! File: 3066C.PROP ! Database: PEPDB ! Date: 18-FEB-1994:14:15:52 coverpage: title_1: EMISSION LINES IN HIGH REDSHIFT QSOS sci_cat: QUASARS & AGN sci_subcat: QUASAR EMISSION proposal_for: EROS pi_fname: E. MARGARET pi_lname: BURBIDGE pi_inst: UC, SAN DIEGO pi_country: USA pi_phone: (619) 534-4477 keywords_1: UV SPECTROSCOPY, QUASAR, keywords_2: EMISSION LINE PROFILE, ABUNDANCE EVOLUTION hours_pri: 2.19 num_pri: 1 fos: Y ! end of coverpage abstract: line_1: We will use the FOS to measure the strength of the He I line_2: lambda 584 line in the UV in a QSO which has a good probability line_3: of having light at that wavelength. We will demonstrate the line_4: ability of the FOS to detect weak emission lines against a line_5: background of weak absorption lines in a faint object with line_6: the degraded performance due to the slit losses, decreased line_7: resolution, possible increased scattered light and greater line_8: than expected particle-induced background. From this line line_9: we will determine the relative abundance of Helium in the line_10: early universe. ! ! end of abstract general_form_proposers: lname: BEAVER fname: EDWARD inst: UC, SAN DIEGO country: USA ! lname: BURBIDGE fname: E. MARGARET inst: UC, SAN DIEGO country: USA ! lname: MARGON fname: BRUCE inst: WASHINGTON, UNIVERSITY OF country: USA ! lname: ANGEL fname: J. ROGER mi: P. inst: ARIZONA, UNIVERSITY OF country: USA ! lname: BARTKO fname: FRANK inst: MARTIN MARIETTA CORPORATION country: USA ! lname: DAVIDSEN fname: ARTHUR mi: F. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: HARMS fname: RICHARD mi: J. inst: APPLIED RESEARCH CORPORATION country: USA ! lname: BOHLIN fname: RALPH inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: FORD fname: HOLLAND mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Observations of CSO 38 will yield a determination of the cosmic abundance line_2: of helium at a look back time of more than 75% of the age of the universe and line_3: characterize the ability of the FOS to measure weak emission lines line_4: in faint objects. We will determine the helium abundance by line_5: comparing the strength of the He I lambda 584 recombination line with the line_6: strengths of other emission lines which we will measure from the ground. The line_7: He I lambda 584 emission line has never been measured, and measurements of line_8: this line and HeII lambda 304 are important HST goals. Additionally, we may line_9: be able to set constraints on the ionization level of the intergalactic line_10: medium of the early universe, a major indicator of the constituent parts of line_11: the early universe. Determining the initial cosmic helium abundance can in line_12: principle refine our estimate of the baryon number of the universe. line_13: CSO 38 is one of the best objects available to us with which we can line_14: perform this test, both scientifically and from a technical standpoint. The FOS line_15: ability to measure emission lines differs from the performance predicted line_16: before launch in several ways. These include light loss, loss of resolution, line_17: and greater than predicted background. The signal-to-noise per diode for a line_18: 5900s exposure will be approximately 35, assuming that the 1.0 arc sec ! question: 2 section: 2 line_1: diameter FOS aperture transmits 33% of the incident light. We have also line_2: included a short exposure with the 4.3 arc second aperture to obtain an line_3: accurate flux for the scientific analysis. This will also be useful for line_4: testing the predicted light loss through the 1.0 arc second aperture. line_5: This observation will demonstrate the ability of the HST to take high quality line_6: spectra of high-redshift emission-line objects. ! question: 3 section: 1 line_1: This proposal contains 1 object which will be observed with line_2: G160L and the red detector of the FOS. S/N will be 20 per line_3: diode allowing us to detect a weak emission line. line_4: A very short exposure will be used to measure the absolute line_5: flux. All exposures are cycle 0. ! question: 4 section: 1 line_1: The main point of this program is demonstrate the ability of the HST and FOS line_2: to observe high-redshift objects and to determine the Helium abundace in the line_3: early universe. The important emission lines for this determination line_4: cannot be measured from the ground or with IUE in any known object. ! question: 5 section: 1 line_1: The signal-to-noise calculation assumed transmission line_2: through the 1.0 arc second diameter aperture of 33% at 2100 line_3: Angstroms, and a total HST+FOS efficiency due to all other line_4: components of 3.4% with G160L at 2114 Angstroms. line_5: The particle-induced background is assumed to be 0.01 c/s/d. ! question: 6 section: 1 line_1: The OV prerequisite programs for all observations are: line_2: Prop ID 2188, 2189, 1441, 1442, and 1443 line_3: The SV prerequisite program for all observations is: line_4: Prop ID 2195 ! question: 7 section: 1 line_1: To characterize the performance of the HST + FOS, we will line_2: measure the flux in a weak emission line, superposed on absorption, line_3: in the total observation as well as in shorter segments of line_4: the total integration. We will compare the flux levels in line_5: portions to check the particle-induced background subtraction. line_6: We will do spectral deconvolution to determine the effect line_7: of the decreased spectral resolution of the FOS on our line_8: observations. The abundance determination will be performed line_9: by comparing the measured emission-line strength to optical line_10: lines and the predictions of published models. ! question: 8 section: 1 line_1: We will schedule ground-based observations at Lick Observatory line_2: as close to the HST observations in time as possible in order line_3: to check FOS fluxes and obtain the strengths of optical line_4: emission lines for comparison. ! !end of general form text general_form_address: lname: BURBIDGE fname: E. MARGARET category: PI inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO addr_1: CASS DEPT., C-011 city: LA JOLLA state: CA zip: 92093 country: USA phone: (619) 534-4477 telex: FAX: (619) 534-6316 ! lname: COHEN fname: ROSS mi: D. category: CON inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO addr_1: CASS DEPT., C-011 city: LA JOLLA state: CA zip: 92093 country: USA phone: (619) 534-2664 telex: FAX: (619) 534-6316 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: CSO38 descr_1: QUASAR pos_1: RA = 10H 11M 55.599S +/- 1.0", pos_2: DEC = 29D 41' 41.50" +/- 1.0", pos_3: PLATE-ID = 021H equinox: 2000 pm_or_par: NO rv_or_z: Z=2.62 fluxnum_1: 1 fluxval_1: V=16.0 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: CSO38 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.2S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 1.5; req_2: SPATIAL SCAN; req_3: GROUP 1-4 WITHIN 60D; req_4: CYCLE 0 / 1-4 ! linenum: 1.500 targname: CSO38 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 22S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 700000 req_1: ONBOARD ACQ FOR 2-4; ! linenum: 2.000 targname: ^ config: ^ opmode: ACQ aperture: ^ sp_element: ^ num_exp: 1 time_per_exp: 22S fluxnum_1: 1 priority: ^ ! linenum: 3.000 targname: ^ config: ^ opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 100S s_to_n: 5 fluxnum_1: ^ priority: ^ param_1: STEP-PATT=SINGLE ! linenum: 4.000 targname: ^ config: ^ opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 5900S s_to_n: 35 fluxnum_1: ^ priority: ^ param_1: STEP-PATT=SINGLE ! ! end of exposure logsheet scan_data: line_list: 1 fgs_scan: cont_dwell: D dwell_pnts: 2 dwell_secs: 0.00 scan_width: 7.0000 scan_length: 4.3000 sides_angle: 90.0000 number_lines: 6 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 2.1500 wid_offset: 3.5000 ! ! end of scan data