! File: 3065C.PROP ! Database: PEPDB ! Date: 18-FEB-1994:14:13:01 coverpage: title_1: HIGH SIGNAL-TO-NOISE QSO LINE PROFILES 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, LYMAN ALPHA hours_pri: 1.95 num_pri: 1 fos: Y ! end of coverpage abstract: line_1: We will use the FOS to measure the strengths and profiles line_2: of emission lines in the UV in a bright, low-redshift QSO. line_3: We will present a high signal-to-noise spectrum which is line_4: essentially unaffected by the HST optical problems. line_5: These observations will be combined with optical observations line_6: of similar quality and lead to improved models of the line_7: structure of the broad-line region of QSOs. ! ! 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: The broad emission lines present in QSO spectra are probably produced line_2: by clouds of gas moving at velocities around 10000 km/s at distances of line_3: order one to ten parsecs from the source of continuum radiation. The line_4: emission-line profiles produced by these clouds depend on both the dynamics line_5: of the clouds and the emission properties of the individual clouds. Several line_6: models for the broad-emission-line region have been developed that predict line_7: shapes for line profiles which are in reasonable agreement with line_8: observations. These models include: radiatively accelerated clouds line_9: (Blumenthal and Mathews, 1979), clouds accelerated by quasar winds (Weymann line_10: et al., 1982), and cloud motion along parabolic orbits (Kwan and Carroll, line_11: 1982). line_12: Because the overall line shapes do not provide a definitive test of line_13: the possible dynamical models, more subtle systematic properties of the line_14: emission-line profiles must be considered. Systematic QSO emission-line line_15: profile differences (Mathews and Wampler, 1985) and redshift differences line_16: (Gaskell, 1982 and Wilkes, 1984, 1986) have been observed. The line_17: interpretation of these data in terms of the dynamics and internal line_18: obscuration and geometry of the broad-emission-line region is limited by line_19: the quality of the observations and the statistical nature of the problem. line_20: These data already provide direct evidence for an inhomogeneous, line_21: multi-component broad emission line region. With further observations, the line_22: quality of the data will improve. ! question: 2 section: 2 line_1: We propose to observe the bright, low-redshift QSO CSO 251 with one line_2: of the high resolution UV gratings of the FOS. These observations will line_3: demonstrate the capabilities of the FOS and HST to produce line_4: high-signal-to-noise spectra of QSOs. Additionally, when we combine the UV line_5: spectral observations with the FOS described in this proposal with optical line_6: observations we will be able to study in detail profile differences and line_7: redshift differences of interesting emission-line pairs. Observations of line_8: this low redshift QSO will allow a comparison of Ly alpha, with H beta, line_10: [OIII] lambda 5007, and H alpha in the optical. The UV data obtained with line_11: this program will be at much higher resolution and signal-to-noise ratio line_12: than previous UV data on Seyferts and QSOs (taken with the IUE); the Lyman line_13: alpha profile should be unaffected by the absorption which affects this line_14: line in high redshift QSOs; and we will be able to measure the profiles of line_15: all lines in the same object, unlike previous studies of QSO line profiles. line_16: The [O III] line is probably near the systemic redshift of the QSO and line_17: provides a reference for the redshift difference studies. Observations of H line_18: alpha in the IR by Espey et al. (1989) show a median redshift difference of line_19: 1000 km/s between H alpha and C IV lambda 1549. Ly alpha is usually near line_20: the C IV redshift. This difference might be the result of a BELR that line_21: contains a low-ionization region that is optically thick and a separate line_22: optically thin high-ionization region (for example Mathews 1986). The Ly ! question: 2 section: 3 line_1: alpha emission-line profile compared to H beta can be used to estimate the line_2: Ly alpha / H beta ratio in each region. One prediction of this model is line_3: that at velocities where the optically thin component dominates, the Ly line_4: alpha / H beta ratio should be near the recombination value i.e. very line_5: large. Normalized emission line pairs can be divided to compare line flux line_6: ratios as a function of velocity (Shuder, 1982, 1984). From simple line_7: arguments based on H alpha and H beta profiles, Shuder was able to show line_8: that velocity must inrease inwards in the broad-line region. Detailed line_9: comparisons of several lines, including those from both the fully and line_10: partially ionized zones, combined with predictions from photoionization line_11: models should allow us to reach much more detailed conclusions. line_13: Blumenthal, G. R., and Mathews, W. G. 1979, Ap. J., 233, 479. line_14: Espey, B. R., Carswell, R. F., Bailey, J. A., Smith, M. G., and line_15: Ward, M. J. 1989, Ap. J., 342, 666. line_16: Gaskell, C. M. 1982, Ap. J., 263, 79. line_17: Kwan, J., and Carroll, T. J. 1982, Ap. J., 261, 25. line_18: Mathews, W. G. 1986, Ap. J., 305, 187. line_19: Mathews, W. G., and Wampler, E. J. 1985, P.A.S.P., 97, 966. line_20: Shuder, J. M. 1982, Ap. J., 259, 48. line_21: Shuder, J. M. 1984, Ap. J., 280, 491. ! question: 2 section: 4 line_1: Weymann, R. J., Scott, J. S., Schiano, A. V. R., and Christiansen, line_2: W. A. 1982, Ap. J., 262, 497. line_3: Wilkes, B. J. 1984, M.N.R.A.S., 207, 73. line_4: Wilkes, B. J. 1986, M.N.R.A.S., 218, 331. ! question: 3 section: 1 line_1: This proposal contains 1 object which will be observed with line_2: G130H grating and FOS blue detector. S/N will be line_3: 30 per diode, enabling us to measure accurate line profiles. line_4: A short observation with the 4.3 arc line_5: second square aperture will be used to measure absolute fluxes. ! question: 4 section: 1 line_1: The main point of this program is to demonstrate the line_2: capability of the HST and FOS to take high signal-to-noise line_3: spectra of objects with broad emission lines. We will use line_4: these data to model the structure of the broad-line region line_5: of QSOs. For comparison with models, ratios of line from line_6: different regions must be measured in the same object. line_7: Adequate signal-to-noise and resolution cannot be obtained line_8: either by observing low-redshift objects with the IUE or line_9: the rest optical lines of high-redshift lines in the IR. line_10: High resolution and high signal-to-noise studies in the line_11: optical region alone do not include enough lines formed in line_12: different portions of the emission-line region for a line_13: detailed analysis. ! question: 5 section: 1 line_1: The signal-to-noise calculation assumed transmission line_2: through the 1.0 arc second diameter of 27% and a total line_3: HST+FOS efficiency (for all other components) of 0.01% line_4: at Lyman alpha with G130H and the blue detector. ! 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: We will measure line strength ratios and profile differences line_2: for UV and optical lines. The measurements will be compared line_3: to predictions of photoinization models and simple kinematic line_4: 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 to measure provide line_3: an estimate of the absolute flux to test the HST flux calibration line_4: and to provide additional scientific input. ! !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: CSO251 name_2: TON1187 descr_1: QUASAR pos_1: RA = 10H 13M 03.173S +/- 1.0", pos_2: DEC = 35D 51' 23.13" +/- 1.0", pos_3: PLATE-ID = 01R3 equinox: 2000 pm_or_par: NO rv_or_z: Z=0.0786 fluxnum_1: 1 fluxval_1: V=15.0 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: CSO251 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.6S 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: CSO251 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 11S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 700000 req_1: ONBOARD ACQ FOR 2-4; req_2: GROUP 1-4 WITHIN 60D; req_3: CYCLE 0 / 1-4 ! linenum: 2.000 targname: ^ config: ^ opmode: ACQ aperture: ^ sp_element: ^ num_exp: 1 time_per_exp: 11S fluxnum_1: 1 priority: ^ ! linenum: 3.000 targname: ^ config: ^ opmode: ACCUM aperture: ^ sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 100S s_to_n: 3 fluxnum_1: ^ priority: ^ param_1: STEP-PATT=SINGLE ! linenum: 4.000 targname: ^ config: ^ opmode: ACCUM aperture: 1.0 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 6900S s_to_n: 30 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