coverpage: title_1: UV SPECTRA OF LOW-REDSHIFT-QSOS AUGMENTATION: title_2: CYCLE 4 CARRYOVER sci_cat: QUASARS & AGN sci_subcat: AUG/FOS proposal_for: AUG/FOS cont_id: 4079 pi_fname: E. MARGARET pi_lname: BURBIDGE pi_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO pi_country: USA pi_phone: 619-534-4477 hours_pri: 5.38 num_pri: 2 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: COHEN fname: ROSS mi: D. 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: JUNKKARINEN fname: VESA mi: T. inst: UC, SAN DIEGO 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: PG0026+12: After a binary search target acquisition with the blue line_2: detector, the following exposure will be taken in ACCUM mode: line_3: Blue G130H, 1.0" aperture. Then switch to the red side line_4: and do a peak up with the 0.5" aperture followed by spectra with line_5: G270H and G190H with the 1.0" aperture. line_6: The order of sides may be switched. line_7: MC1548+114A: 25 minute WFC exposure with F702W. Place the 8" off the line_8: the standard center of WF3 to ensure that the entire region of line_9: interest avoids the charge trap. ! 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 and line_2: polarimetry 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: Optical polarimetry and photometry will be performed using the line_2: facilities of Steward Observatory. 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. This imposes no requirements on HST line_6: scheduling except as noted in question 5. line_7: Coordinates for a few objects need to be determined to the accuracy line_8: required for target acquisition. These can easily be obtained from line_9: the guide star data base using the existing software. line_10: There are a number of related FOS IDT GTO proposals in cycles 0, 1, line_11: and 2. Most of these observations were originally written as portions line_12: of observations begun in those proposals. Thus the observations line_13: included here contain both the baseline and augmented portions. Some line_14: observations were moved from augmented to baseline proposals to line_15: balance this. ! 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: 1 name_1: PG0026+12 name_2: GSC-I 602 1173 descr_1: E,313,321,923, descr_2: H,515,519 pos_1: RA = 0H 29M 13.710S +/- 0.3", pos_2: DEC = 13D 16' 3.86" +/- 0.3", pos_3: PLATE-ID = 028X equinox: 2000 pm_or_par: NO rv_or_z: Z=0.142 fluxnum_1: 1 fluxval_1: V=15.14 +/- 0.05 fluxnum_2: 2 fluxval_2: F(1500)=2.0 +/- 0.5 E-14 ! targnum: 9 name_1: MC1548+114A descr_1: E,314,321, descr_2: H,515,519 pos_1: RA = 15H 50M 43.599S +/- 1.0", pos_2: DEC = 11D 20' 47.74" +/- 1.0", pos_3: PLATE-ID = 00J1 equinox: 2000 pm_or_par: NO rv_or_z: Z=0.436 acqpr_1: COMP fluxnum_1: 1 fluxval_1: V=17.0 +/- 1.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.500 targname: PG0026+12 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 6.5S fluxnum_1: 2 priority: 1 param_1: BRIGHT = 700000 param_2: FAINT = 330 req_1: ONBOARD ACQ FOR 1.55; req_2: GROUP 1.5-1.9 NO GAP; req_3: CYCLE 4 / 1.5-1.9 comment_1: red side time would be 1.7S ! linenum: 1.550 targname: PG0026+12 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 9600S s_to_n: 15 fluxnum_1: 2 priority: 1 ! linenum: 1.560 targname: PG0026+12 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 2 priority: 1 param_1: SCAN-STEP-X=0.3 param_2: SCAN-STEP-Y=0.3 param_3: SEARCH-SIZE-X=3 param_4: SEARCH-SIZE-Y=3 req_1: ONBOARD ACQ FOR 1.59-1.9; comment_1: peak up after side switch comment_2: recommended by instrument scientist comment_3: A new BSTA is OK with us if it comment_4: is easier to schedule. ! linenum: 1.590 targname: PG0026+12 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 540S s_to_n: 15 fluxnum_1: 2 priority: 1 ! linenum: 1.900 targname: PG0026+12 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 828S s_to_n: 15 fluxnum_1: 2 priority: 1 ! linenum: 20.000 targname: MC1548+114A config: WFPC2 opmode: IMAGE aperture: WF3 sp_element: F702W num_exp: 1 time_per_exp: 1500S fluxnum_1: 1 priority: 1 req_1: CYCLE 4; req_2: POS TARG -5.66,-5.66 comment_1: pos target should move the object comment_2: 8" off nominal in the V3 direction. ! ! end of exposure logsheet ! No scan data records found