! File: 4120C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:09:31:31 coverpage: title_1: UV SPECTRA OF LOW-REDSHIFT-QSOS: title_2: CYCLE 3 AND LATER OBSERVATIONS sci_cat: QUASARS & AGN sci_subcat: GTO/FOS proposal_for: GTO/FOS cont_id: 1026 pi_fname: E. MARGARET pi_lname: BURBIDGE pi_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO pi_country: USA pi_phone: 619-534-4477 hours_pri: 7.10 num_pri: 5 wf_pc: Y fos: Y ! end of coverpage abstract: line_1: This proposal contains observations which will help to complete a number of FOS line_2: IDT scientific programs. These programs are not in direct conflict with line_3: approved GO or GTO programs, but explore wavelength or signal-to-noise regimes line_4: not covered by other programs, or else they concentrate on objects of special line_5: interest. These programs will lead to a better understanding of the structure line_6: and kinematics of the broad-line region by studies of very high signal-to-noise line_7: line profiles in low redshift QSOs. The same data will also provide line_8: measurements of weak lines which will lead to improved photoionization models. line_10: This data set will yield high quality absorption line line_11: data for studies of specific absorption line systems and an independent sample line_12: for studies of absorption line evolution. ! ! end of abstract general_form_proposers: lname: HARMS fname: RICHARD mi: J. inst: APPLIED RESEARCH CORPORATION country: USA ! lname: ALLEN fname: RICHARD mi: G. inst: UNIVERSITY OF ARIZONA country: USA ! lname: ANGEL fname: J. ROGER mi: P. inst: UNIVERSITY OF ARIZONA country: USA ! lname: BARTKO fname: FRANK inst: UNAFFILIATED country: USA ! lname: BEAVER fname: EDWARD inst: UC, SAN DIEGO country: USA ! lname: BOHLIN fname: RALPH mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: BURBIDGE fname: E. MARGARET title: PI inst: UC, SAN DIEGO country: USA ! lname: DAVIDSEN fname: AURTHUR mi: F. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: FORD fname: HOLLAND mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: HARTIG fname: GEORGE mi: F. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: MARGON fname: BRUCE mi: H. inst: UNIVERSITY OF WASHINGTON country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: NAB0205+02: After a binary search target acquisition with the red line_2: detector, the following exposures will be taken in RAPID mode: line_3: Red G270H 1230s, Red G190H 3300s. The 1.0" aperture will be used. line_4: PG 2302+029: After a binary search target acquisition with the red line_5: detector, the following exposure will be taken in RAPID mode: line_6: Red G270H 3300s. The 1.0" aperture will be used. line_7: 1E0302+029: After a binary search target acquisition with the red line_8: detector, a 7 point peak up will be done to center the object in line_9: the 0.25X2.0 slit. Then the following exposure will be taken in line_10: rapid mode: Red G270H 3700s. The 0.25X2.0 slit will be used. line_11: PKS0454-220: A 1200s WFC exposures with whatever broad band filter line_12: is available with WFC II. line_13: 3C 286: A 1200s PC exposures with one of the red filters line_14: available with WFC II. ! question: 4 section: 1 line_1: The HST UV capability is needed to measure Lyman-alpha and C IV line_2: lambda1549 and other lines in low redshift QSOs. By combining HST and line_3: optical spectra, it is possible to study line pairs such as line_4: Lyman-alpha and H-alpha with accurate wavelengths, good sampling of line_5: broad lines and good signal to noise. HST and optical spectra are line_6: needed to measure accurate emission line intensities for weak lines line_7: over a large range of rest wavelengths in individual objects. Emission line_8: line velocity differences cannot be easily determined from IUE data line_9: combined with ground based data because the IUE wavelength calibration line_10: is uncertain. QSO emission line profile studies using IR data or IUE line_11: data are limited by the available low signal to noise. The evolution line_12: of C IV lambda1549 absorption systems and the Lyman-alpha forest at line_13: redshifts from 0.0 to 1.06 and 1.63 respectively can only be studied line_14: from space. ! question: 4 section: 2 line_1: The collecting area of HST and the sensitivity of the FOS and GHRS line_2: make it possible to obtain spectra with the signal to noise needed to line_3: carry out these studies of QSOs at wavelengths below the atmospheric line_4: cutoff. ! question: 7 section: 1 line_1: These observations will be reduced using the standard spectroscopy line_2: reduction software available for FOS data. Calibration line_3: will be done using the results of SV observations. line_4: The emission lines in the spectra of QSOs will be analyzed by using line_5: IRAF / STSDAS and other existing software to measure line strengths. line_6: Blended lines and the continuum will be subtracted from the strong line_7: broad emission lines to determine line profiles which will be compared line_8: to emission lines observed in the optical and to the predictions of line_9: kinematical models. The line strengths will be compared to results line_10: from photoionization models. Additional analysis will be done by line_11: dividing broad line profiles to obtain line ratios as a function of line_12: velocity (Shuder 1982). line_13: The absorption features in QSO spectra will be measured using existing line_14: software that has been used for optical data and the early HST line_15: spectra. The evolution of C IV lambda1549 absorption systems with line_16: redshift will be studied by counting these systems and carrying out line_17: the necessary statistical analysis. Unidentified lines below line_18: Ly-alpha emission are candidate Ly-alpha forest lines and will line_19: contribute to studies of the evolution of these absorbers. Metal line line_20: systems will be studied by using curves of growth to obtain estimates line_21: and limits to column densities. ! question: 8 section: 1 line_1: line_2: Optical spectroscopy and line_3: photometry will be performed using the facilities of Lick Observatory. line_4: We will try to make the optical observations simultaneous with the line_5: HST UV observations if possible. ! question: 9 section: 1 line_1: Collaborators have received data from a number of GTO programs, SAT, line_2: and ERO programs. Related programs which have had observations are as line_3: follows: line_4: 1026 - ``UV Spectra of Low-Redshift-QSOs'', line_5: 1027 - ``UV Spectra of QSOs with z$> 3.1$'', line_6: 1029 - ``Spectropolarimetry of QSOs, Blazars, and AGN'', and line_7: 1033 - ``Search for Misdirected BL Lac Objects''. line_8: Low resolution observations of three high redshift QSOs have not line_9: revealed any with light at He II lambda 304. Observations of UM 675 line_10: have shown that any He I Gunn--Peterson effect is small, that He I line_11: absorption lines are not strong, that predictions of the ``Lyman line_12: valley'' may be correct, and that low redshift Ly-alpha is more line_13: prevalent than expected. Observations of low redshift QSOs (including line_14: 3C 273) have shown even more clearly that Ly-alpha absorption occurs line_15: in greater numbers than expected, as well as showing emission--line line_16: profile differences more clearly than from earlier data. line_17: Unexpectedly, Ly-alpha is narrower than H-alpha. ! question: 9 section: 2 line_1: ``HST Imaging of the Inner 3 Arcseconds of NGC 1068 in the Light of [O line_2: III] lambda5007'', I.N.Evans, H.C.Ford, A.L.Kinney, R.R.J.Antonucci, line_3: L.Armus, and S.Caganoff, {\it Ap.J.(Lett.)}, {\bf 369}, L27, 1991. line_4: ``Faint Object Camera Observations of a Globular Cluster Nova Field'', line_5: B.Margon, S.F.Anderson, R.A.Downes, R.C.Bohlin, and P.Jakobsen, {\it line_6: Ap.J.(Lett.)}, {\bf 369}, L71, 1991. line_7: ``Far--Ultraviolet Spectroscopy of the Quasar UM 675 with the Faint line_8: Object Spectrograph on the Hubble Space Telescope'', E.A.Beaver, line_9: E.M.Burbidge, R.D.Cohen, V.T.Junkkarinen, R.W.Lyons, E.I.Rosenblatt, line_10: G.F.Hartig, B.Margon, and A.F.Davidsen, {\it Ap.J.(Lett.)}, {\bf 377}, line_11: L1, 1991. line_12: ``The Ultraviolet Absorption Spectrum of 3C 273'', J.N.Bahcall, line_13: B.T.Jannuzi, D.P.Schneider, G.F.Hartig, R.Bohlin, and V.Junkkarinen, line_14: {\it Ap.J.(Lett.)}, {\bf 377}, L5, 1991. line_15: ``Faint Object Spectrograph Spectroscopy of Resolved Structure in the line_16: Nucleus of NGC 1068'', S.Caganoff, R.R.J.Antonucci, H.C.Ford, line_17: G.A.Kriss, G.Hartig, L.Armus, I.N.Evans, E.Rosenblatt, R.C.Bohlin, and line_18: A.L.Kinney, {\it Ap.J.(Lett.)}, {\bf 377}, L9, 1991. line_19: ``Faint Object Spectrograph Observations of the Low-Luminosity Seyfert line_20: Galaxy NGC 1566'', G.A.Kriss, G.F.Hartig, L.Armus, W.P.Blair, line_21: S.Caganoff, and L.Dressel, {\it Ap.J.(Lett.)}, {\bf 377}, L13, 1991. ! question: 10 section: 1 line_1: The majority of the resources required for this project other than the line_2: normal facilities of a university (librarys, offices, etc.) were line_3: supplied by NASA to the members of the FOS IDT for these projects. line_4: These include all the computing facilities required for the completion line_5: of data reduction and analysis. line_6: Optical and IR ground--based observing facilities and support are line_7: provided by the University of California and the University of line_8: Arizona. ! !end of general form text general_form_address: lname: BURBIDGE fname: E. MARGARET category: PI inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO addr_1: CASS 0111, UCSD addr_2: 9500 GILMAN DRIVE city: LA JOLLA state: CA zip: 920930111 country: USA phone: 619-534-4477 ! ! end of general_form_address records fixed_targets: targnum: 2 name_1: NAB0205+02 name_2: GSC-I 40 162 name_3: MRK586 descr_1: E,313,321,923, descr_2: H,515,519 pos_1: RA = 2H 7M 49.848S +/- 0.3", pos_2: DEC = 2D 42' 55.32" +/- 0.3", pos_3: PLATE-ID = 0086 equinox: 2000 pm_or_par: NO rv_or_z: Z=0.155 fluxnum_1: 1 fluxval_1: V=15.4 +/- 0.5 fluxnum_2: 2 fluxval_2: F(1900)=1.0 +/- 0.2 E-14 ! targnum: 4 name_1: PKS0454-22 descr_1: E,314,321, descr_2: H,515,516 pos_1: RA = 4H 56M 8.903S +/- 0.3", pos_2: DEC = -21D 59' 9.38" +/- 0.3", pos_3: PLATE-ID = 029V equinox: 2000 pm_or_par: NO rv_or_z: Z=0.534 fluxnum_1: 1 fluxval_1: V=16.1 +/- 0.5 ! targnum: 12 name_1: PG2302+029 descr_1: E,313,321,923, descr_2: H,515,519 pos_1: RA = 23H 4M 44.956S +/- 0.3", pos_2: DEC = 3D 11' 46.42" +/- 0.3", pos_3: PLATE-ID = 02JH equinox: 2000 pm_or_par: NO rv_or_z: Z=1.044 fluxnum_1: 1 fluxval_1: V=16.0 +/- 1.0 fluxnum_2: 2 fluxval_2: F(2430)=1.75 +/- 0.3 E-15 ! targnum: 18 name_1: 1E0302-223 descr_1: E,313, descr_2: H,515,519 pos_1: RA = 03H 04M 49.823S +/- 0.3", pos_2: DEC = -22D 11' 51.91" +/- 0.3", pos_3: PLATE-ID = 025C equinox: 2000 pm_or_par: NO rv_or_z: Z=1.40 fluxnum_1: 1 fluxval_1: V=16.3 +/- 0.5 fluxnum_2: 2 fluxval_2: F(2380) = 2.0 +/- 0.2 E-15 ! targnum: 20 name_1: 3C286 descr_1: E,314,321, descr_2: H,515,516 pos_1: RA=13H 31M 8.293S +/- 0.3", pos_2: DEC=30D 30' 32.86" +/- 0.3", pos_3: PLATE-ID = 009L equinox: 2000 pm_or_par: NO rv_or_z: Z=0.849 comment_1: THIS OBSERVATION HAS BEEN SWAPPED comment_2: FROM ANOTHER FOS IDT GTO PROGRAM, comment_3: NUMBER 1032. THE REST OF THAT comment_4: PROGRAM IS BEING WITHDRAWN.THE PI comment_5: WAS H. FORD, AND IS NOW comment_6: E. M. BURBIDGE. fluxnum_1: 1 fluxval_1: V=17.25+/-1.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 2.500 targname: NAB0205+02 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 7.5S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 700000 req_1: ONBOARD ACQ FOR 2.59-2.9; req_2: SEQ 2.5-2.9 NO GAP; req_3: CYCLE 3 / 2.5-2.9 ! linenum: 2.590 targname: NAB0205+02 config: FOS/RD opmode: RAPID aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 1230S s_to_n: 30 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 ! linenum: 2.900 targname: NAB0205+02 config: FOS/RD opmode: RAPID aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 3300S s_to_n: 30 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 ! linenum: 6.500 targname: PG2302+029 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 7.5S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 700000 req_1: ONBOARD ACQ FOR 6.59; req_2: SEQ 6.5-6.59 NO GAP; req_3: CYCLE 3 / 6.5-6.59 ! linenum: 6.590 targname: PG2302+029 config: FOS/RD opmode: RAPID aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 3300S s_to_n: 30 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 ! linenum: 15.000 targname: PKS0454-22 config: WFC opmode: IMAGE aperture: ANY sp_element: F128LP num_exp: 1 time_per_exp: 1200S fluxnum_1: 1 priority: 1 req_1: CYCLE 9 /15 comment_1: EXACT FILTER CHOICE WILL DEPEND ON comment_2: WHAT IS AVAILABLE WITH THE comment_3: REPLACEMENT WF/PC ! linenum: 41.000 targname: 1E0302-223 config: FOS/RD 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 42; req_3: CYCLE 3 /41-43 ! linenum: 42.000 targname: 1E0302-223 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 22S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 43.0; req_2: SPATIAL SCAN ! linenum: 43.000 targname: 1E0302-223 config: FOS/RD opmode: RAPID aperture: 0.25X2.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 3700S s_to_n: 30 fluxnum_1: 2 priority: 1 param_1: READ-TIME=40 ! linenum: 50.000 targname: 3C286 config: PC opmode: IMAGE aperture: ALL sp_element: F850LP num_exp: 1 time_per_exp: 1200S fluxnum_1: 1 priority: 1 req_1: CYCLE 9 / 50 comment_1: THIS OBS. WAS TAKEN FROM FOS IDT GTO comment_2: PGM. NUMBER 1032. THE REST OF THAT PGM comment_3: IS BEING WITHDRAWN.THE PI WAS H. FORD, comment_4: AND IS NOW E. M. BURBIDGE.EXACT FILTER comment_5: CHOICE WILL DEPEND ON WHAT IS comment_6: AVAILABLE WITH THE REPLACEMENT WF/PC ! ! end of exposure logsheet scan_data: line_list: 42.0 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: 0.2 wid_offset: ! ! end of scan data