! $Id: 5177,v 6.1 1994/08/24 19:38:17 pepsa Exp $ coverpage: title_1: PHYSICAL CONDITIONS IN LOW Z ABSORPTION LINE SYSTEMS IN QSOS: title_2: CYCLE 4 sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: GTO/HRS cont_id: 1191 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: 13.72 num_pri: 1 fos: Y ! end of coverpage abstract: line_1: In PG 1630+377, we will use the HRS to measure lines of line_2: He I at 584A, and we will use the FOS (in a different line_3: proposal) to measure associated Ly-alpha and Ly-beta lines. line_4: The relative abundance of He I determined this way should line_5: yield clues to the conditions in the Lyman-alpha forest line_6: clouds and the IGM at high 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 ! lname: SMITH fname: HARDING mi: E. inst: UC, SAN DIEGO country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: PG1630+377: Following a target acq, a 16254s exposure will be made line_2: with the GHRS and G140L in the large science aperture. The target acq. line_3: will be done in two steps. First a spiral search with return to the line_4: brightest point, then an acq/peak to improve the centering in the 2.0" line_5: aperture. We will measure the dark from the corner diodes. line_6: The wavelength scale will be centered at 1317 Angstroms, and cover line_7: approximately from 1170A--1463A. ! question: 3 section: 2 line_1: The HRS spectra will be broken into approximately 5 minute segments to line_2: allow for shifting in wavelength to correct for geomagnetic and line_3: thermal drifts. Additionally, the 5 minute observations will be line_4: grouped into longer exposure logsheet lines (approx. 65 and 70 min). line_5: Each of these segments will be preceded by a SPYBAL and a wavelength line_6: lamp observation. The SPYBALs will correct for drifts perpendicular line_7: to the diode array and the wavelength lamps will allow us to correct line_8: for errors in the thermal and magnetic drift models, as well as errors line_9: in resetting the carrousel after the SPYBALs. The SPYBALs should line_10: occur close in time to the observations, but should NOT be placed line_11: between the wavelength lamp and the observations of the object. line_12: This proposal should run after the HRS side 1 is returned to service. ! question: 4 section: 1 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. The He lines cannot be studied in the optical. Some line_5: of the lines on PKS 0735 could be observed in the optical in high line_6: redshift systems in other objects, but they would be confused with line_7: lines in the heavily populated Lyman-alpha forest. Additionally, we line_8: can compare the UV absorption to optical absorption lines which would line_9: not be seen in high redshift systems. The HST image is line_10: required to show the absorbing object which would be hidden under the line_11: quasar point spread function in the optical image. ! question: 5 section: 1 line_1: ! question: 6 section: 1 line_1: Because of the large wavelength drifts which will occur over the line_2: course of the entire observation, periodic measurements of the line_3: wavelength scale are required in order to reconstruct the spectrum of line_4: this faint object. They are also required both to check on the line_5: accuracy of the carrousel repositioning after the SPYBALs and to line_6: correct for any errors in the model of thermal and magnetic drift. line_7: Individual wavelength calibrations for the HRS observations of PKS0735 line_8: will also help to reduce the errors for intercomparison of absorption line_9: line profiles between different grating settings and between HRS and line_10: ground based data. For PG1630, accurate wavelengths are required to line_11: identify lines of He I with associated H I Lyman lines observed with the line_12: FOS. ! ! 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: 1 name_1: PG1630+377 descr_1: E,313, descr_2: H,515,519 pos_1: RA = 16H 32M 1.101S +/- 0.5", pos_2: DEC = 37D 37' 49.45" +/- 0.5", 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 +/- 0.5 fluxnum_2: 2 fluxval_2: F(1500) = 4.2 +/- 1.0 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 41.000 targname: PG1630+377 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 41.4S fluxnum_1: 1 priority: 1 param_1: BRIGHT = RETURN, param_2: MAP = DEF, param_3: SEARCH-SIZE=3, param_4: LOCATE=YES req_1: ONBOARD ACQ FOR 41.1; req_2: SEQ 41.0-42.35; req_3: CYCLE 4 / 41.0-42.35; comment_1: USED 4.6 SEC STEP-TIMES. comment_2: IF THIS PROGRAM IS BROKEN INTO comment_3: PARTS, REPEAT LINES 41.0 AND 41.1 comment_4: AS NECESSARY. ! linenum: 41.100 targname: PG1630+377 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 357.0S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 42.0-42.35 comment_1: USED 3.5S SEC STEP-TIMES. comment_2: THIS ACQ REFINES THE CENTERING comment_3: AFTER B-FIELD & THERMAL SHIFTS. ! linenum: 42.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1317 num_exp: 1 time_per_exp: 1M priority: 1 req_1: CALIB FOR 42.05 NO SLEW; req_3: SEQ 42.0-42.05 NO GAP; comment_1: THE Y-BAL. FOR 42.05 SHOULD BE DONE comment_2: PRIOR TO LINE 42.0. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 42.0 AND 42.05. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL; comment_6: W/O DRIFT ! linenum: 42.050 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 14 time_per_exp: 300.8S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 42.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1317 num_exp: 1 time_per_exp: 1M priority: 1 req_1: CALIB FOR 42.15 NO SLEW; req_3: SEQ 42.1-42.15 NO GAP; comment_1: THE Y-BAL. FOR 42.15 SHOULD BE DONE comment_2: PRIOR TO LINE 42.1. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 42.1 AND 42.15. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL comment_6: W/O DRIFT ! linenum: 42.150 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 14 time_per_exp: 300.8S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 42.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1317 num_exp: 1 time_per_exp: 1M priority: 1 req_1: CALIB FOR 42.25 NO SLEW; req_3: SEQ 42.20-42.25 NO GAP; comment_1: THE Y-BAL. FOR 42.25 SHOULD BE DONE comment_2: PRIOR TO LINE 42.20. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 42.2 AND 42.25. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL comment_6: W/O DRIFT. ! linenum: 42.250 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 13 time_per_exp: 300.8S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! linenum: 42.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1317 num_exp: 1 time_per_exp: 1M priority: 1 req_1: CALIB FOR 42.35 NO SLEW; req_3: SEQ 42.30-42.35 NO GAP; comment_1: THE Y-BAL. FOR 42.35 SHOULD BE DONE comment_2: PRIOR TO LINE 42.30. DO NOT INSERT A comment_3: SPYBAL AND MOVE CAROUSEL BETWEEN comment_4: LINES 42.30 AND 42.35. comment_5: SEQ IS TO OBTAIN A WAVELENGTH CAL comment_6: W/O DRIFT ! linenum: 42.350 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 13 time_per_exp: 300.8S s_to_n: 6.5 fluxnum_1: 2 priority: 1 param_1: STEP-PATT = 3, param_2: CENSOR = YES ! ! end of exposure logsheet ! No scan data records found