coverpage: title_1: PHYSICAL CONDITIONS IN LOW Z ABSORPTION LINE SYSTEMS IN QSOS title_2: AUGMENTATION: CYCLE 4 CARRYOVER sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: AUG/HRS cont_id: 4867 pi_title: DR. pi_fname: EDWARD pi_lname: BEAVER pi_inst: UC, SAN DIEGO pi_country: USA pi_phone: (619) 534-1878 keywords_1: QUASAR, SPECTROSCOPY, ABSORPTION LINES hours_pri: 3.03 num_pri: 1 fos: Y pi_position: RESEARCH PHYSICIST ! end of coverpage abstract: line_1: In PG 1630+377, line_2: we will use the FOS to line_3: measure associated Ly-alpha and Ly-beta lines. The relative line_4: abundance of He I determined this way should yield clues to line_5: the conditions in the Lyman-alpha forest clouds and in the line_6: IGM at moderate redshift. ! ! end of abstract general_form_proposers: lname: COHEN fname: ROSS mi: D. inst: UC, SAN DIEGO country: USA ! lname: BEAVER fname: EDWARD title: PI mi: A. inst: UC, SAN DIEGO country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Following a binary search target acquisition in the 4.3" aperture with line_2: the red detector, and two peak-up acquisitions in the 0.3" aperture line_3: (critical and non critical), two external exposures will be made with line_4: the FOS and the 0.5" aperture in ACCUM mode. line_5: First, a 2000s observation with G270H line_6: and then a 2660s observation with G190H will be made. line_7: A default length wavelength calibration will be taken with line_8: each scan. ! question: 4 section: 1 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. These absorption lines cannot be measured in the optical. ! question: 6 section: 1 line_1: Experience has shown that the FOS has siginficant wavelength line_2: errors due to the uncertainty in the setting of the filter/ line_3: grating wheel. In many cases this is not a problem, but for line_4: this program we require greater accuracy because we must line_5: know whether lines detected in two FOS settings line_6: belong to the same system. There are generally no line_7: suitable interstellar absorption lines in G190H, and those line_8: (sometimes strong) lines in G270H may be contaminated by line_9: the Lyman alpha forest in this object. ! 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_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 He I line_20: systems will be studied by using curves of growth to obtain estimates line_21: and limits to column densities. ! question: 9 section: 1 line_1: PI has received data from a number of line_2: GTO programs, SAT, and ERO programs. Related line_3: programs which have had observations are as line_4: follows: line_5: 1026 - ``UV Spectra of Low-Redshift-QSOs'': related, line_6: 1027 - ``UV Spectra of QSOs with z> 3.1'': not related, line_7: 1190 - ``FUV Emission LIne Profiles of W Serpentis line_8: Binaries'': not related line_11: Observations of UM 675 have shown line_12: that any He I Gunn--Peterson effect is small, that line_13: He I absorption lines are not strong, that line_14: predictions of the ``Lyman valley'' may be line_15: correct, and that low redshift Ly-alpha is more line_16: prevalent than expected. Observations of low line_17: redshift QSOs (including 3C 273) have shown even line_18: more clearly that Ly-alpha absorption occurs in line_19: greater numbers than expected, as well as showing line_20: emission--line profile differences more clearly line_21: than from earlier data. Unexpectedly, Ly-alpha line_22: is {\it narrower} than H-alpha. line_23: ``Far--Ultraviolet Spectroscopy of the Quasar UM ! question: 9 section: 2 line_1: 675 with the Faint Object Spectrograph on the line_2: Hubble Space Telescope'', E.A.Beaver, line_3: E.M.Burbidge, R.D.Cohen, V.T.Junkkarinen, line_4: R.W.Lyons, E.I.Rosenblatt, G.F.Hartig, B.Margon, line_5: and A.F.Davidsen, {\it Ap.J.(Lett.)}, {\bf 377}, line_6: L1, 1991. line_7: ``First Results from the GHRS: UV Spectra of a line_8: Starburst Knot in NGCC 1068'', Hutchings, J.B., line_9: Bruhweiler, G.C., Boggess, A., Heap, S.R., Ebbets, line_10: D.C., Beaver, E., Rosenblatt, E., Truonmg, K.Q., line_11: Perez, M., and Westmacott, R., 1991, APJ line_12: (Letters), 377, 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 GHRS 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. ! !end of general form text general_form_address: lname: COHEN fname: ROSS category: CON inst: UNIV. OF CALIF., SAN DIEGO addr_1: CASS 0111 UCSD addr_2: 9500 Gilman Drive city: LA JOLLA state: CA zip: 920930111 country: USA phone: (619) 534-2664 telex: 534-6316 (FAX) ! lname: BEAVER fname: EDWARD 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) 534-1878 telex: 534-6316 (FAX) ! ! end of general_form_address records fixed_targets: targnum: 5 name_1: PG1630+377 descr_1: E,313,321, descr_2: H,515,519 pos_1: RA = 16H 32M 1.101S +/- 0.2", pos_2: DEC = 37D 37' 49.45" +/- 0.2", pos_3: PLATE-ID = 01RW equinox: 2000 pm_or_par: NO rv_or_z: Z=1.471 fluxnum_1: 1 fluxval_1: V = 15.96+/- 1.0 fluxnum_2: 2 fluxval_2: F(1500) = 5.0 +/- 1.0 E-15 fluxnum_3: 3 fluxval_3: F(2200) = 3.8 +/- 1.0 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 42.000 targname: PG1630+377 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=700000 param_2: FAINT=330 req_1: ONBOARD ACQ FOR 42.1; req_2: SEQ 42.0-42.5 NO GAP; req_3: CYCLE 4 / 42.0-42.5; ! linenum: 42.100 targname: PG1630+377 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=4 param_3: SEARCH-SIZE-Y=4 param_4: SCAN-STEP-X=0.18 param_5: SCAN-STEP-Y=0.18 req_1: ONBOARD ACQ FOR 42.2; ! linenum: 42.200 targname: PG1630+377 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 7S fluxnum_1: 1 priority: 1 param_1: TYPE=UP, param_2: SEARCH-SIZE-X=5 param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-X=0.052 param_5: SCAN-STEP-Y=0.052 req_1: ONBOARD ACQ FOR 42.4-42.5; ! linenum: 42.400 targname: WAVE config: FOS/RD opmode: ACCUM aperture: 0.5 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 42.45; comment_1: DO NOT MOVE THE FILTER/GRATING comment_2: WHEEL BETWEEN 42.4 AND 42.45 ! linenum: 42.450 targname: PG1630+377 config: FOS/RD opmode: ACCUM aperture: 0.5 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2000S s_to_n: 40 fluxnum_1: 3 priority: 1 ! linenum: 42.470 targname: WAVE config: FOS/RD opmode: ACCUM aperture: 0.5 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 42.500; comment_1: DO NOT MOVE THE FILTER/GRATING comment_2: WHEEL BETWEEN 42.470 AND 42.5 ! linenum: 42.500 targname: PG1630+377 config: FOS/RD opmode: ACCUM aperture: 0.5 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 2660S s_to_n: 35 fluxnum_1: 3 priority: 1 ! ! end of exposure logsheet