! $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