! File: 4366C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:23:27:53 coverpage: title_1: HOT STELLAR POPULATIONS AND THEIR RADIAL GRADIENTS title_2: IN DENSE GLOBULAR CLUSTER CORES: CYCLE3 MEDIUM sci_cat: HOT STARS sci_subcat: UV-BRIGHT STARS proposal_for: GO pi_fname: STANISLAV pi_mi: G pi_lname: DJORGOVSKI pi_inst: CALTECH pi_country: USA hours_pri: 4.08 hours_par: 4.08 num_pri: 3 num_par: 3 wf_pc: Y foc: Y funds_amount: 133152 funds_length: 24 funds_date: OCT-93 off_fname: EARL off_lname: FREISE off_title: DIRECTOR,SPONS.RES. off_inst: 1590 off_addr_1: OFFICE OF SPONSORED RESEARCH off_addr_2: CALIFORNIA INSTITUTE OF TECHNOLOGY off_city: PASADENA off_state: CA off_zip: 91125 off_country: USA off_phone: (818) 356-6357 ! end of coverpage abstract: line_1: The goal of this program is to use both the resolving power and the far-UV line_2: imaging capability of HST to study the nature of hot stellar populations and line_3: their radial gradients in the centers of globular clusters that have undergone line_4: core collapse, or are close to it. This continues a Cycle 2 program which used line_5: the PC to study the radial gradients among the brighter stars, red giants, line_6: subgiants, and horizontal branch (HB) stars. Examination of archival IUE data line_7: has indicated that the gradients are present even at far-UV wavelengths. If line_8: this is true, some centrally concentrated hot stellar population must be line_9: present, e.g., faint BHB stars, blue stragglers, stripped red giant cores, line_10: merged stars, or some new, as yet unknown type of objects (recall the recent line_11: UIT discoveries of luminous hot UV stars in globulars). High-resolution line_12: observations of dense cluster cores in the far-UV are needed in order to check line_13: on the existence of population gradients among the hot stars, and establish line_14: their nature. Such data would provide essential input for theoretical models line_15: (as yet, our understanding of the gradients is very poor), and may be relevant line_16: for the origins of x-ray sources and millisecond pulsars in globular clusters, line_17: as well as the sources of far-UV light in elliptical galaxies. We propose line_18: parallel observations of outer fields using WFC, which would increase the line_19: radial baseline for the study of gradients, and substantially increase the line_20: true efficiency of the program. ! ! end of abstract general_form_proposers: lname: DJORGOVSKI fname: STANISLAV title: PI mi: G inst: CALTECH country: USA ! lname: KING fname: IVAN mi: R inst: UC-BERKELEY country: USA ! lname: PIOTTO fname: GIAMPAOLO inst: UNIVERSITA DI PADOVA country: ITALY esa: Y ! lname: MEYLAN fname: GEORGES inst: EUROPEAN SOUTHERN OBSERVATORY country: GERMANY esa: Y ! lname: WEIR fname: NICHOLAS inst: CALTECH country: USA ! lname: PHINNEY fname: STERL mi: E inst: CALTECH country: USA ! lname: CHERNOFF fname: DAVID mi: F inst: CORNELL UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: No changes. ! question: 3 section: 1 line_1: Our proposed sample contains three Galactic globular clusters, namely: NGC line_2: 6093, 6681, and 7099. Two of them have a definitive or probable PCC morphology, line_3: and all are highly concentrated. Previous space UV data (IUE or ANS) exist for line_4: all of them, and all are classified as being "blue" or "extremely blue" in their line_5: FUV colors (see de Boer 1985, A&A 142, 321, and references therein). For 6093 line_6: 7099 there are some GO and GTO observations proposed, but not in the far UV, line_7: which is essential for this project. For NGC 6681 there is only one, line_8: single-bandpass observation (by one of us, King, in his GTO program). None of line_9: the GTO or previous GO proposals (except for our own, related Cycle 2 proposal) line_10: mention anything about color and population gradients; we are not aware that any line_11: other group is planning to perfom similar science with the HST. Our proposed line_12: observing strategy is rather simple: for each target cluster, obtain images of line_13: the central region with the FOC/48 and F140W, F220W, F342W, and F430W filters; line_14: at the same time, obtain images in the parallel mode of an outer cluster field line_15: using the PC with F336W and F439W filters (U and B bands). For the primary FOC line_16: observations, we will use the F342W and F430W exposures to generate multicolor line_17: diagrams and transformations, in order to separate the intrinsically blue line_18: objects from spurious ones wich may be due to the red leaks in the F140W and line_19: F220W bands. An important part of this program are the parallel exposures with line_20: the WFC, 6.5 arcmin from the center of each cluster. These should supplement our line_21: central exposures (both from this program, and the PC exposures from our Cycle 2 line_22: program), thus providing an additional baseline for studies of radial gradients, line_23: as well as useful data for color-magnitude diagrams. ! question: 3 section: 2 line_1: None. ! question: 4 section: 1 line_1: We have already pursued the study of color and population gradients from the line_2: ground, e.g., with excellent seeing images from ESO, and have a continuing line_3: effort in this direction. However, even the best ground-based exposures are no line_4: match for the resolving power of the HST, especially in the crowded regions of line_5: dense globular cluster cores, as shown by numerous examples. Furthermore, the line_6: key goal of this proposal is to study the color and population gradients in the line_7: far-UV, which is impossible from the ground. This should probe the centrally line_8: concentrated hot stellar populations, for which there is practically no useful line_9: information in the ground-based data. The only data which do exist are low line_10: spatial resolution (or NO resolution) data from IUE, OAO, and ANS satellites. We line_11: conducted an exhaustive archival study of these, and found many interesting line_12: hints that the gradients persist in the far-UV (Djorgovski & Piotto 1992, AJ line_13: 104, 2112). However, these results are severely limited by the lack of angular line_14: resolution, and real imaging with HST should reveal much more. ! question: 4 section: 2 line_1: We estimated the exposures on the basis of the previous experience with FOC line_2: images of globular clusters (cf. Paresce et al. 1991; and numerous exposures line_3: obtained by King in engineering exposures of globular clusters). Both King and line_4: Meylan have a considerable hands-on experience with the relevant or similar FOC line_5: observations. We used the observed central surface brightnesses in the V band line_6: from our CCD photometry and the photoelectric UBV colors to scale the exposures line_7: relative to successful observations of 47 Tuc. A particular care was taken to line_8: estimate the extinction in the far-UV, using the transformations from van Albada line_9: et al. (1981, MNRAS 195, 591). Typical proposed integrations are 40 - 60 minutes line_10: with F140W, and 25 - 35 minutes with F220W, depending on the cluster central line_11: surface brightness. We used the scaling from the FOC Handbook for the F342W and line_12: F430W exposures. For the brighter clusters, we use neutral-density filters line_13: conjunction with F342W and F430W. FOC experience shows that a 2400s exposure in line_14: F430W detects B=24.5; thus our exposures should reach at least to the line_15: main-sequence turnoffs at B=19 to 20, and thus probe the entire population of line_16: blue stragglers, and certainly any hotter objects of a comparable or higher line_17: luminosity. Note that all FOC exposures have parallel WFC exposures, so that the line_18: true efficiency of HST usage is much higher than indicated by the percentage on line_19: the cover page. ! question: 5 section: 1 line_1: None. ! question: 6 section: 1 line_1: None. ! question: 7 section: 1 line_1: Our team has a combined expertise in dealing with the HST data (King, Meylan, line_2: Djorgovski, and Weir), image processing and deconvolutions (Weir, Djorgovski, line_3: and King), stellar photometry in crowded fields, using versions of both Daophot line_4: and Romafot, (Piotto, King, Djorgovski, and Weir), photometry of globular line_5: clusters (King, Djorgovski, Piotto, and Meylan), theoretical interpretation and line_6: modeling (Phinney and Chernoff), and globular cluster dynamics (King, Meylan, line_7: Chernoff, and Phinney). We plan to process and analyse the data primarly at line_8: Caltech (Djorgovski and Weir), and also at Berkeley (King), Padova (Piotto), and line_9: ESO (Meylan). Theoretical modeling and analysis will be done largely at Caltech line_10: (Phinney) and at Cornell (Chernoff). We already have an extensive set of line_11: software for the task, although more software may need to be written for the line_12: specific problems. Especially noteworthy is Weir's Maximum Entropy package for line_13: deconvolutions of the HST images. Considerable computing hardware already exists line_14: at all of our institutions, and we anticipate acquiring a dedicated workstation line_15: at Caltech, which would make the data processing faster and more cost-effective. line_16: To measure the images, we plan to use different HST-PSF-optimized versions of line_17: both Daophot and Romafot. We will also try to use the image deconvolutions to line_18: provide initial star lists for subsequent processing by a standard PSF fitting line_19: package, such as Daophot or Romafot (Weir, Djorgovski, & Piotto 1990). Our main line_20: technique for restoring the images is a Bayesian Maximum Entropy based approach line_21: using a two-dimensional direct image deconvolution driver for the commercial line_22: package MemSys5. For more details see Weir & Djorgovski 1991, Weir 1991, King line_23: et al. 1991, and references therein. (see Phase I prop. for full references) ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: Djorgovski is a PI on two Cycle 1 GO programs (No. 2695, Morphology of PKS line_2: 1614+051, a Quasar-Galaxy Pair at z=3.21; and No. 2698, Lyman-Alpha Imaging of line_3: Young and Forming Galaxies at Large Redshifts), and a Co-I on another GO program line_4: (No. 2583), none of which are related to this proposal. The analysis (held up by line_5: the problems involving PSF modeling, and thus image deconvolutions) is in line_6: progress; at least three papers in major journals are anticipated to result from line_7: this work, and to be submitted over the next few months. Djorgovski is also a PI line_8: on a Cycle 2 program (3458, Stellar Population Gradients in Post-Core-Collapse line_9: Globular Clusters), with the others from this proposal as co-I's, which is line_10: directly relevant for this project. Some data have been received, and are being line_11: analysed. Djorgovski is also a Co-I on two other Cycle 2 programs, neither line_12: of which is related to this proposal. King is a GTO on the FOC team, and is line_13: actively involved in many HST projects; he is also a Co-I on several GO programs line_14: from Cycles 1 and 2. Meylan was an instrument scientist on the FOC team, and is line_15: also involved in several HST projects. Both King and Meylan are coauthors on line_16: several HST-based papers now in press or preparation. Especially relevant for line_17: this proposal is the paper by Paresce et al. 1991, Nature 352, 297. Several of line_18: us (King, Weir, and Djorgovski) authored or coauthored several papers dealing line_19: with the image processing and deconvolution of HST data. See for example King line_20: et al. 1991, AJ 102, 1553. ! question: 9 section: 2 line_1: For all of the Cycle 1 proposals, the analysis is still in progress, although line_2: some results have been published in conference proceedings. For the Cycle 2 line_3: programs, only a portion of the data has been received. One paper has been line_4: submitted to Nature, describing the discovery of a first post-core-collapse line_5: cluster in M31, and another is in a draft form. ! question: 9 section: 3 line_1: "Blue Stragglers in the Core of the Globular Cluster 47 Tucanae", by line_2: Paresce et al. (includes King, Meylan) 1991, Nature 352, 297. line_3: "The Current Ability of HST to Reveal Morphological Structure in Medium line_4: Redshift Galaxies", by King et al. (includes Djorgovski, Weir) 1991, line_5: AJ 102, 1553. line_6: "The First Detection of a Collapsed-Core Globular Cluster in M31", line_7: by Bendinelli et al. (includes Djorgovski, Weir) 1993, submitted to Nature. line_8: + several conference papers, including Djorgovski, King, Weir, and Meylan. ! question: 10 section: 1 line_1: We already have an extensive set of software for the task, although more line_2: software may need to be written for the specific problems. Especially line_3: noteworthy is Weir's Maximum Entropy package for deconvolutions of the HST line_4: images. Considerable computing hardware already exists at all of our line_5: institutions, and we anticipate acquiring a dedicated workstation at Caltech, line_6: which would make the data processing faster and more cost-effective. line_7: There are adequate research facilities (libraries, etc.) at our institutions. line_8: At least one or two Caltech graduate students will be involved in this project. ! !end of general form text general_form_address: lname: DJORGOVSKI fname: STANISLAV mi: G category: PI inst: Caltech addr_1: MAILSTOP 105-24, ROBINSON LAB. addr_2: CALIFORNIA INSTITUTE OF TECHNOLOGY city: PASADENA state: CA zip: 91125 country: USA phone: (818) 356-4415 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC6093 name_2: M80 descr_1: C,201 pos_1: RA = 16H 17M 02.50S +/- 0.15S, pos_2: DEC = -22D 58' 30.0" +/- 1.0" equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 comment_1: GLOBULAR CLUSTER CENTRAL CUSP. comment_2: TOTAL V MAG GIVEN AS FLUXVAL. comment_3: THIS IS THE PRIMARY TARGET, USING comment_4: FOC/96. TARGNUM 4 IS A PARALLEL comment_5: EXPOSURE USING PC, AND CAN BE comment_6: OMITTED IF THE SCHEDULING IS TOO comment_7: DIFFICULT OR IF IT WOULD DELAY comment_8: THE SCHEDULING OF THE PRIMARY comment_9: FOC EXPOSURES. fluxnum_1: 1 fluxval_1: V=7.4 ! targnum: 2 name_1: NGC6681 name_2: M70 descr_1: C,201 pos_1: RA = 18H 43M 12.60S +/- 0.15S, pos_2: DEC = -32D 17' 30.0" +/- 1.0" equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 comment_1: GLOBULAR CLUSTER CENTRAL CUSP. comment_2: TOTAL V MAG GIVEN AS FLUXVAL. comment_3: THIS IS THE PRIMARY TARGET, USING comment_4: FOC/96. TARGNUM 5 IS A PARALLEL comment_5: EXPOSURE USING PC, AND CAN BE comment_6: OMITTED IF THE SCHEDULING IS TOO comment_7: DIFFICULT OR IF IT WOULD DELAY comment_8: THE SCHEDULING OF THE PRIMARY comment_9: FOC EXPOSURES. fluxnum_1: 1 fluxval_1: V=7.9 ! targnum: 3 name_1: NGC7099 name_2: M30 descr_1: C,201 pos_1: RA = 21H 40M 22.00S +/- 0.15S, pos_2: DEC = -23D 10' 44.0" +/- 1.0" equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 comment_1: GLOBULAR CLUSTER CENTRAL CUSP. comment_2: TOTAL V MAG GIVEN AS FLUXVAL. comment_3: THIS IS THE PRIMARY TARGET, USING comment_4: FOC/96. TARGNUM 6 IS A PARALLEL comment_5: EXPOSURE USING PC, AND CAN BE comment_6: OMITTED IF THE SCHEDULING IS TOO comment_7: DIFFICULT OR IF IT WOULD DELAY comment_8: THE SCHEDULING OF THE PRIMARY comment_9: FOC EXPOSURES. fluxnum_1: 1 fluxval_1: V=7.5 ! targnum: 4 name_1: NGC6093-OUTER name_2: M80 descr_1: C,201 pos_1: RA = 16H 17M 02.50S +/- 0.15S, pos_2: DEC = -22D 58' 30.0" +/- 1.0", pos_3: REGION, pos_4: R=15' equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 comment_1: GLOBULAR CLUSTER CENTRAL CUSP. comment_2: TOTAL V MAG GIVEN AS FLUXVAL. comment_3: THIS IS A PARALLEL EXPOSURE FOR comment_4: TARGNUM 1. THIS EXPOSURE CAN BE comment_5: OMITTED IF THE SCHEDULING IS TOO comment_6: DIFFICULT OR IF IT WOULD DELAY comment_7: THE SCHEDULING OF THE PRIMARY comment_8: FOC EXPOSURES. THE COORDINATES comment_9: GIVEN ARE FOR THE PRIMARY EXP. comment_10: ANY ORIENTATION IS OK FOR THIS. fluxnum_1: 1 fluxval_1: V=7.4 ! targnum: 5 name_1: NGC6681-OUTER name_2: M70 descr_1: C,201 pos_1: RA = 18H 43M 12.60S +/- 0.15S, pos_2: DEC = -32D 17' 30.0" +/- 1.0", pos_3: REGION, pos_4: R = 15' equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 comment_1: GLOBULAR CLUSTER CENTRAL CUSP. comment_2: TOTAL V MAG GIVEN AS FLUXVAL. comment_3: THIS IS A PARALLEL EXPOSURE FOR comment_4: TARGNUM 2. THIS EXPOSURE CAN BE comment_5: OMITTED IF THE SCHEDULING IS TOO comment_6: DIFFICULT OR IF IT WOULD DELAY comment_7: THE SCHEDULING OF THE PRIMARY comment_8: FOC EXPOSURES. THE COORDINATES comment_9: GIVEN ARE FOR THE PRIMARY EXP. comment_10: ANY ORIENTATION IS OK FOR THIS. fluxnum_1: 1 fluxval_1: V=7.9 ! targnum: 6 name_1: NGC7099-OUTER name_2: M30 descr_1: C,201 pos_1: RA = 21H 40M 22.00S +/- 0.15S, pos_2: DEC = -23D 10' 44.0" +/- 1.0", pos_3: REGION, pos_4: R = 15' equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 comment_1: GLOBULAR CLUSTER CENTRAL CUSP. comment_2: TOTAL V MAG GIVEN AS FLUXVAL. comment_3: THIS IS A PARALLEL EXPOSURE FOR comment_4: TARGNUM 3. THIS EXPOSURE CAN BE comment_5: OMITTED IF THE SCHEDULING IS TOO comment_6: DIFFICULT OR IF IT WOULD DELAY comment_7: THE SCHEDULING OF THE PRIMARY comment_8: FOC EXPOSURES. THE COORDINATES comment_9: GIVEN ARE FOR THE PRIMARY EXP. comment_10: ANY ORIENTATION IS OK FOR THIS. fluxnum_1: 1 fluxval_1: V=7.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: NGC6093 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F140W num_exp: 1 time_per_exp: 2200S fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; req_2: SAME ORIENT FOR 1.2-1.4 AS 1.1; req_3: GROUP 1.1-1.4 WITHIN 14D; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. comment_3: "SAME ORIENT" AND "GROUP WITHIN" comment_4: CONSTRAINTS MAY BE RELAXED FOR BETTER comment_5: SCHEDULABILITY IF NECESSARY, ALTHOUGH comment_6: THEY ARE PREFERRED. ! linenum: 1.200 targname: NGC6093 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W,F1ND num_exp: 1 time_per_exp: 15M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 1.300 targname: NGC6093 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F220W num_exp: 1 time_per_exp: 25M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 1.400 targname: NGC6093 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W,F2ND num_exp: 1 time_per_exp: 10M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 2.100 targname: NGC6681 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F140W num_exp: 1 time_per_exp: 2200S fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; req_2: SAME ORIENT FOR 2.2-2.4 AS 2.1; req_3: GROUP 2.1-2.4 WITHIN 14D; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. comment_3: "SAME ORIENT" AND "GROUP WITHIN" comment_4: CONSTRAINTS MAY BE RELAXED FOR BETTER comment_5: SCHEDULABILITY IF NECESSARY, ALTHOUGH comment_6: THEY ARE PREFERRED. ! linenum: 2.200 targname: NGC6681 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W,F1ND num_exp: 1 time_per_exp: 15M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 2.300 targname: NGC6681 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F220W num_exp: 1 time_per_exp: 25M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 2.400 targname: NGC6681 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W,F2ND num_exp: 1 time_per_exp: 10M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 3.100 targname: NGC7099 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F140W num_exp: 1 time_per_exp: 2200S fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; req_2: SAME ORIENT FOR 3.2-3.3 AS 3.1; req_3: GROUP 3.1-3.3 WITHIN 14D; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. comment_3: "SAME ORIENT" AND "GROUP WITHIN" comment_4: CONSTRAINTS MAY BE RELAXED FOR BETTER comment_5: SCHEDULABILITY IF NECESSARY, ALTHOUGH comment_6: THEY ARE PREFERRED. ! linenum: 3.200 targname: NGC7099 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F220W num_exp: 1 time_per_exp: 25M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 3.300 targname: NGC7099 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W,F2ND num_exp: 1 time_per_exp: 10M fluxnum_1: 1 priority: 1 req_1: CYCLE3 ; comment_1: FOC/48 MODE IS ACCEPTABLE AND comment_2: EVEN PREFERED, IF AVAILABLE. ! linenum: 4.100 targname: NGC6093-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F336W num_exp: 1 time_per_exp: 2200S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 1.1 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6093. THIS IS comment_3: ONE OF THE PARALLEL EXP. W. LINES 1. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 4.200 targname: NGC6093-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F336W num_exp: 1 time_per_exp: 15M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 1.2 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6093. THIS IS comment_3: ONE OF THE PARALLEL EXP. W. LINES 1. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 4.300 targname: NGC6093-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 25M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 1.3 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6093. THIS IS comment_3: ONE OF THE PARALLEL EXP. W. LINES 1. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 4.400 targname: NGC6093-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 10M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 1.4 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6093. THIS IS comment_3: ONE OF THE PARALLEL EXP. W. LINES 1. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 5.100 targname: NGC6681-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F336W num_exp: 1 time_per_exp: 2200S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 2.1 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6681. THIS IS ONE comment_3: OF THE PARALLEL EXP. W. LINES 2. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 5.200 targname: NGC6681-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F336W num_exp: 1 time_per_exp: 15M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 2.2 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6681. THIS IS ONE comment_3: OF THE PARALLEL EXP. W. LINES 2. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 5.300 targname: NGC6681-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 25M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 2.3 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6681. THIS IS ONE comment_3: OF THE PARALLEL EXP. W. LINES 2. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 5.400 targname: NGC6681-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 10M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 2.4 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC6681. THIS IS ONE comment_3: OF THE PARALLEL EXP. W. LINES 2. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 6.100 targname: NGC7099-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F336W num_exp: 1 time_per_exp: 2200S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 3.1 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC7099. THIS IS ONE comment_3: OF THE PARALLEL EXP. WITH LINES 3. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 6.200 targname: NGC7099-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 25M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 3.2 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC7099. THIS IS ONE comment_3: OF THE PARALLEL EXP. WITH LINES 3. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! linenum: 6.300 targname: NGC7099-OUTER config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 10M fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE3 ; req_2: PAR WITH 3.3 comment_1: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN comment_2: FROM THE CORE OF NGC7099. THIS IS ONE comment_3: OF THE PARALLEL EXP. WITH LINES 3. comment_4: IT CAN BE MODIFIED OR EVEN OMITTED comment_5: IF THE SCHEDULING CONSTRAINTS ARE comment_6: TOO TOUGH. ANY ORIENTATION IS OK. ! ! end of exposure logsheet ! No scan data records found