Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 4366c Report Date: 09-May-96:19:34 Version: ********** Check-in Date: ********** 1.Proposal Title: HOT STELLAR POPULATIONS AND THEIR RADIAL GRADIENTS IN DENSE GLOBULAR CLUSTER CORES: CYCLE3 MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID HOT STARS GO Sub Category UV-BRIGHT STARS ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Stanislav G Djorgovski CALTECH USA ------------------------------------------------------------------------------------ 7. Abstract The goal of this program is to use both the resolving power and the far-UV imaging capability of HST to study the nature of hot stellar populations and their radial gradients in the centers of globular clusters that have undergone core collapse, or are close to it. This continues a Cycle 2 program which used the PC to study the radial gradients among the brighter stars, red giants, subgiants, and horizontal branch (HB) stars. Examination of archival IUE data has indicated that the gradients are present even at far-UV wavelengths. If this is true, some centrally concentrated hot stellar population must be present, e.g., faint BHB stars, blue stragglers, stripped red giant cores, merged stars, or some new, as yet unknown type of objects (recall the recent UIT discoveries of luminous hot UV stars in globulars). High-resolution observations of dense cluster cores in the far-UV are needed in order to check on the existence of population gradients among the hot stars, and establish their nature. Such data would provide essential input for theoretical models (as yet, our understanding of the gradients is very poor), and may be relevant for the origins of x-ray sources and millisecond pulsars in globular clusters, as well as the sources of far-UV light in elliptical galaxies. We propose parallel observations of outer fields using WFC, which would increase the radial baseline for the study of gradients, and substantially increase the true efficiency of the program. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 4.08 par: 4.08 10. Num targs pri: 3 par: 3 ------------------------------------------------------------------------------------ 11. Instruments requested: FOC WF/PC ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 4366c PI: Stanislav G Djorgovski Proposal Title: HOT STELLAR POPULATIONS AND THEIR RADIAL GRADIENTS IN DENSE GLOBULAR CLUSTER CORES: CYCLE3 MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Stanislav G Djorgovski CALTECH USA Ivan R King UC-BERKELEY USA Giampaolo Piotto UNIVERSITA DI PADOVA ITALY X Georges Meylan EUROPEAN SOUTHERN OBSERVATORY GERMANY X Nicholas Weir CALTECH USA Sterl E Phinney CALTECH USA David F Chernoff CORNELL UNIVERSITY USA ------------------------------------------------------------------------------------ 2. Scientific Justification. No changes. ------------------------------------------------------------------------------------ 3. Description of proposed observations. Our proposed sample contains three Galactic globular clusters, namely: NGC 6093, 6681, and 7099. Two of them have a definitive or probable PCC morphology, and all are highly concentrated. Previous space UV data (IUE or ANS) exist for all of them, and all are classified as being "blue" or "extremely blue" in their FUV colors (see de Boer 1985, A&A 142, 321, and references therein). For 6093 7099 there are some GO and GTO observations proposed, but not in the far UV, which is essential for this project. For NGC 6681 there is only one, single- bandpass observation (by one of us, King, in his GTO program). None of the GTO or previous GO proposals (except for our own, related Cycle 2 proposal) mention anything about color and population gradients; we are not aware that any other group is planning to perfom similar science with the HST. Our proposed observing strategy is rather simple: for each target cluster, obtain images of the central region with the FOC/48 and F140W, F220W, F342W, and F430W filters; at the same time, obtain images in the parallel mode of an outer cluster field using the PC with F336W and F439W filters (U and B bands). For the primary FOC observations, we will use the F342W and F430W exposures to generate multicolor diagrams and transformations, in order to separate the intrinsically blue objects from spurious ones wich may be due to the red leaks in the F140W and F220W bands. An important part of this program are the parallel exposures with the WFC, 6.5 arcmin from the center of each cluster. These should supplement our central exposures (both from this program, and the PC exposures from our Cycle 2 program), thus providing an additional baseline for studies of radial gradients, as well as useful data for color-magnitude diagrams. None. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. We have already pursued the study of color and population gradients from the ground, e.g., with excellent seeing images from ESO, and have a continuing effort in this direction. However, even the best ground-based exposures are no match for the resolving power of the HST, especially in the crowded regions of dense globular cluster cores, as shown by numerous examples. Furthermore, the key goal of this proposal is to study the color and population gradients in the far-UV, which is impossible from the ground. This should probe the centrally concentrated hot stellar populations, for which there is practically no useful information in the ground-based data. The only data which do exist are low spatial resolution (or NO resolution) data from IUE, OAO, and ANS satellites. We conducted an exhaustive archival study of these, and found many interesting hints that the gradients persist in the far-UV (Djorgovski & Piotto 1992, AJ 104, 2112). However, these results are severely limited by the lack of angular resolution, and real imaging with HST should reveal much more. We estimated the exposures on the basis of the previous experience with FOC images of globular clusters (cf. Paresce et al. 1991; and numerous exposures obtained by King in engineering exposures of globular clusters). Both King and Meylan have a considerable hands- on experience with the relevant or similar FOC observations. We used the observed central surface brightnesses in the V band from our CCD photometry and the photoelectric UBV colors to scale the exposures relative to successful observations of 47 Tuc. A particular care was taken to estimate the extinction in the far-UV, using the transformations from van Albada et al. (1981, MNRAS 195, 591). Typical proposed integrations are 40 - 60 minutes with F140W, and 25 - 35 minutes with F220W, depending on the cluster central surface brightness. We used the scaling from the FOC Handbook for the F342W and F430W exposures. For the brighter clusters, we use neutral-density filters conjunction with F342W and F430W. FOC experience shows that a 2400s exposure in F430W detects B=24.5; thus our exposures should reach at least to the main-sequence turnoffs at B=19 to 20, and thus probe the entire population of blue stragglers, and certainly any hotter objects of a comparable or higher luminosity. Note that all FOC exposures have parallel WFC exposures, so that the true efficiency of HST usage is much higher than indicated by the percentage on the cover page. ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. None. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. None. Page 4 ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. Our team has a combined expertise in dealing with the HST data (King, Meylan, Djorgovski, and Weir), image processing and deconvolutions (Weir, Djorgovski, and King), stellar photometry in crowded fields, using versions of both Daophot and Romafot, (Piotto, King, Djorgovski, and Weir), photometry of globular clusters (King, Djorgovski, Piotto, and Meylan), theoretical interpretation and modeling (Phinney and Chernoff), and globular cluster dynamics (King, Meylan, Chernoff, and Phinney). We plan to process and analyse the data primarly at Caltech (Djorgovski and Weir), and also at Berkeley (King), Padova (Piotto), and ESO (Meylan). Theoretical modeling and analysis will be done largely at Caltech (Phinney) and at Cornell (Chernoff). We already have an extensive set of software for the task, although more software may need to be written for the specific problems. Especially noteworthy is Weir's Maximum Entropy package for deconvolutions of the HST images. Considerable computing hardware already exists at all of our institutions, and we anticipate acquiring a dedicated workstation at Caltech, which would make the data processing faster and more cost-effective. To measure the images, we plan to use different HST-PSF-optimized versions of both Daophot and Romafot. We will also try to use the image deconvolutions to provide initial star lists for subsequent processing by a standard PSF fitting package, such as Daophot or Romafot (Weir, Djorgovski, & Piotto 1990). Our main technique for restoring the images is a Bayesian Maximum Entropy based approach using a two-dimensional direct image deconvolution driver for the commercial package MemSys5. For more details see Weir & Djorgovski 1991, Weir 1991, King et al. 1991, and references therein. (see Phase I prop. for full references) ------------------------------------------------------------------------------------ 8. Additional comments or special requests. None. Page 5 ------------------------------------------------------------------------------------ 9. Description of previous HST work. Djorgovski is a PI on two Cycle 1 GO programs (No. 2695, Morphology of PKS 1614+051, a Quasar-Galaxy Pair at z=3.21; and No. 2698, Lyman-Alpha Imaging of Young and Forming Galaxies at Large Redshifts), and a Co-I on another GO program (No. 2583), none of which are related to this proposal. The analysis (held up by the problems involving PSF modeling, and thus image deconvolutions) is in progress; at least three papers in major journals are anticipated to result from this work, and to be submitted over the next few months. Djorgovski is also a PI on a Cycle 2 program (3458, Stellar Population Gradients in Post-Core-Collapse Globular Clusters), with the others from this proposal as co-I's, which is directly relevant for this project. Some data have been received, and are being analysed. Djorgovski is also a Co-I on two other Cycle 2 programs, neither of which is related to this proposal. King is a GTO on the FOC team, and is actively involved in many HST projects; he is also a Co-I on several GO programs from Cycles 1 and 2. Meylan was an instrument scientist on the FOC team, and is also involved in several HST projects. Both King and Meylan are coauthors on several HST-based papers now in press or preparation. Especially relevant for this proposal is the paper by Paresce et al. 1991, Nature 352, 297. Several of us (King, Weir, and Djorgovski) authored or coauthored several papers dealing with the image processing and deconvolution of HST data. See for example King et al. 1991, AJ 102, 1553. For all of the Cycle 1 proposals, the analysis is still in progress, although some results have been published in conference proceedings. For the Cycle 2 programs, only a portion of the data has been received. One paper has been submitted to Nature, describing the discovery of a first post-core- collapse cluster in M31, and another is in a draft form. "Blue Stragglers in the Core of the Globular Cluster 47 Tucanae", by Paresce et al. (includes King, Meylan) 1991, Nature 352, 297. "The Current Ability of HST to Reveal Morphological Structure in Medium Redshift Galaxies", by King et al. (includes Djorgovski, Weir) 1991, AJ 102, 1553. "The First Detection of a Collapsed-Core Globular Cluster in M31", by Bendinelli et al. (includes Djorgovski, Weir) 1993, submitted to Nature. + several conference papers, including Djorgovski, King, Weir, and Meylan. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). We already have an extensive set of software for the task, although more software may need to be written for the specific problems. Especially noteworthy is Weir's Maximum Entropy package for deconvolutions of the HST images. Considerable computing hardware already exists at all of our institutions, and we anticipate acquiring a dedicated workstation at Caltech, which would make the data processing faster and more cost-effective. There are adequate research facilities (libraries, etc.) at our institutions. At least one or two Caltech graduate students will be involved in this project. ------------------------------------------------------------------------------------ 11. Address Information Name: STANISLAV G DJORGOVSKI Category: PI Institution: Caltech Address: MAILSTOP 105-24, ROBINSON LAB. CALIFORNIA INSTITUTE OF TECHNOLOGY City: PASADENA State: CA Zip Code: 91125 Country: USA Telephone: (818) 356-4415 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4366c [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 NGC6093 M80 C,201 RA = 16H 17M 02.50S +/- J2000 1 V=7.4 0.15S, DEC = -22D 58' 30.0" +/- 1.0" Comments: GLOBULAR CLUSTER CENTRAL CUSP. TOTAL V MAG GIVEN AS FLUXVAL. THIS IS THE PRIMARY TARGET, USING FOC/96. TARGNUM 4 IS A PARALLEL EXPOSURE USING PC, AND CAN BE OMITTED IF THE SCHEDULING IS TOO DIFFICULT OR IF IT WOULD DELAY THE SCHEDULING OF THE PRIMARY FOC EXPOSURES. ------------------------------------------------------------------------------------------------------------------------------------ 2 NGC6681 M70 C,201 RA = 18H 43M 12.60S +/- J2000 1 V=7.9 0.15S, DEC = -32D 17' 30.0" +/- 1.0" Comments: GLOBULAR CLUSTER CENTRAL CUSP. TOTAL V MAG GIVEN AS FLUXVAL. THIS IS THE PRIMARY TARGET, USING FOC/96. TARGNUM 5 IS A PARALLEL EXPOSURE USING PC, AND CAN BE OMITTED IF THE SCHEDULING IS TOO DIFFICULT OR IF IT WOULD DELAY THE SCHEDULING OF THE PRIMARY FOC EXPOSURES. ------------------------------------------------------------------------------------------------------------------------------------ 3 NGC7099 M30 C,201 RA = 21H 40M 22.00S +/- J2000 1 V=7.5 0.15S, DEC = -23D 10' 44.0" +/- 1.0" Comments: GLOBULAR CLUSTER CENTRAL CUSP. TOTAL V MAG GIVEN AS FLUXVAL. THIS IS THE PRIMARY TARGET, USING FOC/96. TARGNUM 6 IS A PARALLEL EXPOSURE USING PC, AND CAN BE OMITTED IF THE SCHEDULING IS TOO DIFFICULT OR IF IT WOULD DELAY THE SCHEDULING OF THE PRIMARY FOC EXPOSURES. ------------------------------------------------------------------------------------------------------------------------------------ 4 NGC6093- C,201 RA = 16H 17M 02.50S +/- J2000 1 V=7.4 OUTER M80 0.15S, DEC = -22D 58' 30.0" +/- 1.0", REGION, R=15' Comments: GLOBULAR CLUSTER CENTRAL CUSP. TOTAL V MAG GIVEN AS FLUXVAL. THIS IS A PARALLEL EXPOSURE FOR TARGNUM 1. THIS EXPOSURE CAN BE OMITTED IF THE SCHEDULING IS TOO DIFFICULT OR IF IT WOULD DELAY THE SCHEDULING OF THE PRIMARY FOC EXPOSURES. THE COORDINATES GIVEN ARE FOR THE PRIMARY EXP. ANY ORIENTATION IS OK FOR THIS. ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4366c [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 5 NGC6681- C,201 RA = 18H 43M 12.60S +/- J2000 1 V=7.9 OUTER M70 0.15S, DEC = -32D 17' 30.0" +/- 1.0", REGION, R = 15' Comments: GLOBULAR CLUSTER CENTRAL CUSP. TOTAL V MAG GIVEN AS FLUXVAL. THIS IS A PARALLEL EXPOSURE FOR TARGNUM 2. THIS EXPOSURE CAN BE OMITTED IF THE SCHEDULING IS TOO DIFFICULT OR IF IT WOULD DELAY THE SCHEDULING OF THE PRIMARY FOC EXPOSURES. THE COORDINATES GIVEN ARE FOR THE PRIMARY EXP. ANY ORIENTATION IS OK FOR THIS. ------------------------------------------------------------------------------------------------------------------------------------ 6 NGC7099- C,201 RA = 21H 40M 22.00S +/- J2000 1 V=7.5 OUTER M30 0.15S, DEC = -23D 10' 44.0" +/- 1.0", REGION, R = 15' Comments: GLOBULAR CLUSTER CENTRAL CUSP. TOTAL V MAG GIVEN AS FLUXVAL. THIS IS A PARALLEL EXPOSURE FOR TARGNUM 3. THIS EXPOSURE CAN BE OMITTED IF THE SCHEDULING IS TOO DIFFICULT OR IF IT WOULD DELAY THE SCHEDULING OF THE PRIMARY FOC EXPOSURES. THE COORDINATES GIVEN ARE FOR THE PRIMARY EXP. ANY ORIENTATION IS OK FOR THIS. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4366c [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1.1 NGC6093 FOC/96 IMAGE 512X512 F140W 1 2200S 1 1 CYCLE3 SAME ORIENT FOR 1.2-1.4 AS 1.1 GROUP 1.1-1.4 WITHIN 14D Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. "SAME ORIENT" AND "GROUP WITHIN" CONSTRAINTS MAY BE RELAXED FOR BETTER SCHEDULABILITY IF NECESSARY, ALTHOUGH THEY ARE PREFERRED. ------------------------------------------------------------------------------------------------------------------------------------ 1.2 NGC6093 FOC/96 IMAGE 512X512 F342W, 1 15M 1 1 CYCLE3 F1ND Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ 1.3 NGC6093 FOC/96 IMAGE 512X512 F220W 1 25M 1 1 CYCLE3 Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ 1.4 NGC6093 FOC/96 IMAGE 512X512 F430W, 1 10M 1 1 CYCLE3 F2ND Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ 2.1 NGC6681 FOC/96 IMAGE 512X512 F140W 1 2200S 1 1 CYCLE3 SAME ORIENT FOR 2.2-2.4 AS 2.1 GROUP 2.1-2.4 WITHIN 14D Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. "SAME ORIENT" AND "GROUP WITHIN" CONSTRAINTS MAY BE RELAXED FOR BETTER SCHEDULABILITY IF NECESSARY, ALTHOUGH THEY ARE PREFERRED. ------------------------------------------------------------------------------------------------------------------------------------ 2.2 NGC6681 FOC/96 IMAGE 512X512 F342W, 1 15M 1 1 CYCLE3 F1ND Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ 2.3 NGC6681 FOC/96 IMAGE 512X512 F220W 1 25M 1 1 CYCLE3 Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4366c [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 2.4 NGC6681 FOC/96 IMAGE 512X512 F430W, 1 10M 1 1 CYCLE3 F2ND Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ 3.1 NGC7099 FOC/96 IMAGE 512X512 F140W 1 2200S 1 1 CYCLE3 SAME ORIENT FOR 3.2-3.3 AS 3.1 GROUP 3.1-3.3 WITHIN 14D Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. "SAME ORIENT" AND "GROUP WITHIN" CONSTRAINTS MAY BE RELAXED FOR BETTER SCHEDULABILITY IF NECESSARY, ALTHOUGH THEY ARE PREFERRED. ------------------------------------------------------------------------------------------------------------------------------------ 3.2 NGC7099 FOC/96 IMAGE 512X512 F220W 1 25M 1 1 CYCLE3 Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ 3.3 NGC7099 FOC/96 IMAGE 512X512 F430W, 1 10M 1 1 CYCLE3 F2ND Comments: FOC/48 MODE IS ACCEPTABLE AND EVEN PREFERED, IF AVAILABLE. ------------------------------------------------------------------------------------------------------------------------------------ 4.1 NGC6093- PC IMAGE PCALL F336W CR-SPLIT=NO 1 2200S 1 1 CYCLE3 OUTER PAR WITH 1.1 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6093. THIS IS ONE OF THE PARALLEL EXP. W. LINES 1. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ 4.2 NGC6093- PC IMAGE PCALL F336W CR-SPLIT=NO 1 15M 1 1 CYCLE3 OUTER PAR WITH 1.2 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6093. THIS IS ONE OF THE PARALLEL EXP. W. LINES 1. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4366c [ 10] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 4.3 NGC6093- PC IMAGE PCALL F439W CR-SPLIT=NO 1 25M 1 1 CYCLE3 OUTER PAR WITH 1.3 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6093. THIS IS ONE OF THE PARALLEL EXP. W. LINES 1. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ 4.4 NGC6093- PC IMAGE PCALL F439W CR-SPLIT=NO 1 10M 1 1 CYCLE3 OUTER PAR WITH 1.4 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6093. THIS IS ONE OF THE PARALLEL EXP. W. LINES 1. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ 5.1 NGC6681- PC IMAGE PCALL F336W CR-SPLIT=NO 1 2200S 1 1 CYCLE3 OUTER PAR WITH 2.1 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6681. THIS IS ONE OF THE PARALLEL EXP. W. LINES 2. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ 5.2 NGC6681- PC IMAGE PCALL F336W CR-SPLIT=NO 1 15M 1 1 CYCLE3 OUTER PAR WITH 2.2 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6681. THIS IS ONE OF THE PARALLEL EXP. W. LINES 2. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4366c [ 11] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 5.3 NGC6681- PC IMAGE PCALL F439W CR-SPLIT=NO 1 25M 1 1 CYCLE3 OUTER PAR WITH 2.3 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6681. THIS IS ONE OF THE PARALLEL EXP. W. LINES 2. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ 5.4 NGC6681- PC IMAGE PCALL F439W CR-SPLIT=NO 1 10M 1 1 CYCLE3 OUTER PAR WITH 2.4 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC6681. THIS IS ONE OF THE PARALLEL EXP. W. LINES 2. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ 6.1 NGC7099- PC IMAGE PCALL F336W CR-SPLIT=NO 1 2200S 1 1 CYCLE3 OUTER PAR WITH 3.1 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC7099. THIS IS ONE OF THE PARALLEL EXP. WITH LINES 3. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ 6.2 NGC7099- PC IMAGE PCALL F439W CR-SPLIT=NO 1 25M 1 1 CYCLE3 OUTER PAR WITH 3.2 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC7099. THIS IS ONE OF THE PARALLEL EXP. WITH LINES 3. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4366c [ 12] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 6.3 NGC7099- PC IMAGE PCALL F439W CR-SPLIT=NO 1 10M 1 1 CYCLE3 OUTER PAR WITH 3.3 Comments: GLOBULAR CLUSTER FIELD AT 6.5 ARCMIN FROM THE CORE OF NGC7099. THIS IS ONE OF THE PARALLEL EXP. WITH LINES 3. IT CAN BE MODIFIED OR EVEN OMITTED IF THE SCHEDULING CONSTRAINTS ARE TOO TOUGH. ANY ORIENTATION IS OK. ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 4366c [ 13] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOC/96 PC ------------------------------------------------------------------------------------------------------------------------------------ Opmodes IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters CR-SPLIT ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 4.08 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category HOT STARS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category UV-BRIGHT STARS ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE3 ; SAME ORIENT FOR 1.2-1.4 AS 1.1; GROUP 1.1-1.4 WITHIN 14D; SAME ORIENT FOR 2.2-2.4 AS 2.1; GROUP 2.1-2.4 WITHIN 14D; SAME ORIENT FOR 3.2-3.3 AS 3.1; GROUP 3.1-3.3 WITHIN 14D; PAR WITH 1.1 PAR WITH 1.2 PAR WITH 1.3 PAR WITH 1.4 PAR WITH 2.1 PAR WITH 2.2 PAR WITH 2.3 PAR WITH 2.4 PAR WITH 3.1 PAR WITH 3.2 PAR WITH 3.3 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F140W F342W,F1ND F220W F430W,F2ND F336W F439W ------------------------------------------------------------------------------------------------------------------------------------ Target Names NGC6093 M80 NGC6681 M70 NGC7099 M30 NGC6093-OUTER NGC6681-OUTER NGC7099-OUTER ------------------------------------------------------------------------------------------------------------------------------------