!   $Id: 5208,v 5.1 1994/07/27 15:55:05 pepsa Exp $

coverpage:

  title_1:         STAR FORMATION HISTORIES AND STELLAR POPULATIONS IN
    title_2:       LOCAL GROUP IRREGULAR GALAXIES
    sci_cat:       GALAXIES & CLUSTERS
    sci_subcat:    STELLAR POPULATIONS
    proposal_for:  GTO/WF2
    pi_fname:      JOHN
    pi_lname:      TRAUGER
    pi_inst:       2370
    pi_country:    USA
    hours_pri:     3.03
    num_pri:       1
    wf_pc:         Y
    realtime:      N
    time_crit:     Y
! end of coverpage

abstract:

    line_1:        Stellar populations preserve the star formation histories of galaxies
    line_2:        and thus are useful windows for viewing galactic evolutionary
    line_3:        processes.  In this project we will use the superior sensitivity of
    line_4:        WFPC-2 to measure stellar populations in the outer
    line_5:        regions of Local Group irregular galaxies.  Irregulars usually have
    line_6:        star-forming cores that are superimposed on background sheets
    line_7:        containing redder, older stars.  H-R diagrams constructed from these
    line_8:        data will allow us to probe outer region star formation histories
    line_9:        during the past 1-10 Gyr.  The results from this program thus will
    line_10:       include an improved understanding of the Pop II components of
    line_11:       irregular galaxies, as well as new insights into the way that these
    line_12:       galaxies have formed stars.  For example, these observations will be
    line_13:       sensitive to bursts of star formation within the the past 5-7 Gyr from
    line_14:       the relative numbers of AGB versus RGB tip stars.  They will also
    line_15:       address the question of when the bulk of the redder stars formed in
    line_16:       small galaxies.  Some theoretical models suggest these should be
    line_17:       ancient objects that formed in violent star bursts (e.g. CDM models),
    line_18:       while other data suggest smaller galaxies form more slowly than giant
    line_19:       spirals, and these differences should appear in the background stellar
    line_20:       populations.

!
! end of abstract

general_form_proposers:

  lname:           TRAUGER
    fname:         JOHN
    title:         PI
    inst:          2370
    country:       USA

!

  lname:           BURROWS
    fname:         CHRIS
    inst:          STSCI
    country:       USA

!

  lname:           CLARKE
    fname:         JOHN
    inst:          UNIV. OF MICHIGAN
    country:       USA

!

  lname:           CRISP
    fname:         DAVID
    inst:          JPL
    country:       USA

!

  lname:           HOESSEL
    fname:         JOHN
    inst:          UNIV. OF WISCONSIN
    country:       USA

!

  lname:           GALLAGHER
    fname:         JAY
    inst:          UNIV. OF WISCONSIN
    country:       USA

!

  lname:           GRIFFITHS
    fname:         RICHARD
    inst:          JOHNS HOPKINS UNIV
    country:       USA

!

  lname:           HESTER
    fname:         JEFF
    inst:          ARIZONA STATE UNIV.
    country:       USA

!

  lname:           HOLTZMAN
    fname:         JOHN
    inst:          LOWELL OBSERVATORY
    country:       USA

!

  lname:           MOULD
    fname:         JEREMY
    inst:          CALTECH
    country:       USA

!

  lname:           WESTPHAL
    fname:         JAMES
    inst:          CALTECH
    country:       USA

!
! end of general_form_proposers block

general_form_text:

  question:        3
    section:       1
    line_1:        1000s x 4 exposures in V and I.

!

  question:        4
    section:       1
    line_1:        This program is designed to build on ground-based observations by
    line_2:        providing (1) better angular resolution (1 pc at 1Mpc---we still have
    line_3:        to work at low stellar densities to avoid excessive crowding), (2) much
    line_4:        improved discrimination against confusion by background galaxies, and
    line_5:        (3) substantial reduction in the I band sky background.
    line_7:        Exposure times are based on modelling of K and M stars with
    line_8:        STLOOK2, and effective use of orbits.  Even at 1000s, the dominant
    line_9:        source of noise will be the sky background rather than read noise.

!

  question:        13
    section:       1
    line_1:        This proposal forms an important part of the `Stellar Populations'
    line_2:        section of the peer-reviewed WFPC-2 GTO program.

!
!end of general form text

general_form_address:

  lname:           Trauger
    fname:         John
    title:         PI
    category:      PI
    inst:          2370
    country:       USA

!
! end of general_form_address records

fixed_targets:

    targnum:       1
    name_1:        LMC-HALO
    descr_1:       E,305,911
    pos_1:         RA  =  05H 14M 33S +/- 1" ,
    pos_2:         DEC = -65D 21' 00"   +/- 1"
    equinox:       1950

!
! end of fixed targets

! No solar system records found

! No generic target records found

exposure_logsheet:

    linenum:       1.000
    sequence_1:    DEFINE
    sequence_2:    WF-IMAGE
    targname:      #
    config:        WFPC2
    opmode:        IMAGE
    aperture:      WFALL-FIX
    sp_element:    #
    num_exp:       #
    time_per_exp:  1S
    priority:      1
    param_1:       CR-SPLIT = 0.5
    param_2:       ATD-GAIN = 15
    req_1:         CYCLE 4 / 2-3 ;
    req_2:         SEQ 2-3 NO GAP ;
    req_3:         PCS MODE F / 2-3 ;
    req_4:         ORIENT 180D +/- 45D / 2-3

!

    linenum:       2.000
    sequence_1:    USE
    sequence_2:    WF-IMAGE
    targname:      LMC-HALO
    sp_element:    F555W
    num_exp:       2
    time_per_exp:  X2000

!

    linenum:       3.000
    sequence_1:    USE
    sequence_2:    WF-IMAGE
    targname:      LMC-HALO
    sp_element:    F814W
    num_exp:       2
    time_per_exp:  X2000

!
! end of exposure logsheet

! No scan data records found