! $Id: 5366,v 4.1 1994/07/27 17:08:55 pepsa Exp $
coverpage:
title_1: THE CHRONOLOGY OF THE GALACTIC HALO AND DISK
title_2: CYCLE4HIGH
sci_cat: GALAXIES & CLUSTERS
sci_subcat: STELLAR POPULATIONS
proposal_for: GO
cont_id: 2419
pi_fname: ROBERT
pi_mi: J
pi_lname: ZINN
pi_inst: YALE UNIVERSITY
pi_country: UNITED STATES
pi_phone: 203-432-3017
hours_pri: 15.30
num_pri: 7
wf_pc: Y
off_fname: SUZANNE
off_lname: POLMAR
off_title: DIR GRANTS&CONTRACT
off_inst: 3900
off_addr_1: YALE UNIVERSITY
off_addr_2: GRANT AND CONTRACT ADMINISTRATION
off_addr_3: 12 PROSPECT PLACE
off_city: NEW HAVEN
off_state: CT
off_zip: 06511
off_country: UNITED STATES
off_phone: 203-432-2460
! end of coverpage
abstract:
line_1: Observations with the WFPC2 will be used to construct color-magnitude
line_2: diagrams that precisely determine the magnitude and color of the
line_3: main-sequence turnoff and lower giant branch, and allow the ages
line_4: of 7 globular clusters to be derived. Four are metal-rich clusters of
line_5: the disk population and three are very metal-poor clusters near the
line_6: galactic center. Only the HST can provide the very high resolution
line_7: necessary for photometry to the required faint limits in the crowded
line_8: fields of these clusters. The ages of the clusters will be measured
line_9: from the c-m diagrams using several techniques, and will be compared
line_10: with each other and with the ages derived for other clusters from
line_11: ground-based observations. Our investigation will yield the first
line_12: chronology of the halo and thick disk clusters near the galactic
line_13: center, where star formation may have proceeded more rapidly than
line_14: in the outer, lower density regions. Age differences > 3 Gys. are
line_15: now known to exist among the globular clusters in the outer halo,
line_16: and the addition of our results will indicate the timescales of
line_17: halo and disk formation as functions of galactocentric distance.
line_18: This will tightly constrain theories of the evolution of the Galaxy.
line_19: This proposal is a resubmission of a GO proposal that had to be
line_20: largely deferred until after the repair mission.
!
! end of abstract
general_form_proposers:
lname: ZINN
fname: ROBERT
inst: 3900
country: UNITED STATES
!
lname: CARNEY
fname: BRUCE
inst: 2990
country: UNITED STATES
!
lname: CHRISTIAN
fname: CAROL
inst: 1502
country: UNITED STATES
!
lname: DA COSTA
fname: GARY
inst: 4110
country: AUSTRALIA
!
lname: DEMARQUE
fname: PIERRE
inst: 3900
country: UNITED STATES
!
lname: HEASLEY
fname: JAMES
inst: 2192
country: UNITED STATES
!
lname: JANES
fname: KENNETH
inst: 1420
country: UNITED STATES
!
lname: OLSZEWSKI
fname: EDWARD
inst: 1212
country: UNITED STATES
!
lname: SEITZER
fname: PATRICK
inst: 2660
country: UNITED STATES
!
! end of general_form_proposers block
general_form_text:
question: 3
section: 1
line_1: Our program is designed to obtain high-precision relative photometry for
line_2: all the stars in the WFPC2 fields. This will allow us to determine
line_3: the mean positions of the cluster principal sequences with much
line_4: greater precision than the photometry of an individual star. Since it
line_5: is the relative locations of these sequences that yield the differences
line_6: in cluster ages, our major goals can be achieved even if the zero points
line_7: of our photometry are difficult to determine. The zero points are
line_8: unlikely to be a problem because they will be set by ground-based
line_9: observations (see below).
line_10: The PC chip of the WFPC2 will be used to photometer the regions of
line_11: highest stellar density, while the WFC chips will record the outer
line_12: regions and the star fields surrounding the clusters. 3 or 4 long
line_13: exposures per filter will be taken of a field close to the center of
line_14: each cluster. The long exposures are designed to achieve S/N > 50 at
line_15: 2 mag. below the expected turnoffs of the clusters, which should
line_16: enable us to achieve the required photometric accuracy in these dense
line_17: fields. Three short exposures at the same positions will provide an
line_18: extension of the PC's dynamic range to brighter stars in the field
line_19: (horizontal branch & lower giant branch). We will also take sets of
line_20: 3 or 4 long and three short exposures per filter of fields offset from
line_21: the first ones by 20 arcsecs in the directions away from the
line_22: cluster centers. These observations, which will overlap to some
line_23: extent with the central sets, will provide important additional
!
question: 3
section: 2
line_1: information on the principal cluster sequences. Ground-based
line_2: photometry of the brighter stars in these more radially distant fields,
line_3: which will be possible given their lower densities, will provide the
line_4: calibration of the WFPC2 observations. The WFPC2 observations will be
line_5: made with the F555W and F814W filters, for which straightforward
line_6: transformations to the V and I bands of the standard Cousins system
line_7: will be possible. The WFC images of the area around each cluster and
line_8: ground-based observations of comparison fields outside the tidal radii
line_9: of the clusters will be used to assess the contamination of the
line_10: cluster fields by non-cluster members.
!
question: 4
section: 1
line_1: Members of our team have constructed c-m diagrams of three of our
line_2: targets using large ground-based telescopes under excellent conditions,
line_3: and have achieved only limited success. Heasley, Janes, Christian, and
line_4: Montgomery (1993, in preparation) observed NGC 6293 with the CFHT and
line_5: its high resolution camera. Although their data have extremely small
line_6: images for ground-based observations, 0.5 arcsec FWHM, severe image
line_7: crowding in the central region of the cluster limited the quality of
line_8: the photometry. Accurate photometry was possible in the outer regions
line_9: of the cluster, but there confusion from numerous field stars limits
line_10: the precision to which the principal sequences of the clusters can be
line_11: defined. The same problem was encountered by Fullton, Carney, and
line_12: Seitzer (1993 in preparation) in their investigation of NGC 5927,
line_13: which they observed in 0.8 arcsec seeing with the CTIO 4m telescope.
line_14: Again the central regions of the cluster were inaccessible and in the
line_15: outer regions, where faint photometry was possible, the c-m diagram
line_16: is swamped by field stars.
line_17: This problem will be solved by the greater resolution of the WFPC2,
line_18: which will enable us to do precise photometry to the required faint
line_19: levels in fields where cluster stars outnumber the field stars.
line_20: Although our scientific objectives have not been met by our previous
line_21: photometry of NGC 6293 and 6352 with the PC, these data have shown
line_22: that the project is feasible with the WFPC2.
!
!
!
question: 9
section: 1
line_1: Our previous HST work consisted of the Cycle 1 proposal, GO 2419,
line_2: "The Chronology of the Formation of the Galactic Halo and Disk".
line_3: The present proposal is a continuation of this earlier project which
line_4: did receive some telescope time to see if it was feasible with the
line_5: impaired HST. Hence, this proposal has the same title, scientific
line_6: objectives, and P.I. and Co-I's as this earlier project.
!
question: 10
section: 1
line_1: The computational, image display, and software resources available at
line_2: Yale, Boston University, Arizona, North Caroline, Hawaii, Michigan,
line_3: Berkeley, and the Anglo-Australian Observatory (AAO) will be used for
line_4: the data reduction and analysis. The ground-based observations that
line_5: are necessary to support this project will be made with the telescopes
line_6: of Yale, Hawaii, Arizona, and AAO. The resources of Yale's Center for
line_7: Solar and Space Research will be used for the computation of
line_8: evolutionary tracks and isochrones. Graduate students
line_9: will take part in the data reduction, the acquisition of the
line_10: ground-based observations, and the theoretical computations.
!
!end of general form text
general_form_address:
lname: Zinn
fname: Robert
category: PI
inst: 3900
addr_1: Dept. of Astronomy
addr_2: Yale University
addr_3: Box 6666 260 Whitney Avenue
city: New Haven
state: CT
zip: 06511
country: United States
phone: 203-432-3017
telex: zinn@astro0.astro.yale.edu
!
! end of general_form_address records
fixed_targets:
targnum: 1
name_1: NGC5927-POS1
descr_1: C,201
pos_1: PLATE-ID = 0619,
pos_2: RA = 15H 27M 59.055S +/- 2",
pos_3: DEC = -50D 39' 54.99" +/- 2"
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 22.2 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.6 , TYPE = G0
!
targnum: 2
name_1: NGC5927-POS2
descr_1: C,201
pos_1: XI-OFF = +20" +/- 1",
pos_2: ETA-OFF = -20" +/- 1",
pos_3: FROM 1
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 22.2 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.6 , TYPE = G0
!
targnum: 3
name_1: NGC6293-POS1
descr_1: C,201
pos_1: PLATE-ID = 067P,
pos_2: RA = 17H 10M 10.239S +/- 2",
pos_3: DEC = -26D 34' 57.39" +/- 2"
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 22.0 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.4 , TYPE = G0
!
targnum: 4
name_1: NGC6293-POS2
descr_1: C,201
pos_1: XI-OFF = -20" +/- 1",
pos_2: ETA-OFF = -20" +/- 1",
pos_3: FROM 3
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 22.0 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.4 , TYPE = G0
!
targnum: 5
name_1: NGC6333-POS1
descr_1: C,201
pos_1: PLATE-ID = 06AM,
pos_2: RA = 17H 19M 10.850S +/- 2",
pos_3: DEC = -18D 31' 08.54" +/- 2"
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 21.8 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.2 , TYPE = G0
!
targnum: 6
name_1: NGC6333-POS2
descr_1: C,201
pos_1: XI-OFF = -20" +/- 1",
pos_2: ETA-OFF = +20" +/- 1",
pos_3: FROM 5
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 21.8 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.2 , TYPE = G0
!
targnum: 7
name_1: NGC6352-POS1
descr_1: C,201
pos_1: PLATE-ID = 0689,
pos_2: RA = 17H 25M 27.270S +/- 2",
pos_3: DEC = -48D 25' 27.55" +/- 2"
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 20.7 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 18.1 , TYPE = G0
!
targnum: 8
name_1: NGC6352-POS2
descr_1: C,201
pos_1: XI-OFF = +20" +/- 1",
pos_2: ETA-OFF = -20" +/- 1",
pos_3: FROM 7
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 20.7 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 18.1 , TYPE = G0
!
targnum: 9
name_1: NGC6541-POS1
descr_1: C,201
pos_1: PLATE-ID = 06AR,
pos_2: RA = 18H 08M 9.160S +/- 2",
pos_3: DEC = -43D 41' 52.75" +/- 2"
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 20.6 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 18.0 , TYPE = G0
!
targnum: 10
name_1: NGC6541-POS2
descr_1: C,201
pos_1: XI-OFF = -20" +/- 1",
pos_2: ETA-OFF = -20" +/- 1",
pos_3: FROM 9
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 20.6 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 18.0 , TYPE = G0
!
targnum: 11
name_1: NGC6624-POS1
descr_1: C,201
pos_1: PLATE-ID = 060E,
pos_2: RA = 18H 23M 44.007S +/- 2",
pos_3: DEC = -30D 21' 32.86" +/- 2"
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 21.6 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.0 , TYPE = G0
!
targnum: 12
name_1: NGC6624-POS2
descr_1: C,201
pos_1: XI-OFF = -28" +/- 1",
pos_2: ETA-OFF = +00" +/- 1",
pos_3: FROM 11
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 21.6 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.0 , TYPE = G0
!
targnum: 13
name_1: NGC6637-POS1
descr_1: C,201
pos_1: PLATE-ID = 060G,
pos_2: RA = 18H 31M 19.527S +/- 2",
pos_3: DEC = -32D 21' 17.76" +/- 2",
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 21.7 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.1 , TYPE = G0
!
targnum: 14
name_1: NGC6637-POS2
descr_1: C,201
pos_1: XI-OFF = +20" +/- 1",
pos_2: ETA-OFF = +20" +/- 1",
pos_3: FROM 13
equinox: 2000.0
fluxnum_1: 1
fluxval_1: V = 21.7 , TYPE = G0
fluxnum_2: 2
fluxval_2: V = 19.1 , TYPE = G0
!
! end of fixed targets
! No solar system records found
! No generic target records found
exposure_logsheet:
linenum: 1.000
sequence_1: DEFINE V
targname: #
config: WFPC2
opmode: IMAGE
aperture: PC1-FIX
sp_element: F555W
num_exp: #
time_per_exp: 10S
s_to_n: 28.9
fluxnum_1: #
priority: 1
param_1: SUM=1X1,
param_2: READ=YES,
param_3: CR-SPLIT=NO,
param_4: CLOCKS=NO,
param_5: ATD-GAIN=15
req_1: CYCLE 4;
!
linenum: 2.000
sequence_1: DEFINE I
targname: #
config: WFPC2
opmode: IMAGE
aperture: PC1-FIX
sp_element: F814W
num_exp: #
time_per_exp: 10S
s_to_n: 28.9
fluxnum_1: #
priority: 1
param_1: SUM=1X1,
param_2: READ=YES,
param_3: CR-SPLIT=NO,
param_4: CLOCKS=NO,
param_5: ATD-GAIN=15
req_1: CYCLE 4;
!
linenum: 3.000
sequence_1: USE V
targname: NGC5927-POS1
num_exp: 3
time_per_exp: X5
fluxnum_1: 2
req_2: SEQ 3-10 NO GAP;
!
linenum: 4.000
sequence_1: USE V
targname: NGC5927-POS1
num_exp: 4
time_per_exp: X60
fluxnum_1: 1
!
linenum: 5.000
sequence_1: USE I
targname: NGC5927-POS1
num_exp: 3
time_per_exp: X7
fluxnum_1: 2
!
linenum: 6.000
sequence_1: USE I
targname: NGC5927-POS1
num_exp: 4
time_per_exp: X80
fluxnum_1: 1
!
linenum: 7.000
sequence_1: USE V
targname: NGC5927-POS2
num_exp: 3
time_per_exp: X5
fluxnum_1: 2
!
linenum: 8.000
sequence_1: USE V
targname: NGC5927-POS2
num_exp: 4
time_per_exp: X60
fluxnum_1: 1
!
linenum: 9.000
sequence_1: USE I
targname: NGC5927-POS2
num_exp: 3
time_per_exp: X7
fluxnum_1: 2
!
linenum: 10.000
sequence_1: USE I
targname: NGC5927-POS2
num_exp: 4
time_per_exp: X80
fluxnum_1: 1
!
linenum: 11.000
sequence_1: USE V
targname: NGC6293-POS1
num_exp: 3
time_per_exp: X4
fluxnum_1: 2
req_2: SEQ 11-18 NO GAP;
!
linenum: 12.000
sequence_1: USE V
targname: NGC6293-POS1
num_exp: 4
time_per_exp: X50
fluxnum_1: 1
!
linenum: 13.000
sequence_1: USE I
targname: NGC6293-POS1
num_exp: 3
time_per_exp: X6
fluxnum_1: 2
!
linenum: 14.000
sequence_1: USE I
targname: NGC6293-POS1
num_exp: 4
time_per_exp: X70
fluxnum_1: 1
!
linenum: 15.000
sequence_1: USE V
targname: NGC6293-POS2
num_exp: 3
time_per_exp: X4
fluxnum_1: 2
!
linenum: 16.000
sequence_1: USE V
targname: NGC6293-POS2
num_exp: 4
time_per_exp: X50
fluxnum_1: 1
!
linenum: 17.000
sequence_1: USE I
targname: NGC6293-POS2
num_exp: 3
time_per_exp: X6
fluxnum_1: 2
!
linenum: 18.000
sequence_1: USE I
targname: NGC6293-POS2
num_exp: 4
time_per_exp: X70
fluxnum_1: 1
!
linenum: 19.000
sequence_1: USE V
targname: NGC6333-POS1
num_exp: 3
time_per_exp: X3.5
fluxnum_1: 2
req_2: SEQ 19-26 NO GAP;
!
linenum: 20.000
sequence_1: USE V
targname: NGC6333-POS1
num_exp: 4
time_per_exp: X50
fluxnum_1: 1
!
linenum: 21.000
sequence_1: USE I
targname: NGC6333-POS1
num_exp: 3
time_per_exp: X5
fluxnum_1: 2
!
linenum: 22.000
sequence_1: USE I
targname: NGC6333-POS1
num_exp: 4
time_per_exp: X60
fluxnum_1: 1
!
linenum: 23.000
sequence_1: USE V
targname: NGC6333-POS2
num_exp: 3
time_per_exp: X3.5
fluxnum_1: 2
!
linenum: 24.000
sequence_1: USE V
targname: NGC6333-POS2
num_exp: 4
time_per_exp: X50
fluxnum_1: 1
!
linenum: 25.000
sequence_1: USE I
targname: NGC6333-POS2
num_exp: 3
time_per_exp: X5
fluxnum_1: 2
!
linenum: 26.000
sequence_1: USE I
targname: NGC6333-POS2
num_exp: 4
time_per_exp: X60
fluxnum_1: 1
!
linenum: 27.000
sequence_1: USE V
targname: NGC6352-POS1
num_exp: 3
time_per_exp: X1.2
fluxnum_1: 2
req_2: SEQ 27-36 NO GAP;
!
linenum: 28.000
sequence_1: USE V
targname: NGC6352-POS1
num_exp: 2
time_per_exp: X16
fluxnum_1: 1
!
linenum: 29.000
sequence_1: USE I
targname: NGC6352-POS1
num_exp: 3
time_per_exp: X2
fluxnum_1: 2
!
linenum: 30.000
sequence_1: USE I
targname: NGC6352-POS1
num_exp: 2
time_per_exp: X26
fluxnum_1: 1
!
linenum: 31.000
sequence_1: USE V
targname: NGC6352-POS1
num_exp: 2
time_per_exp: X16
fluxnum_1: 1
req_3: POS TARG 1.0 , 1.0
!
linenum: 32.000
sequence_1: USE I
targname: NGC6352-POS1
num_exp: 2
time_per_exp: X26
fluxnum_1: 1
req_3: POS TARG 1.0 , 1.0
!
linenum: 33.000
sequence_1: USE V
targname: NGC6352-POS2
num_exp: 3
time_per_exp: X1.2
fluxnum_1: 2
!
linenum: 34.000
sequence_1: USE V
targname: NGC6352-POS2
num_exp: 3
time_per_exp: X16
fluxnum_1: 1
!
linenum: 35.000
sequence_1: USE I
targname: NGC6352-POS2
num_exp: 3
time_per_exp: X2
fluxnum_1: 2
!
linenum: 36.000
sequence_1: USE I
targname: NGC6352-POS2
num_exp: 3
time_per_exp: X26
fluxnum_1: 1
!
linenum: 37.000
sequence_1: USE V
targname: NGC6541-POS1
num_exp: 3
time_per_exp: X1.2
fluxnum_1: 2
req_2: SEQ 37-44 NO GAP;
!
linenum: 38.000
sequence_1: USE V
targname: NGC6541-POS1
num_exp: 4
time_per_exp: X14
fluxnum_1: 1
!
linenum: 39.000
sequence_1: USE I
targname: NGC6541-POS1
num_exp: 3
time_per_exp: X2
fluxnum_1: 2
!
linenum: 40.000
sequence_1: USE I
targname: NGC6541-POS1
num_exp: 3
time_per_exp: X26
fluxnum_1: 1
!
linenum: 41.000
sequence_1: USE V
targname: NGC6541-POS2
num_exp: 3
time_per_exp: X1.2
fluxnum_1: 2
!
linenum: 42.000
sequence_1: USE V
targname: NGC6541-POS2
num_exp: 4
time_per_exp: X14
fluxnum_1: 1
!
linenum: 43.000
sequence_1: USE I
targname: NGC6541-POS2
num_exp: 3
time_per_exp: X2
fluxnum_1: 2
!
linenum: 44.000
sequence_1: USE I
targname: NGC6541-POS2
num_exp: 4
time_per_exp: X26
fluxnum_1: 1
!
linenum: 45.000
sequence_1: USE V
targname: NGC6624-POS1
num_exp: 3
time_per_exp: X2.6
fluxnum_1: 2
req_2: SEQ 45-52 NO GAP;
!
linenum: 46.000
sequence_1: USE V
targname: NGC6624-POS1
num_exp: 4
time_per_exp: X35
fluxnum_1: 1
!
linenum: 47.000
sequence_1: USE I
targname: NGC6624-POS1
num_exp: 3
time_per_exp: X5
fluxnum_1: 2
!
linenum: 48.000
sequence_1: USE I
targname: NGC6624-POS1
num_exp: 4
time_per_exp: X60
fluxnum_1: 1
!
linenum: 49.000
sequence_1: USE V
targname: NGC6624-POS2
num_exp: 3
time_per_exp: X2.6
fluxnum_1: 2
!
linenum: 50.000
sequence_1: USE V
targname: NGC6624-POS2
num_exp: 4
time_per_exp: X35
fluxnum_1: 1
!
linenum: 51.000
sequence_1: USE I
targname: NGC6624-POS2
num_exp: 3
time_per_exp: X5
fluxnum_1: 2
!
linenum: 52.000
sequence_1: USE I
targname: NGC6624-POS2
num_exp: 4
time_per_exp: X60
fluxnum_1: 1
!
linenum: 53.000
sequence_1: USE V
targname: NGC6637-POS1
num_exp: 3
time_per_exp: X3
fluxnum_1: 2
req_2: SEQ 53-62 NO GAP;
!
linenum: 54.000
sequence_1: USE V
targname: NGC6637-POS1
num_exp: 4
time_per_exp: X40
fluxnum_1: 1
!
linenum: 55.000
sequence_1: USE I
targname: NGC6637-POS1
num_exp: 3
time_per_exp: X6
fluxnum_1: 2
!
linenum: 56.000
sequence_1: USE I
targname: NGC6637-POS1
num_exp: 4
time_per_exp: X70
fluxnum_1: 1
!
linenum: 57.000
sequence_1: USE V
targname: NGC6637-POS2
num_exp: 3
time_per_exp: X3
fluxnum_1: 2
!
linenum: 58.000
sequence_1: USE V
targname: NGC6637-POS2
num_exp: 2
time_per_exp: X40
fluxnum_1: 1
!
linenum: 59.000
sequence_1: USE I
targname: NGC6637-POS2
num_exp: 3
time_per_exp: X6
fluxnum_1: 2
!
linenum: 60.000
sequence_1: USE I
targname: NGC6637-POS2
num_exp: 2
time_per_exp: X70
fluxnum_1: 1
!
linenum: 61.000
sequence_1: USE V
targname: NGC6637-POS2
num_exp: 2
time_per_exp: X40
fluxnum_1: 1
req_3: POS TARG 1.0 , 1.0
!
linenum: 62.000
sequence_1: USE I
targname: NGC6637-POS2
num_exp: 2
time_per_exp: X70
fluxnum_1: 1
req_3: POS TARG 1.0 , 1.0
!
! end of exposure logsheet
! No scan data records found