! File: 2624C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:09:30:00 coverpage: title_1: HIGHLY LUMINOUS QUASARS AS GRAVITATIONALLY LENSED OBJECTS sci_cat: QUASARS & AGN sci_subcat: GRAVITATIONAL LENSES proposal_for: GO pi_title: DR. pi_fname: JEAN pi_lname: SURDEJ pi_inst: LIEGE UNIVERSITY pi_country: BELGIUM pi_phone: 32-41-529980 keywords_1: ACTIVE GALAXIES: QUASARS, OBSERVING TECHNIQUES: keywords_2: IMAGING hours_pri: 6.00 num_pri: 9 foc: X time_crit: X pi_position: SCIENTIFIQUE off_fname: RENE off_lname: SIMON off_title: PROFESSOR off_inst: INSTITUT D'ASTROPHYSIQUE, ULG. off_addr_1: AVENUE DE COINTE, 5 off_city: LIEGE off_zip: 4200 off_country: BELGIUM off_phone: 32-41-529980 off_telex: 41264 (ASTRLG) ! end of coverpage abstract: line_1: Considering that the highly luminous quasars (hereafter HLQs, Mv<=-29) line_2: constitute the best extragalactic candidates to search for the presence of line_3: gravitationally lensed images at sub-arcsecond angular scales, we propose to line_4: perform high resolution direct imaging of a small sample of these objects line_5: with the FOC instrument onboard ST. Applying the roll deconvolution line_6: technique to some of the FOC observations line_7: obtained in the F/288 mode will lead to unprecedented high angular resolution line_8: (FWHM ~ 0.02") images of extragalactic objects in the ultraviolet spectral line_9: range. These data will allow us to determine the significance of gravitational line_10: lensing effects in order to improve our knowledge on quasars (structure, line_11: luminosity function, source counts), on the distribution of matter in the line_12: Universe (galaxy masses, intergalactic medium, dark matter) and on the Hubble line_13: parameter. More specific observations of the best potential lensed QSO line_14: candidates identified with ST will be proposed after a careful evaluation of line_15: the preliminary data. ! ! end of abstract general_form_proposers: lname: COURVOISIER fname: THIERRY title: DR. inst: GENEVA OBSERVATORY country: SWITZERLAND esa: X ! lname: KAYSER fname: RAINER title: DR. inst: TORONTO, UNIVERSITY OF country: CANADA ! lname: BORGEEST fname: ULF title: DR. inst: HAMBURG OBSERVATORY country: FRG esa: X ! lname: MAGAIN fname: PIERRE title: DR. inst: EUROPEAN SOUTHERN OBSERVATORY country: FRG esa: X ! lname: REFSDAL fname: SJUR title: DR. inst: HAMBURG OBSERVATORY country: FRG esa: X ! lname: SURDEJ fname: JEAN title: P.I. inst: LIEGE UNIVERSITY country: BELGIUM esa: X ! lname: SWINGS fname: JEAN-PIERRE title: DR. inst: LIEGE UNIVERSITY country: BELGIUM esa: X ! lname: WEIGELT fname: G. title: DR. inst: ERLANGEN UNIVERSITY country: FRG esa: X ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We first propose to image a modest size sample of 9 HLQs (out of a complete line_2: sample of 250 catalogued ones; see Veron-Cetty and Veron, 1987) with the FOC line_3: instrument (f/288 mode, field of 3.7"X3.7"), in order to efficiently select line_4: lensed QSO image candidates with small angular separations. Two observations line_5: at different ST roll angles (difference equal or greater than about 30D +- line_6: 15D) will be taken for two of the targets in order to achieve for these the line_7: highest possible angular resolution with ST (0.02" at lambda = 2000A). The line_8: time exposures, the filters (F210M, F220W, etc.) and the HLQs have been line_9: selected in such a way that still an acceptable S/N (=5) will be obtained for line_10: secondary lensed HLQ images up to 6-7 mag. fainter than the primary ones (mU = line_11: 16.1). Let us recall that the roll deconvolution technique should allow us to line_12: discriminate in two cases the detection of very faint lensed QSO images from line_13: the point spread function structure (specially the spider arm diffraction line_14: spikes of the brighter components (Muller and Weigelt, 1985, 1987). line_15: Note: Depending on the results of this primary program, we may later propose line_16: to carry out further direct imaging, photometric and/or spectroscopic line_17: observations of the most promising lens candidates in order to achieve the line_18: scientific goals exposed in this proposal. ! question: 4 section: 1 line_1: 1. ST/FOC-justification: Our ST proposal fully requires the good dynamic line_2: range and the high angular resolution capabilities of the FOC instrument line_3: (f/288 mode, 3.7"X3.7" field) onboard ST. Using this instrumentation, we line_4: should be able to resolve, at approximately 0.1-0.2" separations, star-like line_5: images whose brightness difference amounts to more than 6-7 mag. For line_6: two HLQs, we shall make use of the roll deconvolution technique described by line_7: Muller and Weigelt (1985, 1987). To apply a successful deconvolution, it is line_8: necessary that the camera resolves the interference fine structure (speckles) line_9: in the telescope point spread function. Only the f/288 mode of the FOC can line_10: resolve the speckle fine structure in the point spread function at short UV line_11: wavelengths since the speckle size at lambda = 2000A is about 0.02". The line_12: pixel size at f/288 is 0.007", i.e. 3X3 pixels per speckle, which is line_13: sufficient. Short UV wavelengths are advantageous because of the high line_14: theoretical resolution at these wavelengths. The pixel size of the FOC at line_15: f/96 is 0.022" and of the PC 0.043", which is not sufficient. ! question: 4 section: 2 line_1: 2. Ground-based observations: While a preliminary version of the present ST line_2: proposal was ready in January 1986, the delay in getting access to ST has, line_3: prompted us to conduct a parallel program from the ground. Since April 1986 line_4: we have regularly applied for observing time at ESO. During the past years, line_5: approximately 20 nights have been allocated to our optical search for line_6: multiply lensed HLQs with separations greater than, typically, 1". Under line_7: an average seeing (FWHM) of 1.2", we have imaged with the ESO/MPI 2.2 line_8: (+ direct CCD camera) a total of 111 HLQs. 25 of these turn out to line_9: be interesting objects on the basis of their morphological appearance line_10: (multiple or elongated image(s), presence of a very nearby galaxy or rich line_11: cluster, etc.). More details may be found in Surdej et al. (1988b). Five of line_12: these 25 HLQs constitute excellent candidates for gravitational lensing. line_13: Three of these five candidates, ESO GL1, ESO GL2 and ESO GL3 are now line_14: confirmed to be definite new cases of multiply lensed quasars (see Surdej line_15: et al., 1987; Magain et al., 1988 and Meylan and Djorgovski, 1988, line_16: respectively). Recent intermediate resolution spectroscopic data of UM673 line_17: and H1413+117 have been taken with the MMT and CFHT telescopes. Specific line_18: radio observations of gravitational lens candidates have also been obtained line_19: (and are presently scheduled) with the Very Large Array. The photometric line_20: monitoring of UM673 is being carried out at ESO since October, 1987. An line_21: ESO key programme on gravitational lensing (complementary observations to line_22: those proposed here) has recently been accepted (Surdej et al., 1989). line_23: Weigelt and his co-workers have a good experience with speckle techniques ! question: 4 section: 3 line_1: and observations from the ground. They have namely performed speckle line_2: interferometric observations of the gravitational lens system PG1115+080 line_3: (Weigelt et al., 1986). ! question: 5 section: 1 line_1: Adopting the V magnitude of the selected HLQs from the catalogue of quasars line_2: by Veron-Cetty and Veron (1987, 1989), and others, we have estimated, for each line_3: of the targets (9 HLQs) to be observed with ST/FOC, their flux at the wave- line_4: length lambda = 2300 A by means of the HST expert assistant available at ESO line_5: ST-ECF. For this purpose, we have selected a spectral index alpha equal to line_6: 0.7. For redshifts z greater than 2, we have applied an additional correction line_7: 10XX(-0.4(z-2)), in order to take into account the blanketing of the QSO line_8: continuum by the Lyman alpha forest. Typically, for a z smaller than 2 HLQ line_9: with mU = 16.5, we find that f(2300) = 2.7 10(-15) erg/cm2/s/A. We have then line_10: calculated the expected count rates per pixel for different filters between line_11: 1500 and 3000 A (where it is possible to achieve the highest angular line_12: resolution) and for the following conditions: i) the different flux values of line_13: the HLQs listed in the target list, ii) the f/288 mode of the FOC, line_14: iii) the expected size of the point spread function caused line_15: by aberrations = 100 pixels (= 10X10 pixels = 0.07"X0.07"), iv) the efficiency line_16: of the optics and detector (updated values at ST-ECF), v) the maximal count line_17: rate should be 0.4 counts/(pixel.s) if the 512X512 pixel mode is adopted (i.e. line_18: 3.7"X3.7"). We found very encouraging results for different filters (cf. the line_19: exposure logsheet). The exposure times have been estimated such that the S/N line_20: ratio obtained for the integrated image of the HLQs should be very near to line_21: 150, allowing us to detect secondary images up to 6-7 magnitudes fainter. line_22: Although we initially intended to observe each of our targets with two line_23: different roll angles (for roll deconvolution), we had to restrict this ! question: 5 section: 2 line_1: possibility to only two HLQs, because of the (new) time constraints. line_2: The total exposure time (9HLQs, 11 visits) therefore amounts to: 290 min. line_3: + 11 X (20 + 5.5) min. = 9.5 hours. ! question: 6 section: 1 line_1: Because we would like to detect very faint lensed HLQ images, dark time is line_2: requested for all our observations. Furthermore, as said before, the roll line_3: deconvolution technique requires two exposures at different roll angles. line_4: The change in roll angles should be about 30D +/- 15D between observations line_5: of a same HLQ. Please note that the exact value of the roll angle at the line_6: moment of the observations is not important ... what does really matter line_7: is that the difference between two roll angle values pertaining to the line_8: observation of a same HLQ is equal to + or - 30D +/- 15D. ! question: 7 section: 1 line_1: Using the reduction facilities (MIDAS, IHAP, etc.) available in our home line_2: institutes (IAL Space, Liege; ST-ECF/ESO, Garching bei Munchen; Hamburger line_3: Sternwarte, Hamburg; Observatoire de Geneve, Sauverny and Physikalisches line_4: Institut, Erlangen), we shall be able to reduce and analyse all the FOC line_5: images obtained with ST. Hardware and software needed for applying the roll line_6: deconvolution technique are available at the Physics Institute of Erlangen. line_7: Sophisticated numerical programs dealing with "gravitational optometry" line_8: have already been developed at the Hamburg Observatory (Schramm and Kayser, line_9: 1987; Kayser and Schramm, 1988) ... and strongly await new cases of line_10: gravitational lens systems. ! question: 10 section: 1 line_1: Reduction and analysis of the FOC images will be made by ourselves at our line_2: home institutes in Liege, Geneve, Munchen, Erlangen and Hamburg. Most of us line_3: have a good experience in using MIDAS and IHAP programs. Various travel line_4: grants will allow us to have frequent exchanges, visits, etc. ! !end of general form text general_form_address: lname: SURDEJ fname: JEAN title: DR. category: PI inst: INSTITUT D'ASTROPHYSIQUE addr_1: UNIVERSITE DE LIEGE addr_2: AVENUE DE COINTE, 5 city: LIEGE B-4200 country: BELGIUM ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PKS0005-239 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 04JK, pos_2: RA = 00H 08M 00.320S +/- 0.5", pos_3: DEC = -23D 39' 18.01" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.41 fluxnum_1: 1 fluxval_1: V = 16.5 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 2.6 +/- 0.7 E-15 ! targnum: 2 name_1: PG0117+213 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 021K, pos_2: RA = 01H 20M 17.252S +/- 0.5", pos_3: DEC = +21D 33' 46.36" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.493 fluxnum_1: 1 fluxval_1: V = 16.1 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 3.9 +/- 1.1 E-15 ! targnum: 3 name_1: Q0254-334 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 02IV, pos_2: RA = 02H 56M 47.848S +/- 0.5", pos_3: DEC = -33D 15' 26.43" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.849 fluxnum_1: 1 fluxval_1: V = 16.0 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 4.3 +/- 1.2 E-15 ! targnum: 4 name_1: UM485 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 00BB, pos_2: RA = 12H 15M 49.794S +/- 0.5", pos_3: DEC = -00D 34' 33.99" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 2.69 fluxnum_1: 1 fluxval_1: V = 17.7 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 9.0 +/- 2.5 E-16 ! targnum: 5 name_1: PG1338+416 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 00XY, pos_2: RA = 13H 41M 00.768S +/- 0.5", pos_3: DEC = +41D 23' 13.90" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.219 fluxnum_1: 1 fluxval_1: V = 16.1 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 4.0 +/- 1.1 E-15 ! targnum: 6 name_1: Q1349+001 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 02OA, pos_2: RA = 13H 51M 50.429S +/- 0.5", pos_3: DEC = -00D 07' 39.75" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.426 fluxnum_1: 1 fluxval_1: V = 16.0 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 4.3 +/- 1.2 E-15 ! targnum: 7 name_1: MARK679 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 01PT, pos_2: RA = 14H 23M 26.119S +/- 0.5", pos_3: DEC = +32D 52' 21.10" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.904 fluxnum_1: 1 fluxval_1: V = 16.7 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 2.2 +/- 0.6 E-15 ! targnum: 8 name_1: PG1630+377-R1 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 01RW, pos_2: RA = 16H 32M 01.097S +/- 0.5", pos_3: DEC = +37D 37' 49.57" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.466 fluxnum_1: 1 fluxval_1: V = 16.1 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 4.0 +/- 1.1 E-15 ! targnum: 9 name_1: PG1630+377-R2 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 01RW, pos_2: RA = 16H 32M 01.097S +/- 0.5", pos_3: DEC = +37D 37' 49.57" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.466 fluxnum_1: 1 fluxval_1: V = 16.1 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 4.0 +/- 1.1 E-15 ! targnum: 10 name_1: Q2300-445-R1 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 031D, pos_2: RA = 23H 03M 21.673S +/- 0.5", pos_3: DEC = -44D 10' 28.32" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.943 fluxnum_1: 1 fluxval_1: V = 16.4 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 2.9 +/- 0.8 E-15 ! targnum: 11 name_1: Q2300-445-R2 descr_1: GALAXY; QUASAR pos_1: PLATE-ID = 031D, pos_2: RA = 23H 03M 21.673S +/- 0.5", pos_3: DEC = -44D 10' 28.32" +/- 0.5" equinox: J2000.0 rv_or_z: Z = 1.943 fluxnum_1: 1 fluxval_1: V = 16.4 +/- 0.3 fluxnum_2: 2 fluxval_2: F(2300) = 2.9 +/- 0.8 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PKS0005-239 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 30M s_to_n: 150 fluxnum_1: 2 priority: 1 req_1: DARK TIME / 1-11 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED ! linenum: 2.000 targname: PG0117+213 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 20M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED ! linenum: 3.000 targname: Q0254-334 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F220W, F2ND num_exp: 1 time_per_exp: 20M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED ! linenum: 4.000 targname: UM485 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F220W, F1ND num_exp: 1 time_per_exp: 45M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED ! linenum: 5.000 targname: PG1338+416 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 20M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED ! linenum: 6.000 targname: Q1349+001 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F220W, F2ND num_exp: 1 time_per_exp: 20M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED ! linenum: 7.000 targname: MARK679 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 40M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED ! linenum: 8.000 targname: PG1630+377-R1 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 20M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED comment_2: FOR ROLL DECONVOLUTION WITH EXP. 9. comment_3: THIS IS THE FIRST OF A PAIR OF comment_4: EXPOSURES (8 AND 9) TO BE TAKEN WITH comment_5: DIFFERENT ROLL ANGLES (DIFFERENCE = comment_6: + OR - 30D+/-15D). ! linenum: 9.000 targname: PG1630+377-R2 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 20M s_to_n: 150 fluxnum_1: 2 priority: 1 req_1: ORIENT 30D +/- 15D FROM 8 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED comment_2: FOR ROLL DECONVOLUTION WITH EXP. 8. comment_3: THIS IS THE SECOND OF A PAIR OF comment_4: EXPOSURES (8 AND 9) TO BE TAKEN WITH comment_5: DIFFERENT ROLL ANGLES (DIFFERENCE = comment_6: + OR - 30D+/-15D). ! linenum: 10.000 targname: Q2300-445-R1 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 27M s_to_n: 150 fluxnum_1: 2 priority: 1 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED comment_2: FOR ROLL DECONVOLUTION WITH EXP. 11. comment_3: THIS IS THE FIRST OF A PAIR OF comment_4: EXPOSURES (10 AND 11) TO BE TAKEN WITH comment_5: DIFFERENT ROLL ANGLES (DIFFERENCE = comment_6: + OR - 30D+/-15D). ! linenum: 11.000 targname: Q2300-445-R2 config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F210M num_exp: 1 time_per_exp: 27M s_to_n: 150 fluxnum_1: 2 priority: 1 req_1: ORIENT 30D +/- 15D FROM 10 comment_1: S. I. ALPHA = 0.7 HAS BEEN ASSUMED comment_2: FOR ROLL DECONVOLUTION WITH EXP. 10. comment_3: THIS IS THE SECOND OF A PAIR OF comment_4: EXPOSURES (10 AND 11) TO BE TAKEN WITH comment_5: DIFFERENT ROLL ANGLES (DIFFERENCE = comment_6: + OR - 30D+/-15D). ! ! end of exposure logsheet ! No scan data records found