! File: 4118C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:09:27:21 coverpage: title_1: DO GALAXIES PRODUCE QUASAR ABSORPTION LINES? : title_2: CYCLE 2 sci_cat: QUASARS & AGN proposal_for: AUG/OS cont_id: 4118 pi_title: DR. pi_fname: JOHN pi_mi: N. pi_lname: BAHCALL pi_inst: INSTITUTE FOR ADVANCED STUDY pi_country: USA pi_phone: (609) 734-8054 keywords_1: QUASAR, SPECTROSCOPY, ABSORPTION LINE, GALAXY, keywords_2: GRAVITATIONAL LENS hours_pri: 4.73 num_pri: 11 wf_pc: X fos: X pi_position: DR. JOHN N. BAHCALL off_fname: ALLEN off_lname: ROWE off_title: ASSOC DIR ADM/FIN off_addr_1: INSTITUTE FOR ADVANCED STUDY off_addr_2: OLDEN LANE off_city: PRINCETON off_state: NJ off_zip: 08540 off_country: USA off_phone: (609) 734-8205 off_telex: 837680 ! end of coverpage abstract: line_1: line_2: SPECTRA WILL BE OBTAINED WITH THE FOS FOR A NUMBER OF QUASARS THAT HAVE A line_3: SMALL ANGULAR SEPARATION ON THE SKY FROM GALAXIES OR GALAXY VOIDS, INCLUDING line_4: MARK 205, 3C 232, PKS 2020-370, THE GRAVITATIONALLY LENSED QUASAR, 2237+0305, 4 line_5: OBJECTS BEHIND THE BOOTES GALAXY VOID, US 1329 (BEHIND THE BAHCALL-SONEIRA line_6: GALAXY VOID), AND 5C 03.44 (BEHIND M 31). THE SPECTRA WILL BE USED TO TEST THE line_7: HYPOTHESIS THAT SOME METALLIC QUASAR ABSORPTION SYSTEMS ARE CAUSED BY VERY line_8: LARGE GALAXY HALOS OR DISKS. WF/PC IMAGES WILL ALSO BE OBTAINED OF THE LENSING line_9: GALAXY, 2237+0305, IN ORDER TO LOCATE ACCURATELY THE QUASAR POSITION AND line_10: MEASURE THE SURFACE BRIGHTNESS OF THE INNER REGION OF THE GALAXY. ST line_11: OBSERVATIONS ARE REQUIRED BECAUSE, FOR THE SMALL REDSHIFTS AT WHICH GALAXIES line_12: WITH LARGE ANGULAR SIZE ARE FOUND, THE RESONANT ATOMIC LINES ARE IN THE line_13: ULTRAVIOLET. ! ! end of abstract general_form_proposers: lname: BAHCALL fname: JOHN mi: N. inst: INSTITUTE FOR ADVANCED STUDY country: USA ! lname: RATNATUNGA fname: KAVAN inst: INSTITUTE FOR ADVANCED STUDY country: USA ! lname: BAHCALL fname: NETA mi: A. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Eleven objects behind galaxy halos or voids will be observed with the FOS. line_2: Cycle 1 (1-6 months, SV) = Exposures 4,5,6,22,24,38,40 line_3: Cycle 2 (7-18 months) = Exposures 1,2,3,8,9,10,14,15,22,23,33-37,39 line_4: Cycle 3 + 4 (19-30 months) = Exposures 7,11,12,13,16,17,18,19,20,21 line_6: Exposures 6,24 and 40 should be taken consecutively. They will fix the line_7: position of the quasar relative to the center of the galaxy 2237+0305. It line_8: would be desirable if the low dispersion observation with the FOS, exposure 22, line_9: could be scheduled within one week of exposures 6, 24 and 40 although it is not line_10: essential. We want to avoid large variations of the quasar relative to the line_11: galaxy in the period between the imaging exposures 6,24, and 40 and the line_12: spectroscopic observation in exposure 22. line_14: Exposures 6, 24 and 40 should be centered on the center of one CCD line_15: (immaterial which one). ! question: 4 section: 1 line_1: ST observations are required to reach the relevant ultraviolet wavelengths at line_2: which the absorption features occur. For 2237+0305, ST observations are needed line_3: to locate the quasar images and to measure the characteristics of the inner line_4: region of the galaxy, a well as to study the absorption lines. ! question: 5 section: 1 line_1: Exposures 6, 24, and 40 should be taken consecutively. They will fix the line_2: position of the quasar relative to the center of the galaxy 2237+0305. It line_3: would be desirable if the low dispersion observation with the FOS, exposure 22, line_4: could be scheduled within one week of exposures 6, 24, and 40 although it is line_5: not essential. We want to avoid large variations of the quasar relative to the line_6: galaxy in the period between the imaging exposures 6, 24, and 40 and the line_7: spectroscopic observation in exposure 22. ! question: 6 section: 1 line_1: Exposures 6 and 24 should be taken consecutively. Exposures 6, 24, and 40 line_2: should be centered on thhe center of one CCD (immaterial which one). line_4: Parallel observations should be as long as possible and in dark time (if line_5: scheduling permits). ! question: 7 section: 1 line_1: The spectra of 3C 232 will be analyzed collaboratively with B. Savage line_2: (University of Wisconsin) to determine what absorption lines are produced by line_3: the intervening galaxy NGC 3067. An additional FOS observation of this object line_4: with G130H will be obtained by Savage in his proposal entitled: "Absorption by line_5: Extragalactic Gaseous Halos." line_7: Data reduction and analysis for the other spectroscopic observations will be line_8: performed at IAS, using the IAS VAX facilities and peripherals. The images of line_9: 2237+0305 will be analyzed with the image processing system developed by D. line_10: Schneider. Quasar continuum intensities and emission-line equivalent widths line_11: will be measured at KPNO by R. Green. ! question: 8 section: 1 line_1: Improved positions for the quasars will be measured optically at KPNO by R. line_2: Green using existing plates. ! question: 10 section: 1 line_1: Full computing support will be supplied by IAS. Research collaborators are line_2: available. ! question: 13 section: 1 line_1: Spectra will be obtained with the FOS for a number of quasars that have a small line_2: angular separation on the sky from galaxies or galaxy voids, including Mark line_3: 205, 3C 232, PKS 2020-370, the gravitationally lensed quasar, 2237+0305, 4 line_4: objects behind the Bootes galaxy void, US 1329 (behind the Bahcall-Soneira line_5: galaxy void), and 5C 03.44 (behind M 31). The spectra will be used to test the line_6: hypothesis that some metallic quasar absorption systems are caused by very line_7: large galaxy halos or disks. WF/PC images will also be obtained of the lensing line_8: galaxy, 2237+0305, in order to locate accurately the quasar position and to line_9: measure the surface brightness of the inner region of the galaxy. ! !end of general form text general_form_address: lname: BAHCALL fname: JOHN mi: N. title: DR. category: PI inst: INSTITUTE FOR ADVANCED STUDY addr_1: OLDEN LANE city: PRINCETON state: NJ zip: 08540 country: USA phone: (609) 734-8054 telex: 837680 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PG1411+442 name_2: PB1732 descr_1: E,313 pos_1: RA = 14H 13M 48.3S +/- 0.1S, pos_2: DEC = +44D 00' 13" +/- 1.0" equinox: 2000 pm_or_par: NO rv_or_z: Z=0.089 fluxnum_1: 1 fluxval_1: V = 15.0 +/- 0.2 ! targnum: 2 name_1: PG1538+477 descr_1: E,313 pos_1: RA = 15H 39M 34.8S +/- 0.1S, pos_2: DEC = +47D 35' 31" +/- 1.0" equinox: 2000 pm_or_par: NO rv_or_z: Z=0.770 fluxnum_1: 1 fluxval_1: V = 16.0 +/- 0.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PG1411+442 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.3S priority: 1 req_1: ONBOARD ACQ FOR 1.1; req_2: SEQ 1.0-5.0 NO GAP ; req_3: CYCLE 2 / 1-6.5 comment_1: SEQ 1-5 MUST BE MERGED comment_2: INTO SAME OBSSET ! linenum: 1.100 targname: PG1411+442 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 2S priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 2.0,3.0,4.0 ; req_2: SPATIAL SCAN ! linenum: 2.000 targname: PG1411+442 config: FOS/RD opmode: RAPID aperture: 0.25X2.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 800S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 ! linenum: 3.000 targname: PG1411+442 config: FOS/RD opmode: RAPID aperture: 0.25X2.0 sp_element: G190H wavelength: 1900 num_exp: 1 time_per_exp: 2000S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 ! linenum: 4.000 targname: PG1411+442 config: FOS/BL opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3S priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 5.0 ; req_2: SPATIAL SCAN ! linenum: 5.000 targname: PG1411+442 config: FOS/BL opmode: RAPID aperture: 0.25X2.0 sp_element: G130H wavelength: 1300 num_exp: 1 time_per_exp: 8200S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 ! linenum: 6.000 targname: PG1538+477 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 8.2S priority: 1 req_1: ONBOARD ACQ FOR 6.1; req_2: SEQ 6.0-6.5 NO GAP ! linenum: 6.100 targname: PG1538+477 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 8S priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 6.5 ; req_2: SPATIAL SCAN ! linenum: 6.500 targname: PG1538+477 config: FOS/RD opmode: RAPID aperture: 0.25X2.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 2000S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: READ-TIME=40 ! ! end of exposure logsheet scan_data: line_list: 1.1,4.0,6.1 fgs_scan: cont_dwell: D dwell_pnts: 9 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: 0.2000 wid_offset: 0.0000 ! ! end of scan data