! File: 3418C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:07:07:05 coverpage: title_1: QUASAR ABSORPTION LINE SURVEY: CYCLE 1 FOS PART II sci_cat: QUASARS & AGN proposal_for: GO large_proj: X key_proj: X longterm: 3 cont_id: 2424 pi_title: DR. pi_fname: JOHN pi_mi: N. pi_lname: BAHCALL pi_inst: INSTITUTE FOR ADVANCED STUDY, PRINCETON pi_country: USA pi_phone: 609-734-8054 keywords_1: SPECTROSCOPY QUASARS, ABSORPTION/EMISSION LINES, keywords_2: GALAXIES, HALOS/CLUSTERS/VOIDS, INTERGALACTIC MEDIUM hours_pri: 104.00 num_pri: 47 fos: Y funds_amount: 1288653 funds_length: 36 funds_date: SEP-91 pi_position: PROFESSOR off_fname: MARVIN off_mi: L. off_lname: GOLDBERGER off_title: DIRECTOR off_inst: INSTITUTE FOR ADVANCED STUDY off_addr_1: OLDEN LANE off_city: PRINCETON off_state: NJ off_zip: 08540 off_country: USA ! end of coverpage abstract: line_1: The establishment of a homogeneous data base of quasar absorption lines using line_2: the diagnostic survey proposed here will form the basis for an attack on line_3: fundamental cosmological and astrophysical problems: What are the physical, line_4: dynamical and evolutionary properties of the intergalactic medium? What is line_5: the strength, shape and origin of the UV background radiation? What limits line_6: can be set upon the primordial He/H and D/H ratios? What has been the line_7: chemical and dynamical evolution of gaseous galactic disks and halos? What line_8: physical processes govern the ionization of this gas? What physical processes line_9: govern the acceleration of thermal and relativistic plasma in radio quiet and line_10: radio loud quasars? How has gaseous structure in the universe evolved on line_11: scales of 1 Mpc to 100 Mpc? The discrimatory power of the survey and the line_12: efficient use of HST were the primary criteria used in constructing the survey, line_13: which takes account of all relevant GTO observations. Exposure times are based line_14: upon IUE archival data. Ground-based observations of all program objects will line_15: be made to monitor variability and to complement the HST observations. The line_16: survey contains a primary list of 103 quasars with 0.3 < Z_em < 2.0, 18 line_17: additional bright quasars to be observed with the FOS to provide candidates for line_18: future HRS follow up, and a supplementary list of 49 fainter quasars for a line_19: damped Ly-alpha survey. A plausible extrapolation of ground-based data line_20: suggests that the primary survey will detect 275 Ly-alpha and 60 CIV systems. ! ! end of abstract general_form_proposers: lname: BAHCALL fname: JOHN title: P.I. mi: N. inst: INSTITUTE FOR ADVANCED STUDY, PRINCETON country: USA ! lname: SARGENT fname: W. inst: CALIFORNIA INSTITUTE OF TECHNOLOGY country: USA ! lname: WEYMANN fname: RAY mi: J. inst: OBSERVATORY OF THE CARNEGIE INSTITUTION IN WASHINGTON country: USA ! lname: BERGERON fname: JACQUELINE inst: INSTITUTE FOR ASTROPHYSICS, PARIS country: FRANCE esa: X ! lname: BOKSENBERG fname: A. inst: ROYAL GREENWICH OBSERVATORY country: UK esa: X ! lname: HARTIG fname: GEORGE inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: JANNUZI fname: BUELL mi: T. inst: INSTITUTE FOR ADVANCED STUDY, PRINCETON country: USA ! lname: SCHNEIDER fname: DONALD mi: P. inst: INSTITUTE FOR ADVANCED STUDY, PRINCETON country: USA ! lname: SAVAGE fname: BLAIR inst: WISCONSIN, UNIVERSITY OF country: USA ! lname: TURNSHEK fname: DAVID mi: A. inst: UNIVERSITY OF PITTSBURGH country: USA ! lname: WOLFE fname: A. mi: M. inst: ASTROPHYSICS AND SPACE SCIENCES,UCSD country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: FOS high-resolution (~ 1200) exposures will be taken of a primary sample of 103 line_2: objects and an additional list of 18 bright objects. Full HST wavelength line_3: coverage (exposures with G130H, G190H, and G270H) will be obtained for all line_4: objects for which IUE and/or ground-based data indicate that this is feasible line_5: (see details of observing algorithm in question 2, section IV ). A S/N ratio of line_6: 30 is expected to be achieved in neach high-resolution exposure. For a line_7: supplementary list of 49 objects, and for 71 sources in the primary list, G160L line_8: exposures will be taken to identify a subset of objects containing sufficient line_9: ultraviolet flux to permit observations with the R = 1200 gratings. A line_10: convenient summary of our observing program is shown in Table 1 (attached). line_11: Observations that will be obtained from the HST archive are denoted by "GTO" or line_12: are enclosed in parentheses; exposure times that were calculated directly from line_13: IUE data are denoted by asterisk. Each exposure will be taken in the 1.0 arcsec line_14: aperture. The software by which the target is centered on the aperture is line_15: expected to permit the measurement of wavelengths to an absolute accuracy line_16: corresponding to 25 km/s or better. This will be sufficient to permit efficient line_17: follow-up measurements in the radio (and optical). We will consider using a line_18: smaller aperture to obtain even higher accuracy in wavelength measurements line_19: after the first year, since it is likely that the experience gained in the line_20: operation of the observatory in the first year will be important in acquiring line_21: targets efficiently in the smaller apertures. NOTE: WITH DEGRADED OPTICS AND line_22: FOS UV PROB, SOME GHRS OBS WERE ALSO REQUESTED . DUE TO GHRS SIDE 1 PROB, THE line_23: GHRS OBS HAVE BEEN SWITCHED BACK TO THE FOS AND ARE IN THIS SEPARATE FILE. ! question: 4 section: 1 line_1: HST observations are required in order to observe the strong line_2: resonance lines of the most abundant elements, which are in line_3: the ultraviolet (inaccessible to terrestrial observations) for line_4: the small and moderate redshifts considered in our primary line_5: sample. Ground-based observations partially determine the line_6: character of the absorbing systems at larger redshifts, but line_7: spectra must be obtained at smaller redshifts to establish the line_8: evolution of the absorbing systems (see equation 1 of question 2), line_9: to permit optical identifications, to search for gas in known line_10: voids and clusters of galaxies, and to allow sufficient resolution line_11: and signal-to-noise to permit answering the scientific questions line_12: listed in section III of question 2. Quasar absorption lines have line_13: been studied extensively from the ground (see the review articles line_14: listed at the end of section II of question 2), but of course only line_15: in the accessible optical region. ! question: 5 section: 1 line_1: The total amount of exposure (164 hours) and spacecraft (211 hours) time line_2: are required to rpoduce a data base of sufficient size to answer what we line_3: consider to be the most important issues regarding quasar abs orption line_4: lines. (For details, see question 2.) Our program has a built-in line_5: oversubscription factor of 10%. Since quasars are known to vary line_6: significantly in brightness on a time scale of months to years, some of line_7: our targets will be much fainter at the time of HST observation than line_8: the values we used to calculate the FOS exposure times. Ground based line_9: photometry of the quasars will be acquired a few months before the line_10: scheduled HST observations; if the object is discovered to be line_11: abnormally faint, another target will be subsitituted. line_13: For a summary of our proposed observations see Table 1. ! question: 6 section: 1 line_1: We recommend that the STScI develop and implement a standard way of line_2: performing efficient FOS background monitoring. The results of the line_3: monitoring will be usefil to all FOS observers. We request an on-board line_4: arc for each of the exposures for accurate wavelength calibration. We line_5: would like all observations of a given object to be obtained within a line_6: ten day interval. Since quasars are known to vary in brightness, the line_7: data for all wavelengths must be taken nearly simultaneously in order line_8: to determine the spectral energy distribution. NOTE: GHRS OBSERVATIONS FOR THE line_9: FOLLOWING TARGETS HAVE NOW BEEN CHANGED TO FOS/BL G130H BECAUSE OF line_10: GHRS SIDE 1 PROBLEM. THESE NEW FOS OBSERVATIONS ARE IN ADDITION TO THOSE line_11: SCHEDULED AS PART OF PROGRAM 2424. SOME OBJECTS WERE DROPPED FROM GHRS line_12: BUT WILL NOT BE OBSERVED THIS CYCLE WITH FOS/BL BECAUSE OF TIME CONSTRAINTS line_13: 1) MC40031-707 drop line_14: 2) PG0043+039 drop line_15: 3) TON28 Switched line_16: 4) 3C351.0 Switched line_17: 5) B21512+37 drop line_18: 6) MARK205 drop line_19: 7) PG1049-005 drop line_20: 8) PG1259+593 Switched line_22: THE FOS/RD OBSERVATIONS FOR THESE TARGETS REMAIN IN PROPOSAL 2424. line_23: THE REQUIREMENT FOR SCHEDULING THESE WITH THE FOS/RD OBSERVATIONS IS DROPPED. ! question: 7 section: 1 line_1: The answer to this question is too long to fit in RPSS format; please see line_2: the original proposal form for a detailed discussion of our data reduction line_3: and analysis plans. ! question: 8 section: 1 line_1: The answer to this question is too long to fit in RPSS format; please see line_2: the original proposal form for a detailed discussion. ! question: 9 section: 1 line_1: Four members of our collaboration (Bahcall, Boksenberg, Savage, and line_2: Weymann) have GTO programs that involve the use of the FOS, HRS, FOC, line_3: and WF/PC. We list only those programs that are directly related to line_4: quasar absorption lines: 1015, 1018, 1022, 1024-6, 1140, 1142-6, line_5: 1163, 1165, 1166, and 1235. ! question: 10 section: 1 line_1: The participating institutions will supply access to ground-based line_2: telescope facilities at the AAT, Las Campanas, La Palma, La Silla, line_3: and Palomar Observatory. These facilities will be used to support line_4: our HST survey by timely ground-based observations of the sources line_5: (see answer to question 8). In addition, undergraduate and line_6: graduate students will be available at each of the academic line_7: institutions. Major computing facilities and existing software line_8: analysis programs will be supplied by all of the participating line_9: institutions. The usual secretarial and administrative facilities line_10: will also be provided at each institution. The Institute for line_11: Advanced Study will also provide guest facilities for all line_12: members of the collaboration when they come to Princeton to carry line_13: out analysis tasks. ! !end of general form text general_form_address: lname: BAHCALL fname: JOHN mi: N. title: DR. category: PI inst: INSTITUTE FOR ADVANCED STUDY addr_1: OLDEN LANE city: PRINCETON state: NJ zip: 08540 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: 3C351.0 descr_1: GALAXY; AGN; QUASAR pos_1: RA = 17H 04M 41.3S +/- 0.1S , pos_2: DEC = +60D 44' 30" +/- 1.0", pos_3: PLATE-ID=00T2 equinox: 2000 rv_or_z: Z=0.371 fluxnum_1: 1 fluxval_1: V = 15.50 +/- 0.1 ! targnum: 2 name_1: TON28 descr_1: GALAXY; AGN; QUASAR pos_1: RA = 10H 04M 02.6S +/- 0.1S , pos_2: DEC = +28D 55' 35" +/- 1.0", pos_3: PLATE-ID=021H equinox: 2000 rv_or_z: Z=0.329 fluxnum_1: 1 fluxval_1: V = 15.80 +/- 0.1 ! targnum: 3 name_1: PG1259+593 descr_1: GALAXY; AGN; QUASAR pos_1: RA = 13H 01M 12.9S +/- 0.1S , pos_2: DEC = +59D 02' 06.9" +/- 1.0", pos_3: PLATE-ID=01R2 equinox: 2000 rv_or_z: Z=0.472 fluxnum_1: 1 fluxval_1: V = 15.70 +/- 0.1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: 3C351.0 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 11.81S priority: 1 req_1: CYCLE 1; req_2: ONBOARD ACQ FOR 1.10 ; ! linenum: 1.100 targname: 3C351.0 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1.74S priority: 1 param_1: TYPE=UP req_1: CYCLE 1; req_2: ONBOARD ACQ FOR 2.00; req_3: SPATIAL SCAN ; ! linenum: 2.000 targname: 3C351.0 config: FOS/BL opmode: RAPID aperture: 0.25X2.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 300.00M fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 req_1: CYCLE 1 ; ! linenum: 3.000 targname: TON28 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 15.57S priority: 1 req_1: CYCLE 1; req_2: ONBOARD ACQ FOR 3.10 ; ! linenum: 3.100 targname: TON28 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 2.30S priority: 1 param_1: TYPE=UP req_1: CYCLE 1; req_2: ONBOARD ACQ FOR 4.00; req_3: SPATIAL SCAN ; ! linenum: 4.000 targname: TON28 config: FOS/BL opmode: RAPID aperture: 0.25X2.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 325.00M fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 req_1: CYCLE 1 ; ! linenum: 5.000 targname: PG1259+593 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 14.20S priority: 1 req_1: CYCLE 1; req_2: ONBOARD ACQ FOR 5.10 ; ! linenum: 5.100 targname: PG1259+593 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 2.10S priority: 1 param_1: TYPE=UP req_1: CYCLE 1; req_2: ONBOARD ACQ FOR 6.00; req_3: SPATIAL SCAN ; ! linenum: 6.000 targname: PG1259+593 config: FOS/BL opmode: RAPID aperture: 0.25X2.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 360.00M fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 req_1: CYCLE 1 ; ! ! end of exposure logsheet scan_data: line_list: 1.10, 3.10, 5.10 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 0.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 0.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2000 wid_offset: 0.0000 ! ! end of scan data