COVERPAGE: TITLE_1: M3: AN IDEAL LABORATORY FOR TESTING STELLAR EVOLUTION AND DYNAMICS: TITLE_2: CYCLE4 HIGH SCI_CAT: COOL STARS SCI_SUBCAT: OLD CLUSTERS PROPOSAL_FOR: GO TIME_CRIT: Y PI_FNAME: FLAVIO PI_LNAME: FUSI PECCI PI_INST: 6426 PI_COUNTRY: ITALY PI_PHONE: 39-51-259321 HOURS_PRI: 6.39 HOURS_PAR: 0.00 NUM_PRI: 1 NUM_PAR: 0 WF_PC: Y OFF_FNAME: BRUNO OFF_LNAME: MARANO OFF_TITLE: DIRECTOR OFF_INST: 6426 OFF_ADDR_1: OSSERVATORIO ASTRONOMICO OFF_ADDR_2: VIA ZAMBONI 33 OFF_CITY: BOLOGNA OFF_ZIP: 40126 OFF_COUNTRY: ITALY OFF_PHONE: +39-51-259404 ABSTRACT: LINE_1: We propose WFPC2 observations of the Galactic globular cluster M3 in LINE_2: UVI and the mid-UV (F218W). This will be the first COMPLETE sample of LINE_3: Post-main sequence stars over the entire area of the cluster. It will LINE_4: allow the most stringent test of stellar evolutionary models and will LINE_5: yield crucial observational input for the study of star interactions LINE_6: and dynamics within a cluster. The results should have wide LINE_7: applicability including: (1) the most accurate test of the ``stellar LINE_8: clock'' used in dating globular clusters; (2) a complete survey of very LINE_9: fast evolutionary stages and rare (trace) stellar types (e.g. UV-bright LINE_10: stars, blue stragglers, binaries) along with their radial distributions, LINE_11: which will provide fundamental information for internal cluster dynamics LINE_12: and for the origin of UV light from elliptical galaxies. LINE_13: LINE_14: The cluster M3 is the ideal target for this purpose. We already have LINE_15: ground-based photometry of about 18000 stars: the best complete CMD, the LINE_16: largest complete Luminosity Function for Post-MS stars, and the largest LINE_17: sample of blue straggler stars (BSS) ever obtained for a globular LINE_18: cluster from the ground. The tests we propose require even larger LINE_19: samples which can only be achieved by observing the cluster core which LINE_20: is not resolved from the ground. GENERAL_FORM_PROPOSERS: LNAME: FUSI PECCI FNAME: FLAVIO INST: 6426 COUNTRY: ITALY ESA: Y LNAME: FERRARO FNAME: FRANCESCO R. INST: 6426 COUNTRY: ITALY ESA: Y LNAME: CACCIARI FNAME: CARLA INST: 6426 COUNTRY: ITALY ESA: Y LNAME: BUONANNO FNAME: ROBERTO INST: 6436 COUNTRY: ITALY ESA: Y LNAME: CORSI FNAME: CARLO E. INST: 6436 COUNTRY: ITALY ESA: Y LNAME: ROOD FNAME: ROBERT T. INST: 3730 COUNTRY: USA ESA: LNAME: DORMAN FNAME: BEN INST: 3730 COUNTRY: USA ESA: LNAME: FAHLMAN FNAME: GREG G. INST: 4618 COUNTRY: CANADA ESA: LNAME: RICHER FNAME: HARVEY B. INST: 4618 COUNTRY: CANADA ESA: LNAME: BURGARELLA FNAME: DENIS INST: 5446 COUNTRY: FRANCE ESA: Y LNAME: LAGET FNAME: MICHEL INST: 5446 COUNTRY: FRANCE ESA: Y LNAME: DE MARCHI FNAME: GUIDO INST: 3470 COUNTRY: USA ESA: LNAME: PARESCE FNAME: FRANCESCO INST: 3470 COUNTRY: USA ESA: GENERAL_FORM_ADDRESS: ! Address information for the Principal Investigator (PI): LNAME: FUSI PECCI FNAME: FLAVIO CATEGORY: PI INST: 6426 ADDR_1: OSSERVATORIO ASTRONOMICO ADDR_2: VIA ZAMBONI 33 CITY: BOLOGNA ZIP: 40126 COUNTRY: ITALY PHONE: 39-51-259321 TELEX: (SPAN) 37907::FLAVIO, FAX: +39-51-259407 GENERAL_FORM_TEXT: QUESTION: 3 ! Description of proposed observations. SECTION: 1 LINE_1: WFPC2 observations of the Galactic globular cluster M3 = NGC 5272 will be LINE_2: taken using 4 filters, i.e. F555W, F814W, F336W, and F218W. In particular, LINE_3: the PC1 will be pointing the cluster center, for each of the 4 filters, LINE_4: while the three WFC mosaics will map adjacent fields in the same bands. LINE_5: Two sets of exposures are planned, separated by a period of time suitable LINE_6: to study photometric variability (ranging from a few days up to a few weeks). LINE_7: Therefore, the second pointing has to be made at a given roll-angle to map LINE_8: the same area of the cluster. LINE_9: Since this program aims at obtaining accurate photometric measurements for LINE_10: all the evolved stars, and not at detecting and measuring the faintest LINE_11: possible objects, the observational strategy is to optimize the degree LINE_12: of completeness (down to a fixed magnitude limit, even at the very cluster LINE_13: center) and the photometric quality of the individual measures. LINE_14: Hence, exposure times for each filter have been computed (based on the LINE_15: WFPC2 Instrument Handbook) (1) to be adequate to reach S/N=15 at about LINE_16: 2 mag below the turnoff, i.e. V=21, in the wide band filters (UVI) and LINE_17: V=19 with F218W, and (2) to be subdivided into sets of appropriate LINE_18: sub-exposures short enough to avoid blooming from the brightest (V=13) LINE_19: giants. In fact, strong charge transfer from highly saturated bright LINE_20: objects would prevent the detection and measure of fainter stars, so LINE_21: decreasing strongly the degree of completeness specially in the very LINE_22: crowded central regions. QUESTION: 3 SECTION: 2 LINE_1: The exposure times have been computed by adopting a readout noise of LINE_2: rn=14e, E(B-V)=0.01, and the following recipe to estimate the total LINE_3: exposure time (to obtain a desired S/N) and the maximum length of each LINE_4: sub-exposure (to avoid blooming at >100000 counts/central px) LINE_5: LINE_6: Filter Type V S/N Blooming at V Type LINE_7: -------------------------------------------------------------------- LINE_8: F555W G0 21 15 13 K0 (GB-tip) LINE_9: F814W G0 21 12 13 K0 (GB-tip) LINE_10: F336W G0 21 10 16 B0 (Bright HB, P-AGB) LINE_11: F218W F0 19 10 16 B0 (Bright HB, P-AGB) QUESTION: 4 ! Justification of need for HST observations. SECTION: 1 LINE_1: The HST characteristics exploited in these observations are the high LINE_2: angular resolution coupled with the large field of view. This will allow LINE_3: to construct the complete luminosity function for all the evolved stars LINE_4: (brighter than the turnoff) including those located in the very central LINE_5: regions, and to detect complete samples of special stars (e.g. blue LINE_6: stragglers and post-AGB) checking also their possible intrinsic variability. LINE_7: By adding to the HST sample the complementary photometric sample we already LINE_8: secured from ground-based observations for the stars located in the external LINE_9: regions of the cluster (about 18000 stars measured so far), we will obtain LINE_10: the first complete sample ranging from the very center out to the cluster LINE_11: outskirts. This sample is at least 3 to 6 times larger than can possibly LINE_12: be obtained in the future from the ground even in extremely good seeing LINE_13: conditions, and by far more extended in spatial coverage than in any GTO LINE_14: program. In essence, only coupling ground based and HST observations one can LINE_15: obtain the complete luminosity function for the whole cluster, a crucial LINE_16: tool for a ``new generation'' of studies on stellar evolution and dynamics. LINE_17: Note that, besides ensuring completeness, the high angular resolution also LINE_18: yields precision photometry of the evolved stars (brighter than turnoff) down LINE_19: to the cluster center. Aiming at reaching S/N > 10 for stars two mag fainter LINE_20: than the turnoff, we guarantee a high photometric accuracy (1sigma < 0.05mag) LINE_21: for magnitudes and colors of all the stars brighter than the turnoff. LINE_22: Such an high internal accuracy is required by the need e.g. to unambiguously LINE_23: separate AGB from RGB stars, to recognize sharp but weak features in the RGB QUESTION: 4 SECTION: 2 LINE_1: luminosity function (such as the RGB-bump), to accurately determine the maximum LINE_2: RGB and AGB luminosity, to detect BSS candidates, to put into evidence LINE_3: small amplitude variability, etc. QUESTION: 5 ! Description of special scheduling requirements. SECTION: 1 LINE_1: To avoid the impact of blooming due to the brightest stars in the LINE_2: observed fields, we must subdivide the exposures into many short LINE_3: sub-exposures, which also allows us to check the individual star LINE_4: variability. To increase the time baseline, we have divided the LINE_5: observations into two groups separated by a period of time (from a LINE_6: few days up to a few weeks, depending on the optimization within the LINE_7: HST scheduling system). This implies the need for two visits on the LINE_8: target, with the same roll angle to guarantee the observation of the LINE_9: same fields in the cluster. QUESTION: 7 ! Data reduction and analysis plans. SECTION: 1 LINE_1: The computing facilities available in Bologna and Rome (see item 10 LINE_2: below) and the photometric package ROMAFOT (Buonanno et al. 1983), LINE_3: specifically prepared to deal with highly accurate photometry in crowded LINE_4: fields and purposely updated to handle HST data, will allow a complete LINE_5: processing of the data using the standard calibration information. LINE_6: This package has already been used to carry out several photometric studies LINE_7: published by our group on the main journals and, in particular, to make LINE_8: all the photometric measures available for the complementary samples of LINE_9: stars located in the external regions of the cluster. LINE_10: Short visits at the STScI or ST-ECF might be necessary to deal with some LINE_11: specific aspects (like calibrations and photometric checks). Reductions of LINE_12: some test fields will be carried out also with alternative packages LINE_13: (e.g., DAOPHOT) for comparison. QUESTION: 9 ! Description of previous HST work. SECTION: 1 LINE_1: Two programs have been previously granted HST observing time, namely LINE_2: GO2583 (Cycle 1): ``Color-Magnitude Diagrams of a Sample of Globular LINE_3: Clusters in M31'', and GO3726 (cycle 2): ``Globular Clusters in M31''. LINE_4: These programs (which have been re-submitted and granted observing time LINE_5: in cycle 4) are indirectly related since one of their original goals LINE_6: is a direct measure of the HB star luminosities to be used as standard LINE_7: candles for a precise determination of globular cluster distances and LINE_8: ages. One of the basic aims of the present proposal is indeed the ultimate LINE_9: check of the so-called ``stellar-clock'' which represents the complement LINE_10: to the observables to yield the age of any stellar aggregate. LINE_11: With GO 2583 13 clusters were observed with the FOC/96 + F430W and accurate LINE_12: surface brightness profiles were obtained, along with the related photometric LINE_13: and structural parameters. These results are of far superior quality than LINE_14: what can be obtained from ground-based observations, and are comparable to LINE_15: the results on galactic globular clusters. The two cluster families show very LINE_16: similar characteristics. We have found the first evidence of a PCC cluster LINE_17: in M31. These results was presented at the Workshop ``Science with the Hubble LINE_18: Space Telescope'' held in Baia Chia in July 1992 and in two papers. LINE_19: With GO3726 one cluster was observed with the FOC/96 + F342W and F140W in LINE_20: order to explore the possibility of obtaining a C-M diagram of at least LINE_21: the brightest and hottest stars even in presence of the known HST aberration. LINE_22: The data reduction and analysis is presently being carried on, but it is LINE_23: evident that only the restored HST can provide useful results. QUESTION: 10 ! Resources to be supplied by investigator's institution(s). SECTION: 1 LINE_1: Italy: LINE_2: Computing: our Institutes in Bologna and Rome are equipped with several LINE_3: Workstations (DEC, IBM) and numerous peripherals specifically devoted to LINE_4: the analysis of HST data. LINE_5: Research Assistance and Students: there are typically 10 graduate students in LINE_6: Astronomy in Bologna, part of which already work on HST-related projects. LINE_7: Research assistance will be secured. LINE_8: Funds: Our personal research grants are sufficient to cover all the expenses LINE_9: conceivably required to complete this program along with other HST LINE_10: projects in which we may be involved. The facilities of the ST-ECF are LINE_11: also available, if needed. LINE_12: LINE_13: University of Virginia: LINE_14: Facilities: The Department of Astronomy has several SUN workstations LINE_15: which can be used to assist in data reduction if necessary. These are LINE_16: also adequate to perform the stellar model and population synthesis LINE_17: computations necessary to interpret the data. A very large grid of LINE_18: stellar models has already been computed. LINE_19: Funds: Current funds from a related NASA Long Term Astrophysics Grant LINE_20: are adequate. ! This is the end of the General Form FIXED_TARGETS: TARGNUM: 1 NAME_1: NGC5272 NAME_2: M3 DESCR_1: C,201 POS_1: RA = 13H 39M 52.94S +/- 0.1S, POS_2: DEC = +28D 37' 37.9" +/- 1" EQUINOX: 1950.0 FLUXNUM_1: 1 FLUXVAL_1: SURF-BKG(V)=16.3 +/- 0.1, B-V=0.7 FLUXNUM_2: 2 FLUXVAL_2: V=21, TYPE=G0V, E(B-V)=0.01 FLUXNUM_3: 3 FLUXVAL_3: V=19, TYPE=F0, E(B-V)=0.01 FLUXNUM_4: 4 FLUXVAL_4: V=26, TYPE=M0, E(B-V)=0.01 COMMENT_1: Flux1=central surface brightness COMMENT_2: in mag/arcsec-2 for ACQ only. COMMENT_3: Flux2, 3 and 4 are cluster stars COMMENT_4: for exposure time calculation EXPOSURE_LOGSHEET: LINENUM: 1.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F555W PARAM_1: ATD-GAIN=15 NUM_EXP: 2 TIME_PER_EXP: 3S S_TO_N: 3 S_TO_N_TIME: 6S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; GROUP 1-8 NO GAP; REQ_2: SAME ORIENT FOR 1.1-8 AS 1 COMMENT_1: 2 EXPOSURES OF 3 SEC EACH TO AVOID COMMENT_2: BLOOMING FROM V=13 K0 STARS LINENUM: 1.100 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F555W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 100S S_TO_N: 50 S_TO_N_TIME: 400S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; SEQ 1.1-1.4 NO GAP COMMENT_1: 4 EXPOSURES OF 100S EACH TO REACH COMMENT_2: SNR=50 2 MAG BELOW TURNOFF COMMENT_3: GROUP 1.1-1.4 DITHERED LINENUM: 1.200 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F555W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 100S S_TO_N: 50 S_TO_N_TIME: 400S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, 0.0 COMMENT_1: SAME AS IN LINENUM 1.1 LINENUM: 1.300 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F555W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 100S S_TO_N: 50 S_TO_N_TIME: 400S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG 0.0, +0.07 COMMENT_1: SAME AS IN LINENUM 1.1 LINENUM: 1.400 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F555W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 100S S_TO_N: 50 S_TO_N_TIME: 400S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, +0.07 COMMENT_1: SAME AS IN LINENUM 1.1 LINENUM: 2.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F814W PARAM_1: ATD-GAIN=15 NUM_EXP: 2 TIME_PER_EXP: 3S S_TO_N: 3 S_TO_N_TIME: 6S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4 COMMENT_1: 2 EXPOSURES OF 3 SEC EACH TO AVOID COMMENT_2: BLOOMING FROM V=13 K0 STARS LINENUM: 2.100 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F814W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 140S S_TO_N: 50 S_TO_N_TIME: 560S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; SEQ 2.1-2.4 NO GAP COMMENT_1: 4 EXPOSURES OF 140S EACH TO REACH COMMENT_2: SNR=50 2 MAG BELOW TURNOFF COMMENT_3: GROUP 2.1-2.4 DITHERED LINENUM: 2.200 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F814W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 140S S_TO_N: 50 S_TO_N_TIME: 560S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, 0.0 COMMENT_1: SAME AS IN LINENUM 2.1 LINENUM: 2.300 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F814W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 140S S_TO_N: 50 S_TO_N_TIME: 560S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG 0.0, +0.07 COMMENT_1: SAME AS IN LINENUM 2.1 LINENUM: 2.400 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F814W PARAM_1: ATD-GAIN=15 NUM_EXP: 1 TIME_PER_EXP: 140S S_TO_N: 50 S_TO_N_TIME: 560S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, +0.07 COMMENT_1: SAME AS IN LINENUM 2.1 LINENUM: 3.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F336W PARAM_1: ATD-GAIN=15 NUM_EXP: 2 TIME_PER_EXP: 70S S_TO_N: 12 S_TO_N_TIME: 140S FLUXNUM_1: 3 PRIORITY: 1 REQ_1: CYCLE 4 COMMENT_1: 2 EXPOSURES OF 70S EACH TO AVOID COMMENT_2: BLOOMING FROM V=15 B0 STARS LINENUM: 3.100 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F336W PARAM_1: ATD-GAIN=15, CR-SPLIT=NO NUM_EXP: 1 TIME_PER_EXP: 800S S_TO_N: 20 S_TO_N_TIME: 3200S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; SEQ 3.1-3.4 NO GAP COMMENT_1: 4 EXPOSURES OF 800S EACH COMMENT_2: GROUP 3.1-3.4 DITHERED LINENUM: 3.200 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F336W PARAM_1: ATD-GAIN=15, CR-SPLIT=NO NUM_EXP: 1 TIME_PER_EXP: 800S S_TO_N: 20 S_TO_N_TIME: 3200S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, 0.0 COMMENT_1: SAME AS IN LINENUM 3.1 LINENUM: 3.300 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F336W PARAM_1: ATD-GAIN=15, CR-SPLIT=NO NUM_EXP: 1 TIME_PER_EXP: 800S S_TO_N: 20 S_TO_N_TIME: 3200S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG 0.0, +0.07 COMMENT_1: SAME AS IN LINENUM 3.1 LINENUM: 3.400 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F336W PARAM_1: ATD-GAIN=15, CR-SPLIT=NO NUM_EXP: 1 TIME_PER_EXP: 800S S_TO_N: 20 S_TO_N_TIME: 3200S FLUXNUM_1: 2 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, +0.07 COMMENT_1: SAME AS IN LINENUM 3.1 LINENUM: 4.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F255W PARAM_1: ATD-GAIN=7 NUM_EXP: 1 TIME_PER_EXP: 300S S_TO_N: 6 S_TO_N_TIME: 1200S FLUXNUM_1: 3 PRIORITY: 1 REQ_1: CYCLE 4; SEQ 4.0-4.3 NO GAP COMMENT_1: 4 EXPOSURES OF 300S EACH TO AVOID COMMENT_2: BLOOMING FROM V=15 B0 STARS COMMENT_3: GROUP 4.0-4.3 DITHERED LINENUM: 4.100 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F255W PARAM_1: ATD-GAIN=7 NUM_EXP: 1 TIME_PER_EXP: 300S S_TO_N: 6 S_TO_N_TIME: 1200S FLUXNUM_1: 3 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, 0.0 COMMENT_1: SAME AS IN LINENUM 4.0 LINENUM: 4.200 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F255W PARAM_1: ATD-GAIN=7 NUM_EXP: 1 TIME_PER_EXP: 300S S_TO_N: 6 S_TO_N_TIME: 1200S FLUXNUM_1: 3 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG 0.0, +0.07 COMMENT_1: SAME AS IN LINENUM 4.0 LINENUM: 4.300 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F255W PARAM_1: ATD-GAIN=7 NUM_EXP: 1 TIME_PER_EXP: 300S S_TO_N: 6 S_TO_N_TIME: 1200S FLUXNUM_1: 3 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG +0.07, +0.07 COMMENT_1: SAME AS IN LINENUM 4.0 LINENUM: 5.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F555W PARAM_1: ATD-GAIN=7 NUM_EXP: 2 TIME_PER_EXP: 1200s S_TO_N: 9 S_TO_N_TIME: 2200S FLUXNUM_1: 4 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG 77.78, 77.78 COMMENT_1: offset to 110'' from center LINENUM: 6.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F814W PARAM_1: ATD-GAIN=7 NUM_EXP: 2 TIME_PER_EXP: 600S S_TO_N: 9 S_TO_N_TIME: 1200S FLUXNUM_1: 4 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: SAME POS FOR 6 AS 5 COMMENT_1: offset to 110'' from center LINENUM: 7.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F555W PARAM_1: ATD-GAIN=7 NUM_EXP: 2 TIME_PER_EXP: 1200S S_TO_N: 9 S_TO_N_TIME: 2200S FLUXNUM_1: 4 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: POS TARG 155.56, 155.56 COMMENT_1: offset to 220'' from center LINENUM: 8.000 TARGNAME: NGC5272 CONFIG: WFPC2 OPMODE: IMAGE APERTURE: PC1-FIX SP_ELEMENT: F814W PARAM_1: ATD-GAIN=7 NUM_EXP: 2 TIME_PER_EXP: 600S S_TO_N: 9 S_TO_N_TIME: 1200S FLUXNUM_1: 4 PRIORITY: 1 REQ_1: CYCLE 4; REQ_2: SAME POS FOR 8 AS 7 COMMENT_1: offset to 220'' from center ! End of RPSS template