! File: 5002C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:14:36:01 coverpage: title_1: THE INNER REGIONS OF QUASARS -- REPEAT FOR HOPR#0104 sci_cat: QUASARS & AGN sci_subcat: QUASAR EMISSION proposal_for: RPT/GO longterm: 2 cont_id: 2578 pi_title: DR. pi_fname: BEVERLEY pi_mi: J. pi_lname: WILLS pi_inst: TEXAS, UNIVERSITY OF pi_country: USA pi_phone: 512-471-3424 keywords_1: QUASARS, SPECTRA hours_pri: 1.16 num_pri: 1 fos: Y pi_position: ASSISTANT PROFESSOR off_fname: STEPHEN off_mi: A. off_lname: MONTI off_title: VICE PROVOST off_inst: THE UNIVERSITY OF TEXAS AT AUSTIN off_city: AUSTIN off_state: TX off_zip: 78712 off_country: USA ! end of coverpage abstract: line_1: An axisymmetric geometry for the inner few parsesc of quasars is strongly line_2: suggested by several new investigations. A mass-luminosity relation has been line_3: suggested as well as a dependence of ionization of the Broad Line Region on line_4: continuum luminosity. These recent studies offer exciting prospects for line_5: probing the innermost regions by means of orientation-dependent emission line line_6: ratios, equivalent widths and profiles, and continuum spectra, including line_7: luminosities in the radio, UV, and X-ray regions.We propose to measure the UV line_8: line and continuum (FOS) spectra (rest wavelengths>1170A) in a complete line_9: sample of 3CR radio quasars extended to include quasars with measured X-ray line_10: flux densities and a range of radio core-dominance. These spectra are being line_11: extended by ground-based observations to ~8000A, to cover high and low line_12: ionization lines in the same quasar, and the HST sample itself is being line_13: complemented by higher redshift quasars where the strong lines of Ly-alpha,CIV line_14: lambda 1549, and CIIIlambda1909 are being observed from the ground. Some of line_15: several questions that we hope to answer are: 1. Is their evidence for massive line_16: accretion disks? (via equivalent width distributions and correlations with line_17: radio core-dominance for lines of different ionization).2. Are the line widths line_18: and fluxes correlated with the radio, UV or X-ray continuum properties? Is the line_19: result the same for all lines, in particular Fe II, C IV and H-Beta? What can line_20: this tell us about the kinematics and geometry of the BLR 3? What is the origin ! ! end of abstract general_form_proposers: lname: NETZER fname: H. inst: TEL AVIV UNIVERSITY country: ISRAEL ! lname: BROWNE fname: I.W.A. inst: MANCHESTER, UNIVERSITY OF country: UK ! lname: WILLS fname: BEVERLEY title: P.I. mi: J. inst: TEXAS, UNIVERSITY OF country: USA ! lname: WILLS fname: DEREK inst: TEXAS, UNIVERSITY OF country: USA ! lname: BALDWIN fname: JACK mi: A. inst: CTIO (NOAO) country: USA ! lname: FERLAND fname: GARY mi: J. inst: OHIO STATE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Our sample is based on a complete subset of 3CR quasars. 3CR, line_2: being a low frequency survey, selects an almost random line_3: distribution of orientations to the line of sight, ideal for the line_4: observations of line width and equivalent width distributions. line_5: There is much other information available for this well-studied line_6: subset and other scientific advantages are mentioned in the line_7: scientific justification. However, in a set of randomly oriented line_9: quasars there are very few high R sources (less than half a source line_10: expected at random with R > 10 on the simple beaming hypothesis). line_11: Thus we extend the 3CR subset to include quasars from higher line_12: frequency radio surveys that favor those with dominant radio line_13: cores. This "extended 3CR" sample is taken from all those radio- line_14: selected QSOs (quasars) observed with the Einstein Observatory line_15: (Browne and Murphy 1986). Nearly all were detected. We further line_16: select those with luminosity in the extended radio emission, line_17: Log(ext), from 26.5 to 27.6 (ergs/s, q=0, H=50 km/s/Mpc). The line_18: extended emission is essentially unbeamed, and this sample gives line_19: us a wide range of the ratio of core to extended radio emission line_20: from about 0.01 to 100 (at v_o = 6 cm), and a wide range of X-ray, line_21: optical and radio core luminosity. For HST observations we propose line_22: to observe those with V < 18.5 and z < 2.1, which allows us to line_23: observe all Ly-Alpha profiles available with HST. ! question: 3 section: 2 line_1: (The remainder of higher z either have been or will be observed line_2: from the ground). Within these lumonisity, redshift, and magnitude line_3: limits about half constitute a complete sample of 3CR quasars. This line_4: "extended 3CR" sample then has several observational advantages: line_5: * The sample extends to larger R, so is more suitable for tests of line_6: beaming, or other correlations with radiocore luminosity. line_7: * The low L(ext) favors small z, and therefore brighter quasars, line_8: that are quicker to observe and have more information (e.g. CIV line_9: profiles etc.) available from other sources. line_10: * Low L(ext) means more low z sources, so there is better linear line_11: resolution from radio structure. line_12: * Being biased toward lower z, the sample is more suitable for line_13: comparison with AGN of lower luminosity,e.g., Seyfert 1's and line_14: broad line radio galaxies. line_15: * The lower z and therefore brighter sample will be easier to line_16: study in the future with IR and X-ray techniques. line_17: We propose to obtain FOS spectra for 42 quasars above rest line_18: wavelengths of 1160A, to observed wavelengths of 4800A, where the line_19: spectra will overlap with our ground based observations from line_20: ~ 3500A to ~ 8000A. We aim for s/n = 10 in the continuum at the line_21: center of each wavelength setting. In this way we will cover all line_22: available strong lines with sufficient s/n to measure accurate line_23: line intensities, central wavelengths and line widths. ! question: 4 section: 1 line_1: If we are to measure UV lines and continua in a complete sample line_2: we must observe quasars of all redshifts. HST is essential for line_3: obtaining the data in low z quasars. line_4: -- we need CIV and other UV lines in a large sample to test line_5: correlations of equivalent widths and velocity widths with other line_6: parameters. line_7: -- we need to cover the UV continuum for a large enough sample to line_8: investigate the relation between X-ray and UV luminosities. line_9: Previously 2500A has been chosen as a standard UV wavelength line_10: accessible for many z's from the ground, but this spectral region line_11: has large contributions from blended Fe II emission. line_12: If we are to investigate the ionization/kinematic structure of the line_13: BLR we must cover a wide wavelength range in individual quasars. We line_14: need to cover a wide range in optical depth (e.g. Ly-Alpha to line_15: H-Beta, and Fe II (UV) to Fe I (opt), ionization, and possible dust line_16: optical depth (e.g. He II 1640 to He II 4686). line_17: We and others have carried out extensive statistical studies line_18: between line and continuum parameters that have lead us to the line_19: need for observations of emission lines in complete samples, line_20: requiring ST for UV lines and continuum in the low redshift members line_21: of the sample. We have attempted some of the proposed correlations line_22: using ground-based observations and the archives of the line_23: International Ultraviolet Explorer Observatory. ! question: 4 section: 2 line_1: Most of the IUE data, obtained in exposures of several hours, line_2: are quite noisy, and of course are only available for the very line_3: brightest quasars. There are problems with absolute flux line_4: calibration due to centering of the object, uncertainties of the line_5: effects of lamp and other pre-exposures, including after-glow line_6: from astronomical exposures. Centering accuracy and temperature line_7: shifts affect the wavelength accuracy. The velocity resolution of line_8: IUE is not adequate to investigate line profiles, to deblend line_9: blended lines, e.g., He II 1640 and O III 1663, and to discriminate line_10: against absorption lines. The statistical spectral analyses we are line_11: proposing would be impossible without HST, and so have never been line_12: attempted before. ! question: 5 section: 1 line_1: Number of objects: line_2: The total number of objects is not very large considering the line_3: number of parameters we wish to investigate statistically, and line_4: our previous statistical studies of less complete samples suggest line_5: that we cannot do with fewer objects. We would rather have more, line_6: but this would not be practical, as there are no more quasars line_7: sufficiently bright at UV-optical wavelengths over the limited line_8: range of L(ext) that we have chosen. Increasing the sample by line_9: extending the range of L(ext) is certainly a possibility we have line_10: considered, bu this would introduce yet another variable into the line_11: statistics -- one we strongly suspect would affect the correlations line_12: we seek. This could be considered in the future, after we have line_13: examined the present sample. line_14: Exposure time calculations: line_15: We have formed a composite quasar spectrum from below Ly-Alpha to line_16: beyond H-Alpha, using 12 luminous quasars from our ground-based line_17: observations, and from our own IUE observations. We then proceed line_18: for each quasar as follows: line_19: 1. Redshift the standard spectrum to that of the quasar. line_20: 2. Apply a standard Galactic reddening curve to the entire line_21: spectrum, using the values of E(B-V) from the maps given by line_22: Burstein and Heiles (1981). ! question: 5 section: 2 line_1: 3. Scale the spectrum so that the V-magnitude in the observer's line_2: frame, determined from the spectrum in part 2., agrees with line_3: that given by published values (Veron-Cetty and Veron 1987) line_4: or our own spectrophotometry. line_5: 4. Multiply this spectrum by the expected HST FOS response for line_6: different grating settings and cameras, and by the curve line_7: representing the wavelength dependent light losses in the 1" line_8: aperture (as these were given in the STScI Newsletter of July line_9: 1988). We have scaled this taking into account the Angstrom per line_10: diode given in the FOS handbook, so that the spectrum is line_11: converted to the number of counts expected per diode per second line_12: (Table 4.2-1 (1), see example in the figure). line_13: 5. We have then calculated the exposure time according to the line_14: formula (Table 4.2-4(9)) given in the handbook, assuming line_15: standard observing procedure and for s/n = 10 for the central line_16: wavelength of the given spectral region. line_17: 6. For the fainter objects we have checked the importance of the line_18: contribution of the Galactic background, using the formula line_19: (table 4.3-1 (13)) from the FOS Handbook. line_20: 7. In cases where an important line falls near a wavelength of low line_21: detector response we increased the exposure time accordingly. line_22: We use the blue digicon rather than the red for G190H if an line_23: important emission line falls between about 1550 and 1700 A. ! question: 7 section: 1 line_1: Initially, some data reduction may be done at STScI to gain line_2: familiarity with quirks in the data, but we expect most of the line_3: reduction to be done using the regularly-updated versions of IRAF line_4: available at the University of Texas and Ohio State University, line_5: together with some local imaging processing software and hardware. line_7: The FOS spectra will be combined with ground-based data at the line_8: University of Texas. Analysis will be done by all team members. line_9: Aspects of the analysis requiring photoionization modeling for line_10: comparison with the individual quasar spectra, etc. will be made line_11: under the direction of H. Netzer and G.J. Ferland. ! question: 8 section: 1 line_1: None, apart from obtaining observing time at McDonald Observatory line_2: for the ground-based spectroscopy. It is not crucial that this be line_3: obtained at exactly the same time as HST data, since most of the line_4: objects in the program are not rapid variables. However, we are line_5: monitoring the photometric variability of objects in the 3CR line_6: sample (Netzer, Wills, Wills, and Ferland -- observations at Wise line_7: Observatory, Tel Aviv University, Israel), a program that will line_8: give us information on changes in optical flux density. We will line_9: attempt to obatin ground-based spectra close in time to the HST line_10: observations, where possible. ! question: 10 section: 1 line_1: Data Analysis facilities, ground-based telescope time, salaries for line_2: senior personnel during the more than two months of time that will line_3: be needed for the data reduction and interpretation. Computer time, line_4: student assistance beyond that requested in the proposal. ! !end of general form text general_form_address: lname: WILLS fname: BEVERLEY mi: J. title: DR. category: PI inst: UNIVERSITY OF TEXAS, AUSTIN addr_1: DEPT. OF ASTRONOMY city: AUSTIN state: TX zip: 78712 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PKS2216-03 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 02O6, pos_2: RA = 22H 18M 52.08S +/- 0.3", pos_3: DEC = -03D 35' 37.4" +/- 0.3" equinox: 2000 rv_or_z: Z = 0.901 comment_1: KNOWN VARIABLE. EXPOSURE TIMES TO comment_2: BE ADJUSTED AS CLOSE TO OBSERVING comment_3: TIME AS FEASIBLE fluxnum_1: 1 fluxval_1: V = 16.6 +/- 1.0 fluxnum_2: 2 fluxval_2: F-CONT(1943) = 2.17 E-15 fluxnum_3: 3 fluxval_3: F-CONT(2767) = 1.69 E-15 fluxnum_4: 4 fluxval_4: F-CONT(4020) = 1.08 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.110 targname: PKS2216-03 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 15S priority: 1 param_1: BRIGHT=33000 param_2: FAINT=660 req_1: ONBOARD ACQ FOR 1.12-1.32; req_2: GROUP 1.11-1.32 WITHIN 48H; req_3: CYCLE 2; comment_1: AT 15-SEP-1993 +/- 7 D; comment_2: OR AT 15-OCT-1993 +/- 7 D; comment_3: OR AT 13-NOV-1993 +/- 7 D ! linenum: 1.120 targname: PKS2216-03 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 11.1M s_to_n: 8.53 fluxnum_1: 2 priority: 1 req_1: CYCLE 2; ! linenum: 1.220 targname: PKS2216-03 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 8.1M s_to_n: 8.53 fluxnum_1: 3 priority: 1 req_1: CYCLE 2; ! linenum: 1.320 targname: PKS2216-03 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G400H wavelength: 4000 num_exp: 1 time_per_exp: 4.9M s_to_n: 8.53 fluxnum_1: 4 priority: 1 req_1: DARK TIME; req_2: CYCLE 2; ! ! end of exposure logsheet ! No scan data records found