! File: 4939C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:11:20:56 coverpage: title_1: QUASAR ABSORPTION LINE SURVEY: CYCLE 2 OBSERVATIONS title_2: OBSERVATIONS OF 3C249-1 sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: GO large_proj: Y key_proj: Y longterm: 3 cont_id: 2424 pi_fname: JOHN pi_mi: N. pi_lname: BAHCALL pi_inst: INSTITUTE FOR ADVANCED STUDY, PRINCETON, N.J. pi_country: USA pi_phone: 609-734-8058 hours_pri: 7.42 num_pri: 1 fos: Y funds_amount: 1751269 funds_length: 48 off_fname: ALLEN off_lname: ROWE off_title: ASSOCIATE DIRECTOR off_inst: INSTITUTE FOR ADVANCED STUDY off_addr_1: FULD HALL off_addr_2: OLDEN LANE off_city: PRINCETON off_state: NJ off_zip: 08540 off_country: U.S.A. off_phone: 609-734-8200 ! end of coverpage abstract: line_1: THIS SUBMISSION is a change to P3791 to replace an object that line_2: it is not possible to acquirer with the Binary Search procedure line_3: with another object from our program. The object which has been line_4: removed is IR0450-2958. We are replacing it with 3C249-1 line_5: The Quasar Absorption Line Survey of bright sources is an efficient observing line_6: program designed to provide a homogeneous data base of absorption features. line_7: The data will reveal absorption regions in galaxies, in clusters of line_8: galaxies, in voids, in large-scale structures, in Lyman ALPHA clouds, and wi line_9: provide information about damped Lyman ALPHA and Lyman-limit systems. line_10: The survey will determine, with high SNR, the profiles of > 200 emission lines. line_11: Using the estimated numbers of observed absorption lines, including archi line_12: val data, the program was designed to determine the cosmic evolution of line_13: absorption systems. High resolution spectra of a sample of quasars will line_14: be obtained with the FOS; the spectra will have a rest frame equivalent line_15: width detection limit for unresolved absorption lines of 0.3 A. ! ! end of abstract general_form_proposers: 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: Y ! lname: BOKSENBERG fname: A. inst: ROYAL GREENWICH OBSERVATORY country: UK esa: Y ! 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: SAVAGE fname: BLAIR inst: WISCONSIN, UNIVERSITY OF country: USA ! lname: SCHNEIDER fname: DONALD mi: P. inst: INSTITUTE FOR ADVANCED STUDY, PRINCETON 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 ! lname: BAHCALL fname: JOHN title: PI mi: N. inst: INSTITUTE FOR ADVANCED STUDY, PRINCETON country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Observations for the Quasar Absorption Line Survey will be distributed line_2: equally over three cycles (1-3). The quasars will in general line_3: be observed at high resolution ($1300$) through the 0.25 by 2.0 arcsecond line_4: slit. For these observations the desired signal to noise ratio is 30 (per line_5: diode). The FOS red side with the G190H and G270H gratings will be used to line_6: cover the wavelength range 1600 to 3300 angstroms. The FOS blue side and line_7: G130H grating will be used to cover the range from 1100 to 1600 angstroms. line_8: Since the G130H observations require a great deal of time, for some objects line_9: low resolution G160L exposures through the 1.0 arcsecond apt. are used instead. line_10: These are designed to find targets suitable for future cycle G130H observations line_11: and do not require signal to noise of 30. For eash object a single Binary line_12: acquisition is used followed by peak up acquisitions into the slit. ! question: 4 section: 1 line_1: HST observations are required to observe the strong resonant line_2: absorption lines and the various emission lines of the most abundant line_3: elements, which are in the ultraviolet (inaccessible to terrestrial line_4: observations) for the small and moderate redshifts investigated in line_5: this project. Ground-based observations partially determine the line_6: character of the absorbing systems and emission line regions at larger line_7: redshifts, but spectra must be obtained in the ultraviolet to line_8: establish the cosmological evolution of the known types of absorbing line_9: systems and emission line regions, to permit optical identifications, line_10: to search for gas in known voids and clusters of galaxies, to test line_11: for large scale structure in absorbing systems, and to make possible line_12: follow-up high resolution studies of the physical conditions and of line_13: the chemical (and isotopic) abundances. IUE observations do not have line_14: sufficiently high signal-to-noise ratios for our sample of objects to line_15: permit answering the scientific questions listed in the section on line_16: scientific justification. Quasar absorption and emission lines have line_17: been studied extensively from the ground (see the review articles line_18: listed in the scientific justification), but of course only in the line_19: accessible optical region. ! question: 5 section: 1 line_1: No Realtime data needed ! question: 6 section: 1 line_1: We would like all observations of a given object to be obtained within line_2: a ten day interval. Since quasars are known to vary in brightness, the line_3: data for all wavelengths must be taken nearly simultaneously in order line_4: to determine the spectral energy distribution. Our observations of a line_5: given object are currently linked with NO GAP inorder to be more line_6: efficient in the use of spacecraft time (only one acquisition needed). ! question: 7 section: 1 line_1: The answer to this question is too long for the RPSS format; please line_2: see the paper submission for phase 1. ! question: 8 section: 1 line_1: See paper submission for phase 1. ! question: 9 section: 1 line_1: See paper submission for phase 1. ! question: 10 section: 1 line_1: See paper submission for phase 1. ! !end of general form text general_form_address: lname: BAHCALL fname: JOHN mi: N. category: PI inst: INSTITUTE FOR ADVANCED STUDY addr_1: OLDEN LANE, BUILDING E city: PRINCETON, N.J. state: NJ zip: 08540 country: U.S.A. phone: 609-734-8058 telex: 229 734 IAS UR ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: 3C249-1 descr_1: E,314,321 pos_1: RA = 11H 04M 13.9S +/- 0.1S, pos_2: DEC = +76D 58' 58.2" +/- 1.0", pos_3: PLATE-ID=02D3 equinox: 2000 rv_or_z: Z=0.311 fluxnum_1: 1 fluxval_1: V = 15.72 +/- 0.1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: 3C249-1 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 14.46S priority: 1 req_1: CYCLE 2; req_2: ONBOARD ACQ FOR 1.10 ; ! linenum: 1.100 targname: 3C249-1 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 2.13S priority: 1 param_1: TYPE=UP req_1: CYCLE 2; req_2: ONBOARD ACQ FOR 2.00; req_3: SPATIAL SCAN ; ! linenum: 2.000 targname: 3C249-1 config: FOS/BL opmode: RAPID aperture: 0.25X2.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 340M fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 req_1: CYCLE 2 ; ! ! end of exposure logsheet scan_data: line_list: 1.10 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 90.0000 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