! File: 1035C.PROP ! Database: PEPDB ! Date: 15-FEB-1994:23:12:36 coverpage: title_1: BL LAC OBJECTS: AO 0235 + 164: title_2: CYCLE 3 AND 9 OBSERVATIONS sci_cat: QUASARS & AGN sci_subcat: GTO/FOS proposal_for: GTO/FOS cont_id: 1035 pi_fname: E. MARGARET pi_lname: BURBIDGE pi_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO pi_country: USA pi_phone: 619-534-4477 hours_pri: 4.68 num_pri: 1 wf_pc: Y fos: Y ! end of coverpage abstract: line_1: AO0235+164 is an unusual case of a BL Lac object with very weak emission lines, line_2: 2 metallic line absorptions at z = 0.524, 0.851, and variable 21-cm absorption line_3: at z = 0.524. It has a faint emission-line companion 2 arc sec south with z = line_4: 0.524 and another companion 1.3 arc sec East. Special goals for it will be line_5: examination of L alpha absorption at both absorption redshifts, search for UV line_6: emission lines, search for luminosity between AO0235+164 and the (variable?) line_7: companion, or around AO itself, and study of all intervening objects. UV line_8: spectropolarimetry of all objects is planned in another program. ! ! 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: AO 0235+164: 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 3000s, REd G160L 5000s. line_4: The 1.0" aperture will be used. line_5: A 1200s WFC exposure will be done with a B filter. 600s exposures line_6: will be done with an R filter and a wide band filter. line_7: The exact choice will depend on whatever filters line_8: are 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 the low redshift absorption systems. line_3: Good measurements in this object are impossible with the IUE. line_4: Observations of similar systems at higher redshift in the optical are not line_5: suitable because we with to use these observations to study the evolution of line_6: damped Lyman-alpha systems. ! question: 4 section: 2 line_1: The collecting area of HST and the sensitivity of the FOS 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 long observations of AO 0235+164 should only be done if the V line_2: magnitude is less than 17.5. We will monitor the object on a regular line_3: basis and notify the Space telescope science institute when this line_4: condition has been met. We will not require that the object be line_5: observed when it is at its peak brightness, so ability to schedule line_6: within a few months should be sufficient. ! 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: Any emission lines in the spectra will be analyzed by using line_5: IRAF / STSDAS and other existing software to measure line strengths. line_9: The line strengths will be compared to results line_10: from photoionization models. line_13: The absorption features in the spectra will be measured using existing line_14: software that has been used for optical data and the early HST line_15: spectra. The 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_11: Some of these observations were originally written as portions line_12: of observations begun GTO 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: We will attempt to determine the redshift of the BL Lac object AO 0235 + line_2: 164 and the nature of the associated nebulosity. ! !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: AO0235+164 descr_1: E,316,325, descr_2: H,515,516,519 pos_1: RA=2H 38M 38.913S +/- 0.3", pos_2: DEC=16D 36' 59.76" +/- 0.3", pos_3: PLATE-ID = 01G9 equinox: 2000 pm_or_par: NO rv_or_z: Z=.94 fluxnum_1: 1 fluxval_1: V=16.5 +/- 2.0 fluxnum_2: 2 fluxval_2: F(1800)=8 +/- 4 E-17 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: AO0235+164 config: WFC opmode: IMAGE aperture: W1 sp_element: F492M num_exp: 1 time_per_exp: 1200S fluxnum_1: 1 priority: 1 req_2: CYCLE 9 / 1-1.4; req_3: ORIENT 84D +/- 69D / 1-1.4; comment_1: ANGLES +/- 180 D FROM ABOVE ARE OK comment_2: THE OFFSET USED FROM TABLE 12 WAS 315D comment_3: EXACT CHOICE OF FILTER AND EXPOSURE comment_4: WILL DEPEND ON CHARACTERISTICS OF comment_5: WF/PC II (LINES 1.0-1.4) ! linenum: 1.200 targname: AO0235+164 config: WFC opmode: IMAGE aperture: W1 sp_element: F128LP num_exp: 1 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=0.5 req_1: SEQ 1.2-1.4 NO GAP comment_1: THE FILTERS USED IN 1.0-1.4 MAY BE comment_2: CHANGED. THIS DEPENDS ON THE comment_3: FILTERS AVAILABLE WITH WF/PC II. ! linenum: 1.400 targname: AO0235+164 config: WFC opmode: IMAGE aperture: W1 sp_element: F791W num_exp: 1 time_per_exp: 600S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=0.5 ! linenum: 5.000 targname: AO0235+164 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 5.5S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 6.0-7; req_2: SEQ 5-7 NO GAP; req_4: REQ UPDATE / 5-7; req_5: CYCLE 3 / 5-7; comment_1: EXPOSURE WILL BE DONE AFTER comment_2: DETERMINATION THAT OBJECT IS BRIGHT comment_3: ENOUGH FROM GROUND-BASED PHOTOMETRY ! linenum: 6.000 targname: AO0235+164 config: FOS/RD opmode: RAPID aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 3000S s_to_n: 20 fluxnum_1: 1 priority: 2 param_1: READ-TIME=40 ! linenum: 7.000 targname: AO0235+164 config: FOS/RD opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 5000S s_to_n: 10 fluxnum_1: 1 priority: 2 param_1: READ-TIME=40 ! ! end of exposure logsheet ! No scan data records found