Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 4559c Report Date: 09-May-96:19:42 Version: ********** Check-in Date: ********** 1.Proposal Title: UV SPECTRA OF GLOBULAR CLUSTERS AND GALAXY CORES - CYCLE 3 MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID GALAXIES & CLUSTERS GO Sub Category STELLAR POPULATIONS ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone David Burstein ARIZONA STATE UNIVERSITY USA ------------------------------------------------------------------------------------ 7. Abstract An understanding of stellar populations in galaxies at large redshifts depends upon interpretation of their integrated spectra. Unfortunately, integrated light techniques have not yet matched the precision possible with detailed color-magnitude diagrams (CMD's), and a definitive connection between the two approaches has yet to be made. HST has the unique ability to bridge the gap between the integrated light and CMD methods of analyzing stellar populations. This permits, for the first time, direct comparison of the two techniques for important fiducial systems such as Local Group globular clusters and the bright cores of nearby galaxies. We propose to address theintegrated light side of this comparison by obtaining high signal-to- noise ultraviolet spectra with the FOS of selected globular clusters and galaxy nuclei and analyzing them in the context of a large existing set of supporting IUE and ground-based data which we have assembled. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 12.87 par: 0 10. Num targs pri: 4 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 4559c PI: David Burstein Proposal Title: UV SPECTRA OF GLOBULAR CLUSTERS AND GALAXY CORES - CYCLE 3 MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi David Burstein ARIZONA STATE UNIVERSITY USA Robert W. O'Connell UNIVERSITY OF VIRGINIA USA Chi-Chao Wu COMPUTER SCIENCES CORPORATION USA Jay A. Frogel OHIO STATE UNIVERSITY USA James A. Rose UNIVERSITY OF NORTH CAROLINA USA Marica Rieke STEWARD OBSERVATORY USA Michael J. Tripico UNIVERSITY OF MARYLAND USA ------------------------------------------------------------------------------------ 3. Description of proposed observations. The principal observing requirements for this program are: (a) accessibility to the 2200-3300A region and (b) a minimum S/N of 20 for spectral resolution elements of ~10A for wavelengths >2500A. All of the program objects are extended sources. Our requirements can only be met in reasonable integration times by using the FOS with gratings and the 1" circular aperture (as this is the FOS aperture with the best absolute calibration). Following the technique developed for our P2298 program, we will center on each object using FOS ACQ/PEAK-UP together with the G270H grating, to peak up on the center while also obtaining short integration spectra of the region around each central object. Three separate FOS spectra are needed for each centered object: a) The Blue Digicon (FOS/Blue) will be used to obtain a low S/N spectrum for 1150-1700A, using the G130H grating. (Note: The scattered light problem with the G160L grating precludes its use for this program.) These observations are essential to determine the contribution of the "UV-upturn" population's flux in the galaxy cores and stars hotter than 15000 K in the globulars, to remove their effects from the longer wavelength data. b) The Red Digicon (FOS/Red) will be used to obtain: (i) A high S/N, 8.0A resolution spectrum from 2200-3300A, using the G270H grating; and (ii) A high S/N, 10.0A resolution spectrum from 3250-4800A, using the G400H grating. We propose to use the G400H grating for three reasons: 1) It provides the overlap with ground-based data that is critical to zero point the HST spectra to ground-based spectra (2) it measures important features such as NH, CN and Ca II at the same spatial resolution as the UV data; (3) obtaining a spectrum at this wavelength adds very little additional time to our program; hence we get valuable additional data at a small cost. There is a 60A overlap between gratings G270H and G400H. There is a gap between G130H and G270H covering 1700-2200A, where no data will be obtained. IUE spectra indicate that the flux from our targets is least here, so no useful information will be missed. All S/N ratios are calculated per spectral resolution element. In addition to meeting our scientific criteria, the targets for this program were selected for expected UV brightness, relatively low background contamination and extinction, and, for the M33 globulars, for possible CMD determinations. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. a) High S/N observations at spectral resolutions of ~10A in the region 2200- 3300A are required. Only HST can provide data of the required quality on galaxy cores and globular clusters. The small aperture observations of the M33 globular clusters will maximize the signal of the clusters relative to the background light of the galaxy. This proposal is a continuation of the Cycle 1 proposal P2298, the FOS observations for which are yet to be obtained. Our proposal is related to a number of ongoing and proposed IUE and HST programs involving various combinations of the co-PI's of this proposal. Among our group, we have previous or ongoing IUE observations of: normal F-K main sequence stars; G-K giant stars; elliptical galaxies, M31 globular clusters (poor S/N) and Seyfert galaxies. Several of us are also involved in separate FOS and FOC Cycle 2 and Cycle 3 proposals, the goals of which are to examine other important aspects of the complex problem of stellar populations, and with UV imaging observations made with or proposed for the Astro-1 and Astro-2 missions. The combined ground-based data available to us from our own separate programs include integrated spectra for ~700 galaxies, including recent data on the disks of spiral galaxies; stellar spectra for ~1000 stars; and visible/IR spectra energy distributions for ~200 galaxies. We are in the final stages of assembling an ultraviolet stellar 'library' comprised of high S/N IUE low dispersion spectra of ~2000 stars, derived from merging information from ~10,000 IUE spectra. Some of the results of these ongoing studies are cited in the Scientific Justification section. b) We have estimated average fluxes centered at 5 wavelengths for each object, based in most cases on extrapolations from IUE data. V magnitudes with a 1" circular aperture are estimated from available photoelectric photometry. These data are listed at the end of this section. Effects of galactic extinction have been included in the flux calculations. If our spectra achieve the required S/N for these 5 wavelength regions, they will yield the desired S/N for the whole spectrum. The spectral resolutions used in the calculations of S/N are: 100A at 1500A, 8A at 2500A, 2800A and 3100A, and 10.0A at wavelengths 3500A and longer. About 10A spectral resolution is the maximum from which reliable UV absorption line indices can be determined. As FOS/Blue is much less sensitive than FOS/Red at all wavelengths >1600A, our strategy is to use FOS/Blue only for the G130H observations (we cannot use the G160L due to scattered light problems). FOS/Red will be used for the G270H and G400H observations. FOS ACQ/PEAK-UP will be used with the FOS/RD side and G270H to do a series of spatial scans to peak up on each object. The short integration spectra obtained during the peak-up procedure provide a rough estimate of the spectrum of the regions surrounding each object. Object log Continuum Flux (ergs/cm2/s/A) 1500A 2500A 2800A 3100A 3500A V mag G130H G270H G270H G270H G400H 1" circ M33 'b' -15.95 -16.00 - 16.00 -15.90 -15.75 17.3 M33 'd' -15.10 -15.45 -15.50 -15.55 -15.40 16.9 M32 nuc -15.75 -15.40 -15.05 -14.55 -14.40 15.1 M31 nuc -15.35 - 15.55 -15.30 -14.85 -14.70 13.9 ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. Since all of the objects in this program will have low UV flux levels, avoidance of additional sources of background, such as the Gegenshein, is desirable. Positions of the centers of galaxies and globular clusters in the UV may be different at a signifcant level (0.5'') from the apparent optical centers as observed from the ground. Hence, ACQ/PEAK-UP is needed to center on each object. Page 4 ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. The spectra will be reduced to absolute fluxes, the three spectral regions combined and reliable S/N estimates obtained. We will use HST and IDL software for this phase. The spectral line features of each spectrum will be inter- compared and measured in a consistent manner according to methods we have already developed using IUE observations of stars (Fanelli et al. 1990, 1991,1992). Corresponding visible and infrared spectral energy distributions of the same objects will be added, providing complete wavelength coverage from 1200A to 2.2 microns, with <10 ang. resolution out to 1 micron. Ground-based observations with 1"-2" spatial resolution are now commonplace. Observations at >4500A are little affected by atmospheric refraction. FOS spectra in the 3200-3800A region are absolutely essential to accurately tie together ground-based and HST spectral energy distributions. As part of the overall analysis, the spectral line indices of 700 stars measured by Burstein, Faber and collaborators, of 300 stars measured by Rose, and of 200 stars measured by O'Connell will be combined into a unified data base. The reprocessing of all stellar observations made by IUE of reasonable S/N (over 10,000 spectra for ~2000 stars) will be finished by the end of 1992 (DB, RWO, CCW, Ralph Bohlin and Linda Stryker). Both these IUE stellar 'libarary' spectra and the HST/FOS spectra will be analyzed in the manner of Fanelli et al. Over 40 UV absorption line indices and colors have been calibrated for stars in terms of temperature, metallicity and gravity. We find that, while overall line blanketing is very sensitive to all three parameters, the differential absorption line strengths are primarily sensitive to temperature. This fact will aid in the separation of the contribution of different kinds of stellar populations to the mid-UV spectrum of galaxies. The full UV-to-IR spectral energy distributions of the targets will then be analyzed in two independent ways: 1) With the optimizing spectral synthesis program of O'Connell; 2) Using the evolutionary modeling methods developed by Faber, Burstein and collaborators and by Rose, which give greater emphasis to the correlations among the absorption-line indices. A primary goal of the project is to compare the populations of the globular clusters, as inferred from these analyses, to the known CMD's obtained by other HST observers. It is obviously essential that the deduced ages and metallicities of these two different approaches agree. Any discrepencies will require careful study. Such CMDs will be obtained with HST with COSTAR, and may also be obtained in the near future from seeing-compensated ground-based observations. UV integated spectroscopy of these clusters can only be obtained with HST. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. See response to Item 5. Page 5 ------------------------------------------------------------------------------------ 9. Description of previous HST work. a) P1170: UV SPECTROSCOPY OF LOW-REDSHIFT ACTIVE GALAXIES (P.I. BOGGESS; including Wu). This GTO program is not related to present proposal. P2298: STELLAR POPULATIONS OF GLOBULAR CLUSTERS AND GALAXIES (P.I. D. BURSTEIN). Is directly related to the present proposal. P2389: SUPER STAR CLUSTERS IN NEARBY GALAXIES (P.I. R.W. O'CONNELL) This GO program is not related to the present proposal. P2416: IMAGERY AND SPECTROSCOPY OF SUPER-METAL-POOR GALAXIES (P.I. R. DUFOUR; including Wu). This GO program is marginally related to present proposal. P2434: A STUDY OF THE CHEMICAL COMPOSITION AND VELOCITY STRUCTURE OF THE YOUNG SUPERNOVA REMANNT AD 1006 (P.I. C.-C. WU). This GO program is not related to the present proposal. P2607: BLACK HOLES IN A COMPLETE SAMPLE OF VIRGO ELLIPTICAL GALAXIES (P.I. W. JAFFE; including O'Connell). This GO program is related to the present program in terms of the study of integrated stellar populations. P2719: PAGB STARS IN ELLIPTICAL AND BULGE DOMINATED NEARBY GALAXIES (P.I. F. BERTOLA; including Burstein). This GO program is directly related to the present proposal. P3621: THE PARTIALLY-BURNED EJECTA OF SNR 1006 (P.I. C.-C. WU). This GO program is not related to the present proposal. P3728: IMAGING THE HOT STELLAR CONTENT OF EARLY-TYPE GALAXIES (P.I. F. Bertola; DB also). This GO program is directly related to the present proposal in terms of integrated stellar population studies. b) P2298: WFC images taken of all four M31 globular clusters; offset star positions measured. Astrometric positions for star/cluster positions obtained Aug 1992. FOS observations to be obtained Jan 1993. F336 WFC images of one cluster (K58) shows that it has a much more irregular appearance in the UV than in the optical, and changed where we would point the FOS aperture. P2719: FOC/48 F150W+F130LP images obtained of the centers of M31, M32 and NGC 205. Individual hot stars seen in all three galaxies; they are main sequence OB stars in NGC 205, likely PAGB stars in M31 and M32. M31 has a bar-like structure near its center, and the brightest part (nucleus?) is offset by ~1" from the center of the isophotes. PAGB contribution to 'UVX' component depends on response function of filters+FOC+OTA, which is still being determined. c) Bertola, F., Bressan, A., Burstein, D., Buson, L.M., Chiosi, C. and di Serego Alighieri, S. 1992, 'Far-UV Imaging of Elliptical and Bulge-Dominated Nearby Galaxies', to appear in the proceedings of Baia Chia, Sardinia conference ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). The majority of support from our home institutions comes in the form of computer facilities. All of us have workstations of various kinds that require maintenance. Part of this maintenance is provided by our own institutions. These workstations run a variety of software, including STSDAS, IDL and IRAF, as well as data reduction programs tailored to our own needs. Graduate student salaries are provided, in part, by teaching assistantships at many of our institutions that are universities. The data base of UV stellar spectra, to contain several thousand stars by mid-1992, is maintained on the UVa SUN/VAX cluster by O'Connell and his graduate students, and is supported by an extensive set of IDL and other spectral analysis software. This will be extensively used in the interpretation of our HST spectra. ------------------------------------------------------------------------------------ 11. Address Information Name: DAVID BURSTEIN Category: PI Institution: Arizona State University Address: DEPT PHYSICS AND ASTRONOMY ARIZONA STATE UNIVERSITY City: TEMPE State: AZ Zip Code: 852871504 Country: USA Telephone: 602-965-3561 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4559c [ 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 M31-GAL-NUC E,301 RA = 0H 42M 44.4S +/- 0.07S, 2000 V = -300 BKG 1 V = 13.9 +/- 0.3 M31-NUCLEUS- DEC = +41D 16' 08.0" +/- EXT 2 B-V = 1.02 +/- 0.05, E(B-V) = 0.08 ONLY 1.0" 3 F-CONT(1500) = 4.5 +/- 0.3 E-16 4 F-CONT(2500) = 2.8 +/- 0.3 E-16 5 F-CONT(2800) = 5.0 +/- 0.3 E-16 6 F-CONT(3100) = 1.4 +/- 0.2 E-15 7 F-CONT(3500) = 2.0 +/- 0.2 E-15 Comments: V MAG ESTIMATED IN 1" CIRCULAR APER S/N CALCULATIONS FOR FLUXNUM 3-7 ARE FOR SPECTRAL RESOLUTIONS OF 3 - 100A, 4 - 4.7A, 5 - 4.7A 6 - 4.7A, 7 - 6.85A POSITION FROM EARLIER HST OBS ------------------------------------------------------------------------------------------------------------------------------------ 2 M32-GAL-NUC E,303 RA = 0H 42M 41.9S +/- 0.07S, 2000 V = -200 BKG 1 V = 15.1 +/- 0.3 M32-NUCLEUS- DEC = +40D 51' 55.0" +/- EXT 2 B-V = 0.9 +/- 0.05, E(B-V) = 0.08 ONLY 1.0" 3 F-CONT(1500) = 1.8 +/- 0.3 E-16 4 F-CONT(2500) = 4.0 +/- 0.4 E-16 5 F-CONT(2800) = 8.9 +/- 0.2 E-16 6 F-CONT(3100) = 2.8 +/- 0.2 E-15 7 F-CONT(3500) = 4.0 +/- 0.2 E-15 Comments: V MAG ESTIMATED IN 1" CIRCULAR APER S/N CALCULATIONS FOR FLUXNUM 3-7 ARE FOR SPECTRAL RESOLUTIONS OF 3 - 100A, 4 - 4.7A, 5 - 4.7A 6 - 4.7A, 7 - 6.85A POSITION FROM EARLIER HST OBS ------------------------------------------------------------------------------------------------------------------------------------ 3 M33-B-EXT- D,201 RA = 1H 34M 43.741S +/- 2000 V = -100 BKG 1 V = 17.3 +/- 0.5 CLUSTER-M33 0.04S, EXT 2 B-V = 0.4 +/- 0.05, E(B-V) = 0.05 DEC = +30D 47' 38.00" +/- 3 F-CONT(1500) = 1.1 +/- 0.5 E-16 0.5" 4 F-CONT(2500) = 1.0 +/- 0.5 E-16 5 F-CONT(2800) = 1.0 +/- 0.5 E-16 6 F-CONT(3100) = 1.3 +/- 0.5 E-16 7 F-CONT(3500) = 1.8 +/- 0.5 E-16 Comments: V MAG ESTIMATED IN 1" CIRCULAR APER INDIVIDUAL STARS IN CLUSTER HAVE MAGS 4-7 MAG FAINTER S/N CALCULATIONS FOR FLUXNUM 3 -7 ARE FOR SPECTRAL RESOLUTIONS OF 3 - 100A, 4 - 4.7A, 5 - 4.7A 6 - 4.7A, 7 - 6.85A POSITION FROM GASP ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4559c [ 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| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 4 M33-D-EXT- D,201 RA = 1H 33M 55.12S +/- 2000 V = -200 BKG 1 V = 16.9 +/- 0.5 CLUSTER-M33 0.04S, EXT 2 B-V = 0.1 +/- 0.05, E(B-V) = 0.05 DEC = +30D 47' 58.08" +/- 3 F-CONT(1500) = 7.9 +/- 0.5 E-16 0.5" 4 F-CONT(2500) = 3.5 +/- 0.4 E-16 5 F-CONT(2800) = 2.8 +/- 0.5 E-16 6 F-CONT(3100) = 2.8 +/- 0.5 E-16 7 F-CONT(3500) = 4.0 +/- 0.5 E-16 Comments: V MAG ESTIMATED IN 1" CIRCULAR APER INDIVIDUAL STARS IN CLUSTER HAVE MAGS 4-7 MAG FAINTER S/N CALCULATIONS FOR FLUXNUM 3 -7 ARE FOR SPECTRAL RESOLUTIONS OF 3 - 100A, 4 - 4.7A, 5 - 4.7A 6 - 4.7A, 7 - 6.85A POSITION FROM GASP ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4559c [ 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 M31-GAL-NUC FOS/RD ACQ/ 4.3 G270H 2700 TYPE=UP 1 14S 5 1 ONBOARD ACQ FOR PEAK 1.3-1.5 SPATIAL SCAN SEQ 1.0-1.5 NO GAP CYCLE 3 / 1-4.5 Comments: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= G270H; ------------------------------------------------------------------------------------------------------------------------------------ 1.1 M31-GAL-NUC FOS/RD ACQ/ 1.0 G270H 2700 TYPE=UP 1 20S 5 1 ONBOARD ACQ FOR PEAK 1.3-1.5 SPATIAL SCAN Comments: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ 1.2 M31-GAL-NUC FOS/RD ACQ/ 0.5 G270H 2700 TYPE=UP 1 30S 5 1 ONBOARD ACQ FOR PEAK SCAN-STEP=0.35 1.3-1.5 SEARCH-SIZE=3 Comments: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ 1.3 M31-GAL-NUC FOS/RD ACCUM 1.0 G270H 2700 1 3650S 39 5 1 Comments: S_TO_N IS CALCULATED FOR 4.7A RESOLUTION AT 2800A ------------------------------------------------------------------------------------------------------------------------------------ 1.4 M31-GAL-NUC FOS/RD ACCUM 1.0 G400H 4000 1 500S 40 7 1 Comments: S_TO_N IS CALCULATED FOR 6.85A RESOLUTION AT 3500A ------------------------------------------------------------------------------------------------------------------------------------ 1.5 M31-GAL-NUC FOS/BL ACCUM 1.0 G130H 1300 1 1750S 13 3 1 Comments: S_TO_N IS CALCULATED FOR 100A RESOLUTION AT 1500A ------------------------------------------------------------------------------------------------------------------------------------ 2 M32-GAL-NUC FOS/RD ACQ/ 4.3 G270H 2700 TYPE=UP 1 15S 5 1 ONBOARD ACQ FOR PEAK 2.3-2.5 SPATIAL SCAN SEQ 2.0-2.5 NO GAP Comments: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= G270H; ------------------------------------------------------------------------------------------------------------------------------------ 2.1 M32-GAL-NUC FOS/RD ACQ/ 1.0 G270H 2700 TYPE=UP 1 20S 5 1 ONBOARD ACQ FOR PEAK 2.3-2.5 SPATIAL SCAN Comments: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ 2.2 M32-GAL-NUC FOS/RD ACQ/ 0.5 G270H 2700 TYPE=UP 1 30S 5 1 ONBOARD ACQ FOR PEAK SCAN-STEP=0.35 2.3-2.5 SEARCH-SIZE=3 Comments: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4559c [ 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 ------------------------------------------------------------------------------------------------------------------------------------ 2.3 M32-GAL-NUC FOS/RD ACCUM 1.0 G270H 2700 1 2100S 40 5 1 Comments: S_TO_N IS CALCULATED FOR 4.7A RESOLUTION AT 2800A ------------------------------------------------------------------------------------------------------------------------------------ 2.4 M32-GAL-NUC FOS/RD ACCUM 1.0 G400H 4000 1 384S 50 7 1 Comments: S_TO_N IS CALCULATED FOR 6.85A RESOLUTION AT 3500A ------------------------------------------------------------------------------------------------------------------------------------ 2.5 M32-GAL-NUC FOS/BL ACCUM 1.0 G130H 1300 1 2200S 6 3 1 Comments: S_TO_N IS CALCULATED FOR 100A RESOLUTION AT 1500A ------------------------------------------------------------------------------------------------------------------------------------ 3 M33-B-EXT- FOS/RD ACQ/ 4.3 G270H 2700 TYPE=UP 1 74S 5 1 ONBOARD ACQ FOR CLUSTER-M33 PEAK 3.3-3.5 SPATIAL SCAN SEQ 3.0-3.5 NO GAP Comments: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= G270H; ------------------------------------------------------------------------------------------------------------------------------------ 3.1 M33-B-EXT- FOS/RD ACQ/ 1.0 G270H 2700 TYPE=UP 1 92S 5 1 ONBOARD ACQ FOR CLUSTER-M33 PEAK 3.3-3.5 SPATIAL SCAN Comments: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ 3.2 M33-B-EXT- FOS/RD ACQ/ 0.5 G270H 2700 TYPE=UP 1 141S 5 1 ONBOARD ACQ FOR CLUSTER-M33 PEAK SCAN-STEP=0.35 3.3-3.5 SEARCH-SIZE=3 Comments: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ 3.3 M33-B-EXT- FOS/RD ACCUM 1.0 G270H 2700 1 3400S 15 5 1 CLUSTER-M33 Comments: S_TO_N IS CALCULATED FOR 4.7A RESOLUTION AT 2800A ------------------------------------------------------------------------------------------------------------------------------------ 3.4 M33-B-EXT- FOS/RD ACCUM 1.0 G400H 4000 1 1500S 20 7 1 CLUSTER-M33 Comments: S_TO_N IS CALCULATED FOR 6.85A RESOLUTION AT 3500A ------------------------------------------------------------------------------------------------------------------------------------ 3.5 M33-B-EXT- FOS/BL ACCUM 1.0 G130H 1300 1 1900S 5 3 1 CLUSTER-M33 Comments: S_TO_N IS CALCULATED FOR 100A RESOLUTION AT 1500A ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4559c [ 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 M33-D-EXT- FOS/RD ACQ/ 4.3 G270H 2700 TYPE=UP 1 27S 5 1 ONBOARD ACQ FOR CLUSTER-M33 PEAK 4.3-4.5 SPATIAL SCAN SEQ 4.0-4.5 NO GAP Comments: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= G270H; ------------------------------------------------------------------------------------------------------------------------------------ 4.1 M33-D-EXT- FOS/RD ACQ/ 1.0 G270H 2700 TYPE=UP 1 34S 5 1 ONBOARD ACQ FOR CLUSTER-M33 PEAK 4.3-4.5 SPATIAL SCAN Comments: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ 4.2 M33-D-EXT- FOS/RD ACQ/ 0.5 G270H 2700 TYPE=UP 1 52S 5 1 ONBOARD ACQ FOR CLUSTER-M33 PEAK SCAN-STEP=0.35 4.3-4.5 SEARCH-SIZE=3 Comments: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ------------------------------------------------------------------------------------------------------------------------------------ 4.3 M33-D-EXT- FOS/RD ACCUM 1.0 G270H 2700 1 1575S 20 5 1 CLUSTER-M33 Comments: S_TO_N IS CALCULATED FOR 4.7A RESOLUTION AT 2800A ------------------------------------------------------------------------------------------------------------------------------------ 4.4 M33-D-EXT- FOS/RD ACCUM 1.0 G400H 4000 1 650S 20 7 1 CLUSTER-M33 Comments: S_TO_N IS CALCULATED FOR 6.85A RESOLUTION AT 3500A ------------------------------------------------------------------------------------------------------------------------------------ 4.5 M33-D-EXT- FOS/BL ACCUM 1.0 G130H 1300 1 500S 7 3 1 CLUSTER-M33 Comments: S_TO_N IS CALCULATED FOR 100A RESOLUTION AT 1500A ------------------------------------------------------------------------------------------------------------------------------------ Scan Paramters Form Proposal ID: 4559c [ 11] ------------------------------------------------------------------------------------------------------------------------------------ Data ID: 1 Exposure Logsheet lines: 1.0,2.0,3.0,4.0 FGS Scan: DWELL Dwell Only: dwell points/line: 3 Seconds per dwell: 1.00 Scan width (arc-secs): 0.0000 Scan length (arc-secs): 2.8000 Angle between sides (degrees) 90.00 Number of lines: 1 Scan rate (arc-sec/sec): 0.0000 PA of first scan line (degrees) 0.000 Scan frame (CEL or S/C): S/C Length Offset (arc-sec): 1.4000 Width Offset (arc-sec): 0.0000 ------------------------------------------------------------------------------------------------------------------------------------ Data ID: 2 Exposure Logsheet lines: 1.1,2.1,3.1,4.1 FGS Scan: DWELL Dwell Only: dwell points/line: 6 Seconds per dwell: 1.00 Scan width (arc-secs): 0.7000 Scan length (arc-secs): 3.5000 Angle between sides (degrees) 90.00 Number of lines: 2 Scan rate (arc-sec/sec): 0.0000 PA of first scan line (degrees) 90.000 Scan frame (CEL or S/C): S/C Length Offset (arc-sec): 1.7500 Width Offset (arc-sec): 0.3500 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 4559c [ 12] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/RD FOS/BL ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/PEAK ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters TYPE=UP SCAN-STEP=0.35 SEARCH-SIZE=3 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 12.87 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category GALAXIES & CLUSTERS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category STELLAR POPULATIONS ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 1.3-1.5; SPATIAL SCAN; SEQ 1.0-1.5 NO GAP; CYCLE 3 / 1-4.5; ONBOARD ACQ FOR 2.3-2.5; SEQ 2.0-2.5 NO GAP; ONBOARD ACQ FOR 3.3-3.5; SEQ 3.0-3.5 NO GAP; ONBOARD ACQ FOR 4.3-4.5; SEQ 4.0-4.5 NO GAP; ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements G270H G400H G130H ------------------------------------------------------------------------------------------------------------------------------------ Target Names M31-GAL-NUC M31-NUCLEUS-ONLY M32-GAL-NUC M32-NUCLEUS-ONLY M33-B-EXT-CLUSTER-M33 M33-D-EXT-CLUSTER-M33 ------------------------------------------------------------------------------------------------------------------------------------