! File: 2695C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:10:25:13 coverpage: title_1: MORPHOLOGY OF PKS 1614+051, A QUASAR-GALAXY PAIR AT Z=3.21 sci_cat: QUASARS & AGN proposal_for: GO pi_title: P.I. pi_fname: S. pi_lname: DJORGOVSKI pi_inst: CALTECH pi_country: USA pi_phone: (818)-356-4415 keywords_1: QUASARS-HIGH-REDSHIFT-GALAXIES-GALAXY INTERACTIONS- keywords_2: GALAXY FORMATION. hours_pri: 7.90 num_pri: 1 wf_pc: X funds_amount: 77131 funds_length: 27 funds_date: JUN-91 pi_position: ASSOCIATE PROFESSOR off_fname: DR. EARL off_lname: FREISE off_title: DIR., SPONS. RESCH. off_inst: CALTECH off_addr_1: MS 213-06,CALTECH off_city: PASADENA off_state: CA, off_zip: 91125 off_country: USA off_phone: (818)-356-4415 off_telex: 188192 OR 675425 ! end of coverpage abstract: line_1: The galaxy companion to the quasar PKS 1614+051 at z = 3.21 is one of the most line_2: distant non-QSO objects known. Ground-based observations suggest that the line_3: quasar and its galaxy companion are interacting, and that the galaxy may harbor line_4: an active nucleus. This putative interaction occurs at an epoch when quasars line_5: first appear in large numbers, and we may be witnessing an event responsible line_6: for the turn-on of the quasar activity in this system. The redshift of this line_7: system implies that it is less than 20% the current age of the universe, giving line_8: us a unique opportunity to study the star formation history and stellar line_9: population of a young and possibly forming galaxy, or a compact group of line_10: galaxies. High-resolution imaging with the HST will reveal the nature of the line_11: interaction between the companion and the quasar, and allow us to address basic line_12: questions of the nature and evolution of galaxies at extremely high redshifts, line_13: and the origins of galactic activity in the early universe. We propose line_14: imaging in the band containing the Ly alpha emission line, as well as in a line_15: broad-band line-free band to sample the stellar continuum. ! ! end of abstract general_form_proposers: lname: DICKINSON fname: M. inst: CALIFORNIA, UNIVERSITY OF, BERKELEY country: USA ! lname: STRAUSS fname: M. inst: CALTECH country: USA ! lname: WEIR fname: N. inst: CALTECH country: USA ! lname: THOMPSON fname: D. inst: CALTECH country: USA ! lname: SMITH fname: J. inst: CALTECH country: USA ! lname: SPINRAD fname: H. inst: CALIFORNIA, UNIVERSITY OF, BERKELEY country: USA ! lname: DJORGOVSKI fname: S. title: P.I. inst: CALTECH country: USA ! lname: MCCARTHY fname: P. inst: OCIW country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: This revised proposal reflects our reassessment and suggested modifications of line_2: the original proposal, and resulting recommendations by the TAC. The changes in line_3: the scope of the proposal are as follows: Instead of exposures in a narrow line_4: band centered on the redshifted Ly alpha emission line, which are now rendered line_5: impractical, we propose to use a broad-band V filter (F555W), which contains line_6: the Ly alpha line, and some continuum as well. We also decided to eliminate any line_7: FOC/96 exposures, and replace them and the red-continuum PC exposures with an line_8: alternative set of PC exposures with F850LP, which should sample the line-free line_9: continuum, and provide a good color baseline relative to the V band. Since the line_10: PC exposures provide more signal per unit time than the FOC/96 exposures, and line_11: there is no instrument setup change (all of our exposures are with PC6, line_12: which has the best-behaved PSF), there is some time saving. With PC6 + F555W, line_13: we wish to obtain one exposure each of 5 and 10 minutes, two of 20, and six line_14: exposures of 30 minutes. With PC6 + F850LP, we wish to obtain one exposure each line_15: of 10 and 20 minutes, two of 30 minutes, and two of 2000 sec. The shorter line_16: exposures are intended to assure that we will have some unsaturated images of line_17: the quasar itself; the longer ones are intended to add up the S/N for the line_18: fainter components of the system. This also automatically takes care of the line_19: CR redundancy. The total net exposure time is thus 6.861 hours. According to the line_20: RPSS resource estimator, the total spacecraft time is 7.894 hours, and the net line_21: efficiency is thus 86.9 %. ! question: 4 section: 1 line_1: We have already pursued the ground-based optical imaging and spectroscopy as line_2: far as is practical with 3 to 5-m class telescopes. We also have high-quality line_3: VLA maps, and are obtaining more high-resolution spectra and near-IR images. line_4: The understanding of this unique system is now limited only by the seeing. line_5: At this redshift, 1 PC pixel corresponds to about 200 h-1 pc, which should line_6: enable us to explore the morphology of the continuum, ionized gas, and star line_7: formation on subgalactic scales. ! question: 5 section: 1 line_1: Assuming the integration times and instrument setups described in question 3, line_2: our estimates of the S/N, using the Handbook, the Preliminary Report on HST line_3: Performance for Cycle 1 GO's, and the materials provided at the recent STScI line_4: workshop, with the increase factor t = 5, give the range S/N ~ 10 - 30 line_5: for putative individual bright emission regions in the system. For the line_6: galaxy companion of PKS 1614+051 we obtain S/N ~ 50 - 80 integrated line_7: over the whole object. ! question: 7 section: 1 line_1: We have working image processing and data analysis packages at our home line_2: institutions, including a superb Maximum Entropy image restoration package, line_3: which was exported to the STScI, and assorted other software (Lucy, Wiener, line_4: and other methods). We have done extensive image restoration experiments, line_5: using both real and simulated HST data. We are confident that we can restore line_6: the effective angular resolution of the HST images comparable to those line_7: proposed here down to the angular resolution of about 0.1 arcsec, with the line_8: photometric distortions well understood. ! question: 10 section: 1 line_1: Our institutions have extensive computing and other research facilities line_2: (libraries, etc.), and there is no shortage of additional graduate students line_3: which can participate in this project. Along with the support requested line_4: with the present proposal, we should have quite adequate resources to line_5: analyse the data and publish the results very rapidly. ! !end of general form text general_form_address: lname: DJORGOVSKI fname: S. mi: G. title: PROF. category: PI inst: CALIF. INSTITUTE OF TECHNOLOGY addr_1: MS 105-24 city: PASADENA state: CA zip: 91125 country: USA ! lname: DJORGOVSKI fname: S. title: PROF. category: PI inst: CALTECH addr_1: ASTRONOMY, MS 105-24 addr_2: CALTECH city: PASADENA state: CA zip: 91125 country: USA phone: 818-356-4415 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PKS1614+051 descr_1: GALAXY; QUASAR COMPANION pos_1: RA = 16H 14M 09.2S +/- 1", pos_2: DEC = +05D 06' 57" +/- 1" equinox: 1950 pm_or_par: N rv_or_z: Z = 3.215 comment_1: FAINT GALAXY 6.5 ARCSEC FROM comment_2: AN 18 MAG QUASAR. BOTH OBJECTS comment_3: SHOULD BE INCLUDED IN THE SAME comment_4: CCD FRAMES. THE COORDINATES comment_5: GIVEN ARE FOR THE MID-POINT comment_6: BETWEEN THE TWO OBJECTS. fluxnum_1: 1 fluxval_1: R = 24.0 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PKS1614+051 config: PC opmode: IMAGE aperture: P6 sp_element: F555W num_exp: 1 time_per_exp: 300S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 comment_1: FAINT GALAXY 6.5 ARCSEC FROM comment_2: AN 18 MAG QUASAR. BOTH OBJECTS comment_3: SHOULD BE INCLUDED IN THE SAME comment_4: CCD FRAMES. THE COORDINATES comment_5: GIVEN ARE FOR THE MID-POINT comment_6: BETWEEN THE TWO OBJECTS. ! linenum: 2.000 targname: PKS1614+051 config: PC opmode: IMAGE aperture: P6 sp_element: F555W num_exp: 1 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ! linenum: 3.000 targname: PKS1614+051 config: PC opmode: IMAGE aperture: P6 sp_element: F555W num_exp: 2 time_per_exp: 1200S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ! linenum: 4.000 targname: PKS1614+051 config: PC opmode: IMAGE aperture: P6 sp_element: F555W num_exp: 6 time_per_exp: 1800S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ! linenum: 5.000 targname: PKS1614+051 config: PC opmode: IMAGE aperture: P6 sp_element: F850LP num_exp: 1 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ! linenum: 6.000 targname: PKS1614+051 config: PC opmode: IMAGE aperture: P6 sp_element: F850LP num_exp: 2 time_per_exp: 1200S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ! linenum: 7.000 targname: PKS1614+051 config: PC opmode: IMAGE aperture: P6 sp_element: F850LP num_exp: 4 time_per_exp: 1900S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 1 ! ! end of exposure logsheet ! No scan data records found