! File: 5710_v3final.prop ! Database: PEPDB ! Date: 22-FEB-1994:18:19:00 coverpage: title_1: WF/PC OBSERVATIONS OF THE MOST LUMINOUS GALAXY IN THE UNIVERSE; title_2: THE IRAS SOURCE FSC 10214+4724: CYCLE 4 CARRY-OVER sci_cat: GALAXIES & CLUSTERS sci_subcat: DISTANT GALAXIES proposal_for: GO/CAR cont_id: 4575 pi_fname: BARUCH pi_mi: T pi_lname: SOIFER pi_inst: CALTECH pi_country: US hours_pri: 2.4 num_pri: 1 wf_pc: Y funds_length: 12 off_fname: EARL off_mi: J off_lname: FREISE off_title: DIR.,SP. RES. off_inst: 1590 off_addr_1: 1201 E. CALIFORNIA BLVD. off_city: PASADENA off_state: CA off_zip: 91125 off_phone: (818)356-6357 ! end of coverpage abstract: line_1: We propose high spatial resolution imaging with the Planetary Camera and line_2: Wide Field Camera of the most luminous known galaxy in the Universe, the line_3: IRAS source FSC10214+4724. This object appears to share many properties line_4: with nearby Ultraluminous Infrared Galaxies, but is 3 orders of magnitude line_5: more luminous. It is also an exceedingly gas rich system, having ~10^12 line_6: solar masses of molecular gas. The purpose of the proposed observations line_7: is to establish the morphology of the underlying galaxy(s) on a 1 Kpc line_8: scale and thereby clarify whether this is an interaction between two line_9: or more well formed gas rich galaxies or is a galaxy in the process of line_10: formation. Such a determination will help establish whether the power line_11: source of this system is a dust enshrouded quasar or star formation in a line_12: newly forming galaxy. ! ! end of abstract general_form_proposers: lname: SOIFER fname: BARUCH title: PI mi: T inst: CALTECH country: USA esa: N ! lname: NEUGEBAUER fname: GERRY inst: CALTECH country: USA esa: N ! lname: WEIR fname: NICHOLAS inst: CALTECH country: USA esa: N ! lname: WERNER fname: MICHAEL mi: W. inst: JPL country: USA esa: N ! lname: EISENHARDT fname: PETER mi: R. inst: JPL country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We wish to obtain the best possible S/N and angular resolution line_2: on the target with the PC. Our cycle 3 Phase II proposal line_3: called for filter F725LP, but this is no longer available. line_4: The best available choice given the redness of our object is line_5: F814W. Because of the success of the servicing mission, line_6: we no longer require a PSF calibration star observation. line_7: Because we will be limited by read noise, our intent is to line_8: maximize the individual exposure times for the individual PC line_9: exposures, and stack individual exposures. line_10: Thus we set CR-SPLIT = NO. line_11: Our allocation of 2.4 hours of spacecraft time will allow 3 orbits line_12: to be scheduled with a total of about 6400 seconds of integration. line_13: The first orbit exposure may be cut down to 2000s or so if it is line_14: needed in order to allow extra time for initial guide star line_15: acquisition. The next two orbits should be as long as can be line_16: fit in an alignment. Each exposure will be at a slightly line_17: different position to reduce the effects of hot pixels line_18: on the data. To minimize changes in the PSF, these positions line_19: will be separated by integer numbers of PC pixels. This should line_20: permit us to do a reasonable job of detecting cosmic ray events. line_21: We also require the three orbits be grouped to minimize PSF line_22: changes. To avoid potential row or column related problems, each line_23: position is on a different row and column. ! question: 3 section: 2 line_1: No special orientation wrt N or E is needed, line_2: however the star "B" 28" E and 25" S of our target line_3: may potentially be bright enough to cause charge bleeding, line_4: therefore it should not fall on the PC chip. This should not line_5: be a problem as these distances will result in a minimum line_6: column or row separation of over 600 pixels from the target. line_7: On the other hand the star "A" 13" east of our target should line_8: fall on the PC to provide a PSF monitor on the long target line_9: exposure frames. To obtain the best possible angular resolution line_10: we will need fine lock for the observations. ! question: 4 section: 1 line_1: Figure 1 of section 2 of our Phase I proposal illustrates the line_2: best ground based imaging of FSC10214+4724 that has been line_3: obtained. This figure, obtained in good seeing, shows that line_4: there is complex structure in the source over the central 1.5" line_5: of the source, corresponding to the central 7.5 kpc. line_6: Distinguishing the morphology of the galaxy requires line_7: significantly better spatial resolution than is afforded by line_8: figure 1, and the only platfrom for achieving this resolution is line_9: the HST. ! question: 5 section: 1 line_1: Because high angular resolution of an object with complex line_2: morphology is the key to the success of our proposal, line_3: we request that the three orbits be grouped together line_4: to minimize time variations in the PSF. line_5: We require slight repositioning of the target to three distinct line_6: locations separated by 0.5" (several pixels) in the xy frame of line_7: PC to ensure that blemishes do not degrade more than one line_8: third of the data at any spatial point. The orientation of these line_9: positions on the sky is irrelevant and therefore this should line_10: not create any additional scheduling restrictions. ! question: 6 section: 1 line_1: Because we will always be read noise limited and our target is line_2: extremely faint we require the longest possible uninterrupted line_3: exposure times to achieve the best S/N for our allocated time. line_4: This is particularly necessary if we are to detect tidal tails line_5: or other signs of a merger which may be at very low surface line_6: brightness levels. ! question: 7 section: 1 line_1: The image of FSC10214+4724 shown in our Phase I proposal line_2: shows a clearly complex structure comprised of two or three line_3: "knots" surrounded by an additional halo of extended emission. line_4: The central goal of this program is to determine whether the line_5: morphology of the system is that of two or more well formed line_6: interacting galaxies, or the unknown but presumably line_7: amorphous appearance of a galaxy in the process of forming. It line_8: is clear that to answer this question image restoration will be line_9: required to alleviate the problem of the degraded HST image line_10: quality. ! question: 7 section: 2 line_1: One of us (NW) has extensive experience in using Maximum line_2: Entropy techniques to restore images obtained with HST (Weir line_3: and Djorgovski, 1990a,b - see Phase I proposal for references line_4: and figures). Weir has also developed (Weir, 1992) an line_5: extension of the Maximum Entropy image reconstruction line_6: technique that explicitly provides for structures at several line_7: spatial scales. The comparison of the "classical" Maximum line_8: Entropy reconstruction with the multi-channel Maximum line_9: Entropy restoration of simulated image data is shown in figure line_10: 2 of our Phase I proposal, where the signal to noise in the line_11: simulated data is approximately the same as we expect in the line_12: images we propose to obtain here. Fundamentally the multi- line_13: channel technique chooses the lowest spatial frequency line_14: structure that adequately represents the data, invoking higher line_15: spatial frequencies only when they provide clearly superior line_16: modeling of the data. This approach will be ideal for line_17: extracting the maximum reliable information from the raw line_18: frames that will have the complex structure of the source line_19: convolved with the HST PSF. We shall use the STScI tool TINY line_20: TIM to generate model HST PSF's, as well as using our PSF line_21: calibration observation both as a template PSF and as a test of line_22: our ability to perform the deconvolution successfully. ! question: 9 section: 1 line_1: Imaging of a Complete Sample of the Nearest Infrared Quasars line_2: - (D.Sanders U. Hawaii, PI, B.T. Soifer, G. Neugebauer Co-I's) - line_3: this project is not directly related to the current project. line_5: Werner (Co-I) is a Co-I on program P-2595: "The Luminosity line_6: Function of the Trapezium Cluster" (J. Stauffer, PI) This line_7: program is not related to the present proposal. line_9: Observations from both of the above proposals have been line_10: obtained and are being analyzed. No results have yet been line_11: published. ! question: 10 section: 1 line_1: Sun Workstations at Caltech and JPL line_3: We have state of the art image processing software line_4: that will be used for processing HST images, including line_5: the multi-channel MaxEnt image restoration package line_6: developed by Nick Weir. ! !end of general form text general_form_address: lname: Soifer fname: Baruch mi: T category: PI inst: Caltech addr_2: MAIL CODE 320 47 addr_3: 1201 EAST CALIFORNIA BOULEVARD city: Pasadena state: CA zip: 91125 country: USA phone: (818)395-6626 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: IRAS10214+4724F descr_1: E,319,322,325,918,920 pos_1: RA = 10H 21M 31.14S +/- 0.5", pos_2: DEC = +47D 24' 22.9" +/- 0.5" equinox: 1950 rv_or_z: Z = 2.286 comment_1: CENTRAL SURF. BRIGHTNESS EST. FROM comment_2: R=20.5 IN ROWAN ROBINSON ET AL 1991 comment_3: + GUESS THAT HALF LIGHT IN CENTRAL comment_4: 1". EST FOR 1-4" DIAM EXTENDED comment_5: STRUCTURE IS THEN AVG. SURF(R)=23.7 comment_6: SURF-CONT VALUES FROM comment_7: 1992 ROWAN ROBINSON ET AL PREPRINT. fluxnum_1: 1 fluxval_1: SURF(R)=21.0 +/- 0.5 fluxnum_2: 2 fluxval_2: SURF-CONT(7500)= 6 +/- 3 E-18 fluxnum_3: 3 fluxval_3: SURF-CONT(8000)= 6 +/- 3 E-18 fluxnum_4: 4 fluxval_4: SURF-CONT(8500)= 6 +/- 3 E-18 fluxnum_5: 5 fluxval_5: SURF-CONT(9000)= 7 +/- 3 E-18 fluxnum_6: 6 fluxval_6: SURF-CONT(9500)= 8 +/- 4 E-18 fluxnum_7: 7 fluxval_7: SURF(R)=23.7 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: IRAS10214+4724F config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F814W num_exp: 1 time_per_exp: 2200.00S s_to_n: 8 s_to_n_time: 2200S fluxnum_1: 4 priority: 1 param_1: CR-SPLIT = NO req_1: SEQ 1-3 NO GAP; req_2: POS TARG +0.000, +0.000; req_3: CYCLE 4 / 1-3; req_4: SAME ORIENT FOR 2-3 AS 1; comment_1: ADJUST EXP TIME +INFINITY/-10% TO FIT comment_2: IN AN ALIGNMENT. comment_4: FOR ALL 3 EXPOSURES USE OPTIMUM comment_5: CENTER SUBJECT TO KEEPING STAR 13.3"W comment_6: OF TARGET ON PC1 AS PSF MONITOR. ! linenum: 2.000 targname: IRAS10214+4724F config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F814W num_exp: 1 time_per_exp: 2200.00S s_to_n: 8 s_to_n_time: 2200S fluxnum_1: 4 priority: 1 param_1: CR-SPLIT = NO req_1: POS TARG +0.230, +0.460; comment_1: ADJUST EXP TIME +INFINITY/-10% comment_2: TO FIT IN AN ALIGNMENT. comment_3: SMALL POS TARG OFFSETS USED comment_4: FOR HELP IN OVERCOMING HOT comment_5: PIXELS, ETC. ! linenum: 3.000 targname: IRAS10214+4724F config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F814W num_exp: 1 time_per_exp: 2200.00S s_to_n: 8 s_to_n_time: 2200S fluxnum_1: 4 priority: 1 param_1: CR-SPLIT = NO req_1: POS TARG +0.460, -0.230; comment_1: ADJUST EXP TIME +INFINITY/-10% comment_2: TO FIT IN AN ALIGNMENT. comment_3: SMALL POS TARG OFFSETS USED comment_4: FOR HELP IN OVERCOMING HOT comment_5: PIXELS, ETC. ! ! ! end of exposure logsheet ! No scan data records found