coverpage: title_1: UV SPECTRA OF LOW-REDSHIFT QSOS, HE I title_2: AUGMENTATION: CYCLE 4 CARRYOVER sci_cat: QUASARS & AGN sci_subcat: AUG/FOS proposal_for: AUG/FOS cont_id: 4078 pi_fname: E. MARGARET pi_lname: BURBIDGE pi_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO pi_country: USA pi_phone: 619-534-4477 hours_pri: 2.90 num_pri: 1 fos: Y ! end of coverpage abstract: line_1: In a collaborative program with the GHRS IDT, we will study absorption line_2: from He I in the Lyman alpha forest clouds and in the intergalactic line_3: medium at high z to determine conditions in the early universe. line_4: Lyman alpha and beta lines will be measured in this proposal. The He I line_5: lines will be measured in another proposal. ! ! 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:A specially designed series of peak-ups will be performed to center the line_2:brightest object to +/-0.08" and a 2250s ACCUM observation performed with the line_3:0.3" aperture, G270H grating, and red detector. A blind offset of 0.485" will line_4:be made to the second brightest object and another 2250s ACCUM observation will line_5:be made. Because the two targets are separated by only 0.485", a conventional line_6:peakup beginning with the 4.3" aperture would not work, while starting with a line_7:binary search places restrictions on the orientation and still requires a line_8:complex peakup because of the relatively large positional uncertainty following line_9:BSTA. Likewise for an interactive target acquisition. line_10:The errors in the measurements of offset stars and possible proper line_11:motion are too large to allow any simple scheme of offsets followed by peakups. line_12:The error budget is very small because the separation of the two brightest line_13:components is 0.48" so the maximum error that can be tolerated is 0.24" which line_14:means the one sigma error along the line connecting the two brightest components line_15:should not exceed 0.08". There are no WF images of the PG1115+080 field and the line_16:PC images of PG 1115+080 do not include the best offset stars. Ground based line_17:images (from CFHT) include the best offset stars but appear rotated relative to line_18:the PC images by 1.35 degrees. The error in the correction of the CCD rotation line_19:combined with centering and offset errors plus plausible proper motion (over 5 line_20:years) exceed the error budget allowable for acquisition of one of the fainter line_21:gravitational lens images and completely rule out direct offsets to either of line_22:the two brightest components from the best offset star about 51" away. ! question: 4 section: 1 line_1: He I lambda 584 cannot be observed redshifted into the optical in any line_2: known quasar. This object is one of the two best candidates for line_3: making these measurements. The associated Lyman-alpha and beta lines line_4: in this object also lie in the UV. ! 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 ! 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 standard calibrations. line_4: The absorption features in QSO spectra will be measured using existing line_5: software that has been used for optical data and the early HST line_6: spectra. The H I column densities for comparison with the He I line_7: will be determined from curve-of-growth fits to L-alpha and L-beta. ! 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. line_10: There are a number of related FOS IDT GTO proposals in cycles 0-3. line_11: These observations were originally written as portions line_12: of observations begun in those proposals. ! 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: 4 name_1: PG1115+080A1 descr_1: E,313,323,923, descr_2: H,515,519 pos_1: RA = 11H 18M 16.934S +/- 1.0", pos_2: DEC = 07D 45' 58.53" +/- 1.0", pos_3: PLATE-ID = 00ZW, equinox: 2000 pm_or_par: NO rv_or_z: Z=1.722 acqpr_1: COMP fluxnum_1: 1 fluxval_1: V=17.0 +/- 1.0 fluxnum_2: 2 fluxval_2: F(2500)=1.5 +/- 0.3 E-15 ! targnum: 7 name_1: PG1115+080A2 descr_1: E,313,323,923, descr_2: H,515,519 pos_1: R = 0.485" +/- 0.03", pos_2: PA = 18.4D +/- 2D, pos_3: FROM 4, pos_4: PLATE-ID = 00ZW, equinox: 2000 pm_or_par: NO rv_or_z: Z=1.722 acqpr_1: COMP fluxnum_1: 1 fluxval_1: V=17.3 +/- 1.0 fluxnum_2: 2 fluxval_2: F(2500)=1.1 +/- 0.3 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.0 targname: PG1115+080A1 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1.39S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=0.61 param_2: SCAN-STEP-Y=0.61 param_3: SEARCH-SIZE-X=5 param_4: SEARCH-SIZE-Y=5 req_1: ONBOARD ACQ FOR 2.0; req_2: SEQ 1.0-4.0 NO GAP; req_3: CYCLE 4 / 1.0-4.0; ! linenum: 2.0 targname: PG1115+080A1 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 1.5S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=0.3 param_2: SCAN-STEP-Y=0.3 param_3: SEARCH-SIZE-X=4 param_4: SEARCH-SIZE-Y=4 req_1: ONBOARD ACQ FOR 2.5 ! linenum: 2.5 targname: PG1115+080A1 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.6S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=0.17 param_2: SCAN-STEP-Y=0.17 param_3: SEARCH-SIZE-X=4 param_4: SEARCH-SIZE-Y=4 req_1: ONBOARD ACQ FOR 2.6 ! linenum: 2.6 targname: PG1115+080A1 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 15.8S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-X=0.06 param_2: SCAN-STEP-Y=0.06 param_3: SEARCH-SIZE-X=5 param_4: SEARCH-SIZE-Y=5 req_1: ONBOARD ACQ FOR 3.0 ! linenum: 3.0 targname: PG1115+080A1 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2250S s_to_n: 15 fluxnum_1: 2 priority: 1 ! linenum: 4.0 targname: PG1115+080A2 config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2250S s_to_n: 15 fluxnum_1: 2 priority: 1 comment_1: Blind offset after line 3.0 comment_2: Total move is 0.485" ! ! end of exposure logsheet ! No scan data records found