! File: 3268C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:00:39:44 coverpage: title_1: UV SPECTRA OF QSOS WITH Z > 3.1: title_2: CYCLE 2 OBSERVATIONS sci_cat: QUASARS & AGN sci_subcat: GTO/FOS proposal_for: GTO/FOS cont_id: 1027 pi_fname: E. MARGARET pi_lname: BURBIDGE pi_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO pi_country: USA pi_phone: 619-534-4477 hours_pri: 2.42 num_pri: 2 fos: Y ! end of coverpage abstract: line_1: This proposal contains observations which will help to complete one FOS line_2: IDT scientific program. line_3: In a collaborative programs with the GHRS IDT, we will study absorption line_4: from He I and He II in the Lyman alpha forest clouds and in the intergalactic line_5: medium at high z to determine conditions in the early universe. line_6: We will observe the extreme UV rest spectrum of QSOs with z > line_7: 2.9, to examine HeI and HeII in absorption and/or emission, as well as line_8: He I in some lower z QSOs. Perform Gunn-Peterson test for smooth line_9: intergalactic helium. These observations are primarily exploratory to line_10: find quasars with light at these short wavelengths. We will also line_11: Study the continuum shape of QSOs from 300 A (rest) to lambda line_12: > 2500A (rest). ! ! 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: For each object, the following observations will be made with the blue line_2: detector and the large aperture: binary search target acquisition, line_3: 1200s G160L, 600s Prism. ! question: 4 section: 1 line_1: There are no known QSOs with redshifts high enough to study the He II line_2: lambda304 line in the optical. The He II lambda304 Gunn--Peterson test line_3: is predicted to be interesting around redshifts 3 to 5. Similar line_4: arguments are true for He I lambda584. ! 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: 5 section: 1 line_1: The special requirement REQ UPDATE is included here because epoch 2000 line_2: coordinates have not yet been determined with GASP. These will be line_3: done by us very shortly. - NOTE: GASP coords were obtained by observers line_4: and subsequently entered into the proposal. REQ UPDATE special requirements line_5: were then removed. -June 1992 ! question: 6 section: 1 line_1: The wavelength region of greatest interest in these objects is at the line_2: shortest wavelength. This is strongly contaminated by geocoronal line_3: lines of Lyman-alpha and O I during the day, particularly with the line_4: large aperture we will be using. Thus the G160L observations must be line_5: done in DARK TIME. ! 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. ! 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. ! question: 13 section: 1 line_1: FOS spectra will be obtained of 5 quasars with z > 3.1 to examine HeI and line_2: HeII in absorption and/or emission and perform the Gunn-Peterson test for line_3: smooth intergalactic helium. ! !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: 7 name_1: UM670 descr_1: E,313, descr_2: H,515,519 pos_1: RA = 1H 17M 23.338S +/- 0.1", pos_2: DEC = -08D 41' 32.38" +/- 0.1", pos_3: PLATE-ID = 00WP equinox: 2000 pm_or_par: NO rv_or_z: Z=3.16 fluxnum_1: 1 fluxval_1: V=17.4 +/- 1.0 ! targnum: 12 name_1: 1334-005 name_2: UM590 descr_1: E,313, descr_2: H,515,519 pos_1: RA = 13H 36M 47.132S +/- 0.1", pos_2: DEC = -0D 48' 57.74" +/- 0.1", pos_3: PLATE-ID = 02OA, equinox: 2000 pm_or_par: NO rv_or_z: Z=2.85 fluxnum_1: 1 fluxval_1: V=17 +/- 1.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 27.000 targname: 1334-005 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 164.1S fluxnum_1: 1 priority: 1 param_1: BRIGHT=700000 req_1: ONBOARD ACQ FOR 27.6-27.7; req_2: SEQ 27.0-27.7 NO GAP; req_3: CYCLE 2 / 27.0-27.7; ! linenum: 27.600 targname: 1334-005 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L wavelength: 1650 num_exp: 1 time_per_exp: 1200S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 req_1: DARK TIME; ! linenum: 27.700 targname: 1334-005 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: PRISM wavelength: 3500 num_exp: 1 time_per_exp: 600S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40, ! linenum: 35.500 targname: UM670 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 199S fluxnum_1: 1 priority: 1 param_1: BRIGHT=700000 req_1: ONBOARD ACQ FOR 35.6-35.7; req_2: SEQ 35.5-35.7 NO GAP; req_3: CYCLE 2 / 35.5-35.7; ! linenum: 35.600 targname: UM670 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L wavelength: 1650 num_exp: 1 time_per_exp: 1200S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 req_1: DARK TIME; ! linenum: 35.700 targname: UM670 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: PRISM wavelength: 3500 num_exp: 1 time_per_exp: 600S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40, ! ! end of exposure logsheet ! No scan data records found