! $Id: 5692,v 28.1 1995/01/26 21:12:58 pepsa Exp $ coverpage: title_1: A STUDY OF THE ARCSECOND GRAVITATIONAL LENS 1422+231 title_2: CYCLE 4 CARRYOVER sci_cat: QUASARS & AGN sci_subcat: GRAVITATIONAL LENSES proposal_for: GO/CAR cont_id: 4402 pi_fname: CHRIS pi_mi: D. pi_lname: IMPEY pi_inst: STEWARD OBSERVATORY pi_country: USA pi_phone: 602-621-6522 hours_pri: 4.00 num_pri: 5 fos: Y funds_amount: 81920 funds_length: 12 off_fname: MICHAEL off_mi: A. off_lname: CUSANOVICH off_title: V.P. FOR RESEARCH off_inst: UNIVERSITY OF ARIZONA off_addr_1: ADMINISTRATION BLDG 601 off_addr_2: UNIVERSITY OF ARIZONA off_city: TUCSON off_state: AZ off_zip: 85721 off_country: USA off_phone: 602-621-3513 ! end of coverpage abstract: line_1: We propose spectroscopy and imaging of the four components of the line_2: candidate gravitational lens 1422+231. This is the brightest of the line_3: few known examples of subarcsecond multiply imaged quasars. It was line_4: selected from a survey of 1750 flat spectrum radio sources which line_5: should be particularly effective at finding subarcsecond lenses. line_6: With V = 16.5 (all components) and z = 3.62, this is one of the line_7: most apparently luminous objects in the universe. Spectroscopy line_8: of optical counterparts to the four radio components will clearly line_9: establish whether or not the system is a gravitational lens, and line_10: imaging with the FOC (in prop 5699) is very likely to identify the lens, even if line_11: it is a highly subluminous galaxy. A system with line_15: four components offers the prospect of a large number of constraints line_16: on the lensing model. Moreover, the radio sources are compact line_17: and highly polarized, and so very likely to be variable. 1422+231 line_18: could therefore be used in a VLA or VLBA monitoring campaign to line_19: derive a new estimate of the Hubble constant using up to three line_20: time delays. Confirmation of the lens can only be done from space. ! ! end of abstract general_form_proposers: lname: IMPEY fname: CHRIS title: PI mi: D. inst: STEWARD OBSERVATORY country: USA ! lname: FOLTZ fname: CRAIG mi: B. inst: MULTIPLE MIRROR TELESCOPE country: USA ! lname: BROWNE fname: IAN mi: W. inst: NUFFIELD RADIO ASTRONOMY LABORATORIES country: UNITED KINGDOM esa: Y ! lname: PATNAIK fname: ALOK mi: R. inst: NUFFIELD RADIO ASTRONOMY LABORATORIES country: UNITED KINGDOM esa: Y ! lname: SHAPIRO fname: IRWIN inst: HARVARD SMITHSONIAN CENTER FOR ASTROPHYSICS country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose two observations of the candidate gravitational lens 1422+231. line_2: The first is spectroscopy of individual radio components A, B, C, and D using line_3: the FOS red side with grating G570H which gives wavelength coverage from 4600 to line_4: 6800 Angstroms. Exposure times are calculated assuming that the system is indeed line_5: a lens, and that the optical fluxes scale with the radio fluxes. Fluxes for the line_6: sum of A+B+C are taken from Figure 2. The 0.3 arcsec circular aperture will be line_7: used; any larger and the components will not be separated, any smaller is not line_8: practical with the PSF of the HST. An integration time of 1500 seconds line_9: will give a S/N = 15 per resolution element in the continuum at 4800 Angstroms line_10: for components A and B, and 3000 seconds will give S/N = 14 for component C. line_11: High S/N spectra of A, B, and C are essential to confirm the lens hypothesis. line_12: High redshift quasars generally have similar continuum shapes, and there is line_13: already one case of an (unlensed) quasar pair with virtually identical spectra line_14: and a small velocity difference (Djorgovski et al. 1987, Ap.J., 321, L17). line_15: Limited S/N has so far hampered the interpretation of one other subarcsecond line_16: lens (Bahcall et al. 1992, in press); we note however that 1208+101 is line_17: considerably fainter than our candidate system. If D is a lens component, an line_18: integration time of 6200 seconds will be used to get a S/N = 7 in the putative line_19: Lyman-alpha line, allowing a clear-cut test of this fourth component. question: 3 section: 2 line_1: Addition by P. Stanley: line_3: This program consists of 2 visits. Visit 1 uses the FOS in imaging mode line_4: to obtain data on whether the onboard tar acq s/w acquires A line_5: or B. Offsets are performed from the acq assumed to be of component B - the line_6: 1st offset is to A, the second in the opposite directions. If images 1,2 contain line_7: the expected components, lines 10-14 will be used in visit 2. If images 1,3 line_8: contain the components, it means we acquired component A instead of B line_9: and lines 20-24 will executed. We will use the SAVE EPHEMERIS line_10: (Re-use target offset capability) prior to executing the subsequent visit. ! question: 4 section: 1 line_1: The small separation of the components of this candidate gravitational lens line_2: system mean that observations from HST are essential for these observations. line_3: The overall extent of the radio source is 1.3 arcsec, the separation between line_4: A and B is 0.5 arcsec, and the separation between B and C is 0.8 arcsec (see line_5: Figure 1). While imaging of 1422+231 might be possible from the ground under line_6: the very best conditions, FOC observations still offer substantial advantages. line_7: Since the PSF gives a core of 10% of the image flux with a FWHM of only 0.07 line_8: arcsec, the bright components A, B, and C are expected to be well separated. line_9: Moreover, the presence of three bright point sources in the field means that line_10: image deconvolution will be well constrained, which is an advantage in the line_11: search for the lens. Confirmation of the 1422+231 system as a gravitational line_12: lens relies mostly on spectroscopy of components A, B, and C. The capabilities line_13: of HST in making this observation are unique, no ground-based facility can line_14: compete. Successful HST confirmation of the lens system will lead to important line_15: ground-based follow-up at radio wavelengths. The lens conponents are well line_16: separated with the VLA or VLBA, and are compact and polarized. Compactness line_17: and high polarization implies that they are also highly likely to be variable. line_18: A radio monitoring program offers the exciting possibility of a new geometric line_19: determination of the Hubble Constant, in a system where up to three time delays line_20: can be measured. (FOC exps in prop 5691) ! question: 4 section: 2 line_1: line_2: Figure 2 shows the flux density of the sum of the three brightest components A, line_3: B, and C. The FOS exposure time calculations are based on the assumption that line_4: the relative fluxes of all four components is given by their relative radio line_5: fluxes (this assumption is confirmed by recent, unpublished imaging of the line_6: system in the near infrared). Count rates are calculated at two wavelength, line_7: in the middle of the continuum shortward of Lyman-alpha at 4800 Angstroms, line_8: and at the half power of the Lyman-alpha line around 5700 Angstroms. The line_9: calculated count rates for components A, B, C, and D are 0.18, 0.18, 0.088, line_10: and 0.0044 ct/s/diode at 4800 Angstroms, and 0.60, 0.60, 0.30, and 0.015 line_11: ct/s/diode at 5700 Angstroms (this assumes that all the components have line_12: Lyman-alpha with the same equivalent width). The exposure times are calculated line_13: to give S/N = 15 for components A (1500 sec), B (1500 sec), and C (3000 sec), line_14: and to give S/N = 7 at half power of the predicted Lyman-alpha line in component line_15: D (6200 sec). ! question: 5 section: 1 line_1: Due to the minimal separation and nearly equal brightness of components line_2: A and B, the offsets performed by the 4 stage peakup in lines 1-4 will be line_3: measured and uplinked prior to the start of visit 2 (lines 10-14 or 20-24). line_4: The selected visit 2 observations must be at the same roll and line_5: with the same guide stars as visit 1. ! ! question: 9 section: 1 line_1: a. List HST program numbers and titles: line_2: GO Program 2524 "Spectropolarimetry of Bright Quasars" - not related line_3: GO Program 3732 "Spectropolarimetry of Bright Quasars" - not related line_4: GO Program 3648 "Imaging of BL Lac Host Galaxies and Environments" - not related line_5: b. Summarize the main results obtained from previous related programs: line_6: GO Program 2524 - Cycle 1, data received and reduced, paper submitted line_7: GO Program 3732 - Cycle 2, data received and reduced, paper submitted line_8: GO Program 3648 - Cycle 2, data recieved and reduced, paper in preparation ! question: 10 section: 1 line_1: The University of Arizona will provide central computing services (hard disks, line_2: networks, tape drives) in support of this project. One undergraduate will be line_3: able to work on this project through funds provided by the Arizona Space Grant. line_4: We will also be supported by the University of Arizona in follow-up ground-based line_5: activities, such as VLA and VLBA monitoring of the radio lens components for line_6: brightness variations that could lead to a new determination of the Hubble line_7: constant. ! !end of general form text general_form_address: lname: IMPEY fname: CHRIS mi: D. category: PI inst: Steward Observatory addr_1: STEWARD OBSERVATORY addr_2: UNIVERSITY OF ARIZONA city: TUCSON state: AZ zip: 85721 country: USA phone: 602-621-6522 telex: 467175 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: QSO1422P231-B name_2: PKS descr_1: E, 314, 323 pos_1: RA = 14H 24M 38.094S +/- 0.004S, pos_2: DEC = +22D 56' 00.59" +/- 0.05", pos_3: plate-id=01TM equinox: 2000 pm_or_par: NO rv_or_z: Z=3.62 comment_1: SUBARCSECOND GRAVITATIONAL LENS comment_2: COMPONENT B, VLBI RADIO POSITION; comment_3: Component from which remainder comment_4: of B offset positions are derived. fluxnum_1: 1 fluxval_1: B = 18.4 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 1.7 fluxnum_3: 3 fluxval_3: F-LINE(1216) = 5 +/- 1 E-15 targnum: 2 name_1: QSO1422P231-BOFF1 name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=+0.028S+/- 0.05S, pos_2: DEC-OFF=+0.32" +/- 0.05", POS_3: FROM 1, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: First offset position for visit 1; COMMENT_2: Should be component A targnum: 3 name_1: QSO1422P231-BOFF2 name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=-0.028S +/- 0.05S, pos_2: DEC-OFF=-0.32" +/- 0.05", POS_3: FROM 1, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: Second offset position for visit 1; COMMENT_2: Should be blank targnum: 4 name_1: QSO1422P231B-OFF-A name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=+0.028S +/- 0.05S, pos_2: DEC-OFF=+0.32" +/- 0.05", POS_3: FROM 1, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: OFFSET FROM B TO A targnum: 5 name_1: QSO1422P231B-OFF-C name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=-0.024S +/- 0.05S, pos_2: DEC-OFF=-0.75" +/- 0.05", POS_3: FROM 1, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: OFFSET FROM B TO C targnum: 6 name_1: QSO1422P231B-OFF-D name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=+0.068S +/- 0.05S, pos_2: DEC-OFF=-0.81" +/- 0.05", POS_3: FROM 1, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: OFFSET FROM B TO D targnum: 7 name_1: QSO1422P231A name_2: PKS descr_1: E, 314, 323 pos_1: RA = 14H 24M 38.122S +/- 0.05", pos_2: DEC = +22D 56' 00.91" +/- 0.05", pos_3: plate-id=01TM equinox: 2000 pm_or_par: NO comment_1: Component from which remainder comment_2: of A offset positions are derived. targnum: 8 name_1: QSO1422P231A-OFF-B name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=-0.028S +/- 0.05S, pos_2: DEC-OFF=-0.32" +/- 0.05", POS_3: FROM 7, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: OFFSET FROM A TO B targnum: 9 name_1: QSO1422P231A-OFF-C name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=-0.052S +/- 0.05S, pos_2: DEC-OFF=-1.07" +/- 0.05", POS_3: FROM 7, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: OFFSET FROM A TO C targnum: 10 name_1: QSO1422P231A-OFF-D name_2: PKS descr_1: E, 314, 323 pos_1: RA-OFF=+0.040S +/- 0.05S, pos_2: DEC-OFF= -1.13" +/- 0.05", POS_3: FROM 7, pos_4: plate-id=01TM equinox: 2000 pm_or_par: NO COMMENT_1: OFFSET FROM A TO D ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: QSO1422P231-B config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-Y=1.23, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-X=1.23, req_1: CYCLE 4 / 1-24; req_2: ONBOARD ACQ FOR 2; linenum: 2 targname: QSO1422P231-B config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-Y=0.61, param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2 param_4: SCAN-STEP-X=0.61, req_1: ONBOARD ACQ FOR 3; ! linenum: 3 targname: QSO1422P231-B config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 30s fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-Y=0.17, param_2: SEARCH-SIZE-X=5, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.17, req_1: ONBOARD ACQ FOR 4; ! linenum: 4 targname: QSO1422P231-B config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 38s fluxnum_1: 1 priority: 1 param_1: SCAN-STEP-Y=0.052, param_2: SEARCH-SIZE-X=5, param_3: SEARCH-SIZE-Y=5 param_4: SCAN-STEP-X=0.052, req_1: ONBOARD ACQ FOR 5-7; COMMENT_1: SAVE ACQ INFORMATION FROM 1-4 COMMENT_2: FOR USE IN 10-14 OR 20-24. ! linenum: 5 targname: QSO1422P231-B config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 640.0S s_to_n: fluxnum_1: priority: req_1: non-int; ! linenum: 6 targname: QSO1422P231-BOFF1 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 640.0S s_to_n: fluxnum_1: priority: 1 req_1: non-int; comment_1: This image should contain the A comp. comment_2: if B was correct acquired. Will be comment_3: blank if A was acquired. ! linenum: 7 targname: QSO1422P231-BOFF2 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 640.0S s_to_n: fluxnum_1: priority: req_1: non-int; comment_1: This image will be blank if comment_2: B was correctly acquired. Will comment_3: contain B if A was acquired. ! linenum: 10 targname: QSO1422P231-B config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 38S s_to_n: fluxnum_1: priority: param_1: SEARCH-SIZE-X=5, param_2: SEARCH-SIZE-Y=5, PARAM_3: SCAN-STEP-Y=0.052, param_4: SCAN-STEP-X=0.052, req_1: SAME ORIENT FOR 10-14 as 1; req_2: AFTER 1 BY 20D; REQ_3: COND IF B FOUND/10-14; REQ_4: ONBOARD ACQ FOR 11-14; comment_1: Req ephemeris correction /10-14 comment_2: Use SAME GS and ORIENT as /10-14 ! linenum: 11 targname: QSO1422P231-B config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 1200S s_to_n: 35 fluxnum_1: 1 priority: 1 req_1: SEQ 10-14 NO GAP; comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! linenum: 12 targname: QSO1422P231B-OFF-A config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 1200S s_to_n: 35 fluxnum_1: 1 priority: 1 comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! linenum: 13 targname: QSO1422P231B-OFF-C config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 2400S s_to_n: 35 fluxnum_1: 1 priority: 1 comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! linenum: 14 targname: QSO1422P231B-OFF-D config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 2 time_per_exp: 2400S s_to_n: 8 fluxnum_1: 1 priority: 1 comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! linenum: 20 targname: QSO1422P231-B config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 38S s_to_n: fluxnum_1: priority: param_1: SEARCH-SIZE-X=5, param_2: SEARCH-SIZE-Y=5, param_3: SCAN-STEP-Y=0.052, param_4: SCAN-STEP-X=0.052, req_1: SAME ORIENT FOR 20-24 as 1; req_2: SEQ 20-24 NO GAP; REQ_3: AFTER 1 BY 20D; REQ_4: COND IF A FOUND/20-24; req_5: ONBOARD ACQ FOR 21-24; comment_1: Req ephemeris correction /20-24; comment_2: Use SAME GS and ORIENT as /20-24 ! linenum: 21 targname: QSO1422P231-B config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 1200S s_to_n: 35 fluxnum_1: 1 priority: 1 comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! linenum: 22 targname: QSO1422P231A-OFF-B config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 1200S s_to_n: 35 fluxnum_1: 1 priority: 1 comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! linenum: 23 targname: QSO1422P231A-OFF-C config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 1 time_per_exp: 2400S s_to_n: 35 fluxnum_1: 1 priority: 1 comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! linenum: 24 targname: QSO1422P231A-OFF-D config: FOS/RD opmode: ACCUM aperture: 0.3 sp_element: G570H num_exp: 2 time_per_exp: 2400S s_to_n: 8 fluxnum_1: 1 priority: 1 comment_1: S/N AT 6000 ANGSTROMS comment_2: BLOCKING FILTER WG 375 ! ! end of exposure logsheet ! No scan data records found