! File: 3685C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:16:14:27 coverpage: title_1: MORPHOLOGY OF DISTANT GALAXIES sci_cat: GALAXIES & CLUSTERS sci_subcat: FAINT GALAXIES proposal_for: AUG/OS pi_title: PROF. pi_fname: IVAN pi_mi: R. pi_lname: KING pi_inst: UNIVERSITY OF CALIFORNIA, BERKELEY pi_country: USA pi_phone: (510)642-2206 keywords_1: DISTANT GALAXY, DISTANT GALAXY CLUSTER hours_pri: 8.67 hours_par: 8.67 num_pri: 4 num_par: 4 wf_pc: Y foc: Y pi_position: PROF. OF ASTRONOMY ! end of coverpage abstract: line_1: This is a proposal to study the morphology of distant galaxies, a line_2: field that has lagged far behind what has been learned from line_3: spectroscopic work. The targeted galaxies all have been extensively line_4: observed from the ground. line_5: Nearly all are in the redshift range line_6: 0.24-0.65. Ground-based data include broad-baseline 4-color line_7: photometry and, in nearly all cases, redshifts. The targets include line_8: a rich X-ray cluster that is surprisingly deficient in blue galaxies, line_9: and three other fields that each have numerous galaxies that have line_10: been richly observed from the ground. Each field will be observed line_11: with the WFC, while a parallel observation observes a similarly line_12: well-studied galaxy with the FOC at greater resolving power. line_13: These observations will take the first crucial step toward line_14: investigating the morphology of the rich sample of medium-redshift line_15: galaxies in the Koo-Kron redshift surveys. ! ! end of abstract general_form_proposers: lname: KING fname: IVAN title: PROF. mi: R. inst: UNIV. OF CALIFORNIA country: U.S.A. ! lname: MACKAY fname: CRAIG title: DR. mi: D. inst: UNIVERSITY OF CAMBRIDGE country: U.K. esa: Y ! lname: CRANE fname: PHILIPPE title: DR. inst: EUROPEAN SOUTHERN OBSERVATORY country: GERMANY ! lname: KOO fname: DAVID title: DR. mi: C. inst: LICK OBSERVATORY, UNIV OF CALIFORNIA country: U.S.A. ! lname: KRON fname: RICHARD title: DR. mi: G. inst: UNIVERSITY OF CHICAGO country: U.S.A. ! ! end of general_form_proposers block general_form_text: question: 2 section: 0 line_1: ! question: 3 section: 0 line_1: (1) SA68.2-T2-1-2, FOC; par CL0016+16, WFC+F785LP; 175M line_2: (2) SA68.17123, FOC; par rich field, WFC+F785LP; 117M line_3: (3) SA68.12760, FOC; par rich field, WFC+F785LP; 117M line_4: (4) SA68.8624, FOC; par rich field, WFC+F785LP; 117M line_5: All FOC exposures are F/48 with F130LP. line_7: NOTE: The parallel exposures are scientifically more important, line_8: but the FOC is taken as primary SI in order to insure better line_9: pointing with it. line_11: These targets (except the first, to which the TAC gave highest line_12: priority) have been changed since the Phase 1 proposal. This change line_13: better furthers the original scientific purpose: each WFC field line_14: contains a large number of galaxies with 4 ground-based colors and line_15: known redshifts, while the FOC exposure provides higher resolution line_16: on a similarly well-studied galaxy. ! question: 4 section: 0 line_1: This entire program is dependent on the superior resolving power of line_2: HST, whose applicability has been demonstrated by SAO Program 3121. line_3: All objects have been observed exhaustively from the ground. ! question: 5 section: 0 line_1: Program SAO-3121 demonstrated that much can be done with a line_2: single-orbit exposure but that the fainter galaxies require a line_3: longer exposure time. In addition, by moving from F555W to F785LP line_4: we shift our observations to a wavelength that is optimized for the line_5: galaxies of redshift around 0.5. line_7: Cl0016+16 gets the longest exposure, becuse it is the most line_8: important target. The other fields, with nearly 4 times the line_9: exposure of SAO-3121, should also give good morphology. line_11: In comparison with the somewhat marginal results achieved with the line_12: FOC48 in SAO-3121, we choose a longer exposure and the widest line_13: possible band. Since there is no danger of overflowing the line_14: 255-count pixel capacity, we choose the doubled field size. ! question: 6 section: 1 line_1: Note that all FOC exposures have parallel WFC exposures (so that line_2: the true efficiency of HST usage is much higher than indicated by line_3: the percentage on the cover page). ORIENT is a requirement on all line_4: primary exposures, in order to get the indispensable WFC fields. ! question: 6 section: 2 line_1: It is assumed that PSF's will be available without the need to add line_2: observations to this program to secure them. ! question: 7 section: 1 line_1: At Berkeley are a VMS cluster and a Sun cluster. King has a line_2: Microvax II GPX and a Sun IPC with a gigabyte disk. For software he line_3: has been using Vista, DAOPHOT, and IRAF/STSDAS. line_5: At Santa Cruz Koo has one RA to help with analysis. They have a very line_6: extensive SUN, Silicon Graphics, IBM, and VAX cluster system. Koo line_7: personally has one SUN 4/110 and SUN Sparc 1+ with 1.6 Gbyte of line_8: disk. At UCSC there is good WF/PC expertise, with Faber and her line_9: team; Koo is a former WF/PC Instrument Scientist; and he and Garth line_10: Illingworth are co-I's with R. Griffiths as PI on the Medium Deep line_11: Survey Key Project to study distant galaxy morphology. line_13: At the University of Chicago, Kron has a Sun Sparcstation and 1.2 line_14: Gbytes of disk storage. Very extensive experience in image line_15: reduction has been obtained in the environment of FOCAS running line_16: under IRAF. At Fermilab, Kron has a cluster of Silicon Graphics line_17: machines, plus several gigabytes of disk storage. IRAF has been line_18: installed, and several other software packages for image reduction line_19: are in the process of being evaluated. (This activity is in the line_20: context of a development effort for a new "Digital Sky Survey" to be line_21: undertaken with Princeton, the Institute for Advanced Study, and the line_22: University of Chicago.) ! question: 7 section: 2 line_1: In addition, for ground-based follow-up, King and Koo have access to line_2: the UCO Lick 2.5m and Keck 10m telescopes, Kron to the ARC 3.5m, line_3: Crane to all the facilities of ESO, and Mackay to the 4.2m and 2.4m line_4: telescopes at La Palma. line_6: The images will be restored at Berkeley, with Fourier and line_7: Richardson-Lucy techniques, and probably by the era of Cycle 2 with line_8: the MEMSYS MaxEnt program of that time. (The latter will be done at line_9: STScI if the software is not available at Berkeley.) Further study line_10: and analysis will consist of morphological study by Koo and Kron, line_11: who have collaborated extensively on such projects for many years. line_13: Mackay has access to the extensive astronomical computing facilities line_14: at Cambridge, and Crane to the very large complex at ESO. ! question: 9 section: 1 line_1: Previous HST observing time: line_3: SAO-3121, MORPHOLOGY OF FAINT GALAXIES - PART II line_4: GTO-1277, IMAGING OF M31-GROUP GALAXIES line_5: GTO-1278, SPECTROSCOPY OF THE CENTERS OF M31, M32, AND NGC 205 line_6: GTO-1279, STRUCTURE OF GLOBULAR CLUSTERS line_7: GTO-1280, COLLAPSED CORES OF GLOBULAR CLUSTERS line_8: GTO-1281, THE FAINT POPULATION IN BAADE'S WINDOW line_9: GTO-1282, IMAGING OF HIGH-REDSHIFT FIELD GALAXIES AND CLUSTERS line_10: GTO-3217, (continuation of 1280) line_11: GTO-3218, (continuation of 1279) line_12: GTO-3219, (continuation of 1277) line_13: GTO-3325, (continuation of 1279, 3218) line_15: The only one of the above that is closely related to this proposal is 3121. line_16: The main part of the project is finished and published. Some additional study line_17: will be done by Koo and Kron, however. line_19: Koo is a Co-I in the "Medium Deep Survey" Key project. That is a broad line_20: exploratory survey, however, whereas the present proposal is specifically aimed line_21: at galaxies for which there is already extensive ground-based information. line_23: Crane has GTO programs, none of which impinge on the present proposal. ! question: 9 section: 2 line_1: Main results from previous related programs: line_3: 3121 produced a report that I am told was quite useful to the Cycle line_4: 1 Re-TAC, and also the publication below. line_6: Otherwise all I have gotten up to now is a pair of exposures on the line_7: center of Omega Centauri, which are in the early stages of line_8: reduction, along with exposures of the center of M32 and of the line_9: collapsed-core globular cluster NGC7099. line_11: In Cycle 1 I have put all of 1281 and all of the 1279 exposures on line_12: NGC6624. ! question: 9 section: 3 line_1: Publications resulting from the above: line_3: "The Current Ability of HST to Reveal Morphological Structure in line_4: Medium-Redshift Galaxies", King, I.R., et al. (8 other authors), line_5: Astron. J., 102, 1553, 1991. ! question: 10 section: 0 line_1: Hardware/software as above. Postdoc + RA's. GTO funding (from line_2: NASA). ! !end of general form text general_form_address: lname: KING fname: IVAN mi: R. title: PROF. category: PI inst: UNIVERSITY OF CALIFORNIA, BERKELEY addr_1: ASTRONOMY DEPARTMENT addr_2: UNIVERSITY OF CALIFORNIA city: BERKELEY state: CA zip: 94720 country: U.S.A. phone: (510)642-2206 telex: (910)366-7114 from_date: 15-MAR-92 to_date: 31-DEC-99 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SA68.2-T2-1-2 descr_1: I,603 pos_1: RA=00H 15M 27.0S+/-.1S, pos_2: DEC=+16D 12' 46"+/-1" equinox: 1950 rv_or_z: Z=0.30 ! targnum: 2 name_1: CL0016+16 descr_1: F,404 pos_1: RA=00H 15M 58.32S +/- 0.1S, pos_2: DEC=+16D 09' 37" +/- 1" equinox: 1950 ! targnum: 3 name_1: SA68.17123 descr_1: I,603 pos_1: RA=00H 14M 44.2S+/-.1S, pos_2: DEC=+15D 50' 25"+/-1" equinox: 1950 ! targnum: 4 name_1: SA68.13837 descr_1: F,403 pos_1: RA=00H 14M 42.6S +/- 0.1S, pos_2: DEC=+15D 43' 42" +/- 1" equinox: 1950 ! targnum: 5 name_1: SA68.12760 descr_1: I,603 pos_1: RA=00H 13M 55.0S+/-.1S, pos_2: DEC=+15D 41' 50"+/-1" equinox: 1950 ! targnum: 6 name_1: SA68.8624 descr_1: F,403 pos_1: RA=00H 14M 00.5S +/- 0.1S, pos_2: DEC=+15D 35' 30" +/- 1" equinox: 1950 ! targnum: 7 name_1: SA68.6024 descr_1: I,603 pos_1: RA=00H 15M 13.6S+/-.1S, pos_2: DEC=+15D 31' 03"+/-1" equinox: 1950 ! targnum: 8 name_1: SA68.5658 descr_1: F,403 pos_1: RA=00H 14M 46.2S +/- 0.1S, pos_2: DEC=+15D 30' 37" +/- 1" equinox: 1950 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: SA68.2-T2-1-2 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F180LP num_exp: 1 time_per_exp: 175M priority: 1 req_1: ORIENT 88.0D +/- 0.1D; req_2: CYCLE 2 /1-8 ! linenum: 2.000 targname: CL0016+16 config: WFC opmode: IMAGE aperture: ALL sp_element: F785LP num_exp: 1 time_per_exp: 175M priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PAR comment_1: INTENDED TO BE PARALLEL WITH 1 ! linenum: 3.000 targname: SA68.17123 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F180LP num_exp: 1 time_per_exp: 117M priority: 1 req_1: ORIENT 153.3D +/- 0.1D ! linenum: 4.000 targname: SA68.13837 config: WFC opmode: IMAGE aperture: ALL sp_element: F785LP num_exp: 1 time_per_exp: 117M priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PAR comment_1: INTENDED TO BE PARALLEL WITH 3 ! linenum: 5.000 targname: SA68.12760 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F180LP num_exp: 1 time_per_exp: 117M priority: 1 req_1: ORIENT 138.2D +/- 0.1D ! linenum: 6.000 targname: SA68.8624 config: WFC opmode: IMAGE aperture: ALL sp_element: F785LP num_exp: 1 time_per_exp: 117M priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PAR comment_1: INTENDED TO BE PARALLEL WITH 5 ! linenum: 7.000 targname: SA68.6024 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F180LP num_exp: 1 time_per_exp: 117M priority: 1 req_1: ORIENT 236.2D +/- 0.1D ! linenum: 8.000 targname: SA68.5658 config: WFC opmode: IMAGE aperture: ALL sp_element: F785LP num_exp: 1 time_per_exp: 117M priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PAR comment_1: INTENDED TO BE PARALLEL WITH 7 ! ! end of exposure logsheet ! No scan data records found