! File: 4575C.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: CYCLE3 HIGH sci_cat: GALAXIES & CLUSTERS sci_subcat: DISTANT GALAXIES proposal_for: GO pi_fname: BARUCH pi_mi: T pi_lname: SOIFER pi_inst: CALTECH pi_country: US hours_pri: 3.33 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 underlyinggalaxy(s) on a 1 Kpc line_8: scale and thereby clarify whether this is an line_9: interaction between two or more well formed gas rich galaxies or is line_10: a galaxy in the process of formation. Such a line_11: determination will help establish whether the power source of this line_12: system is a dust enshrouded quasar line_13: or star formation in a 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. The original proposal called for line_3: filter F675W, but after careful reconsideration of the target line_4: spectrum and available filters we have chosen to work with line_5: the F725LP filter instead. This filter has similar throughput line_6: to F675W but our object rises sharply between 0.8 and 1.0 line_7: microns, so the signal level will be higher for a given line_8: integration time. Because we will be limited by read noise, line_9: our intent is to maximize the individual exposure times for line_10: the individual PC exposures, and stack individual exposures. line_11: With our allocation of 5.03 hours of observing time, line_12: accounting for acquisition setup time this should permit a line_13: total of about 213 minutes of integration. This should be 4 line_14: exp of about 37 min and 2 of 33 min. While one 30 min. and line_15: 5 37 min. exp would seem more efficient, with the shorter one line_16: allowing for initial GS acq., the resource estimator disagrees. line_17: We want to group the 6 exposures into three pairs at slightly line_18: different positions. The two exposures at each position line_19: should allow good cosmic ray detection, while the three line_20: positions should reduce the effects of blemishes in the chip line_21: on the data. Because at the long effective wavelength of line_22: F725LP the 0.043" PC pixel size is nearly fully sampling the line_23: diffraction pattern, it should be easier to distinguish real ! question: 3 section: 2 line_1: stars from single pixel CR's than is often the case. Therefore line_2: for the case of 6 exposures we favor reducing the number of line_3: exposures per position to 2 at 3 positions rather than 3 line_4: exposures at 2 positions because this will ensure that no line_5: more than 1/3 of the data is lost due to a blemish. These line_6: positions should all have different X coords because of the bad line_7: column in PC 6, and an equilateral triangle with 11 pixel line_8: (0.5") sides, tilted so that all three positions have different line_9: row and columns should be adequate. No special orientation line_10: wrt N or E is needed, however the star "B" 28" E and 25" S of line_11: our target may potentially be bright enough to cause charge line_12: bleeding, therefore it should not fall on PC 6. This should not line_13: be a problem as these distances will result in a minimum line_14: column or row separation of over 600 pixels from the target. line_15: On the other hand the star "A" 13" east of our target should line_16: fall on PC6 to provide a PSF monitor on the long target line_17: exposure frames. The background levels per pixel in 40 line_18: minutes are expected to be 37 e- or more and therefore line_19: preflashing will not be necessary to avoid trapped charge. line_20: This results in less overhead and the noise will be lower. line_21: Because F725LP is not commonly used and morphology is the line_22: crux of our proposal, a PSF calibration with F725LP is needed. line_23: An M0 star has approximately the same spectral shape as our ! question: 3 section: 3 line_1: target within F725LP. This should be done close in time to the line_2: target exposures to avoid any OTA focus change between the line_3: calibration and target observations (within 6 hours maximum, line_4: ideally immediately following, or slightly less desirably, line_5: preceding, the target observations), and also within several line_6: degrees of the target so that the OTA orientation is similar line_7: for both observations. Both target and PSF cal observations line_8: must be done with fine lock, even though the PSF cal exposure line_9: will only last 0.6 second. The PSF cal star position should be line_10: at the center of the equilateral triangle of three target line_11: positions. ! 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: To minimize time variations in the PSF, we request that the line_2: PSF calibration observation (see question 6) be obtained line_3: within a maximum of six hours of the target observations, and line_4: preferably immediately following or preceding the target line_5: observations. (Preceding is slightly less preferable because line_6: of the possibility of over exposure on the PSF star.) We have line_7: selected the M0 star HIC 53637 for the PSF calibration. This line_8: star is within 10 degrees of our main target, so it will line_9: provide a PSF calibration with a similar telescope orientation line_10: to the main target observation. line_12: We also require all exposures to be contiguous to minimize PSF line_13: variations. line_15: We require slight repositioning of the target to three distinct line_16: locations separated by 0.5" (several pixels) in the xy frame of line_17: PC 6 to ensure that blemishes do not degrade more than one line_18: third of the data at any spatial point. The orientation of these line_19: positions on the sky is irrelevant and therefore this should line_20: not create any additional scheduling restrictions. ! question: 6 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, and line_3: because F725LP is not a standard filter with frequent PSF line_4: calibrations, we must obtain a PSF calibration on a star with line_5: similar color to our object in F725LP. We have selected the line_6: M0 star HIC 53637 for this observation, because of its color, line_7: magnitude (to allow good signal levels in 0.5-1 sec integration), line_8: and position within 10 degrees of our target. Because we will line_9: always be read noise limited and our target is extremely faint line_10: we require the longest possible uninterrupted exposure times line_11: to achieve the best S/N for our allocated time. This is line_12: particularly necessary if we are to detect tidal tails or other line_13: signs of a merger which may be at very low surface line_14: 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)356-6626 ! ! 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 ! targnum: 2 name_1: BD+49D2004-CALIB name_2: HIC53637 descr_1: J,704,A,141 pos_1: RA = 10H 58M 23.739S +/- 0.19", pos_2: DEC = +48D 17' 17.28" +/- 0.19" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.006212 ra_pm_unct: 0.002505 dec_pm_val: -0.0810 dec_pm_unct: 0.0250 comment_1: PSF STAR SELECTED TO MATCH TARGET comment_2: COLOR, GIVE GOOD SIGNAL IN 0.5-1SEC comment_3: AND BE W/IN 10DEG OF TARGET SO comment_4: SAME OTA ORIENTATION AND comment_5: CLOSE SCHEDULING IN TIME. fluxnum_1: 1 fluxval_1: V=10.523 +/- 0.009, TYPE=M0 fluxnum_2: 2 fluxval_2: B-V=1.367 +/- 0.005 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: IRAS10214+4724F config: PC opmode: IMAGE aperture: PC6 sp_element: F725LP num_exp: 2 time_per_exp: 2000.00S s_to_n: 8 s_to_n_time: 2200S fluxnum_1: 4 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: SEQ 1-3 NO GAP; req_2: POS TARG +0.00, +0.00; req_3: CYCLE 3 / 1-4; comment_1: ADJUST EXP TIME +INFINITY/-10% TO FIT comment_2: IN AN ALIGNMENT. 2EXP/POS FOR CR comment_3: DETECTION. PRE-FLASH NOT NEEDED BUT comment_4: IF SCHEDULING RESULTS IN DARK TIME comment_5: AND ECLIPTIC LATITUDE >~40DEG SKY comment_6: MAY BE DARK ENOUGH TO NEED PRE-FLASH. ! linenum: 2.000 targname: IRAS10214+4724F config: PC opmode: IMAGE aperture: PC6 sp_element: F725LP num_exp: 2 time_per_exp: 2200.00S s_to_n: 8 s_to_n_time: 2200S fluxnum_1: 4 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: POS TARG +0.353, +0.354 comment_1: ADJUST EXP TIME +INFINITY/-10% comment_2: TO FIT IN AN ALIGNMENT. comment_3: SECOND POS TO AVOID BLEMISHES comment_4: FOR ALL 3 POS USE OPTIMUM comment_5: CENTER SUBJECT TO KEEPING STAR 13.3"W comment_6: OF TARGET ON PC6 AS PSF MONITOR. ! linenum: 3.000 targname: IRAS10214+4724F config: PC opmode: IMAGE aperture: PC6 sp_element: F725LP num_exp: 2 time_per_exp: 2200.00S s_to_n: 8 s_to_n_time: 2200S fluxnum_1: 4 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: POS TARG +0.483, -0.129 comment_1: ADJUST EXP TIME +INFINITY/-10% comment_2: TO FIT IN AN ALIGNMENT. comment_3: THIRD POS TO AVOID BLEMISHES ! linenum: 4.000 targname: BD+49D2004-CALIB config: PC opmode: IMAGE aperture: PC6 sp_element: F725LP num_exp: 1 time_per_exp: 0.60S s_to_n: 40 s_to_n_time: 0.6S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT = NO param_2: PRE-FLASH = YES req_1: POS TARG +0.279, +0.075; req_2: CALIB FOR 1-3; req_3: GROUP 1-4 WITHIN 12H; comment_1: EXP TIME SET ~2E4E- PEAK. S/N PER PIX comment_2: EST AT 0.5" RAD (10% PK). PREFER PSF comment_3: CAL IMMED. FOLLOW TARGET EXPOSURES. comment_4: USE THE SAME ZERO POS FOR TARG SO PSF comment_5: IS NR CNTR OF 3 TARGET POSITIONS. USE comment_6: FINE LOCK SO SAME PNTNG ERRS AS TARG. ! ! end of exposure logsheet ! No scan data records found