! File: 3801C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:19:57:56 coverpage: title_1: SEARCH FOR QSOS SUITABLE FOR SUBSEQUENT OBSERVATION OF HE II 304 title_2: ABSORPTION ARISING IN THE IGM, LY-ALPHA, AND ... PART1 sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: SNAP longterm: 3 pi_title: DR pi_fname: DAVID pi_mi: R. pi_lname: TYTLER pi_inst: CALIFORNIA, UNIVERSITY OF, SAN DIEGO pi_country: USA pi_phone: 619-534-7670 num_pri: 500 num_par: 500 wf_pc: Y foc: Y funds_amount: 514462 funds_length: 24 funds_date: JUL-92 ! end of coverpage abstract: line_1: Ultraviolet images will be obtained in snapshot mode of the 500 known line_2: high-redshift (z > 2.8) QSOs in order to identify the few (about 20) line_3: targets which have sufficient ultraviolet flux for subsequent FOC/FOS line_4: or GHRS observations of He II 304. The detection of absorption by line_5: the Helium II Lyman-alpha line at 304 A, one of the line_6: most exciting prospects of the HST, will provide the first line_7: direct detection of the diffuse intergalactic medium (IGM). The line_8: absence of Gunn-Peterson H I 1215 absorption shows that the IGM is hot line_9: and/or of very low density, thus He I 584 is not expected to be line_10: observable. He II 304--the most promising line--should be observable line_11: from three sources: the diffuse IGM, the discrete Ly-alpha clouds, line_12: and the much rarer metal line absorption systems. The Gunn-Peterson line_13: continuum optical depth is not well constrained by models (range 0.3-3000). line_14: The mere detection of only one QSO below 304 A would rule out many models, line_15: limiting the IGM density, temperature, and ionization mechanisms. Similarly line_16: the total absence of flux from several targets would rule out other models. line_17: Of the 500 targets, 40 should be bright enough for subsequent FOC imaging line_18: in bands above and below 304A, 10 for FOC prism spectra, and 3 for FOS line_19: spectra, which will allow measurement of the He II/H I ratio in Ly-alpha line_20: clouds and the spectral slope of the background ionizing radiation. ! ! end of abstract general_form_proposers: lname: TYTLER fname: DAVID title: PI mi: R. inst: CALIFORNIA, UNIVERSITY OF, SAN DIEGO country: U.S.A. ! lname: LANZETTA fname: KENNETH mi: M. inst: CALIFORNIA, UNIVERSITY OF, SAN DIEGO country: U.S.A. ! lname: TURNSHEK fname: DAVID mi: A. inst: PITTSBURGH, UNIVERSITY OF country: U.S.A. ! lname: HAZARD fname: CYRIL inst: PITTSBURGH, UNIVERSITY OF country: U.S.A. ! lname: MCMAHON fname: RICHARD mi: G. inst: CAMBRIDGE, UNIVERSITY OF country: ENGLAND ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: 3.1 GOAL -- TO FIND TARGETS BRIGHT ENOUGH FOR FOLLOW-UP line_2: 3.2 FOC FILTER CHOICE line_3: 3.3 TARGET SELECTION line_4: 3.4 TARGET POSITIONS line_5: 3.5 TARGET PRIORITIES line_6: 3.6 EXPOSURE TIMES line_7: 3.7 COORDINATED PARALLEL WFC IMAGES line_8: 3.8 32 bit-TELEMETRY line_10: 3.1 GOAL -- TO FIND TARGETS BRIGHT ENOUGH FOR FOLLOW-UP line_11: The ultimate goal is to measure the Gunn-Peterson optical depth of line_12: the IGM at wavelengths less than (1+z)304 A, where emission redshifts line_13: of our QSO targets are in the range 2.84.5. The justification line_6: follows. line_8: The immediate goal is to find the few objects which have AB((1+z)304) line_9: <21. Ideally we would measure the monochromatic magnitude just to the line_10: red of (1+z)304. In practice the FOC filters transmit over a wide line_11: range of wavelengths. Filters are chosen to (1) allow S/N=4.5 in the line_12: image core at AB((1+z)304)=21.5 in less than 10 minutes under normal line_13: background and sky, (2) to show the maximum correlation between the line_14: filter flux and the monochromatic flux at (1+z)304, (3) to have less line_15: than 20 percent of their transmitted flux (from a source with line_16: AB=constant - a fair approximation for the average absorbed QSO line_17: spectrum) coming from wavelengths less than (1+z)304. The last line_18: constraint ensures that we will not be biased against sources if line_19: tau(304) is large and (1+z)304 is in the filter. If we used a filter line_20: to the blue of this, and no flux were observed (very likely), we line_21: would not be able to distinguish between (i) an intrinsically faint line_22: QSO with a steep continuum, (ii) extinction, (iii) intervening line_23: Lyman-limit absorbers or (iv) the He II GP effect. ! question: 3 section: 3 line_1: line_2: The correlation between the monochromatic flux at (1+z)304 and the line_3: filter flux is generally poor for two reasons. (1) Some intervening line_4: Lyman limit absorption systems (LLS) have Lyman limit edges which lie line_5: between (1+z)304 and the effective wavelength of the filter, in which line_6: case the flux at (1+z)304 is much less than that measured in the line_7: filter. (2) Many targets will have LLS edges just to the red of the line_8: filter effective wavelength, so that the bulk of the detected flux is line_9: red-leak. Red leak can be reduced using two filters simultaneously, line_10: but the only suitable combinations are too far to the red of (1+z)304, line_11: in which case there is a much greater chance of an LLS edge between line_12: the filter and (1+z)304, resulting in no major improvement in the line_13: correlation between AB((1+z)304) and AB(filter) (we have checked this). line_15: 3.3 TARGET SELECTION line_16: The target list includes over 500 QSOs with z > 2.8. We have deleted line_17: targets with known damped Ly-a lines because such absorbers remove line_18: all flux below 912A (in the QSO rest frame). But we keep QSOs with line_19: known Lyman-limit systems in the optical, because the Lyman continuum line_20: optical depth decreases as (lambda / 912)**2.9, so that most such line_21: systems at high redshifts have insufficient H I to absorb completely line_22: at 304 A. ! question: 3 section: 4 line_1: 3.4 TARGET POSITIONS line_2: All targets submitted at this time have 1 sigma positional errors of line_3: under 3 arcseconds. Most are 1 arcsecond. Many have GASP positions. line_4: The FOC/f96 512z x 1024 zoomed field of view is 22x22 arcsec. line_6: 3.5 TARGET PRIORITIES line_7: We have calculated the probability that any given target will yield line_8: a successful detection. These probabilities are described in line_9: question 7, section 7.1 under ``experimental plan''. line_11: The PRIORITY which we assign to a target is based on a precise line_12: quantitative scale. We reserve PRIORITY=1 and PRIORITY=2 for a few line_13: follow-up observations which will submitted later in the year. Thus line_14: PRIORITY=3 is the highest in the current proposal. line_15: PRIORITY: Probability associations are as follows. line_16: 3: >0.1, 4: 0.1-0.05, 5: 0.05-0.025, line_17: 6: 0.025-0.01, 7: 0.01-0.005, 8: 0.005-0.0025, 9: <0.0025. line_18: The probability of success decreases by about a factor of two for line_19: each unit increment in priority. A PRIORITY=4 target is then ten line_20: times more likely to succeed that a PRIORITY=7, which means that line_21: observing one priority 4 is equivalent to 10 priority 7 targets. line_22: These Probabilities are for follow-up with the FOS G130H, 4.3 arcsec line_23: aperture, SNR=5 per diode (n=1), 20 hour exposure. Other follow-up ! question: 3 section: 5 line_1: options require less flux, thus priority 9 objects, for example, line_2: have much larger probabilities of success for these modes, and so line_3: they are important targets. PRIORITY >9 will be used for targets line_4: which can be followed up with instruments other than the FOS. line_6: 3.6 EXPOSURE TIMES line_7: For this proposal exposure times are 400 sec for F140W, 660 sec for line_8: F170M, and 550 sec for F190M, all of which should give SNR=4.5 in the line_9: core of an object with at AB(filter)=21.5. From 200 images we expect line_10: only one bogus (chance photon clumping) detection, with this SNR or line_11: larger, lying within 2 arcsec (=nominal 2 sigma radius) of an line_12: expected target position. line_14: To calculate these exposure times we use a dark current of 6e-4 line_15: counts/sec/pixel, a Ly-alpha emission flux of 0.02 cts/sec/pix, and line_16: an OI 1304 flux of 4.3e-3 cts/sec/pix. These rates are all for line_17: unzoomed pixels, which are 0.022x0.022 arcsec for FOC f/96. The line_18: object core is 0.1 arcsec radius, or 64 unzoomed pixels in area. line_20: To convert from AB to counts/sec/object we assume that an object with line_21: AB(filter)=17, E(B-V)=0 (redening is treated elsewhere) gives 48 line_22: cts/sec in F140W, 23 cts/sec in F170M, and 25 cts/sec in F190M. ! question: 3 section: 6 line_1: Longer exposures would be very useful in times of unusually high line_2: background or UV sky emission. Otherwise longer exposures are useful line_3: but not essential, because we only need approximate fluxes, and the line_4: requested times should suffice to detect all targets with AB <21.5 line_5: in the filters. line_7: Shorter exposures are of use, and should be scheduled if helpful. line_9: 3.7 COORDINATED PARALLEL WFC IMAGES line_10: This is a request to try out a new procedure. We understand that it line_11: will complicate the scheduling procedure, and we would prefer that line_12: these parallel images be ignored for the time being, if their line_13: inclusion would otherwise hold up scheduling. line_15: We should like to use the WFC in coordinated parallel mode, which line_16: we understand to mean the following. While we are in coarse track on line_17: a target QSO and obtaining the FOC image, the WFC will obtain a line_18: parallel image of a region of sky some 6 arcminutes away from the line_19: target. The WFC operation should not impact the use of spacecraft line_20: time, hence, e.g. the WFC exposure may have to be shorter than that line_21: with the FOC, to allow the WFC to readout first. line_23: The primary use for the WFC images is to allow us to improve ! question: 3 section: 7 line_1: estimates of the expected position of the target QSO in the FOC line_2: image. This is a new procedure which we are proposing. It is not line_3: essential to our plans, and our current observing program does not line_4: assume that it is implemented, but it will lead to significantly more line_5: efficient use of HST time when executed. line_7: We intend to measure the relative positions of the target QSO, the line_8: stars in the WFC image, and the two guide stars to sub-arcsecond line_9: accuracy on Schmidt plates. CO-I's Hazard and McMahon will do this at line_10: Edinburgh and Cambridge, England. The expected position of the QSO in line_11: the FOC image can then be estimated to sub-arcsecond accuracy, line_12: provided we know the position of the FOC relative to the WFC, and the line_13: telescope roll angle. The FOC-WFC separation is currently known to line_14: about 0.5 arcsec, while the roll angle uncertainty of about 6 line_15: arcminutes translates to a 0.7 arcsec uncertainty in the expected QSO line_16: location in the FOC image. Thus the expected position of the QSO line_17: image core should be known to with an area of 0.5x0.7arcsec (1sigma), line_18: which is only 35 percent of the nominal GASP 1 arcsec positional line_19: area. We would hope to do even better by (1) improving the accuracy line_20: of the relative positions of the guide stars, reducing the line_21: uncertainty in roll, (2) measuring roll angle using stars in the line_22: WFC image, and (3) investigating the variance in the WFC-FOC line_23: separation. The improvement in the expected position of the target ! question: 3 section: 8 line_1: QSO in the FOC image reduces the chance of finding a spurious image line_2: ``core'', and hence allows us to detect targets of fainter magnitude line_3: in a given exposure. The increase in limiting magnitude is 0.2 for line_4: the above numbers, which corresponds to the need for only 0.77 of the line_5: exposure time to reach a given magnitude with a 2-sigma detection line_6: (=95 percent chance that the detection is real). This reduction in line_7: observing time is in principle possible for any FOC program in which line_8: the goal is to detect flux from objects of known positions, and for line_9: which the FOC image itself will not contain enough objects for line_10: internal position measurement. line_12: We choose WFC rather than the PC because we need sky coverage to line_13: detect as many stars as possible which are on sky survey Schmidt line_14: plates. The filter chosen is not critical, but it should have a high line_15: throughput for common M stars. We choose the F555W filter because it line_16: has high thoughput, is similar to V, and is well calibrated and often line_17: used (Maoz, Bahcall et al. 1991). Exposure times of 100 seconds are line_18: chosen to avoid saturating V<17. We expect about 1.1 (saturated) star line_19: of V<17 per field, and 5 with 170.1 arcsec is likely to line_19: occur several times during our 500 exposures, and exposures are not line_20: interrupted during the trail. We are not primarily interested in line_21: object structure, thus trails are not a major problem. They will line_22: complicate flux measurement, but not seriously, since we still learn line_23: a lot simply by determining whether any flux was detected at all. ! question: 4 section: 1 line_1: Extensive ground based and IUE observations have placed strict upper line_2: limits on H I 1215 GP absorption. IUE observations by Tripp et al. line_3: (op cit) show no GP trough from He I 584, as expected from the absence line_4: of H I. He II 304 is by far the most favorable line. It will lie line_5: between 1155 A for z = 2.8, to 1733 A for z = 4.7. line_6: There are no known targets bright enough for IUE observations of He II line_7: 304. Our targets are mostly 2 magnitudes too faint for IUE spectra. ! question: 6 section: 1 line_1: We require flux calibrations for FOC/96 F140W, F170M and F190M of this line_2: proposal. We will also need calibration for some of the following: FOC line_3: F120M, F130M, F140M, F152M, F170M, F190M, F210M, F140W, F175W, F165W line_4: and F195W, depending on the redshifts of the targets happen to be line_5: bright. We would be happy with 0.2 magnitude accuracy near the filter line_6: peak, but we are very sensitive to red-leak, so we also require 0.2 line_7: mag accuracy on the integrated throughput out to 6000 A. line_9: We require 32-bit telemetry to reconstruct pointing, as described above line_10: (Question 3, section 3.8). line_12: Most of our images will be in FOC f/96 F140M. Do we need a flat field line_13: for this wavelength\? ! question: 7 section: 1 line_1: Question 7: Data Reduction and analysis. line_2: Continued in Question 8 line_3: 7.1 Experimental plan - statistical model and HST follow-up line_4: 7.2 Target selection - existing information on targets, positions line_5: 7.3 Basic data Reduction - to flux values and limits line_6: 7.4 Faint Object Detection Procedure line_7: 7.5 Object Positions - FOC and GASP (see also 7.9) line_8: 7.6 Object Fluxed line_9: 7.7 Consistency Checks line_10: 7.8 Follow Up on Detections line_11: 7.9 WFC Positions line_12: 7.10 Scientific Analysis line_13: 7.11 Publications line_15: 7.1 EXPERIMENTAL PLAN -- THE STATISTICAL MODEL AND HST FOLLOW-UP line_16: In principle any QSO with z>2.8 could lead to the detection of the IGM line_17: He II 304 Gunn-Peterson effect. This the minimum redshift to place 304 line_18: A at observed wavelengths >(1+z)304=1155 A, the minimum for HST line_19: observations. Only a few of the 500 known QSOs with z>2.8 will be line_20: bright enough because of Lyman continuum absorption in intervening line_21: systems. The first step is to determine which targets are most likely line_22: to succeed. ! question: 7 section: 2 line_1: The probability that a given QSO is bright enough for follow-up line_2: observations at (1+z)304A depends on eight main factors: (1) brightness line_3: of the QSO in the optical, (2) its continuum spectral slope - alpha, line_4: (3) Galactic redening E(B-V), (4) the Lyman continuum optical depth and line_5: redshift of all known (high redshift) absorption systems, (5) the line_6: redshift and HI column density distribution of unknown absorption line_7: systems at low redshifts, (6) the QSO redshift, (7) the sensitivity of line_8: the various HST instruments at (1+z)304, and (8) the desired SNR, line_9: spectral resolution and the maximum exposure time. line_11: We have collected information on all of these factors. At the time of line_12: writing we use all known information on factors 1,3,4,5,6 and 7, while line_13: we are temporarily using a distribution (Gaussian, mean alpha=0.74, line_14: sigma=0.3), rather than QSO specific values, for spectral slopes. (The line_15: V band magnitudes used and listed for targets are corrected for Lyman- line_16: alpha forest continuum depression of Da=0.39 at 5500 A: the flux line_17: correction factor is 1/(1-0.39p) where p is the fraction of the filter line_18: flux from below rest wavelength 1211 A.) This information is the input line_19: to a statistical model of the experiment, which we use to calculate the line_20: probability distribution for the magnitude of each of the 500 targets line_21: at (1+z)304 A. The probability that each QSO will be bright enough line_22: for follow-up observations with each of four HST instrument modes line_23: (FOC G130H or G160L, GHRS G130L, FOC prism, FOC multiband filters) ! question: 7 section: 3 line_1: follows from the instrumental sensitivities. These probabilities vary line_2: from 0.2 down to below 0.01, depending on the HST instrument, SNR and line_3: exposure time. Most are a few percent. line_5: The target PRIORITIES and exposure time are then assigned using these line_6: probabilities to maximize the efficiency of use of HST time. line_8: Summing up the probabilities for all 500 QSOs we expect that 5 QSOs line_9: will be bright enough for a FOS G130H spectrum with SNR>=5 per diode at line_10: (1+z)304 in 10 hours (n=1, 4.3 arcsec aperture). Some of these five line_11: should be bright enough for SNR>10 in 10 hours. This is the minimum line_12: acceptable spectrum for follow-up, because we need SNR and spectral line_13: resolution to separate absorption by the HeII304 lines of Lyman-alpha line_14: forest clouds (they are common at z>2.8) from the distributed IGM line_15: absorption. It follows that we should try to observe as many of the 500 line_16: targets as possible. The more targets we examine, the less time will be line_17: needed for follow-up spectra, because we should find brighter targets. line_19: Although we will find only about 5 ideal targets out of 500, we expect line_20: to detect flux from 120, of which 60 will have only red-leak flux, 20 line_21: will be suitable for FOC prism spectra and the remaining 40 will have line_22: near the minimum flux for follow-up with FOC multiband images (the line_23: number 5 is reasonably well determined, whereas the 120, 60, 20 and 40 ! question: 7 section: 4 line_1: are approximate at this time). line_3: It will be hard to determine which of the 120 detections are red-leaks line_4: and which have real flux at (1+z)304. Our statistical model predicts line_5: the relative proportions as a function of observed flux. Fortunately line_6: there is a rough correlation between the observed FOC flux and the real line_7: flux at (1+z)304, such that the targets with the largest observed flux line_8: have the largest (1+z)304 flux and are the most likely to have real line_9: flux at (1+z)304. To determine whether any individual QSO has real flux line_10: at (1+z)304 we can either obtain a spectrum, or take FOC images through line_11: double filters (very slow) to reduce red-leak. line_13: We can in fact determine tau(304) from FOC images alone, without line_14: knowing which of the QSOs has real flux at (1+z)304. We would take line_15: images in bands to the blue and red of (1+z)304. Red-leak QSOs will line_16: have about equal flux in each band, as will most QSOs with mostly real line_17: flux if, and only if tau(304)<<1. But some proportion of the objects line_18: will show much less flux in the blue filter, either because of line_19: intervening LLS with edges between the two filters, or because line_20: tau(304)>1. Our model shows that we can deduce tau(304) form the line_21: proportion of QSOs with various flux ratios, provided we have more line_22: than of order 20 (perhaps more) targets with real flux at (1+z)304. line_23: Thus this project will succeed even if we do not find any objects ! question: 7 section: 5 line_1: which are very bright at (1+z)304. line_3: 7.2 PREPARATION OF TARGETS line_4: We have collected the following information on all 500 QSOs with z>2.8: line_5: coordinates, z, V magnitude, B-V, zabs and HI column density N(HI) of line_6: known absorption systems, zabs range in which there are no absorption line_7: systems with large N(HI). line_9: For 300 of them there is no information on absorption systems. For line_10: about 50 others magnitude errors are about 0.5. In the next few weeks line_11: we will collect all existing spectral slope information, and plan line_12: ground based observations to examine absorption systems and improve line_13: magnitudes for those targets which have the highest probability of line_14: being bright at (1+z)304. line_16: We have coordinates accurate to 3 arcsec for 311 of the targets. We line_17: will obtain arcsecond positions for the remainder, using the GASP line_18: system when they are bright enough, and directly measuring Schmidt line_19: plates for the others. line_21: We also intend to begin a quick search for more targets with extremely line_22: high probabilities of being bright. We now know that the ideal z is in line_23: the range 3.00.1 for FOS line_4: 10 hour follow-up spectra, and would like to find 20 more this summer. line_6: 7.3 BASIC DATA REDUCTION for FOC IMAGES line_7: We will begin examining data reduction options and potential problems line_8: in April 1992, with the goal of having operational procedures in place line_9: before the first images arrive. We will practice on archival data. line_11: Images should arrive at UCSD at a rate of about four (two FOC and two line_12: WFC) per day. They will be processed to flux information within a day line_13: or two of receipt, to allow us to check of our observing plan, the line_14: accuracy of the statistical experimental model, and to allow us to line_15: rapidly determine which targets should be re-submitted for follow-up line_16: observations. line_18: We will examine data reduction options and potential problems in detail line_19: before any data arrives, because we will not have the time or manpower line_20: to repeat the reduction of the anticipated 1100 images. Nor do we wish line_21: to cope with the complexity of having images from different epochs line_22: reduced in different ways. ! question: 7 section: 7 line_1: We expect to use our own data reduction rather than the pipeline line_2: because we will have a sufficient number of images to improve on the line_3: pipeline, and we will optimize for our program specific requirement to line_4: detect objects with very low count values against a substantial line_5: background. line_7: We will follow the basic data reduction steps outlined on pages 94-98 line_8: of the FOC Instrument Handbook (May 1990), but our procedures are line_9: likely to differ from the pipeline in at least the following ways. Our line_10: team has extensive experience with photon counting devices which are line_11: very similar to the FOC (Tytler was in Boksenberg's IPCS group). line_13: (1) Since we will receive some 550 FOC images, we may expect to line_14: encounter some relatively rare abnormalities. We will try to identify line_15: these early on. line_17: (2) The dark count will be about 50 percent of the total background and line_18: comparable to or larger than the target core counts. We are then line_19: unusually sensitive to the precise level of the dark count. We will line_20: conduct a thorough examination of the dark count, searching for line_21: temporal variation, dependence on orbital position, large scale line_22: structure across the field of the detector, and small scale line_23: correlations. ! question: 7 section: 8 line_1: line_2: (3) It is known that the crystalline structure of the first photocathode line_3: of image tubes produces small scale structure in flat field images. We line_4: will check the extent of this effect for the FOC, and determine whether line_5: current calibrations correctly register flat field frames and the images line_6: to be corrected. (They may not, because the FOC is powered down between line_7: flat and object exposures.) This is probably not a problem at our low line_8: count values, but is representative of the type of issues to be line_9: investigated. line_11: (4) We will examine whether we will need a flat field at about 1400 A, line_12: because the flats are wavelength dependent, and the lowest wavelength line_13: standard calibration is at 2000 A. Red-leak flux complicates this, but line_14: again it is hopefully not serious at low count values. line_16: (5) We will be very sensitive to all non-poisson features in the images, line_17: such as bad pixels, data drops, and reseaux marks. We will examine line_18: existing information on these and determine if our images can lead to line_19: improvements. line_21: It is clear form the above points, and the discussion of WFC derived line_22: positions below, that many of the data reduction steps can best be line_23: done after we have examined the stack of 500 FOC images. While we would ! question: 7 section: 9 line_1: like not to have to repeat the reduction of the images, experience line_2: suggests that this will probably be necessary. Hence we will store line_3: images at various states of reduction process on optical disks, to line_4: speed up such re-reductions. line_6: Potential problems include temporal and spatial variations in the dark line_7: current and sky background, bad pixels, and trailed images. line_9: 7.4 FAINT OBJECT DETECTION PROCEDURE line_10: Object detection should be straight forward for the few targets which line_11: are bright and of most importance. For the bulk of the 120 images which line_12: will yield detections, the object core will be a few sigma above the line_13: background. line_15: We will design and implement a faint object detection code, which will line_16: find the location and flux of objects, and give the probability that line_17: they are real rather than chance spurious clumps of photons. This code line_18: will work on the geometrically corrected raw photon images, because it line_19: will use the Poisson distribution, which does not apply after dark line_20: subtraction, flat field or flux calibration and geometric distortion line_21: correction. Rather it will also use the frames used for dark, flat line_22: field and flux calibration and geometric distortion correction directly line_23: as an input to a model of the raw count image. This procedure is ! question: 8 section: 1 line_1: statistically valid and will be more accurate than the usual method of line_2: correcting raw counts, especially for low count levels. line_4: The faint object detection code also needs to know the expected position line_5: of the target in the FOC image, and the approximate point spread line_6: function (PSF) in the filter band. A calculated PSF will probably line_7: suffice, but it must be corrected for any image trailing which might line_8: occur when coarse track is lost. In the first instance the expected line_9: position of the target will be obtained from the nominal GASP positions line_10: of the target and guide stars, in the normal way. This should give a line_11: 1 sigma position errors of about 1 arcsec radius. We will check this line_12: value on the 120 targets which will be detected. line_14: 7.5 OBJECT POSITIONS line_15: Currently GASP positions were available or have been obtained for only line_16: about 50 of the 500 targets. We will obtain GASP positions for all the line_17: others which are bright enough for the GASP images. The positions of line_18: the remainder will be will be directly measured for Schmidt plates, line_19: and referenced to the guide stars, preferable those which were actually line_20: used, which will require the measurement of the position of all line_21: potential guide stars, and astrometric solutions after we know which line_22: ones were used. ! question: 8 section: 2 line_1: In the first instance we will search for the target with 2 sigma of the line_2: expected position in the FOC image. Then we will look for detections line_3: over the whole image. In the case where there is an object outside the line_4: 2 sigma circle (5 percent of frames with detection, plus an unknown line_5: number of serendipitous UV bright objects) we must inspect Schmidt line_6: plates to determine whether there are any blue objects in the field. line_8: 7.6 OBJECT FLUXES line_9: We will need the current FOC format dependent photometric line_10: correction, and absolute filter throughput. line_11: This is complicated somewhat by the red-leak. Ideally the flux line_12: calibration accuracy should be more accurate than the photon count error line_13: of about 0.2 mag. line_15: 7.7 CONSISTENCY CHECKS: REFINING THE MODEL line_16: The information obtained from the images (position, flux, background line_17: level) will be logged into the data base and periodically be checked line_18: against predictions. Are are positions as good as we thought (e.g. are line_19: we searching the correct area on in the FOC images\?). Is the line_20: background and limiting flux similar to expectation\? Do we need to line_21: adjust exposure times\? Does the proportion of detections and their line_22: flux distribution, as well as the distribution of upper limits agree line_23: with the statistical model\? If not we must search for the problem: ! question: 8 section: 3 line_1: e.g. inaccurate model parameters. line_3: 7.8 FOLLOW-UP ON DETECTIONS line_4: For each detection we will obtain more accurate optical magnitudes line_5: and spectral slopes at Lick observatory. We will request time spread line_6: throughout the year to speed this up. For the few brightest objects we line_7: will obtain high resolution spectra in the optical, using the Keck line_8: telescope (mag limit should be more than adequate) if necessary. These line_9: spectra will be needed to determine the positions, HI column densities line_10: and velocity dispersions of all absorption systems (mostly Lyman-alpha line_11: clouds) which could have absorption lines in the region around (1+z)304. line_12: This information will be vital for the interpretation of the HST line_13: follow-up data because there is expected to be a lot of HeII304 line line_14: absorption, which would be confused for IGM GP absorption if not line_15: identified. line_17: For each detection, we will also use the current version of the model line_18: to calculate the probability that the target is bright enough for line_19: follow-up observations with different HST instruments. As noted above, line_20: this depends on the unknown amount of red-leak flux, and the probability line_21: of Lyman limit edges between the filter and (1+z)304, parameters which line_22: are handled by the model. We will then submit a selection of these line_23: objects (probably about 20 to 40) for follow-up observation, during ! question: 8 section: 4 line_1: cycle 2, with different FOC filters, and possible with the FOC prism line_2: or even the FOS in exceptional cases. The follow-up observations are line_3: intended to both measure tau(304), and to further reject objects line_4: dominated by red-leak flux. line_6: To plan these follow-up observation, we must know the current status of line_7: all four possible follow-up instrument modes. line_9: The reduction of the follow-up observations will be in the same spirit line_10: as the original images, except that we will now be using different line_11: filters, and possibly the FOC prism or FOS. line_13: 7.9 WFC POSITIONS line_14: A detailed discussion of the purpose of these images was given in line_15: question 3, section 3.7. Coordinated parallel WFC images will be used line_16: together with Schmidt plate astrometry to significantly improve the line_17: accuracy of the expected position of the target within the FOC image, line_18: which will allow us to distinguish fainter objects from photon noise. line_20: The WFC images will reduced in the usual way, with special attention to line_21: factors which effect positions (distortion correction, saturation, line_22: image trail). Details are discussed by Monet in the ``WF/PC Final line_23: Orbit/Science Verification Report'', Feb 1991, who references Gilmozzi ! question: 8 section: 5 line_1: et al. at STScI for updates. Following Monet, a clustering algorithm line_2: will be applied to each image to locate each star, and a solutions to line_3: linear mappings will be used to convert from pixels to arcseconds. line_4: Cubic correction terms give residuals of 10 mas, more than adequate line_5: for our purpose. The position of the WFC will then be known to about line_6: this accuracy. The position of the FOC relative to the WFC, which line_7: currently varies by about 0.5 arcsec for unknown reasons, will then be line_8: used to convert to the relative position of the FOC image. line_10: The HST roll angle will be measured using the positions of the stars line_11: in the WFC image. The roll angle error will be about about 36 arcsec line_12: when there are sufficient stars, which translates to an rotational line_13: angle error of 0.07 arcsec in the expected position of the FOC relative line_14: to the WFC. line_16: We then know the position of the FOC image relative to the stars in the line_17: WFC image. To find the expected position of the QSO target in the FOC line_18: image we then need to know the position of the target relative to the line_19: stars in the WFC image. We will normally simply make direct measurements line_20: of the best available Schmidt plate. This will be done for all 500 line_21: fields. In a few selected cases (e.g. important targets which appear line_22: to lie outside the expected positions) we will also obtain CCD line_23: astrometric images of both the WFC and target star, to check the ! question: 8 section: 6 line_1: accuracy of the process. Note that we only need relative line_2: positions to sub-arcsecond accuracy. We will also measure the positions line_3: of the guide stars to provide checks and allow conversion to a line_4: standard coordinate frame. line_6: We note that the limiting accuracy of this procedure comes from the line_7: motion of the FOC relative to the WFC, and from the relative positions line_8: on the Schmidt plate. The latter can be circumvented with new ground line_9: based images. We will also investigate the accuracy that can be line_10: obtained using GASP positions for both the target and the stars in the line_11: WFC image, since this would be much faster and hence of more use to line_12: other users of the WFC. line_14: If the WFC position estimation is successful, then it should be done line_15: before we apply the faint object detection algorithm to the FOC image. line_17: 7.10 SCIENTIFIC ANALYSIS line_18: Selected objects which will be observed in filters on either side of line_19: (1+z)304 in cycle 2. These fluxes and upper limits will be used as line_20: input into a statistical model which will provide predicted line_21: distributions for the observed fluxes in each of the two filters. The line_22: maximum likelihood method will be used to obtain estimates of the line_23: various parameters in the model, including the number Lyman limit ! question: 8 section: 7 line_1: systems at very low redshifts, their HI column density distribution, line_2: the HeII column density distribution for the Lyman-alpha cloud, the line_3: mean UV spectral slope of the QSOs, and tau(304) -- the main goal. line_4: We have already assembled enough of the parts of this model to know line_5: that it will be unusually complex. Each QSO spectrum is very different, line_6: and of unknown shape. We need values and accurate measurement errors for line_7: the magnitudes, optical spectral slopes and Galactic extinction of each line_8: detected object, and we must treat red-leak correctly by convolving each line_9: of say 100000 simulated spectra (1000 for each of 100 QSOs) with the line_10: FOC filter transmission curves. line_12: Our recent work on a similar global estimation problem line_13: (Tytler and Fan 1992 ApJS 79,1) took two of us about 4 months full time. line_14: The work proposed here is significantly more difficult, and might take line_15: two people about 6 months, but we fully expect that it will work, and line_16: give decisive results. line_18: 7.11 PUBLICATIONS line_19: We expect to publish four papers. (1) A description of the statistical line_20: model and target list. (2) The GASPed coordinates, charts and optical line_21: magnitudes for all 500 targets. (3) The HST measured fluxes, estimate line_22: of red-leak, the resulting estimates of the mean spectral slope and line_23: density of intervening LLS. (4) Estimate of tau(304) based on FOC ! question: 8 section: 8 line_1: images, and implications for the ionization of the IGM. ! question: 9 section: 1 line_1: Title=White Dwarf Stars, ID=2593, PI=Shipman: Tytler is one of 20 CO-Is. line_2: Totally unrelated to this proposal. No data and no publications yet. line_3: See proposal 3660 for HST involvement of Turnshek. ! question: 10 section: 1 line_1: UCSD has one of the largest groups in the world working on QSOs and line_2: especially absorption lines: 5 faculty, 2 research scientists, line_3: 2 postdocs, 7 graduate students and 3 undergraduates. UCSD is also line_4: the home institution for the FOS. We have a much relevant software and line_5: in house expertise. We have regular access to Lick, and hopefully line_6: the Keck observatory, where we will obtain observations of the QSO line_7: targets. We receive partial funding (air ticket only) from the line_8: university for observing trips at Lick. Money is available to line_9: support special (minority) undergraduates. UCSD will also modify line_10: some office space to make room for the three new people and their line_11: workstations. ! !end of general form text general_form_address: lname: TYTLER fname: DAVID mi: R. category: PI inst: CALIFORNIA, UNIVERSITY OF, SAN DIEGO addr_1: CENTER FOR ASTROPHYSICS AND SPACE SCIENCES (CASS) 0111 addr_2: 9500 GILMAN DR. city: LA JOLLA state: CA zip: 92093 country: U.S.A phone: (619) 534-7670 telex: FAX (619) 534 7051 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: 1442+101 descr_1: E,313,314 pos_1: RA = 14H 42M 50.60S +/- 0.1S, pos_2: DEC = +10D 11' 12.20" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.51 ! targnum: 2 name_1: 0130-403 descr_1: E,313,314 pos_1: RA = 1H 30M 50.30S +/- 0.1S, pos_2: DEC = -40D 21' 51.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.02 ! targnum: 3 name_1: 2204-408 descr_1: E,313,314 pos_1: RA = 22H 4M 33.20S +/- 0.1S, pos_2: DEC = -40D 51' 37.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.86 ! targnum: 4 name_1: 0041-266 descr_1: E,313,314 pos_1: RA = 0H 41M 15.20S +/- 0.1S, pos_2: DEC = -26D 38' 35.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.79 ! targnum: 5 name_1: 1946+7658 descr_1: E,313,314 pos_1: RA = 19H 46M 41.00S +/- 0.1S, pos_2: DEC = +76D 58' 26.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 15.85 ! targnum: 6 name_1: 0114-089 descr_1: E,313,314 pos_1: RA = 1H 14M 53.00S +/- 0.1S, pos_2: DEC = - 8D 57' 20.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.86 ! targnum: 7 name_1: 1033+1342 descr_1: E,313,314 pos_1: RA = 10H 33M 47.30S +/- 0.1S, pos_2: DEC = +13D 42' 26.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.00 ! targnum: 8 name_1: 0351-390 descr_1: E,313,314 pos_1: RA = 3H 51M 31.50S +/- 0.1S, pos_2: DEC = -39D 4' 46.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.90 ! targnum: 9 name_1: 0055-269 descr_1: E,313,314 pos_1: RA = 0H 55M 32.60S +/- 0.1S, pos_2: DEC = -26D 59' 25.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.12 ! targnum: 10 name_1: 1159+123 descr_1: E,313,314 pos_1: RA = 11H 59M 14.20S +/- 0.1S, pos_2: DEC = +12D 23' 12.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.35 ! targnum: 11 name_1: 0324-407 descr_1: E,313,314 pos_1: RA = 3H 24M 28.60S +/- 0.1S, pos_2: DEC = -40D 47' 16.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.60 ! targnum: 12 name_1: 0042-2627 descr_1: E,313,314 pos_1: RA = 0H 42M 6.40S +/- 0.1S, pos_2: DEC = -26D 27' 45.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.57 ! targnum: 13 name_1: 0101-304 descr_1: E,313,314 pos_1: RA = 1H 1M 32.10S +/- 0.1S, pos_2: DEC = -30D 25' 53.50" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.88 ! targnum: 14 name_1: 1400+114 descr_1: E,313,314 pos_1: RA = 14H 0M 10.30S +/- 0.1S, pos_2: DEC = +11D 26' 52.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.86 ! targnum: 15 name_1: 1334-005 descr_1: E,313,314 pos_1: RA = 13H 34M 13.10S +/- 0.1S, pos_2: DEC = - 0D 33' 42.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.00 ! targnum: 16 name_1: 0138-381 descr_1: E,313,314 pos_1: RA = 1H 38M 13.80S +/- 0.1S, pos_2: DEC = -38D 8' 13.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.60 ! targnum: 17 name_1: 0143-015 descr_1: E,313,314 pos_1: RA = 1H 43M 18.20S +/- 0.1S, pos_2: DEC = - 1D 35' 30.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.77 ! targnum: 18 name_1: 2359+068 descr_1: E,313,314 pos_1: RA = 23H 59M 6.80S +/- 0.1S, pos_2: DEC = + 6D 53' 12.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.33 ! targnum: 19 name_1: 0105-265 descr_1: E,313,314 pos_1: RA = 1H 5M 48.30S +/- 0.1S, pos_2: DEC = -26D 34' 20.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.05 ! targnum: 20 name_1: 1935-692 descr_1: E,313,314 pos_1: RA = 19H 35M 11.60S +/- 0.1S, pos_2: DEC = -69D 14' 51.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.26 ! targnum: 21 name_1: 0938+119 descr_1: E,313,314 pos_1: RA = 9H 38M 31.80S +/- 0.1S, pos_2: DEC = +11D 59' 12.60" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.95 ! targnum: 22 name_1: 1426-0131 descr_1: E,313,314 pos_1: RA = 14H 26M 28.10S +/- 0.1S, pos_2: DEC = - 1D 31' 57.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.61 ! targnum: 23 name_1: 0930+2858 descr_1: E,313,314 pos_1: RA = 9H 30M 41.40S +/- 0.1S, pos_2: DEC = +28D 58' 53.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.13 ! targnum: 24 name_1: 2231-0015 descr_1: E,313,314 pos_1: RA = 22H 31M 35.10S +/- 0.1S, pos_2: DEC = - 0D 15' 29.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.50 ! targnum: 25 name_1: 0042-264 descr_1: E,313,314 pos_1: RA = 0H 42M 6.20S +/- 0.1S, pos_2: DEC = -26D 27' 42.90" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.39 ! targnum: 26 name_1: 2139-4434 descr_1: E,313,314 pos_1: RA = 21H 39M 14.70S +/- 0.1S, pos_2: DEC = -44D 34' 1.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.63 ! targnum: 27 name_1: 1042+3158 descr_1: E,313,314 pos_1: RA = 10H 42M 36.10S +/- 0.1S, pos_2: DEC = +31D 58' 19.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.63 ! targnum: 28 name_1: 0047-308 descr_1: E,313,314 pos_1: RA = 0H 47M 54.80S +/- 0.1S, pos_2: DEC = -30D 50' 40.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.24 ! targnum: 29 name_1: 0830+115 descr_1: E,313,314 pos_1: RA = 8H 30M 29.90S +/- 0.1S, pos_2: DEC = +11D 33' 52.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.10 ! targnum: 30 name_1: SP43 descr_1: E,313,314 pos_1: RA = 15H 20M 31.20S +/- 0.1S, pos_2: DEC = +41D 22' 36.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.48 ! targnum: 31 name_1: 2158-169 descr_1: E,313,314 pos_1: RA = 21H 58M 50.00S +/- 0.1S, pos_2: DEC = -16D 57' 27.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.50 ! targnum: 32 name_1: 2138-4427 descr_1: E,313,314 pos_1: RA = 21H 38M 48.40S +/- 0.1S, pos_2: DEC = -44D 27' 8.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.86 ! targnum: 33 name_1: 0042-269 descr_1: E,313,314 pos_1: RA = 0H 42M 24.90S +/- 0.1S, pos_2: DEC = -26D 56' 33.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.48 ! targnum: 34 name_1: 1136+122 descr_1: E,313,314 pos_1: RA = 11H 36M 44.10S +/- 0.1S, pos_2: DEC = +12D 14' 45.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.60 ! targnum: 35 name_1: 1317-0507 descr_1: E,313,314 pos_1: RA = 13H 17M 54.10S +/- 0.1S, pos_2: DEC = - 5D 7' 52.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.73 ! targnum: 36 name_1: 0043-265 descr_1: E,313,314 pos_1: RA = 0H 43M 3.10S +/- 0.1S, pos_2: DEC = -26D 33' 33.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.42 ! targnum: 37 name_1: 1327+113 descr_1: E,313,314 pos_1: RA = 13H 27M 34.40S +/- 0.1S, pos_2: DEC = +11D 21' 41.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.20 ! targnum: 38 name_1: 1209+154 descr_1: E,313,314 pos_1: RA = 12H 9M 59.20S +/- 0.1S, pos_2: DEC = +15D 24' 6.30" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.30 ! targnum: 39 name_1: 1500+0431 descr_1: E,313,314 pos_1: RA = 15H 0M 58.80S +/- 0.1S, pos_2: DEC = + 4D 31' 32.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.13 ! targnum: 40 name_1: 0103-260 descr_1: E,313,314 pos_1: RA = 1H 3M 39.60S +/- 0.1S, pos_2: DEC = -26D 2' 55.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.67 ! targnum: 41 name_1: 2318+0119 descr_1: E,313,314 pos_1: RA = 23H 18M 41.30S +/- 0.1S, pos_2: DEC = + 1D 19' 27.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.45 ! targnum: 42 name_1: 0642-506 descr_1: E,313,314 pos_1: RA = 6H 42M 13.40S +/- 0.1S, pos_2: DEC = -50D 38' 6.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.50 ! targnum: 43 name_1: 0057-274 descr_1: E,313,314 pos_1: RA = 0H 57M 47.30S +/- 0.1S, pos_2: DEC = -27D 25' 2.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.48 ! targnum: 44 name_1: 1346+001 descr_1: E,313,314 pos_1: RA = 13H 46M 44.00S +/- 0.1S, pos_2: DEC = + 0D 7' 50.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.81 ! targnum: 45 name_1: 2048+312 descr_1: E,313,314 pos_1: RA = 20H 48M 47.40S +/- 0.1S, pos_2: DEC = +31D 16' 11.20" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.45 ! targnum: 46 name_1: 2050-359 descr_1: E,313,314 pos_1: RA = 20H 50M 35.50S +/- 0.1S, pos_2: DEC = -35D 58' 19.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.10 ! targnum: 47 name_1: 0057-398 descr_1: E,313,314 pos_1: RA = 0H 59M 53.24S +/- 0.1S, pos_2: DEC = -39D 31' 58.12" +/- 1.0" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 19.22 ! targnum: 48 name_1: 0040-279 descr_1: E,313,314 pos_1: RA = 0H 40M 12.20S +/- 0.1S, pos_2: DEC = -27D 58' 26.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.11 ! targnum: 49 name_1: 1631+373 descr_1: E,313,314 pos_1: RA = 16H 31M 3.00S +/- 0.1S, pos_2: DEC = +37D 22' 46.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.60 ! targnum: 50 name_1: 0351-378 descr_1: E,313,314 pos_1: RA = 3H 51M 18.80S +/- 0.1S, pos_2: DEC = -37D 49' 45.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.50 ! targnum: 51 name_1: 0043-259 descr_1: E,313,314 pos_1: RA = 0H 43M 42.20S +/- 0.1S, pos_2: DEC = -25D 55' 11.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.08 ! targnum: 52 name_1: 0043-276 descr_1: E,313,314 pos_1: RA = 0H 43M 48.10S +/- 0.1S, pos_2: DEC = -27D 34' 13.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.23 ! targnum: 53 name_1: 1548+4637 descr_1: E,313,314 pos_1: RA = 15H 48M 32.90S +/- 0.1S, pos_2: DEC = +46D 37' 56.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.92 ! targnum: 54 name_1: 1110+01 descr_1: E,313,314 pos_1: RA = 11H 10M 12.30S +/- 0.1S, pos_2: DEC = + 1D 6' 18.30" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 17.84 ! targnum: 55 name_1: 0830+1009 descr_1: E,313,314 pos_1: RA = 8H 30M 39.40S +/- 0.1S, pos_2: DEC = +10D 9' 58.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.63 ! targnum: 56 name_1: 0401-350 descr_1: E,313,314 pos_1: RA = 4H 3M 10.53S +/- 0.1S, pos_2: DEC = -34D 56' 57.29" +/- 1.0" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 19.42 ! targnum: 57 name_1: 0053-303 descr_1: E,313,314 pos_1: RA = 0H 53M 2.10S +/- 0.1S, pos_2: DEC = -30D 20' 2.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.24 ! targnum: 58 name_1: 0059-287 descr_1: E,313,314 pos_1: RA = 0H 59M 1.70S +/- 0.1S, pos_2: DEC = -28D 45' 44.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.73 ! targnum: 59 name_1: 0050-283 descr_1: E,313,314 pos_1: RA = 0H 50M 52.20S +/- 0.1S, pos_2: DEC = -28D 20' 50.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.11 ! targnum: 60 name_1: 2054-355 descr_1: E,313,314 pos_1: RA = 20H 54M 49.90S +/- 0.1S, pos_2: DEC = -35D 33' 37.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.18 ! targnum: 61 name_1: 0118+0119 descr_1: E,313,314 pos_1: RA = 1H 18M 14.60S +/- 0.1S, pos_2: DEC = + 1D 19' 11.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.32 ! targnum: 62 name_1: 0046-267 descr_1: E,313,314 pos_1: RA = 0H 46M 21.80S +/- 0.1S, pos_2: DEC = -26D 43' 25.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.31 ! targnum: 63 name_1: 0047-307 descr_1: E,313,314 pos_1: RA = 0H 47M 59.00S +/- 0.1S, pos_2: DEC = -30D 43' 8.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.42 ! targnum: 64 name_1: 1235+089 descr_1: E,313,314 pos_1: RA = 12H 35M 22.70S +/- 0.1S, pos_2: DEC = + 8D 57' 36.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.20 ! targnum: 65 name_1: 0131+013 descr_1: E,313,314 pos_1: RA = 1H 31M 14.40S +/- 0.1S, pos_2: DEC = + 1D 20' 55.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.99 ! targnum: 66 name_1: 1304+295 descr_1: E,313,314 pos_1: RA = 13H 4M 39.80S +/- 0.1S, pos_2: DEC = +29D 34' 43.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.01 ! targnum: 67 name_1: 1117-13 descr_1: E,313,314 pos_1: RA = 11H 17M 39.41S +/- 0.1S, pos_2: DEC = -13D 29' 59.80" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.13 ! targnum: 68 name_1: 1640+4628 descr_1: E,313,314 pos_1: RA = 16H 40M 37.20S +/- 0.1S, pos_2: DEC = +46D 28' 1.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.13 ! targnum: 69 name_1: 0241-01 descr_1: E,313,314 pos_1: RA = 2H 41M 29.36S +/- 0.1S, pos_2: DEC = - 1D 46' 42.60" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.31 ! targnum: 70 name_1: 2043-347 descr_1: E,313,314 pos_1: RA = 20H 43M 36.30S +/- 0.1S, pos_2: DEC = -34D 44' 39.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.79 ! targnum: 71 name_1: 1601+3754 descr_1: E,313,314 pos_1: RA = 16H 1M 19.50S +/- 0.1S, pos_2: DEC = +37D 54' 3.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.55 ! targnum: 72 name_1: 0216+080 descr_1: E,313,314 pos_1: RA = 2H 16M 18.20S +/- 0.1S, pos_2: DEC = + 8D 3' 41.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.10 ! targnum: 73 name_1: 2038-371 descr_1: E,313,314 pos_1: RA = 20H 38M 17.60S +/- 0.1S, pos_2: DEC = -37D 11' 6.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.53 ! targnum: 74 name_1: 2212-16 descr_1: E,313,314 pos_1: RA = 22H 12M 44.77S +/- 0.1S, pos_2: DEC = -16D 26' 30.20" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.23 ! targnum: 75 name_1: 0135-42 descr_1: E,313,314 pos_1: RA = 1H 35M 15.60S +/- 0.1S, pos_2: DEC = -42D 39' 30.70" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.59 ! targnum: 76 name_1: 1305+296 descr_1: E,313,314 pos_1: RA = 13H 5M 49.20S +/- 0.1S, pos_2: DEC = +29D 41' 12.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.17 ! targnum: 77 name_1: 1406+123 descr_1: E,313,314 pos_1: RA = 14H 6M 12.80S +/- 0.1S, pos_2: DEC = +12D 21' 21.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.90 ! targnum: 78 name_1: 0052-390 descr_1: E,313,314 pos_1: RA = 0H 54M 45.35S +/- 0.1S, pos_2: DEC = -38D 44' 15.49" +/- 1.0" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 19.55 ! targnum: 79 name_1: 0046-282 descr_1: E,313,314 pos_1: RA = 0H 46M 58.10S +/- 0.1S, pos_2: DEC = -28D 15' 22.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.22 ! targnum: 80 name_1: 2226+0216 descr_1: E,313,314 pos_1: RA = 22H 26M 5.40S +/- 0.1S, pos_2: DEC = + 2D 16' 42.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.81 ! targnum: 81 name_1: 1746+6226 descr_1: E,313,314 pos_1: RA = 17H 46M 14.00S +/- 0.1S, pos_2: DEC = +62D 26' 55.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.13 ! targnum: 82 name_1: 1144-07 descr_1: E,313,314 pos_1: RA = 11H 44M 2.45S +/- 0.1S, pos_2: DEC = - 7D 23' 25.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.08 ! targnum: 83 name_1: 2049-353 descr_1: E,313,314 pos_1: RA = 20H 49M 40.90S +/- 0.1S, pos_2: DEC = -35D 22' 22.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.45 ! targnum: 84 name_1: 0100-283B descr_1: E,313,314 pos_1: RA = 1H 0M 42.40S +/- 0.1S, pos_2: DEC = -28D 19' 20.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.57 ! targnum: 85 name_1: 0059-304B descr_1: E,313,314 pos_1: RA = 0H 59M 51.10S +/- 0.1S, pos_2: DEC = -30D 24' 0.00" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 19.68 ! targnum: 86 name_1: 1050-00 descr_1: E,313,314 pos_1: RA = 10H 50M 46.70S +/- 0.1S, pos_2: DEC = - 0D 0' 50.60" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.72 ! targnum: 87 name_1: 1340+099 descr_1: E,313,314 pos_1: RA = 13H 40M 0.70S +/- 0.1S, pos_2: DEC = + 9D 59' 52.0" +/- 1.0" equinox: 1950 fluxnum_1: 1 fluxval_1: V = 18.80 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: 0040-279 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 2.000 targname: 0041-266 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 3.000 targname: 0042-2627 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 4.000 targname: 0042-264 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 5.000 targname: 0042-269 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 6.000 targname: 0043-259 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 7.000 targname: 0043-265 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 8.000 targname: 0043-276 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 9.000 targname: 0046-267 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 10.000 targname: 0046-282 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 11.000 targname: 0047-307 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 12.000 targname: 0047-308 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 13.000 targname: 0050-283 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 14.000 targname: 0052-390 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 15.000 targname: 0053-303 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 16.000 targname: 0055-269 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 17.000 targname: 0057-274 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 18.000 targname: 0057-398 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 19.000 targname: 0059-287 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 20.000 targname: 0059-304B config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 21.000 targname: 0100-283B config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 22.000 targname: 0101-304 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 23.000 targname: 0103-260 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 24.000 targname: 0105-265 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 25.000 targname: 0114-089 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 26.000 targname: 0118+0119 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 27.000 targname: 0130-403 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 28.000 targname: 0131+013 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 29.000 targname: 0135-42 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 30.000 targname: 0138-381 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 31.000 targname: 0143-015 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 32.000 targname: 0216+080 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 33.000 targname: 0241-01 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 34.000 targname: 0324-407 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 35.000 targname: 0351-378 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 36.000 targname: 0351-390 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 37.000 targname: 0401-350 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 38.000 targname: 0642-506 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 39.000 targname: 0830+1009 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 40.000 targname: 0830+115 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 41.000 targname: 0930+2858 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 42.000 targname: 0938+119 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 43.000 targname: 1033+1342 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 44.000 targname: 1042+3158 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 45.000 targname: 1050-00 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 46.000 targname: 1110+01 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 47.000 targname: 1117-13 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 48.000 targname: 1136+122 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 49.000 targname: 1144-07 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 50.000 targname: 1159+123 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 51.000 targname: 1209+154 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 52.000 targname: 1235+089 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 53.000 targname: 1304+295 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 54.000 targname: 1305+296 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 55.000 targname: 1317-0507 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 56.000 targname: 1327+113 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 57.000 targname: 1334-005 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 58.000 targname: 1340+099 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 59.000 targname: 1346+001 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 60.000 targname: 1400+114 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 61.000 targname: 1406+123 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 62.000 targname: 1426-0131 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 63.000 targname: 1442+101 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 64.000 targname: 1500+0431 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 65.000 targname: 1548+4637 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 66.000 targname: 1601+3754 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 67.000 targname: 1631+373 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 68.000 targname: 1640+4628 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 69.000 targname: 1746+6226 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 70.000 targname: 1935-692 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 71.000 targname: 1946+7658 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 72.000 targname: 2038-371 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 73.000 targname: 2043-347 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 74.000 targname: 2048+312 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 75.000 targname: 2049-353 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 76.000 targname: 2050-359 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 77.000 targname: 2054-355 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 78.000 targname: 2138-4427 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 79.000 targname: 2139-4434 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 80.000 targname: 2158-169 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 81.000 targname: 2204-408 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 3 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 82.000 targname: 2212-16 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F170M wavelength: 1770 num_exp: 1 time_per_exp: 660S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 83.000 targname: 2226+0216 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 84.000 targname: 2231-0015 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 85.000 targname: 2318+0119 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 5 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 86.000 targname: 2359+068 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! linenum: 87.000 targname: 1340+099 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140W wavelength: 1366 num_exp: 1 time_per_exp: 400S fluxnum_1: 1 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: PCS MODE C comment_1: SNAPSHOT EXPOSURE ! ! end of exposure logsheet ! 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