! File: 4559C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:17:39:46 coverpage: title_1: UV SPECTRA OF GLOBULAR CLUSTERS AND GALAXY CORES - CYCLE 3 MEDIUM sci_cat: GALAXIES & CLUSTERS sci_subcat: STELLAR POPULATIONS proposal_for: GO pi_fname: DAVID pi_lname: BURSTEIN pi_inst: ARIZONA STATE UNIVERSITY pi_country: USA hours_pri: 12.87 num_pri: 4 fos: Y funds_length: 12 off_fname: CHAFFINS off_mi: L off_lname: GARY off_title: DIR OSPA off_inst: 1220 off_addr_1: OFFICE OF SPONSORED PROGRAMS ADMINISTRATION off_addr_2: ARIZONA STATE UNIVERSITY off_city: TEMPE off_state: AZ off_zip: 852871603 off_country: USA off_phone: 602-965-2170 ! end of coverpage abstract: line_1: An understanding of stellar populations in galaxies at large line_2: redshifts depends upon interpretation of their integrated spectra. line_3: Unfortunately, integrated light techniques have not yet matched the line_4: precision possible with detailed color-magnitude diagrams (CMD's), line_5: and a definitive connection between the two approaches has yet to line_6: be made. HST has the unique ability to bridge the gap between the line_7: integrated light and CMD methods of analyzing stellar populations. line_8: This permits, for the first time, direct comparison of the two line_9: techniques for important fiducial systems such as Local Group line_10: globular clusters and the bright cores of nearby galaxies. We line_11: propose to address theintegrated light side of this comparison line_12: by obtaining high signal-to-noise ultraviolet spectra with the FOS line_13: of selected globular clusters and galaxy nuclei and analyzing them line_14: in the context of a large existing set of supporting IUE and line_15: ground-based data which we have assembled. ! ! end of abstract general_form_proposers: lname: BURSTEIN fname: DAVID title: PI inst: ARIZONA STATE UNIVERSITY country: USA ! lname: O'CONNELL fname: ROBERT mi: W. inst: UNIVERSITY OF VIRGINIA country: USA esa: N ! lname: WU fname: CHI-CHAO inst: COMPUTER SCIENCES CORPORATION country: USA esa: N ! lname: FROGEL fname: JAY mi: A. inst: OHIO STATE UNIVERSITY country: USA esa: N ! lname: ROSE fname: JAMES mi: A. inst: UNIVERSITY OF NORTH CAROLINA country: USA esa: N ! lname: RIEKE fname: MARICA inst: STEWARD OBSERVATORY country: USA esa: N ! lname: TRIPICO fname: MICHAEL mi: J. inst: UNIVERSITY OF MARYLAND country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The principal observing requirements for this program are: line_2: (a) accessibility to the 2200-3300A region and (b) a minimum S/N of line_3: 20 for spectral resolution elements of ~10A for wavelengths >2500A. line_4: All of the program objects are extended sources. Our requirements line_5: can only be met in reasonable integration times by using the FOS line_6: with gratings and the 1" circular aperture (as this is the FOS line_7: aperture with the best absolute calibration). Following the line_8: technique developed for our P2298 program, we will center on line_9: each object using FOS ACQ/PEAK-UP together with the G270H grating, line_10: to peak up on the center while also obtaining short integration line_11: spectra of the region around each central object. line_12: Three separate FOS spectra are needed for each centered object: line_13: a) The Blue Digicon (FOS/Blue) will be used to obtain a low S/N line_14: spectrum for 1150-1700A, using the G130H grating. (Note: The line_15: scattered light problem with the G160L grating precludes its use line_16: for this program.) These observations are essential to determine line_17: the contribution of the "UV-upturn" population's flux in the line_18: galaxy cores and stars hotter than 15000 K in the globulars, to line_19: remove their effects from the longer wavelength data. line_20: b) The Red Digicon (FOS/Red) will be used to obtain: (i) A high line_21: S/N, 8.0A resolution spectrum from 2200-3300A, using the G270H line_22: grating; and (ii) A high S/N, 10.0A resolution spectrum from line_23: 3250-4800A, using the G400H grating. We propose to use the G400H ! question: 3 section: 2 line_1: grating for three reasons: 1) It provides the overlap with line_2: ground-based data that is critical to zero point the HST spectra to line_3: ground-based spectra (2) it measures important features such as NH, line_4: CN and Ca II at the same spatial resolution as the UV data; line_5: (3) obtaining a spectrum at this wavelength adds very little line_6: additional time to our program; hence we get valuable additional line_7: data at a small cost. line_8: There is a 60A overlap between gratings G270H and G400H. line_9: There is a gap between G130H and G270H covering 1700-2200A, where line_10: no data will be obtained. IUE spectra indicate that the flux from line_11: our targets is least here, so no useful information will be missed. line_12: All S/N ratios are calculated per spectral resolution element. In line_13: addition to meeting our scientific criteria, the targets for this line_14: program were selected for expected UV brightness, relatively low line_15: background contamination and extinction, and, for the M33 line_16: globulars, for possible CMD determinations. ! question: 4 section: 1 line_1: a) High S/N observations at spectral resolutions of ~10A in the line_2: region 2200-3300A are required. Only HST can provide data of the line_3: required quality on galaxy cores and globular clusters. The small line_4: aperture observations of the M33 globular clusters will maximize line_5: the signal of the clusters relative to the background light of the line_6: galaxy. line_7: This proposal is a continuation of the Cycle 1 proposal line_8: P2298, the FOS observations for which are yet to be obtained. Our line_9: proposal is related to a number of ongoing and proposed IUE and HST line_10: programs involving various combinations of the co-PI's of this line_11: proposal. Among our group, we have previous or ongoing IUE line_12: observations of: normal F-K main sequence stars; G-K giant stars; line_13: elliptical galaxies, M31 globular clusters (poor S/N) and Seyfert line_14: galaxies. Several of us are also involved in separate FOS and FOC line_15: Cycle 2 and Cycle 3 proposals, the goals of which are to examine line_16: other important aspects of the complex problem of stellar line_17: populations, and with UV imaging observations made with or line_18: proposed for the Astro-1 and Astro-2 missions. line_19: The combined ground-based data available to us from our own line_20: separate programs include integrated spectra for ~700 galaxies, line_21: including recent data on the disks of spiral galaxies; stellar line_22: spectra for ~1000 stars; and visible/IR spectra energy line_23: distributions for ~200 galaxies. We are in the final stages of ! question: 4 section: 2 line_1: assembling an ultraviolet stellar 'library' comprised of high S/N line_2: IUE low dispersion spectra of ~2000 stars, derived from merging line_3: information from ~10,000 IUE spectra. Some of the results of these line_4: ongoing studies are cited in the Scientific Justification section. line_6: b) We have estimated average fluxes centered at 5 wavelengths for line_7: each object, based in most cases on extrapolations from IUE data. line_8: V magnitudes with a 1" circular aperture are estimated from line_9: available photoelectric photometry. These data are listed at the line_10: end of this section. Effects of galactic extinction have been line_11: included in the flux calculations. line_12: If our spectra achieve the required S/N for these 5 wavelength line_13: regions, they will yield the desired S/N for the whole spectrum. line_14: The spectral resolutions used in the calculations of S/N are: 100A line_15: at 1500A, 8A at 2500A, 2800A and 3100A, and 10.0A at wavelengths line_16: 3500A and longer. About 10A spectral resolution is the maximum line_17: from which reliable UV absorption line indices can be determined. line_18: As FOS/Blue is much less sensitive than FOS/Red at all wavelengths line_19: >1600A, our strategy is to use FOS/Blue only for the G130H line_20: observations (we cannot use the G160L due to scattered light line_21: problems). FOS/Red will be used for the G270H and G400H line_22: observations. ! question: 4 section: 3 line_1: FOS ACQ/PEAK-UP will be used with the FOS/RD side and G270H line_2: to do a series of spatial scans to peak up on each object. The line_3: short integration spectra obtained during the peak-up procedure line_4: provide a rough estimate of the spectrum of the regions surrounding line_5: each object. line_7: Object log Continuum Flux (ergs/cm2/s/A) line_8: 1500A 2500A 2800A 3100A 3500A V mag line_9: G130H G270H G270H G270H G400H 1" circ line_11: M33 'b' -15.95 -16.00 -16.00 -15.90 -15.75 17.3 line_12: M33 'd' -15.10 -15.45 -15.50 -15.55 -15.40 16.9 line_13: M32 nuc -15.75 -15.40 -15.05 -14.55 -14.40 15.1 line_14: M31 nuc -15.35 -15.55 -15.30 -14.85 -14.70 13.9 ! question: 5 section: 1 line_1: Since all of the objects in this program will have low UV line_2: flux levels, avoidance of additional sources of background, line_3: such as the Gegenshein, is desirable. Positions of the centers line_4: of galaxies and globular clusters in the UV may be different at line_5: a signifcant level (0.5'') from the apparent optical centers as line_6: observed from the ground. Hence, ACQ/PEAK-UP is needed to center line_7: on each object. ! question: 7 section: 1 line_1: The spectra will be reduced to absolute fluxes, the three spectral line_2: regions combined and reliable S/N estimates obtained. We will use line_3: HST and IDL software for this phase. The spectral line features line_4: of each spectrum will be inter-compared and measured in a line_5: consistent manner according to methods we have already developed line_6: using IUE observations of stars (Fanelli et al. 1990, 1991,1992). line_7: Corresponding visible and infrared spectral energy line_8: distributions of the same objects will be added, providing line_9: complete wavelength coverage from 1200A to 2.2 microns, with <10 line_10: ang. resolution out to 1 micron. Ground-based observations with line_11: 1"-2" spatial resolution are now commonplace. Observations at line_12: >4500A are little affected by atmospheric refraction. FOS line_13: spectra in the 3200-3800A region are absolutely essential to line_14: accurately tie together ground-based and HST spectral energy line_15: distributions. line_16: As part of the overall analysis, the spectral line indices of line_17: 700 stars measured by Burstein, Faber and collaborators, of 300 line_18: stars measured by Rose, and of 200 stars measured by O'Connell will line_19: be combined into a unified data base. The reprocessing of all line_20: stellar observations made by IUE of reasonable S/N (over 10,000 line_21: spectra for ~2000 stars) will be finished by the end of 1992 (DB, line_22: RWO, CCW, Ralph Bohlin and Linda Stryker). line_23: Both these IUE stellar 'libarary' spectra and the HST/FOS ! question: 7 section: 2 line_1: spectra will be analyzed in the manner of Fanelli et al. Over 40 line_2: UV absorption line indices and colors have been calibrated for line_3: stars in terms of temperature, metallicity and gravity. We find line_4: that, while overall line blanketing is very sensitive to all three line_5: parameters, the differential absorption line strengths are line_6: primarily sensitive to temperature. This fact will aid in the line_7: separation of the contribution of different kinds of stellar line_8: populations to the mid-UV spectrum of galaxies. line_9: The full UV-to-IR spectral energy distributions of the targets line_10: will then be analyzed in two independent ways: 1) With the line_11: optimizing spectral synthesis program of O'Connell; 2) Using the line_12: evolutionary modeling methods developed by Faber, Burstein and line_13: collaborators and by Rose, which give greater emphasis to the line_14: correlations among the absorption-line indices. A primary goal of line_15: the project is to compare the populations of the globular clusters, line_16: as inferred from these analyses, to the known CMD's obtained by line_17: other HST observers. It is obviously essential that the deduced line_18: ages and metallicities of these two different approaches agree. line_19: Any discrepencies will require careful study. Such CMDs will be line_20: obtained with HST with COSTAR, and may also be obtained in the line_21: near future from seeing-compensated ground-based observations. UV line_22: integated spectroscopy of these clusters can only be obtained with line_23: HST. ! question: 8 section: 1 line_1: See response to Item 5. ! question: 9 section: 1 line_1: a) P1170: UV SPECTROSCOPY OF LOW-REDSHIFT ACTIVE GALAXIES (P.I. line_2: BOGGESS; including Wu). This GTO program is not related to line_3: present proposal. line_4: P2298: STELLAR POPULATIONS OF GLOBULAR CLUSTERS AND GALAXIES line_5: (P.I. D. BURSTEIN). Is directly related to the present proposal. line_6: P2389: SUPER STAR CLUSTERS IN NEARBY GALAXIES (P.I. R.W. O'CONNELL) line_7: This GO program is not related to the present proposal. line_8: P2416: IMAGERY AND SPECTROSCOPY OF SUPER-METAL-POOR GALAXIES line_9: (P.I. R. DUFOUR; including Wu). This GO program is marginally line_11: related to present proposal. line_12: P2434: A STUDY OF THE CHEMICAL COMPOSITION AND VELOCITY STRUCTURE line_13: OF THE YOUNG SUPERNOVA REMANNT AD 1006 (P.I. C.-C. WU). This GO line_14: program is not related to the present proposal. line_15: P2607: BLACK HOLES IN A COMPLETE SAMPLE OF VIRGO ELLIPTICAL line_16: GALAXIES (P.I. W. JAFFE; including O'Connell). This GO program line_17: is related to the present program in terms of the study of line_18: integrated stellar populations. line_19: P2719: PAGB STARS IN ELLIPTICAL AND BULGE DOMINATED NEARBY GALAXIES line_20: (P.I. F. BERTOLA; including Burstein). This GO program is directly line_21: related to the present proposal. line_22: P3621: THE PARTIALLY-BURNED EJECTA OF SNR 1006 (P.I. C.-C. WU). line_23: This GO program is not related to the present proposal. ! question: 9 section: 2 line_1: P3728: IMAGING THE HOT STELLAR CONTENT OF EARLY-TYPE GALAXIES line_2: (P.I. F. Bertola; DB also). This GO program is directly related line_3: to the present proposal in terms of integrated stellar population line_4: studies. line_6: b) P2298: WFC images taken of all four M31 globular clusters; line_7: offset star positions measured. Astrometric positions for line_8: star/cluster positions obtained Aug 1992. FOS observations to be line_9: obtained Jan 1993. F336 WFC images of one cluster (K58) shows that line_10: it has a much more irregular appearance in the UV than in the line_11: optical, and changed where we would point the FOS aperture. line_12: P2719: FOC/48 F150W+F130LP images obtained of the centers of M31, line_13: M32 and NGC 205. Individual hot stars seen in all three galaxies; line_14: they are main sequence OB stars in NGC 205, likely PAGB stars in line_15: M31 and M32. M31 has a bar-like structure near its center, and line_16: the brightest part (nucleus?) is offset by ~1" from the center of line_17: the isophotes. PAGB contribution to 'UVX' component depends on line_18: response function of filters+FOC+OTA, which is still being line_19: determined. line_20: c) Bertola, F., Bressan, A., Burstein, D., Buson, L.M., line_21: Chiosi, C. and di Serego Alighieri, S. 1992, 'Far-UV Imaging of line_22: Elliptical and Bulge-Dominated Nearby Galaxies', to appear in the line_23: proceedings of Baia Chia, Sardinia conference ! question: 10 section: 1 line_1: The majority of support from our home institutions comes in the line_2: form of computer facilities. All of us have workstations of line_3: various kinds that require maintenance. Part of this maintenance line_4: is provided by our own institutions. These workstations run a line_5: variety of software, including STSDAS, IDL and IRAF, as well as line_6: data reduction programs tailored to our own needs. line_7: Graduate student salaries are provided, in part, by teaching line_8: assistantships at many of our institutions that are universities. line_9: The data base of UV stellar spectra, to contain several thousand line_10: stars by mid-1992, is maintained on the UVa SUN/VAX cluster by line_11: O'Connell and his graduate students, and is supported by an line_12: extensive set of IDL and other spectral analysis software. This line_13: will be extensively used in the interpretation of our HST spectra. ! !end of general form text general_form_address: lname: BURSTEIN fname: DAVID category: PI inst: Arizona State University addr_1: DEPT PHYSICS AND ASTRONOMY addr_2: ARIZONA STATE UNIVERSITY city: TEMPE state: AZ zip: 852871504 country: USA phone: 602-965-3561 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: M31-GAL-NUC name_2: M31-NUCLEUS-ONLY descr_1: E,301 pos_1: RA = 0H 42M 44.4S +/- 0.07S, pos_2: DEC = +41D 16' 08.0" +/- 1.0" equinox: 2000 rv_or_z: V = -300 acqpr_1: BKG acqpr_2: EXT comment_1: V MAG ESTIMATED IN 1" CIRCULAR APER comment_2: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_3: ARE FOR SPECTRAL RESOLUTIONS OF comment_4: 3 - 100A, 4 - 4.7A, 5 - 4.7A comment_5: 6 - 4.7A, 7 - 6.85A comment_6: POSITION FROM EARLIER HST OBS fluxnum_1: 1 fluxval_1: V = 13.9 +/- 0.3 fluxnum_2: 2 fluxval_2: B-V = 1.02 +/- 0.05, E(B-V) = 0.08 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 4.5 +/- 0.3 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 2.8 +/- 0.3 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 5.0 +/- 0.3 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 1.4 +/- 0.2 E-15 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 2.0 +/- 0.2 E-15 ! targnum: 2 name_1: M32-GAL-NUC name_2: M32-NUCLEUS-ONLY descr_1: E,303 pos_1: RA = 0H 42M 41.9S +/- 0.07S, pos_2: DEC = +40D 51' 55.0" +/- 1.0" equinox: 2000 rv_or_z: V = -200 acqpr_1: BKG acqpr_2: EXT comment_1: V MAG ESTIMATED IN 1" CIRCULAR APER comment_2: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_3: ARE FOR SPECTRAL RESOLUTIONS OF comment_4: 3 - 100A, 4 - 4.7A, 5 - 4.7A comment_5: 6 - 4.7A, 7 - 6.85A comment_6: POSITION FROM EARLIER HST OBS fluxnum_1: 1 fluxval_1: V = 15.1 +/- 0.3 fluxnum_2: 2 fluxval_2: B-V = 0.9 +/- 0.05, E(B-V) = 0.08 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 1.8 +/- 0.3 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 4.0 +/- 0.4 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 8.9 +/- 0.2 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 2.8 +/- 0.2 E-15 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 4.0 +/- 0.2 E-15 ! targnum: 3 name_1: M33-B-EXT-CLUSTER-M33 descr_1: D,201 pos_1: RA = 1H 34M 43.741S +/- 0.04S, pos_2: DEC = +30D 47' 38.00" +/- 0.5" equinox: 2000 rv_or_z: V = -100 acqpr_1: BKG acqpr_2: EXT comment_1: V MAG ESTIMATED IN 1" CIRCULAR APER comment_2: INDIVIDUAL STARS IN CLUSTER HAVE comment_3: MAGS 4-7 MAG FAINTER comment_4: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_5: ARE FOR SPECTRAL RESOLUTIONS OF comment_6: 3 - 100A, 4 - 4.7A, 5 - 4.7A comment_7: 6 - 4.7A, 7 - 6.85A comment_8: POSITION FROM GASP fluxnum_1: 1 fluxval_1: V = 17.3 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.4 +/- 0.05, E(B-V) = 0.05 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 1.1 +/- 0.5 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 1.0 +/- 0.5 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 1.0 +/- 0.5 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 1.3 +/- 0.5 E-16 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 1.8 +/- 0.5 E-16 ! targnum: 4 name_1: M33-D-EXT-CLUSTER-M33 descr_1: D,201 pos_1: RA = 1H 33M 55.12S +/- 0.04S, pos_2: DEC = +30D 47' 58.08" +/- 0.5" equinox: 2000 rv_or_z: V = -200 acqpr_1: BKG acqpr_2: EXT comment_1: V MAG ESTIMATED IN 1" CIRCULAR APER comment_2: INDIVIDUAL STARS IN CLUSTER HAVE comment_3: MAGS 4-7 MAG FAINTER comment_4: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_5: ARE FOR SPECTRAL RESOLUTIONS OF comment_6: 3 - 100A, 4 - 4.7A, 5 - 4.7A comment_7: 6 - 4.7A, 7 - 6.85A comment_8: POSITION FROM GASP fluxnum_1: 1 fluxval_1: V = 16.9 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.1 +/- 0.05, E(B-V) = 0.05 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 7.9 +/- 0.5 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 3.5 +/- 0.4 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 2.8 +/- 0.5 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 2.8 +/- 0.5 E-16 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 4.0 +/- 0.5 E-16 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: M31-GAL-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 14S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 1.3-1.5; req_2: SPATIAL SCAN; req_3: SEQ 1.0-1.5 NO GAP; req_4: CYCLE 3 / 1-4.5; comment_1: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ comment_2: BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= comment_3: G270H; ! linenum: 1.100 targname: M31-GAL-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 20S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 1.3-1.5; req_2: SPATIAL SCAN; comment_1: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 1.200 targname: M31-GAL-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 30S fluxnum_1: 5 priority: 1 param_1: TYPE=UP, param_2: SCAN-STEP=0.35, param_3: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 1.3-1.5; comment_1: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 1.300 targname: M31-GAL-NUC config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 3650S s_to_n: 39 fluxnum_1: 5 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 4.7A RESOLUTION AT 2800A ! linenum: 1.400 targname: M31-GAL-NUC config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 500S s_to_n: 40 fluxnum_1: 7 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 6.85A RESOLUTION AT 3500A ! linenum: 1.500 targname: M31-GAL-NUC config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 1750S s_to_n: 13 fluxnum_1: 3 priority: 1 comment_1: S_TO_N IS CALCULATED comment_2: FOR 100A RESOLUTION AT 1500A ! linenum: 2.000 targname: M32-GAL-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 15S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 2.3-2.5; req_2: SPATIAL SCAN; req_3: SEQ 2.0-2.5 NO GAP; comment_1: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ comment_2: BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= comment_3: G270H; ! linenum: 2.100 targname: M32-GAL-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 20S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 2.3-2.5; req_2: SPATIAL SCAN; comment_1: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 2.200 targname: M32-GAL-NUC config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 30S fluxnum_1: 5 priority: 1 param_1: TYPE=UP, param_2: SCAN-STEP=0.35, param_3: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 2.3-2.5; comment_1: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 2.300 targname: M32-GAL-NUC config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2100S s_to_n: 40 fluxnum_1: 5 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 4.7A RESOLUTION AT 2800A ! linenum: 2.400 targname: M32-GAL-NUC config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 384S s_to_n: 50 fluxnum_1: 7 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 6.85A RESOLUTION AT 3500A ! linenum: 2.500 targname: M32-GAL-NUC config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 2200S s_to_n: 6 fluxnum_1: 3 priority: 1 comment_1: S_TO_N IS CALCULATED comment_2: FOR 100A RESOLUTION AT 1500A ! linenum: 3.000 targname: M33-B-EXT-CLUSTER-M33 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 74S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 3.3-3.5; req_2: SPATIAL SCAN; req_3: SEQ 3.0-3.5 NO GAP; comment_1: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ comment_2: BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= comment_3: G270H; ! linenum: 3.100 targname: M33-B-EXT-CLUSTER-M33 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 92S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 3.3-3.5; req_2: SPATIAL SCAN; comment_1: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 3.200 targname: M33-B-EXT-CLUSTER-M33 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 141S fluxnum_1: 5 priority: 1 param_1: TYPE=UP, param_2: SCAN-STEP=0.35, param_3: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 3.3-3.5; comment_1: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 3.300 targname: M33-B-EXT-CLUSTER-M33 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 3400S s_to_n: 15 fluxnum_1: 5 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 4.7A RESOLUTION AT 2800A ! linenum: 3.400 targname: M33-B-EXT-CLUSTER-M33 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 1500S s_to_n: 20 fluxnum_1: 7 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 6.85A RESOLUTION AT 3500A ! linenum: 3.500 targname: M33-B-EXT-CLUSTER-M33 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 1900S s_to_n: 5 fluxnum_1: 3 priority: 1 comment_1: S_TO_N IS CALCULATED comment_2: FOR 100A RESOLUTION AT 1500A ! linenum: 4.000 targname: M33-D-EXT-CLUSTER-M33 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 27S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 4.3-4.5; req_2: SPATIAL SCAN; req_3: SEQ 4.0-4.5 NO GAP; comment_1: 1ST OF 3 ACQ/PEAK SCANS ONBOARD ACQ comment_2: BLUE-SIDE ACQ/PEAK-SPECTRAL ELEMENT= comment_3: G270H; ! linenum: 4.100 targname: M33-D-EXT-CLUSTER-M33 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 34S fluxnum_1: 5 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 4.3-4.5; req_2: SPATIAL SCAN; comment_1: 2ND OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 4.200 targname: M33-D-EXT-CLUSTER-M33 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 52S fluxnum_1: 5 priority: 1 param_1: TYPE=UP, param_2: SCAN-STEP=0.35, param_3: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 4.3-4.5; comment_1: 3RD OF 3 ACQ/PEAK SCANS ONBOARD ACQ ! linenum: 4.300 targname: M33-D-EXT-CLUSTER-M33 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 1575S s_to_n: 20 fluxnum_1: 5 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 4.7A RESOLUTION AT 2800A ! linenum: 4.400 targname: M33-D-EXT-CLUSTER-M33 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 650S s_to_n: 20 fluxnum_1: 7 priority: 1 comment_1: S_TO_N IS CALCULATED FOR comment_2: 6.85A RESOLUTION AT 3500A ! linenum: 4.500 targname: M33-D-EXT-CLUSTER-M33 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 500S s_to_n: 7 fluxnum_1: 3 priority: 1 comment_1: S_TO_N IS CALCULATED comment_2: FOR 100A RESOLUTION AT 1500A ! ! end of exposure logsheet scan_data: line_list: 1.0,2.0,3.0,4.0 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.4000 wid_offset: 0.0000 ! line_list: 1.1,2.1,3.1,4.1 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.7500 wid_offset: 0.3500 ! ! end of scan data