! $Id: 5304,v 5.1 1994/07/27 16:22:21 pepsa Exp $ coverpage: title_1: QSO ABSORPTION-SELECTED GALAXIES IN THE FIELD OF 3C336--CYCLE 4 HIGH sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: GO pi_fname: CHARLES pi_mi: C. pi_lname: STEIDEL pi_inst: 2630 pi_country: USA pi_phone: 617-253-5084 hours_pri: 7.62 num_pri: 2 wf_pc: Y fos: Y off_fname: DAVID off_lname: HARRIGAN off_title: ASSOC. DIRECTOR, OSP off_inst: 2630 off_addr_1: OFFICE OF SPONSORED PROJECTS off_addr_2: MIT, RM. E19-719 off_addr_3: 77 MASSACHUSETTS AVE. off_city: CAMBRIDGE off_state: MA off_zip: 02139 off_country: USA off_phone: 617-253-2495 ! end of coverpage abstract: line_1: We propose to obtain high resolution WFPC2 images of the field of 3C line_2: 336, a quasar with z=0.927 in whose spectrum 3 foreground MgII line_3: absorption systems with z= 0.472, 0.656, and 0.892 are known, making it line_4: the richest field in a nearly completed survey for absorption--selected line_5: galaxies which we have been conducting using ground-based observations. line_6: Optical and infrared colors, magnitudes, positions, and redshifts have line_7: already been measured; based upon the unusually small impact parameters line_8: of two of these galaxies (z=0.656,0.892) with the line of sight to the line_9: quasar, and the very strong absorption lines observed in the optical line_10: spectra, we can predict with some certainty that they are galaxies line_11: which are producing damped Lyman alpha lines. Using FOS spectra line_12: of the QSO aimed at measuring HI column densities in these two systems line_13: (together with ground- based spectra aimed at detecting ZnII and CrII line_14: absorption lines) and the high resolution WFPC2 images, it will be line_15: possible to establish chemical abundances, dust content, and kpc-scale line_16: morphology for the same galaxies, providing an unprecedentedly complete line_17: picture of apparently normal galaxies at lookback times of one--half line_18: the age of Universe. The fact that there are three absorbing galaxies line_19: in a single field makes the imaging observation a particularly line_20: efficient one for HST. ! ! end of abstract general_form_proposers: lname: STEIDEL fname: CHARLES mi: C. inst: 2630 country: USA ! lname: DICKINSON fname: MARK mi: E. inst: 3470 country: USA ! lname: MEYER fname: DAVID mi: M. inst: 3020 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: FOS spectra using FOS/RD and G190H and G270H wil be obtained of line_2: the quasar 3C336. The object will be observed through the 1.0 aperture line_3: acquiring using an ACQ/BINARY sequence. Exposures of length 3600s line_4: and 2700s, for G190H and G270H, respectively, will line_5: be obtained, in the ACCUM mode. line_6: WFPC-2 observations of the field of 3C336, centering on the line_7: WF2-FIX aperture. We have requested a special ORIENT line_8: of 100 degrees in order to avoid blooming of the bright quasar in line_9: the direction of one of the faint galaxies of interest, and to include line_10: as many galaxies of interest in the field of view. The objects of line_11: primary interest for the WFPC-2 images are faint high redshift line_12: (z=0.3-0.9) galaxies, with the most important objects being closest line_13: to the nominal position (i.e., the quasar) of the field. All of the line_14: WFPC2 exposure will be made with the F702W filter, each exposure line_15: being 1000s in duration, with no CR-SPLIT. The 24 exposure are line_16: broken into 3 groups of 8,8, and 8 exposures respectively, with line_17: the telescope being moved by a small amount (~2 arc sec) line_18: in between groupings.The same orientation angle has been requested line_19: for all of the WFPC-2 exposures. ! question: 4 section: 1 line_1: The program has been carried out to the fullest extent possible line_2: using ground--based observations; HST is essential to perform the line_3: UV spectroscopy necessary to obtain values for the HI column line_4: densities of the z=0.656 and z=0.892 absorbing galaxies, as line_5: the Lyman alpha features are at 2014 Angstroms and 2300 Angstroms, line_6: respectively. The WFPC-2 observations are necessary to obtain kpc-- line_7: scale morphological information for both the absorbing galaxies and line_8: for the other moderate redshift galaxies in the same field for line_9: which spectroscopic redshifts have already been obtained. The HST line_10: images are also needed in order to fully resolve the faint absorbing line_11: galaxies from the relatively bright background QSO. ! question: 5 section: 1 line_1: ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: None of the investigators has been PI of previous HST proposals. ! question: 10 section: 1 line_1: Extensive computing and image processing facilities will be available line_2: at each of the participating institutions, as well as the usual secretarial line_3: and administrative facilities. MIT will provide access to the MDM 1.3m line_4: and 2.4m telescopes on Kitt Peak, for any futher ground--based support line_5: of the program. It is anticipated that a graduate student at MIT will be line_6: invited to participate in the reduction and analysis of the data. line_7: Academic year salaries are provided for Steidel and Meyer by their line_8: respective institutions, and Dickinson will be supported year--round line_9: by STScI. ! !end of general form text general_form_address: lname: Steidel fname: Charles mi: C. category: PI inst: 2630 addr_1: MIT addr_2: Physics Department, Room 6-201 addr_3: 77 Massachusetts Avenue city: Cambridge state: MA zip: 02139 country: USA phone: 617-253-5084 telex: steidel@trystero.mit.edu ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: 3C336.0 name_2: Q1622+2352 descr_1: E,314,325, descr_2: H,515,516 pos_1: PLATE-ID=02BA, pos_2: RA = 16H 24M 39.08S +/- 1.0", pos_3: DEC = +23D 45' 12.6" +/- 1.0" equinox: J2000 rv_or_z: Z=0.927 comment_1: FLUX NEAR 2000 A ASSUMES POWER LAW comment_2: WITH ALPHA=0.7 EXTRAPOLATED FROM comment_3: 3100 A, AND ASSUMES A(2000)=0.24 comment_4: MAGS. FEATURES OF PRIMARY INTEREST comment_5: ARE AT 2000 A AND AT 2300 A. fluxnum_1: 1 fluxval_1: V=17.6 +/- 0.1 fluxnum_2: 2 fluxval_2: E(B-V)=0.03 +/- 0.03 fluxnum_3: 3 fluxval_3: F-CONT(2000)=7.0 +/- 1.0 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2300)=6.0 +/- 1.0 E-16 ! targnum: 2 name_1: 3C336.0-FIELD name_2: Q1622+2352-FIELD descr_1: E,314,325, descr_2: H,515,516 pos_1: RA = 16H 24M 39.08S +/- 1.0", pos_2: DEC = +23D 45' 12.6" +/- 1.0", pos_3: PLATE-ID=02BA equinox: J2000 rv_or_z: Z=0.9 comment_1: OBJECTS OF INTEREST ARE FAINT comment_2: (R=23) GALAXIES IN THE FIELD OF comment_3: THE QSO. THE SURFACE BRIGHTNESS comment_4: IS DIFFICULT TO ESTIMATE, AND comment_5: DEPENDS UPON UNKNOWN MORPHOLOGY. comment_6: DESIRE REACHING SURFACE BRIGHT- comment_7: NESS LIMITS (5 SIGMA) PER *PIXEL* comment_8: OF R=29.8. fluxnum_1: 5 fluxval_1: SURF(R)=25 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: 3C336.0 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 16.5S fluxnum_1: 1 priority: 1 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 1.1,1.2; req_3: GROUP 1.0,1.1,1.2,5.0,6.0,7.0 WITHIN 2D ! linenum: 1.100 targname: 3C336.0 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 3400S fluxnum_1: 4 priority: 1 req_1: CYCLE 4; comment_1: FEATURE OF INTEREST IS A BROAD comment_2: ABSORPTION FEATURE CENTERED AT comment_3: 2300 A. EXPOSURE IS DESIGNED TO comment_4: OBTAIN S/N PER DIODE comment_5: OF APPROX 25 AT THAT WAVELENGTH. ! linenum: 1.200 targname: 3C336.0 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 4400S fluxnum_1: 3 priority: 1 req_1: CYCLE 4; comment_1: FEATURE OF INTEREST IS A BROAD comment_2: ABSORPTION FEATURE CENTERED AT comment_3: 2013 ANGSTROMS. EXPOSURE DESIGNED comment_4: TO GET S/N APPROX. 20 PER DIODE comment_5: IN THE CONTINUUM AT THAT comment_6: WAVELENGTH. ! linenum: 5.000 targname: 3C336.0-FIELD config: WFPC2 opmode: IMAGE aperture: WF2-FIX sp_element: F702W num_exp: 8 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 5 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: ORIENT 100D +/- 10D; req_3: SAME ORIENT FOR 6-7 AS 5; req_4: POS TARG 0,-5 comment_1: FIRST OF 3 POSITIONS, SEPARATED comment_2: BY SMALL SHIFTS. THE ORIENT IS comment_3: TO PLACE U3 AXIS AT SKY PA=10 comment_4: DEGREEES, TO INCLUDE OBJECTS comment_5: OF INTEREST AND TO CONTROL comment_6: DIRECTION OF QSO BLOOMING. ! linenum: 6.000 targname: 3C336.0-FIELD config: WFPC2 opmode: IMAGE aperture: WF2-FIX sp_element: F702W num_exp: 8 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 5 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +1.5,-3.5; comment_1: SECOND comment_2: OF 3 POSITIONS, SEPARATED BY SMALL comment_3: SHIFTS. THE ORIENT IS SPECIFIED comment_4: IN ORDER TO PREVENT BLOOMING OF THE comment_5: QSO IN THE DIRECTION OF ONE OF comment_6: THE GALAXIES OF INTEREST. ! linenum: 7.000 targname: 3C336.0-FIELD config: WFPC2 opmode: IMAGE aperture: WF2-FIX sp_element: F702W num_exp: 8 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 5 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +1.5,-6.5; comment_1: THIRD comment_2: OF 3 POSITIONS, SEPARATED BY SMALL comment_3: SHIFTS. THE ORIENT IS SPECIFIED comment_4: IN ORDER TO PREVENT BLOOMING OF THE comment_5: QSO IN THE DIRECTION OF ONE OF comment_6: THE GALAXIES OF INTEREST. ! ! end of exposure logsheet ! No scan data records found