! $Id: 5436,v 5.1 1994/07/27 17:56:57 pepsa Exp $
coverpage:
title_1: AGE AND POPULATIONS OF SUPER METAL RICH GLOBULAR CLUSTERS
title_2: IN THE GALACTIC BULGE: CYCLE4 MEDIUM
sci_cat: COOL STARS
sci_subcat: OLD CLUSTERS
proposal_for: GO
pi_fname: SERGIO
pi_lname: ORTOLANI
pi_inst: 6470
pi_country: ITALY
pi_phone: 39-49-8293425
hours_pri: 1.39
num_pri: 3
wf_pc: Y
off_fname: FRANCESCO
off_lname: LUCCHIN
off_title: DIRECTOR
off_inst: 6470
off_addr_1: VICOLO DELL'OSSERVATORIO
off_city: PADOVA
off_zip: I-35122
off_country: ITALY
off_phone: 39-49-8293411
! end of coverpage
abstract:
line_1: WFPC2 multicolor observations of THREE among the most metal rich globular
line_2: clusters in the Galactic Bulge are proposed in order to obtain accurate
line_3: turnoff luminosities (and then ages) for the three clusters, together
line_4: with fairly large complete samples of evolved stars.
line_5: The two main scientific goals of the project are the following.
line_6: 1) The age determination allows to set stringent constraints on the
line_7: formation process of the globular cluster system, of the Galactic Bulge,
line_8: and therefore of the Galaxy as a whole; and
line_9: 2) The three clusters represent the best available ``Template Stellar
line_10: Populations'' for super metal rich (SMR), old stellar
line_11: systems, i.e. for the kind of populations which are likely to dominate
line_12: the light of giant elliptical galaxies, and the bulge of spirals.
line_13: In this respect, the present study is meant to obtain
line_14: well understood stellar templates for the population synthesis of
line_15: composite stellar systems. The proposed observations will
line_16: also provide valuable information for such problems as the study of
line_17: very fast evolutionary stages, and rare (trace) stellar species in
line_18: SMR clusters (e.g. UV-bright stars, blue stragglers,
line_19: binaries, etc.) together with their radial distribution.
!
! end of abstract
general_form_proposers:
lname: ORTOLANI
fname: SERGIO
inst: 6470
country: ITALY
esa: Y
!
lname: RENZINI
fname: ALVIO
inst: 6460
country: ITALY
esa: Y
!
lname: GILMOZZI
fname: ROBERTO
inst: 3470
country: USA
esa: Y
!
lname: MARCONI
fname: GIANNI
inst: 6460
country: ITALY
esa: Y
!
lname: BARBUY
fname: BEATRIZ
inst: UNIVERSITY OF SAO PAULO
country: BRAZIL
!
lname: BICA
fname: EDUARDO
inst: UNIVERSITY OF PUERTO ALEGRE
country: BRAZIL
!
! end of general_form_proposers block
general_form_text:
question: 3
section: 1
line_1: For each of the three clusters we propose to obtain WFPC2 exposures
line_2: through the UVI filters (F336W, F555W, F791W). We propose total
line_3: exposures times adequate to reach S/N = 25 in V and I, for stars two
line_4: magnitudes below the TO (V=20 for 6553 and 6528, and around V=22 for
line_5: Terzan 1), and to reach a limiting magnitude 22 in the U band.
line_6: This choice keeps the U-band exposures within acceptable limits, while
line_7: still ensuring the astrophysically relevant information (complete
line_8: coverage of UV-bright objects that could be present in the clusters:
line_9: lue HB, SdO and Post-AGB stars. Given its high reddening, no U-band
line_10: exposures are planned for Terzan 1.
line_11: Blooming effects must be kept to a minimum in order to prevent losses
line_12: greater than a few percent in the effective collecting area. Accurate
line_13: photometry of the brightest cluster members requires short exposures to
line_14: prevent saturation. The exposures will correspondingly be split into
line_15: short, and deep exposures.
!
question: 3
section: 2
line_1:
!
question: 4
section: 1
line_1: The HST characteristic which is exploited in these proposed observations
line_2: is its high angular resolution coupled with large field of view.
line_3: This allows the construction of complete CMDs and luminosity functions
line_4: to distances from the cluster center much smaller than currently
line_5: feasible from the ground, thus dramatically reducing to tolerable levels
line_6: several factors which currently prevent the determination of V(TO) for
line_7: the target clusters with sufficient accuracy (+/- ~0.1 mag) to yield
line_8: meaningful cluster ages: i.e. field contamination, and internal crowding. In
line_9: practice, where the cluster dominates over the field, crowding is so
line_10: severe that we found impossible to accurately reach the MS turnoff from
line_11: the ground, even with outstanding seeing (<~= 0.7 arcsec). Conversely,
line_12: further out where crowding is tolerable for accurate photometry the
line_13: field contamination is overwhelming.
line_14: The same argument holds for the derived luminosity functions, as a high
line_15: photometric accuracy (SIGMA(V-I)~= 0.05 or better) is required, e.g.,
line_16: to unambiguously separate blue stragglers from ordinary MS stars and
line_17: AGB from RGB stars.
!
question: 4
section: 2
line_1: We estimate, from the instruction of the WFPC2 manual, that good
line_2: photometry, with very little statistical and read out noise can be
line_3: obtained at V=22, with the WFPC2 and F555W filter, in a total
line_4: integration time of 200 sec., with a dynamical range of almost 5
line_5: magnitudes. This meets the requirement of the scientific goals presented
line_6: in par. 1 and 2. The split of the 200 sec. integration time into two 100
line_7: sec. exposures reduces the blooming effect of the brightest stars in the
line_8: field of view, and allows removing the cosmic ray contamination.
line_9: An additional short exposure of 15 sec. is required to get optimum
line_10: photometry at the level of the horizontal branch (V=17) and giant branch
line_11: (V=14).
line_12: The same considerations apply to the infrared exposures through the
line_13: W791W filter for which a total exposure time at V=22.0 and V-I=1.2 is
line_14: 100 sec. In this case an additional short exposure of 5 sec. is
line_15: required. In the U-band, 2 x 800 sec. exposures for the clusters NGC
line_16: 6553 and 6528 are required to reach the limit of U=22.0, which
line_17: corresponds to the faintest UV objects that we intend to dectect as
line_18: described in sections 1 and 2.
line_19: A factor 5 longer exposure (in V) has been adopted for the cluster
line_20: Terzan 1 to compensate for its higher galactic obscuration. In the I
line_21: band the calculated total exposure time is 120 sec. For this cluster
line_22: the U exposures are omitted since they would require unrealistically
line_23: long exposure times.
!
question: 5
section: 1
line_1:
!
!
question: 8
section: 1
line_1:
!
question: 9
section: 1
line_1: P2579: THE CALIBRATION OF THE WHITE DWARF DISTANCE SCALE FOR GLOBULAR
line_2: CLUSTERS. (PI A. Renzini) The GO cycle 1 program received 45.80 hours of
line_3: spacecraft time, with SUPPLEMENTAL priority. The program then completed
line_4: the Phase 2, and was cleared for the HST observations. Subsequent to the
line_5: spherical aberration problem the PI asked to DEFER the program to the
line_6: first HST LINE_6:cycle with fully recovered WF/PC capabilities. In a
line_7: broad sense, the present proposal is scientifically related to P2579, as
line_8: they both seek to determine the age of specific globular clusters. In
line_9: the case of P2579 the target is a cluster in the galactic Halo, here are
line_10: three clusters in the galactic Bulge. The two projects are
line_11: complementary to each other.
line_12: P3449: AGE AND POPULATIONS OF SUPERMETAL RICH GLOBULAR CLUSTERS IN THE
line_13: GALACTIC BULGE (PI A. Renzini). This GO Cycle 2 program was approved but
line_14: received SUPPLEMENTAL PRIORITY. No Phase 2 proposal was asked. The
line_15: present proposal is an update of P3449.
line_16: Papers: "HST Observations of Two remarkable Planetary Nebula Nuclei",
line_17: Bond H., Liebert, J., Renzini, A. 1993, in "Science with the Hubble
line_18: Space Telescope", ed. P. Benvenuti & E. Schreier (Garching: ESO), p.
line_19: 139.
!
question: 10
section: 1
line_1: Resources to be supplied by your institution(s) in support of this
line_2: project (e.g., data-analysis capabilities, research assistance, students,
line_3: funds).
line_4: Computing:
line_5: Bologna: Our Institute is equipped with one VAX 8530, one VAX 8800,
line_6: 3 Microvaxes, three Decstations 3100 one of which could be entirely
line_7: dedicated to the present project (if approved), 5Gby mass memory (of
line_8: which one private 0.5 Gby disk), one Gould-DeAnza image processor, one
line_9: Microvax GPX workstation, plus numerous peripherals. There is also ready
line_10: access to the Cray 2 of the Bologna University.
line_11: Padova: Our Institute is equipped with one VAX 8530 one Sun station and
line_12: two Microvax stations. The IHAP package is also available at the HP 1000.
line_13: Research Assistance and Students: there are typically 10 graduate
line_14: students in Astronomy at our Department, part of which already work on
line_15: HST-related projects. Research assistance will be secured.
line_16: Funds:
line_17: Bologna, and Padova: Our research grants are sufficient to cover
line_18: all the expenses conceivably required to complete this together the
line_19: other HST projects in which we may be involved. The facilities of the
line_20: ESA/ESO ST-ECF are also available, if needed.
!
!end of general form text
general_form_address:
lname: ORTOLANI
fname: SERGIO
category: PI
addr_1: DIPARTIMENTO DI ASTRONOMIA
addr_2: VICOLO DELL'OSSERVATORIO 5
city: PADOVA
zip: I-35122
country: ITALY
phone: 39-49-8293425
telex: ASTRPD::ORTOLANI
!
! end of general_form_address records
fixed_targets:
targnum: 1
name_1: NGC6553
descr_1: C,201,913;
descr_2: 913,A,130
pos_1: RA = 18H 06M 11.0S +/- 0.05S,
pos_2: DEC = -25D 55' 1.6" +/- 0.7"
equinox: 1950
fluxnum_1: 1
fluxval_1: V=22.0 +/- 0.1, B-V=+1.7, E(B-V)=0.8
fluxnum_2: 2
fluxval_2: V=16.0 +/- 0.1, B-V=+2.0, E(B-V)=0.8
fluxnum_3: 3
fluxval_3: I=19.0 +/- 0.1, B-V=+1.7, E(B-V)=0.8
fluxnum_4: 4
fluxval_4: I=13.5 +/- 0.1, B-V=+2.0, E(B-V)=0.8
fluxnum_5: 5
fluxval_5: U=22.0 +/- 0.2, B-V=+0.7, E(B-V)=0.8
!
targnum: 2
name_1: NGC6528
descr_1: C,201,913;
descr_2: 913,A,130
pos_1: RA = 18H 01M 37.2S +/- 0.08S,
pos_2: DEC = -30D 03' 34.9" +/- 1.2"
equinox: 1950
fluxnum_1: 1
fluxval_1: V=22.0 +/- 0.1, B-V=+1.7, E(B-V)=0.6
fluxnum_2: 2
fluxval_2: V=16.0 +/- 0.1, B-V=+2.0, E(B-V)=0.6
fluxnum_3: 3
fluxval_3: I=19.0 +/- 0.1, B-V=+1.7, E(B-V)=0.6
fluxnum_4: 4
fluxval_4: I=13.5 +/- 0.1, B-V=+2.0, E(B-V)=0.6
fluxnum_5: 5
fluxval_5: U=22.0 +/- 0.2, B-V=+0.5, E(B-V)=0.6
!
targnum: 3
name_1: TERZAN1
descr_1: C,201,913;
descr_2: 913,A,130
pos_1: RA = 17H 32M 34.0S +/- 0.2S,
pos_2: DEC = -30D 27' 00.0" +/- 3"
equinox: 1950
fluxnum_1: 1
fluxval_1: V=24.5 +/- 0.2, V-I=4.0, E(B-V)=1.6
fluxnum_2: 2
fluxval_2: V=19.5 +/- 0.2, V-I=+3.8, E(B-V)=1.6
fluxnum_3: 3
!
! end of fixed targets
! No solar system records found
! No generic target records found
exposure_logsheet:
linenum: 11.000
targname: NGC6553
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F555W
wavelength: 5550
num_exp: 2
time_per_exp: 100S
s_to_n: 25
s_to_n_time: 200S
fluxnum_1: 1
priority: 1
req_1: CYCLE 4; SAME ORIENT FOR 12-15 AS 11;
!
linenum: 12.000
targname: NGC6553
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F555W
wavelength: 5550
num_exp: 1
time_per_exp: 15S
s_to_n: 100
s_to_n_time: 15S
fluxnum_1: 2
priority: 2
req_1: SAME ORIENT FOR 12-15 AS 11; CYCLE 4;
comment_1: AVOID SATURATION AT V=14
!
linenum: 13.000
targname: NGC6553
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F814W
wavelength: 7829
num_exp: 2
time_per_exp: 50S
s_to_n: 25
s_to_n_time: 100S
fluxnum_1: 3
priority: 1
req_1: CYCLE 4; SAME ORIENT FOR 12-15 AS 11;
!
linenum: 14.000
targname: NGC6553
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F814W
wavelength: 7829
num_exp: 1
time_per_exp: 5S
s_to_n: 100
s_to_n_time: 5S
fluxnum_1: 4
priority: 2
req_1: SAME ORIENT FOR 12-15 AS 11; CYCLE 4;
comment_1: AVOID SATURATION AT V=14
!
linenum: 15.000
targname: NGC6553
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F336W
wavelength: 3344
num_exp: 2
time_per_exp: 800S
s_to_n: 25
s_to_n_time: 1600S
fluxnum_1: 5
priority: 3
req_1: CYCLE 4; SAME ORIENT FOR 12-15 AS 11;
!
linenum: 16.000
targname: NGC6528
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F555W
wavelength: 5550
num_exp: 2
time_per_exp: 100S
s_to_n: 25
s_to_n_time: 200S
fluxnum_1: 1
priority: 1
req_1: CYCLE 4; SAME ORIENT FOR 17-20 AS 16;
!
linenum: 17.000
targname: NGC6528
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F555W
wavelength: 5550
num_exp: 1
time_per_exp: 15S
s_to_n: 100
s_to_n_time: 15S
fluxnum_1: 2
priority: 2
req_1: SAME ORIENT FOR 17-20 AS 16; CYCLE 4;
comment_1: AVOID SATURATION AT V=14
!
linenum: 18.000
targname: NGC6528
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F814W
wavelength: 7829
num_exp: 2
time_per_exp: 50S
s_to_n: 25
s_to_n_time: 100S
fluxnum_1: 3
priority: 1
req_1: CYCLE 4; SAME ORIENT FOR 17-20 AS 16;
!
linenum: 19.000
targname: NGC6528
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F814W
wavelength: 7829
num_exp: 1
time_per_exp: 5S
s_to_n: 100
s_to_n_time: 5S
fluxnum_1: 4
priority: 2
req_1: CYCLE 4; SAME ORIENT FOR 17-20 AS 16;
comment_1: AVOID SATURATION AT V=14
!
linenum: 20.000
targname: NGC6528
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F336W
wavelength: 3344
num_exp: 2
time_per_exp: 800S
s_to_n: 25
s_to_n_time: 1600S
fluxnum_1: 5
priority: 3
req_1: CYCLE 4; SAME ORIENT FOR 17-20 AS 16;
!
linenum: 23.000
targname: TERZAN1
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F814W
wavelength: 7829
num_exp: 1
time_per_exp: 5S
s_to_n: 50
s_to_n_time: 5S
fluxnum_1: 2
priority: 2
req_1: CYCLE 4; SAME ORIENT FOR 24-26 AS 23;
comment_1: AVOID SATURATION FOR V=14 STARS
!
linenum: 24.000
targname: TERZAN1
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F814W
wavelength: 7829
num_exp: 2
time_per_exp: 60S
s_to_n: 25
s_to_n_time: 120S
fluxnum_1: 1
priority: 1
req_1: CYCLE 4; SAME ORIENT FOR 24-26 AS 23;
!
linenum: 25.000
targname: TERZAN1
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F555W
wavelength: 5550
num_exp: 2
time_per_exp: 500S
s_to_n: 25
s_to_n_time: 1000S
fluxnum_1: 1
priority: 1
req_1: CYCLE 4; SAME ORIENT FOR 24-26 AS 23;
!
linenum: 26.000
targname: TERZAN1
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F555W
wavelength: 5550
num_exp: 1
time_per_exp: 30S
s_to_n: 40
s_to_n_time: 30S
fluxnum_1: 2
priority: 2
req_1: CYCLE 4; SAME ORIENT FOR 24-26 AS 23;
!
! end of exposure logsheet
! No scan data records found