! File: 4177C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:12:13:26 coverpage: title_1: PHYSICAL CONDITIONS IN LOW Z ABSORPTION LINE SYSTEMS IN QSOS: title_2: FUTURE OBSERVATIONS 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: 7.48 num_pri: 2 wf_pc: Y fos: Y ! end of coverpage abstract: line_1: In PKS 0735+178, we will observe the Ly-alpha region with the line_2: FOS and shorter wavelengths with the HRS. The line_3: primary goal will be to measure abundances relative to H I line_4: of low ionization ions measured in the optical and in the line_5: Ly-alpha exposure. An image should show the absorbing line_6: object, indicating where in the ISM of the absorber the line_7: measured abundances occur. These observations will allow line_8: comparison with higher redshift QSO absorption line systems line_9: and with absorption from galaxy halos, the leading candidate line_10: for the site of such absorption. line_11: In PG 1630+377, we will use the HRS to line_12: measure lines of He I at 584A, and we will use the FOS (in a line_13: different proposal) to line_14: measure associated Ly-alpha and Ly-beta lines. The relative line_15: abundance of He I determined this way should yield clues to line_16: the conditions in the Lyman-alpha forest clouds and the IGM line_17: 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: PKS 0735+178: Following target acquisition, a 3340S exposure will be line_2: made with the GHRS and G140L in the large aperture. The target acq. line_3: will be done in three 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, and last an image to check on the centering. An FOS line_6: observation will also be made. Following a binary search target line_7: acquisition in the 4.3" aperture with the FOS red detector, a peak-up line_8: will be used to center the object in the 0.25X2.0 slit. After this a line_9: 2420S RAPID mode observation with G190H will be made. The line_10: spectroscopic observations are marked REQ UPDATE, because optical line_11: observations may show that the object is too faint to observe. The WFC line_12: will be used for a 1200s F725LP exposure (or whatever similar filter line_13: is available after the installation of WF/PC II. line_16: PG1630+377: Following target acquisition, a 6300S exposure will be made line_17: with the GHRS and G140L in the large aperture. The target acquisition line_18: will be done in three steps. First a spiral search with return to the line_19: brightest point, then an acq/peak to improve the centering in the 2.0" line_20: aperture, and last an image to check on the centering. The line_21: spectroscopic observation will be split into a number of parts to line_22: help remove the effects of image motion. ! question: 3 section: 2 line_1: 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: Because PKS0735+178 is variable, we must check that it is bright line_2: enough (with optical observations) prior to sceduling. line_3: The HRS target acquisitions for both objects must be done in DARK time line_4: because of the relative brightness of geocoronal Lyman-alpha. ! question: 6 section: 1 line_1: Individual wavelength calibrations for the HRS line_2: observations are required to reduce line_3: the errors for intercomparison of absorption line profiles line_4: between different grating settings and between HRS and line_5: ground based data. line_6: The HRS target acquisitions for both objects must be done line_7: in DARK time because of the relative brightness of line_8: geocoronal Lyman-alpha. ! question: 7 section: 1 line_1: These observations will be reduced using the standard spectroscopy line_2: reduction software available for FOS and HRS data. Calibration line_3: will be done using the results of SV observations. 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. Unidentified lines below line_7: Ly-alpha emission are candidate Ly-alpha forest lines and will line_8: contribute to studies of the evolution of these absorbers. The He I line_9: and metal line systems will be studied by using curves of growth to line_10: obtain estimates and limits to column densities. line_11: The quasar image will be subtracted from the WFC images using existing line_12: software. ! 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: PKS0735+178 name_2: GSC-I 1365 1765 descr_1: E,316,H,515,519 pos_1: RA = 07H 38M 7.376S +/- 0.3", pos_2: DEC = 17D 42' 18.64" +/- .3", pos_3: PLATE-ID = 01LS equinox: 2000 pm_or_par: NO fluxnum_1: 1 fluxval_1: V = 16.5 +/- 2.0 fluxnum_2: 2 fluxval_2: F(1600) = 1.0 +/- 1.0 E-14 ! targnum: 5 name_1: PG1630+377 descr_1: E,313,321, descr_2: H,515,519 pos_1: RA = 16H 32M 1.171S +/- 0.2", pos_2: DEC = 37D 37' 48.69" +/- 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) = 3.0 +/- 1.0 E-15 fluxnum_3: 3 fluxval_3: F(1900) = 2.0 +/- 1.0 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 2.750 targname: PKS0735+178 config: WFC opmode: IMAGE aperture: ANY sp_element: F725LP num_exp: 1 time_per_exp: 1200S fluxnum_1: 1 priority: 1 req_1: CYCLE 9/2.75-4.0 ! linenum: 3.000 targname: PKS0735+178 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.34S fluxnum_1: 1 priority: 1 param_1: BRIGHT = RETURN param_4: LOCATE=YES req_1: ONBOARD ACQ FOR 3.1; req_2: SEQ 3.0-4.0 NO GAP; req_3: CYCLE 9/3.0-4.0; req_4: DARK TIME comment_1: USED 0.26 SEC STEP-TIMES. comment_2: DARK TIME REQ'D DUE TO comment_3: REL BRIGHTNESS OF GEOCORONAL comment_4: BKGRND WRT THE QSO. ! linenum: 3.100 targname: PKS0735+178 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 26.52S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 3.2; comment_1: USED 0.26 SEC STEP-TIMES. comment_2: THIS ACQ REFINES THE CENTERING comment_3: AFTER B-FIELD INDUCED SHIFTS. ! linenum: 3.200 targname: PKS0735+178 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 33.54S fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE = 1 param_2: MAP = END-POINT param_3: LOCATE = NO param_4: FAINT = 0 req_1: ONBOARD ACQ FOR 3.5-4.0; comment_1: TAKE MAP AFTER CENTERING OBJ comment_3: USED 1.73S SEC STEP-TIME. ! linenum: 3.500 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1431.83 num_exp: 1 time_per_exp: 2S priority: 1 req_1: CALIB FOR 4 NO SLEW comment_1: THE OBJECT IS TOO FAINT FOR STANDARD comment_2: Y-BALANCE. THIS WAVE IS FOR comment_3: WAVELENGTH CALIBRATION OF 4.00. THE comment_4: Y-BALANCE FOR 4.00 SHOULD BE DONE comment_5: FROM A WAVELENGTH LAMP ALSO. ! linenum: 4.000 targname: PKS0735+178 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1431.83 num_exp: 1 time_per_exp: 3340S s_to_n: 20 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 comment_1: EXPOSURE TIME MAY BE VARIED OR comment_2: EXPOSURE CANCELED OR POSTPONED comment_3: DEPENDING ON THE RESULTS OF OPTICAL comment_4: OBSERVATIONS ! linenum: 11.000 targname: PKS0735+178 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 param_1: BRIGHT=375000 req_1: ONBOARD ACQ FOR 11.5; req_2: CYCLE 9/11-12.0 ! linenum: 11.500 targname: PKS0735+178 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 param_1: TYPE = UP req_1: ONBOARD ACQ FOR 12.0; req_2: SPATIAL SCAN ! linenum: 12.000 targname: PKS0735+178 config: FOS/RD opmode: RAPID aperture: 0.25X2.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 2420S s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: READ-TIME = 40 req_1: SEQ 11-12 NO GAP; ! linenum: 41.000 targname: PG1630+377 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.34S fluxnum_1: 1 priority: 1 param_1: BRIGHT = RETURN param_4: LOCATE=YES req_1: ONBOARD ACQ FOR 41.1; req_2: SEQ 41.0-41.8 NO GAP; req_3: CYCLE 9/41-41.8; req_4: DARK TIME comment_1: USED 0.26 SEC STEP-TIMES. comment_2: DARK TIME REQ'D DUE TO comment_3: REL BRIGHTNESS OF GEOCORONAL comment_4: BKGRND WRT THE QSO. ! linenum: 41.100 targname: PG1630+377 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 26.52S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 41.2; comment_1: USED 0.26 SEC STEP-TIMES. comment_2: THIS ACQ REFINES THE CENTERING comment_3: AFTER B-FIELD INDUCED SHIFTS. comment_4: NO GAP 41.5-41.8 TO PREVENT LARGE TIME comment_5: INTERVALS BETWEEN EXPS WHICH MAY comment_6: YIELD LARGE B-FIELD INDUCED SHIFTS. ! linenum: 41.200 targname: PG1630+377 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 33.54S fluxnum_1: 2 priority: 1 param_1: SEARCH-SIZE = 1 param_2: MAP = END-POINT param_3: LOCATE = NO param_4: FAINT = 0 req_1: ONBOARD ACQ FOR 41.5; comment_1: TAKE MAP AFTER CENTERING OBJ comment_3: USED 1.73S SEC STEP-TIME. ! linenum: 41.500 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1317 num_exp: 1 time_per_exp: 30S priority: 1 req_1: CALIB FOR 41.6 NO SLEW; req_2: NON-INT / 41.5-41.6 comment_1: NON-INT 41.5-41.6 TO OBTAIN AN ABS comment_2: WAVELENGTH CALIB W/O DRIFT. THE Y-BAL comment_3: FOR 41.600 SHOULD BE DONE FROM A comment_4: WAVELENGTH LAMP PRIOR TO LINE comment_5: 41.5. DO NOT INSERT A SPYBAL AND MOVE comment_6: CAROUSEL BETWEEN LINES 41.5 AND 41.65. ! linenum: 41.600 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 2 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 comment_1: OBS WAS LINKED TO 41.500 NON-INT comment_2: TO OBTAIN AN ACCURATE WAVECAL W/ comment_3: MINIMAL B-FIELD INDUCED DRIFT. ! linenum: 41.650 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 6 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 comment_1: OBS WAS DIVIDED INTO MANY PARTS TO comment_2: HELP REMOVE B-FIELD INDUCED SHIFTS comment_3: AND TO PREVENT TOTAL DATA LOSS. ! linenum: 41.700 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1317 num_exp: 1 time_per_exp: 30S priority: 1 req_1: CALIB FOR 41.75 NO SLEW; req_2: NON-INT / 41.7-41.75; comment_1: THIS WAVE IS FOR WAVELENGTH comment_2: CALIBRATION OF 41.750. THE Y-BAL comment_3: FOR 41.75 SHOULD BE DONE FROM A comment_4: WAVE LAMP BETWEEN LINES 41.65 AND comment_5: 41.7. DO NOT INSERT A SPYBAL AND MOVE comment_6: CAROUSEL BETWEEN LINES 41.7 AND 41.8. ! linenum: 41.750 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 1 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 comment_1: OBS WAS LINKED TO 41.700 NON-INT comment_2: TO OBTAIN AN ACCURATE WAVECAL W/ comment_3: MINIMAL B-FIELD INDUCED DRIFT. ! linenum: 41.800 targname: PG1630+377 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1317 num_exp: 12 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5 comment_1: OBS WAS DIVIDED INTO MANY PARTS TO comment_2: HELP REMOVE B-FIELD INDUCED SHIFTS comment_3: AND TO PREVENT TOTAL DATA LOSS. ! ! end of exposure logsheet scan_data: line_list: 11.5 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 0.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 0.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2 wid_offset: ! ! end of scan data