! File: 4978C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:13:25:36 coverpage: title_1: LYMAN-ALPHA REGION OF QSOS WITH STRONG ABSORPTION LINES: title_2: FUTURE CYCLE OBSERVATIONS - EXPO sci_cat: QUASARS & AGN sci_subcat: QUASAR ABSORPTION proposal_for: GTO/HRS cont_id: 1193 pi_title: DR. pi_fname: EDWARD pi_lname: BEAVER pi_inst: UC, SAN DIEGO pi_country: USA pi_phone: (619) 534-1878 keywords_1: QUASARS, ABSORPTION LINES, 21-CM hours_pri: 1.68 num_pri: 2 wf_pc: Y pi_position: RESEARCH PHYSICIST ! end of coverpage abstract: line_1: FOS spectra have been obtained of the Ly-alpha region of 3 quasars line_2: with 21 cm absorption, 3CR 196, PKS 1229-021, and 3CR 286. line_3: The absorbing object is almost certainly a galaxy disk in each case. line_4: Measurement of the damped Ly-alpha line will determine the H I column line_5: density in the 21 cm absorption system, and comparison with 21 cm will line_6: yield the spin temperature. The number of contributing components will line_7: be determined from existing or new 21 cm observations. Comparison with line_8: optical observations will allow the determination of chemical line_9: abundances with respect to H for elements with low-ionization lines. line_10: Images taken after the new WF/PC installation may identify the line_11: absorbing galaxy and, if so, will allow us to characterize the impact line_12: parameter and Hubble type of galaxies producing damped Ly-alpha line_13: absorption at moderate redshift. Two of these will be done in this line_14: proposal. ! ! end of abstract general_form_proposers: lname: COHEN fname: ROSS inst: UC, SAN DIEGO country: USA ! lname: BEAVER fname: EDWARD inst: UC, SAN DIEGO country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will use the WFC with F702W line_2: to image 3CR 196 and PKS1229-021. 1200S per image. ! question: 4 section: 1 line_1: The absorbing objects are lost in the point spread function of the line_2: quasar in ground-based images. ! question: 7 section: 1 line_1: These observations will be reduced using the standard imaging line_2: reduction software available for WF/PC data. Calibration line_3: will be done using the results of SV observations. line_4: Already existing software will be used to subtract the image of line_5: the background quasar. ! 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 DEPT., C0111 addr_2: 9500 Gilman Drive city: LA JOLLA state: CA zip: 920930111 country: USA phone: (619)534-2664 telex: (619)534-6316(FAX) ! lname: BEAVER fname: EDWARD title: DR. category: PI inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO addr_1: CASS DEPT., C011 addr_2: 9500 Gilman Drive city: LA JOLLA state: CA zip: 920930111 country: USA phone: 619-534-1878 telex: (619)534-6316(FAX) ! ! end of general_form_address records fixed_targets: targnum: 2 name_1: PKS1229-021 name_2: 4C02.55 descr_1: E,314, descr_2: H,515,516 pos_1: RA=12H 31M 59.999S +/- 0.3", pos_2: DEC=-02D 24' 5.34" +/- 0.3", pos_3: PLATE-ID = 00BB equinox: 2000 rv_or_z: Z=1.038 fluxnum_1: 1 fluxval_1: V=16.75+/-1.0 ! targnum: 3 name_1: 3C196 name_2: 4C48.22 descr_1: E,314, descr_2: H,515,516 pos_1: RA=08H 13M 36.059S +/- 0.3", pos_2: DEC=48D 13' 2.49" +/- 0.3", pos_3: PLATE-ID = 02HE equinox: 2000 rv_or_z: Z=0.871 fluxnum_1: 1 fluxval_1: V=17.8+/-1.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 8.000 targname: PKS1229-021 config: WFC opmode: IMAGE aperture: ANY sp_element: F702W num_exp: 1 time_per_exp: 1200S fluxnum_1: 1 priority: 1 req_1: CYCLE 9 / 8 ! linenum: 13.000 targname: 3C196 config: WFC opmode: IMAGE aperture: ANY sp_element: F702W num_exp: 1 time_per_exp: 1200S fluxnum_1: 1 priority: 1 req_1: CYCLE 9 / 13 ! ! end of exposure logsheet ! No scan data records found