! File: 2298C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:04:53:37 coverpage: title_1: STELLAR CONTENT OF GALAXIES AND GLOBULAR CLUSTERS sci_cat: GALAXIES & CLUSTERS sci_subcat: NEARBY GALAXIES proposal_for: GO pi_title: P.I. pi_fname: DAVID pi_lname: BURSTEIN pi_inst: ARIZONA STATE UNIVERSITY pi_country: USA pi_phone: 602-965-3561/4336 keywords_1: GALAXIES: STELLAR POPULATIONS; GLOBULAR CLUSTERS: keywords_2: INTEGRATED SPECTRA hours_pri: 15.00 num_pri: 4 wf_pc: Y fos: Y funds_amount: 170000 funds_length: 12 funds_date: SEP-90 pi_position: PROFESSOR off_fname: GARY off_mi: L. off_lname: CHAFFINS off_title: DIRECTOR off_inst: ARIZONA STATE UNIVERSITY off_addr_1: OFFICE OF SPONSORED PROGRAMS off_city: TEMPE off_state: AZ off_zip: 85287 off_country: USA off_phone: (602) 965-2170 ! end of coverpage abstract: line_1: Our goal is to establish a spectroscopic method which can line_2: reliably distinguish the effects of age from those of line_3: chemical composition in the integrated light of stellar line_4: populations older than one billion years. This program line_5: forms an essential link between two of HST's most powerful line_6: capabilities: detailed color-magnitude diagram (CMD) studies line_7: of nearby galaxies and globular clusters, and integrated line_8: light studies of high redshift galaxies in early phases of line_9: evolution. As a first step, we propose to obtain high line_10: precision FOS ultraviolet spectroscopy of bright, nearby line_11: extragalactic systems, to combine this with ground-based line_12: and IUE data in a comprehensive spectral synthesis analysis, line_13: and to compare the results with independent CMD studies by line_14: HST. Our results will help us to develop an effective method line_15: for interpreting the lower S/N data which will be available line_16: for distant objects at large lookback times. ! ! end of abstract general_form_proposers: lname: BURSTEIN fname: DAVID title: P.I. inst: ARIZONA STATE UNIVERSITY country: USA ! lname: FROGEL fname: JAY title: PROF. mi: A. inst: OHIO STATE UNIVERSITY country: USA ! lname: ROSE fname: JAMES title: PROF. mi: A. inst: NORTH CAROLINA, UNIVERSITY OF country: USA ! lname: RIEKE fname: MARCIA title: PROF. inst: ARIZONA, UNIVERSITY OF country: USA ! lname: O'CONNELL fname: ROBERT title: PROF. mi: W. inst: VIRGINIA, UNIVERSITY OF country: USA ! lname: WU fname: CHI-CHAO title: PROF. inst: STSCI country: USA ! ! 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 2200-3300 angstrom region; line_3: (b) a minimum S/N of 20 for spectral resolution elements of line_4: <10 angstrom for wavelengths >2500 angstroms; and (c) a line_5: desired S/N > 50 for objects where this does not require line_6: integrations longer than ~1 hour. All of the program line_7: objects are extended sources. Our requirements can only be line_8: met in reasonable integration times by using the FOS with line_9: gratings and the 1" square entrance aperture. For this line_10: proposal we assume that no WFC/PC images of these objects line_11: will be accessible to this program at the time of line_12: observations. WFC exposures with the F336W filter provide line_13: the best compromise between the need to locate the center line_14: of the objects relative to offset star(s), and the desire line_15: to examine the extended ultraviolet images of these objects line_16: for the presence of bright, hot stars. line_17: Three separate FOS spectra are needed for each object: line_18: a) The Blue Digicon (FOS/Blue) will be used to obtain a low line_19: S/N spectrum for 1150 - 1700 ang., using the G130H grating. line_20: (Note: We would prefer to use the 160L grating, but feel line_21: we cannot, due to scatter light problems reported on pg. 13 line_22: of FOS Instrument Handbook, Suppl. 1, May 1989.) These line_23: observations are essential to determine the contribution of ! question: 3 section: 2 line_1: stars hotter than 15000 deg K and to remove their effects line_2: from the longer wavelength data. Relatively long exposures line_3: are needed, even for the low (~100 ang) resolution required. line_4: b) The Red Digicon (FOS/Red) will be used to obtain: line_5: (i) A high S/N, 5.5 ang resolution sprectrum from line_6: 2200-3300 ang, using the G270H grating; and (ii) A high S/N, line_7: 8.3 ang reolution spectrum from 3250-4800 ang, using line_8: the G400H grating, which provides overlap with ground-based line_9: data and measures important features such as NH, CN and line_10: Ca II at the same spatial resolution as the UV data. line_11: There is a 50 ang. overlap between gratings G270H and G400H. line_12: There is a 500 ang. gap between G130H and G270H. Since this line_13: gap covers the 1700-2200 ang. region, where IUE spectra line_14: indicate that flux from these objects is at a minimum, this line_15: gap will not be covered with the current set of line_16: observations. All S/N ratios are calculated per spectral line_17: resolution element. In the exposure time calculations, it line_18: is assumed that the FOS/Blue and FOS/Red exposures will be line_19: taken on separate orbits. In addition to meeting our line_20: scientific criteria, the targets for this program were line_21: selected for expected UV brightness, relatively low line_22: background contamination and extinction, and for having line_23: planned GTO observations of CMD's. ! question: 4 section: 1 line_1: High S/N observations at spectral resolutions of 10 ang. in line_2: the region 2200-3300 ang. are required. Only HST can line_3: provide such data. The small aperture observations of M31 line_4: globular clusters possible with HST will maximize line_5: the cluster signal with respect to the of the background line_6: from the bulges and disks of these galaxies. This cannot line_7: be reliably done from the ground. The combined ground-based line_8: data available to us from our own separate programs include line_9: integrated spectra for ~700 galaxies, sellar spectra for line_10: ~500 stars, and visible/IR spectra energy distributions for line_11: ~200 galaxies. Among our group, we have previous or ongoing line_12: observations with IUE of: normal F,G,K main sequence stars; line_13: G,K giant stars; M31 globular cluster (poor S/N); elliptical line_14: galaxies and Seyfert galaxies. By the time of our HST line_16: observations we will have an ultraviolet stellar 'library' line_17: containing ~1500 stars. Some of the results of these line_18: ongoing studies are cited in Section 2 above. ! question: 5 section: 1 line_1: We have estimated average fluxes centered at 5 wavelengths line_2: for each object, based in most cases on extrapolations from line_3: IUE data either of the object itself or of an object of line_4: similar spectral energy distribution. V magnitudes with a line_5: 1" square apertue are estimated from available photoelectric line_6: photometry. If our spectra achieve the required S/N for line_7: these 5 regions, they will yield the desired S/N for the line_8: whole spectrum. The spectral resolutions used in the line_9: calculations of S/N listed in the Exposure section are: line_10: 100 ang. at 1500 ang., 5.5 ang. at 2500 ang., 2800 ang. and line_11: 3100 ang., and 8.3 ang. at wavelengths 3500 ang. and longer. line_12: As FOS/Blue is much less sensitive than FOS/Red at all line_13: wavelengths >1600 ang., our strategy is to use FOS/Blue line_14: only for the G130H observations (we cannot use the G160L line_15: due to scattered light problems), and to integrate for at line_16: least one orbit (~1700 sec). In some cases this procedure line_17: will yield higher S/N for the bluer clusters, thus line_18: permitting us to obtain wavelength resolution higher than line_19: 100 ang. at comparable S/N. FOS/Red will be used for the line_20: G270H and G400H observations. line_21: Object log Continuum Flux (ergs/cm2/s/ang.) line_22: 1500A 2500A 2800A 3100A 3500A line_23: G130H G270H G270H G270H G400H ! question: 5 section: 2 line_1: K58 M31GC -15.85 -15.75 -15.70 -15.45 -15.30 line_2: M II M31GC -15.20 -15.50 -15.20 -15.10 -14.95 line_3: M IV M31GC -14.95 -15.50 -15.60 -15.45 -15.30 line_4: K280 M31GC -15.50 -15.65 -15.40 -15.15 -15.00 ! question: 6 section: 1 line_1: (a) Since all of the objects in this program will have low line_2: UV flux levels, avoidance of additional sources of line_3: background, such as the Gegenshein, is desirable. line_4: (b) N/A ! question: 7 section: 1 line_1: The spectra will be reduced to absolute fluxes, the three line_2: spectral regions combined and reliable S/N estimates line_3: obtained. We will use HST software for this phase. line_4: The spectral line features of each spectrum will be line_5: intercompared and measured in a consistent manner according line_6: to methods we have already developed using IUE observations line_7: of stars. Corresponding visible and infrared spectral line_8: energy distributions of the same objects will be added line_9: (Question 8), providing complete wavelength coverage from line_10: 1200 ang. to 2.2 microns, with <10 ang. resolution out to line_11: 1 micron. Telescopes such as the MMT and the CFHT have line_12: demonstrated that it is possible to obtain ground-based line_13: observations with 1"-2" spatial resolution. Observations line_14: at >4500 ang. are little affected by atmospheric refraction. line_15: As part of the initial analysis, the spectral line indices line_16: of 500 stars measured by Burstein, Faber and collaborators, line_17: of 300 stars measured by Rose, and of 200 stars measured by line_18: O'Connell will be combined into a unified data base. All line_19: stellar observations made by IUE of reasonable S/N (over line_20: 10,000 spectra for ~2000 stars) are being reprocessed by line_21: DB, RWO, CCW, Ralph Bohlin and Linda Stryker. These spectra line_22: will be analyzed in a manner similar to the HST spectra, and line_23: an external calibration of age, metallicity and gravity will ! question: 7 section: 2 line_1: be establshed for each UV index. Preliminary analysis line_2: indicates that the UV line indices between 2400-3200 ang. are line_3: sensitive primarily to temperature, with gravity and line_4: metallicity effects of much less importance (a paper line_5: disussing this is in prepartion). line_6: The full UV-to-IR spectral energy distributions of the line_7: targets will then be analyzed in two independent ways: line_8: 1) With the optimizing spegtral synthesis program of line_9: O'Connell; 2) Using the evolutionary modeling methods line_10: developed by Faber, Burstein and collaborators and by Rose, line_11: which give greater emphasis to the correlations among the line_12: absorption-line indices. A primary goal of the project is line_13: to compare the populations of the globular clusters, as line_14: inferred from these analyses, to the known CMD's obtained line_15: by other HST observers. It is obviously essential that the line_16: deduced ages and metallicities of these two different line_17: approaches agree. Any discrepencies will require careful line_18: study. ! question: 8 section: 1 line_1: Accurate target positions for these objects must be obtained line_2: directly with an HST imaging device, as all of these objects line_3: are extended, and the precise center positions of M31 line_4: globular clusters are difficult to determine from line_5: ground-based observations. All M31 cluster are exepcted to line_6: have WFC exposure obtained in GTO programs for CMD's. line_7: This proposal assumes that no WFC images will be line_8: accessible to us, either through absence or propriety, so line_9: that we will need to make 4 WFC exposures. ! question: 9 section: 1 line_1: (a) N/A line_2: (b) N/A line_3: (c) N/A ! question: 10 section: 1 line_1: The majority of support from our home institutions comes in line_2: the form of computer facilities. Although we can only dimly line_3: perceive what those facilities might be in 1.5 years, it is line_4: probably relevent to list what facilities we currently line_5: have that could reduce HST data it were made avaialble today: line_6: Burstein/ASU: VAX750+1Gb disk+Jupiter 7 Image Disp/Conn to line_7: VAX, IBM, Cray 4MP line_8: O'Connell/UVa: microVAX II+IVAS image disp+1Gb disk; SUN line_9: +AT&T clusters line_10: Frogel/OSU: SUN 386i, VAX 780, microvaxes, Cray line_11: supercomputer line_12: Rose/UNC: SUN 3/60C, Convex, supercomputer line_13: Wu/CSC: Access to STScI facilities line_14: Rieke/UofA: Various mini-computers; Steward Obs. line_15: imaging analysis facilities ! !end of general form text general_form_address: lname: BURSTEIN fname: DAVID title: PROF. category: PI inst: ARIZONA STATE UNIVERSITY addr_1: DEPT. OF PHYSICS AND ASTRONOMY city: TEMPE state: AZ zip: 85287 country: USA phone: 602-965-3561/4336 ! lname: O'CONNELL fname: ROBERT mi: W. title: PROF. category: CON inst: UNIVERSITY OF VIRGINIA addr_1: DEPT. OF ASTRONOMY addr_2: P.O BOX 3818 city: CHARLOTTESVILLE state: VA zip: 22903 country: USA phone: 804-924-7494 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: K58-EXT-CLUSTER-M31 name_2: V55-EXT-CLUSTER-M31 descr_1: EXT-CLUSTER; MODERATELY METAL-RICH descr_2: GLOBULAR CLUSTER IN M31 pos_1: TBD-EARLY, pos_2: RA=0H 40M 26.4S +/- 1.0", pos_3: DEC=+41D 27' 26.3" +/- 1.0" equinox: 2000 rv_or_z: V = -200 acqpr_1: BKG acqpr_2: EXT comment_1: EARLY-ACQ MUST BE TAKEN TO BE ABLE comment_2: TO CENTER CLUSTERS TO <=0.1" IN FOS comment_3: V MAG ESTIMATED IN 1" SQUARE APER comment_4: INDIVIDUAL STARS IN CLUSTER HAVE comment_5: MAGS 4-7 MAG FAINTER comment_6: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_7: ARE FOR SPECTRAL RESOLUTIONS OF comment_8: 3 - 100A, 4 - 5.5A, 5 - 5.5A comment_9: 6 - 5.5A, 7 - 8.3A fluxnum_1: 1 fluxval_1: V = 16.2 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.93 +/- 0.05, E(B-V) = 0.08 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 1.4 +/- 0.3 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 1.8 +/- 0.3 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 2.0 +/- 0.4 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 3.6 +/- 0.5 E-16 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 5.0 +/- 0.5 E-16 ! targnum: 2 name_1: K58-OFFSET descr_1: TO BE FOUND OFFSET STAR descr_2: FOR K58, M31 EXT-CLUST pos_1: RA-OFF = +0S +/- 6S, pos_2: DEC-OFF = +0' +/- 1', pos_3: FROM 1, TBD-EARLY comment_1: TBD-EARLY ! targnum: 3 name_1: MII-EXT-CLUSTER-M31 name_2: K1-EXT-CLUSTER-M31 descr_1: EXT-CLUSTER; MODERATELY METAL-RICH descr_2: GLOBULAR CLUSTER IN M31 pos_1: TBD-EARLY, pos_2: RA = 0H 32M 46.6S +/- 1.0", pos_3: DEC = +39D 34' 39.6" +/- 1.0" equinox: 2000 rv_or_z: V = -200 acqpr_1: BKG acqpr_2: EXT comment_1: EARLY-ACQ MUST BE TAKEN TO BE ABLE comment_2: TO CENTER CLUSTERS TO <=0.1" IN FOS comment_3: V MAG ESTIMATED IN 1" SQUARE APER comment_4: INDIVIDUAL STARS IN CLUSTER HAVE comment_5: MAGS 4-7 MAG FAINTER comment_6: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_7: ARE FOR SPECTRAL RESOLUTIONS OF comment_8: 3 - 100A, 4 - 5.5A, 5 - 5.5A comment_9: 6 - 5.5A, 7 - 8.3A fluxnum_1: 1 fluxval_1: V = 14.5 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.88 +/- 0.05, E(B-V) = 0.08 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 6.3 +/- 0.6 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 3.2 +/- 0.5 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 6.3 +/- 0.6 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 7.9 +/- 0.7 E-16 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 1.1 +/- 0.2 E-15 ! targnum: 4 name_1: MII-OFFSET descr_1: TO BE FOUND OFFSET STAR descr_2: FOR MII, M31 EXT-CLUST pos_1: RA-OFF = +0S +/- 6S, pos_2: DEC-OFF = +0' +/- 1', pos_3: FROM 3, TBD-EARLY comment_1: TBD-EARLY ! targnum: 5 name_1: MIV-EXT-CLUSTER-M31 name_2: K219-EXT-CLUSTER-M31 descr_1: EXT-CLUSTER; VERY METAL-POOR descr_2: GLOBULAR CLUSTER IN M31 pos_1: TBD-EARLY, pos_2: RA = 0H 43M 17.8S +/- 1.0", pos_3: DEC = +39D 49' 12.8" +/- 1.0" equinox: 2000 rv_or_z: V = -200 acqpr_1: BKG acqpr_2: EXT comment_1: EARLY-ACQ MUST BE TAKEN TO BE ABLE comment_2: TO CENTER CLUSTERS TO <=0.1" IN FOS comment_3: V MAG ESTIMATED IN 1" SQUARE APER comment_4: INDIVIDUAL STARS IN CLUSTER HAVE comment_5: MAGS 4-7 MAG FAINTER comment_6: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_7: ARE FOR SPECTRAL RESOLUTIONS OF comment_8: 3 - 100A, 4 - 5.5A, 5 - 5.5A comment_9: 6 - 5.5A, 7 - 8.3A fluxnum_1: 1 fluxval_1: V = 15.9 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.69 +/- 0.05, E(B-V) = 0.08 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 1.1 +/- 0.2 E-15 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 3.2 +/- 0.4 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 2.5 +/- 0.4 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 3.5 +/- 0.5 E-16 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 5.0 +/- 0.5 E-16 ! targnum: 6 name_1: MIV-OFFSET descr_1: TO BE FOUND OFFSET STAR descr_2: FOR MIV, M31 EXT-CLUST pos_1: RA-OFF = +0S +/- 6S, pos_2: DEC-OFF = +0' +/- 1', pos_3: FROM 5, TBD-EARLY comment_1: TBD-EARLY ! targnum: 7 name_1: K280-EXT-CLUSTER-M31 name_2: V282-EXT-CLUSTER-M31 descr_1: EXT-CLUSTER; METAL-RICH descr_2: GLOBULAR CLUSTER IN M31 pos_1: TBD-EARLY, pos_2: RA = 0H 44M 29.5S +/- 1.0", pos_3: DEC = +41D 21' 35.5" +/- 1.0" equinox: 2000 rv_or_z: V = -200 acqpr_1: BKG acqpr_2: EXT comment_1: EARLY-ACQ MUST BE TAKEN TO BE ABLE comment_2: TO CENTER CLUSTERS TO <=0.1" IN FOS comment_3: V MAG ESTIMATED IN 1" SQUARE APER comment_4: INDIVIDUAL STARS IN CLUSTER HAVE comment_5: MAGS 4-7 MAG FAINTER comment_6: S/N CALCULATIONS FOR FLUXNUM 3-7 comment_7: ARE FOR SPECTRAL RESOLUTIONS OF comment_8: 3 - 100A, 4 - 5.5A, 5 - 5.5A comment_9: 6 - 5.5A, 7 - 8.3A fluxnum_1: 1 fluxval_1: V = 15.0 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.95 +/- 0.05, E(B-V) = 0.08 fluxnum_3: 3 fluxval_3: F-CONT(1500) = 3.2 +/- 0.5 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2500) = 2.2 +/- 0.4 E-16 fluxnum_5: 5 fluxval_5: F-CONT(2800) = 4.0 +/- 0.5 E-16 fluxnum_6: 6 fluxval_6: F-CONT(3100) = 7.1 +/- 0.7 E-16 fluxnum_7: 7 fluxval_7: F-CONT(3500) = 1.0 +/- 0.1 E-15 ! targnum: 8 name_1: K280-OFFSET descr_1: TO BE FOUND OFFSET STAR descr_2: FOR K280, M31 EXT-CLUST pos_1: RA-OFF = +0S +/- 6S, pos_2: DEC-OFF = +0' +/- 1', pos_3: FROM 7, TBD-EARLY comment_1: TBD-EARLY ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: K58-EXT-CLUSTER-M31 config: WFC opmode: IMAGE aperture: ALL sp_element: F336W num_exp: 1 time_per_exp: 700S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.2, param_3: PRE-FLASH=YES req_1: CYCLE 1 / 1-32; req_2: EARLY ACQ FOR 2-8 ! linenum: 2.000 targname: K58-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 2-4 NO GAP; req_2: ONBOARD ACQ FOR 3-4 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 3.000 targname: K58-EXT-CLUSTER-M31 config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 4.000 targname: K58-EXT-CLUSTER-M31 config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 5905S s_to_n: 25 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED comment_2: FOR 100A RESOLUTION AT 1500A ! linenum: 5.000 targname: K58-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 5-8 NO GAP; req_2: ONBOARD ACQ FOR 6-8 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 6.000 targname: K58-EXT-CLUSTER-M31 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 7.000 targname: K58-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2756S s_to_n: 30 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 5.5A RESOLUTION AT 2800A ! linenum: 8.000 targname: K58-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 483S s_to_n: 28 fluxnum_1: 7 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 8.3A RESOLUTION AT 3500A ! linenum: 9.000 targname: MII-EXT-CLUSTER-M31 config: WFC opmode: IMAGE aperture: ALL sp_element: F336W num_exp: 1 time_per_exp: 700S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.2, param_3: PRE-FLASH=YES req_1: EARLY ACQ FOR 10-16 ! linenum: 10.000 targname: MII-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 10-12 NO GAP; req_2: ONBOARD ACQ FOR 11-12 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 11.000 targname: MII-EXT-CLUSTER-M31 config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 12.000 targname: MII-EXT-CLUSTER-M31 config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 1680S s_to_n: 33 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 100A RESOLUTION AT 1500A ! linenum: 13.000 targname: MII-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 13-16 NO GAP; req_2: ONBOARD ACQ FOR 14-16 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 14.000 targname: MII-EXT-CLUSTER-M31 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 15.000 targname: MII-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 1939S s_to_n: 46 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 5.5A RESOLUTION AT 2800A ! linenum: 16.000 targname: MII-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 855S s_to_n: 48 fluxnum_1: 7 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 8.3A RESOLUTION AT 3500A ! linenum: 17.000 targname: MIV-EXT-CLUSTER-M31 config: WFC opmode: IMAGE aperture: ALL sp_element: F336W num_exp: 1 time_per_exp: 700S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.2, param_3: PRE-FLASH=YES req_1: EARLY ACQ FOR 18-24 ! linenum: 18.000 targname: MIV-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 18-20 NO GAP; req_2: ONBOARD ACQ FOR 19-20 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 19.000 targname: MIV-EXT-CLUSTER-M31 config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 20.000 targname: MIV-EXT-CLUSTER-M31 config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 1680S s_to_n: 41 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 100A RESOLUTION AT 1500A ! linenum: 21.000 targname: MIV-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 21-24 NO GAP; req_2: ONBOARD ACQ FOR 22-24 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 22.000 targname: MIV-EXT-CLUSTER-M31 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 23.000 targname: MIV-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2009S s_to_n: 29 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 5.5A RESOLUTION AT 2800A ! linenum: 24.000 targname: MIV-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 785S s_to_n: 30 fluxnum_1: 7 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 8.3A RESOLUTION AT 3500A ! linenum: 25.000 targname: K280-EXT-CLUSTER-M31 config: WFC opmode: IMAGE aperture: ALL sp_element: F336W num_exp: 1 time_per_exp: 700S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.2, param_3: PRE-FLASH=YES req_1: EARLY ACQ FOR 26-32 ! linenum: 26.000 targname: K280-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 26-28 NO GAP; req_2: ONBOARD ACQ FOR 27-28 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 27.000 targname: K280-EXT-CLUSTER-M31 config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 28.000 targname: K280-EXT-CLUSTER-M31 config: FOS/BL opmode: ACCUM aperture: 1.0-PAIR sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 5905S s_to_n: 30 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 100A RESOLUTION AT 1500A ! linenum: 29.000 targname: K280-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 24S priority: 1 req_1: SEQ 29-32 NO GAP; req_2: ONBOARD ACQ FOR 30-32 comment_1: WILL NEED TO UPDATE EXPOSURE TIME comment_2: FROM WFC EARLY ACQ EXPOSURE ! linenum: 30.000 targname: K280-EXT-CLUSTER-M31 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 70S priority: 1 comment_1: TO OBTAIN RECORD OF WHERE IN comment_2: CLUSTER OBSERVATION IS MADE. comment_3: INTEGRATION TIME COULD CHANGE, comment_4: DEPENDENT ON ACTUAL FOS MEASURES. comment_5: THIS WILL BE REQUIRED AT EACH comment_6: REPOINTING AT CLUSTER ! linenum: 31.000 targname: K280-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 1935S s_to_n: 36 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 5.5A RESOLUTION AT 2800A ! linenum: 32.000 targname: K280-EXT-CLUSTER-M31 config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 859S s_to_n: 37 fluxnum_1: 7 priority: 1 param_1: STEP-PATT=SINGLE comment_1: S_TO_N IS CALCULATED FOR comment_2: 8.3A RESOLUTION AT 3500A ! ! end of exposure logsheet ! No scan data records found