate of 1"/week at the distance of T Pyx (1 kpc). (This dictates the
    line_10:       timescale of the first 4 proposed visits). We will search
    line_11:       for successively more distant dust and gas from previous eruptions
    line_12:       to determine how much previous debris has now become too faint to see,
    line_13:       and the smallest visible structures in older ejecta. We will also search
    line_14:       for systematic chemical and/or ionization structures in the previous
    line_15:       eruptions ejecta as the expanding nova flash lights it up.
    line_16:       In summary, we expect to be able to resolve spatial and chemical
    line_17:       structures in the ejecta of a nova only a few nova photospheric radii
    line_18:       in size (10 ** 15 cm).
    line_19:       We will also see light echoes and fluorescence from the dust and gas,
    line_20:       respectively, ejected in the last two or three eruptions.

!

  question:        4
    section:       1
    line_1:        The high spatial resolution of HST is essential to reolve the smallest
    line_2:        ejecta features.

!

  question:        5
    section:       1
    line_1:        Narrowband filters at Halpha,
    line_2:        HeII, [NII], [OII] and [OIII], as well as reference images in B and R
    line_3:        will be taken as soon as possible after HST refurbishment
    line_4:        (hopefully before the next eruption
    line_5:        200, and 600 days after eruption. (This proposal is thus, of necessity,
    line_6:        a (rather urgent) GO cycle 4 proposal, a target-of-opportunity proposal,
    line_7:        and a long-term proposal.)
    line_8:        As ejected material expands away from the explosion at roughly
    line_9:        2 * 10 **8 cm/s, the newly formed shell should begin to be resolvable
    line_10:       (0.1-0.2 arcsec) in 5 * 10**6 seconds, i.e. 2 months. After 2 years
    line_11:       groundbased imagery will be able to resolve the inner shell and follow
    line_12:       subsequent evolution and expansion of the ejected gas. This dictates
    line_13:       the timescale and frequency of the last 3 observation sets in the
    line_14:       previous paragraph.

!


!

  question:        8
    section:       1
    line_1:        The first set of observations should be scheduled as soon as possible,
    line_2:        because T Pyx is now overdue for eruption. These "before outburst"
    line_3:        images are important to help interpret changes during outburst.

!

  question:        10
    section:       1
    line_1:        Sparcstation support.

!
!end of general form text

general_form_address:

  lname:           Shara
    fname:         Michael
    category:      PI
    inst:          3470
    addr_1:        3700 San Martin Dr.
    city:          Baltimore
    state:         MD
    zip:           21218
    country:       USA
    phone:         410-516-4543

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        TPYX
    descr_1:       A
    descr_2:       152,161
    pos_1:         RA=09H 04M 41.5S +/- 0.1S,
    pos_2:         DEC=-32D 22' 47" +/- 1"
    equinox:       2000
    fluxnum_1:     1
    fluxval_1:     V=18 +/-1, TYPE=A0

!
! end of fixed targets

! No solar system records found

! No generic target records found

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!

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!

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!

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!

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!

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!

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!

    linenum:       8.100
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    linenum:       9.700
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    req_3:         SAME POS FOR 9.1-9.6 AS 9.7;
    req_4:         TARG OF OPP / 9.1-9.7;
    req_5:         AFTER 8.1 BY 400D +/- 30D;

!
! end of exposure logsheet

! No scan data records found