! File: 3906C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:23:28:45 coverpage: title_1: IMAGING OF A COMPLETE SAMPLE OF THE NEAREST INFRARED QUASARS sci_cat: GALAXIES & CLUSTERS sci_subcat: PECULIAR/INTERACTING proposal_for: GO pi_fname: DAVID pi_mi: B. pi_lname: SANDERS pi_inst: UNIVERSITY OF HAWAII pi_country: USA pi_phone: 808-956-5055 hours_pri: 5.67 num_pri: 5 foc: Y funds_amount: 69909 funds_length: 12 off_fname: MOHEB off_mi: A. off_lname: GHALI off_title: DIRECTOR OF RESEARCH off_inst: UNIVERSITY OF HAWAII off_addr_1: 2540 MAILE WAY off_addr_2: SPALDING-255 off_city: HONOLULU off_state: HI off_zip: 96822 off_country: USA off_phone: 808-956-8612 ! end of coverpage abstract: line_1: We propose high resolution imaging with the Faint Object Camera (FOC/96) of line_2: a complete sample of the nearest infrared quasars that have been discovered in line_3: the IRAS database. These objects appear to represent a critical evolutionary line_4: link between ultraluminous infrared galaxies and optical quasars. The FOC line_5: obseravtions will provide an important test of the hypothesis that all line_6: quasars form through the merger of gas-rich spirals. Ground-based line_7: optical and near-infrared images of our complete sample of IRAS bright galaxies line_8: now indicate that all of the most luminous objects are mergers. A strong line_9: correlation has been discovered between the incidence of AGN spectra, warmer line_10: infrared colors, decreased nuclear separation, and stronger - more pointlike - line_11: optical nuclei with increasing infrared luminosity. The infrared line_12: quasars that we are proposing to observe with HST provide direct line_13: evidence for the transition stage from ultraluminous infrared galaxy line_14: to optical quasar if it can be demonstrated that there exists a continuity line_15: in morphological properties with those observed in the cooler infrard objects. line_16: FOC images in U,B, and V filters will be used to identify double nuclei line_17: and to measure nuclear separations and magnitudes. HST images will line_18: provide a factor 10 - 30 increased resolution over that line_19: attainable from the ground. ! ! end of abstract general_form_proposers: lname: SANDERS fname: DAVID title: PI mi: B. inst: UNIVERSITY OF HAWAII country: USA ! lname: SOIFER fname: BARUCH mi: T. inst: CALTECH country: USA ! lname: NEUGEBAUER fname: GERRY inst: CALTECH country: USA ! lname: SCOVILLE fname: NICK inst: CALTECH country: USA ! lname: WEIR fname: NICK inst: CALTECH country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: FOC/96 images in broad band filters (B,V) will be obtained for the sample of line_2: 6 infrared quasars (from our complete list of 12 - minus the GTO objects line_3: 3C273 and IZw1) that are unresolved in ground-based images. Exposure times line_4: range from 600S - 1200S depending on the B and V magnitudes, and are line_5: sufficient to detect (S/N > 10) double nuclei 6 mag fainter than the line_6: average magnitude for the central 2 arcsec. ! question: 4 section: 1 line_1: The high spatial resolution of HST (0.022" for FOC/96) is critical to line_2: separate anmd resolve possible double nuclei in infrared quasars, nearely line_3: all of which are currently unresolved in ground-based observations. HST line_4: will provide a factor 10-30 increase in spatial resolution over the best line_5: ground-based images. Over the past two years we have vigorously pursued line_6: imaging of both cooler ultraluminous infrared galaxies and our proposed line_7: sample of infrared quasars. All of the cooler ultraluminous infrared line_8: galaxies have been resolved as doubles, but the slightly more distant, and line_9: presumably more evolved infrared quasars have eluded separation. CCD line_10: images (B,g,r,i) have previously been obtained at Palomar for the complete line_11: sample of 12 infrared quasars, allowing us to study their morphology on line_12: ~1" scales. The majority of these objects have also been imaged in line_13: 0.5-0.7" seeing at the CFHT, and although the central brightness profiles line_14: are more oval in shape, no additional sources were resolved. Currently line_15: only two infrared quasars from our complete list of 12 are resolved doubles, line_16: six suggest multiple nuclei, and four still appear to have a dominant line_17: single nucleus, although there is additional evidence (double tails, etc.) line_18: to suggest a merger. Given a factor of 10-30 increased resolution in the line_19: HST images, it is possible that double nuclei will be seen in mearly all line_20: of these objects. ! question: 7 section: 1 line_1: We have demonstrated capability for restoring FOC images using currently line_2: available PSF's for our proposed f/96 filters. One of us (NW) has line_3: described an image model that allows simultaneous restoration of both line_4: extended and sharp structure in an image with little or no pre-processing line_5: of the HST data. This method also allows the capability of fitting line_6: multiple data sets simultaneously and the rejection of cosmic ray line_7: artifacts as a part of the restoration process. Our exposure times line_8: should typically give S/N > 30 in the PSF core for reasonable assumptions line_9: of relative intensity and strength of nuclear sources, and it should be line_10: possible to resolve double nuclei at > 0.04" separation in the restored line_11: images even for intensity ratios as large as 5 mag. Comparison of images line_12: of each object in different filters will aid in the identification of line_13: point sources, and allow us to account for the possibility of variations line_14: in the extinction accross the source. Extinction is much less severe in line_15: the warm infrared galaxies being observed as compared to much cooler line_16: ultraluminous infrared objects such as Arp 220, as evidenced by the large line_17: fraction of observed Seyfert 1 spectra and much less extreme U-B colors. line_18: Any remaining dust screen along the line of sight to the nuclear source line_19: will decrease its observed brightness, but is not calculated to line_20: significantly widen the images of nuclei at B-V wavelengths. ! question: 10 section: 1 line_1: SUN Computers, CCD data reduction software at the IfA. line_2: CONVEX and VAX computers at Caltech. line_3: DBS is supported by an 11-month salaried position at the University line_4: of Hawaii. Funds are requested for part-time support of graduate students line_5: at Caltech (NW) and Hawaii. line_6: Both Caltech and Hawaii have state-of-the-art image processing software line_7: that can be used for processing ST images. NW has demonstrated line_8: capability for successfully applying Bayesian/Maximum Entropy techniques line_9: for restoration of FOC images from HST. ! !end of general form text general_form_address: lname: SANDERS fname: DAVID mi: B. category: PI inst: INSTITUTE FOR ASTRONOMY addr_1: UNIVERSITY OF HAWAII addr_2: 2680 WOODLAWN DRIVE city: HONOLULU state: HI zip: 96822 country: USA phone: 808-956-5055 telex: 808-988-2790 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MRK1014 name_2: IRAS01572+0009 descr_1: E,313,319,320,910,920 pos_1: RA = 01H 59M 50.193S +/- 0.01S, pos_2: DEC = +00D 23' 41.50" +/- 1", pos_3: PLATE-ID=0086 equinox: 2000 rv_or_z: Z = 0.163 comment_1: BV PHOTOMETRY fluxnum_1: 1 fluxval_1: SURF(B)=16.16 fluxnum_2: 2 fluxval_2: SURF(V)=15.7 ! targnum: 2 name_1: IRAS05189-2524 descr_1: E,313,319,320,910,920 pos_1: RA = 05H 21M 01.430S +/- 0.01S, pos_2: DEC = -25D 21' 45.59" +/- 1", pos_3: PLATE-ID=049Y equinox: 2000 rv_or_z: Z = 0.0427 comment_1: BV PHOTOMETRY fluxnum_1: 1 fluxval_1: SURF(B)=17.07 fluxnum_2: 2 fluxval_2: SURF(V)=16.1 ! targnum: 3 name_1: IRAS12071-0444 descr_1: E,317,319,320,910,920 pos_1: RA = 12H 09M 45.141S +/- 0.01S, pos_2: DEC = -05D 01' 13.78" +/- 1", pos_3: PLATE-ID=03O9 equinox: 2000 rv_or_z: Z = 0.129 comment_1: BV PHOTOMETRY fluxnum_1: 1 fluxval_1: SURF(B)=17.85 fluxnum_2: 2 fluxval_2: SURF(V)=16.8 ! targnum: 4 name_1: UGC8058 name_2: MRK231 name_3: IRAS12540+5708 descr_1: E,313,319,320,910,920 pos_1: RA = 12H 56M 14.133S +/- 0.01S, pos_2: DEC = +56D 52' 24.95" +/- 1", pos_3: PLATE-ID=01R1 equinox: 2000 rv_or_z: Z = 0.042 comment_1: BV PHOTOMETRY fluxnum_1: 1 fluxval_1: SURF(B)=14.42 fluxnum_2: 2 fluxval_2: SURF(V)=13.6 ! targnum: 5 name_1: IRAS15206+3342 descr_1: E,317,319,320,910,920 pos_1: RA = 15H 22M 38.094S +/- 0.01S, pos_2: DEC = +33D 31' 36.17" +/- 1", pos_3: PLATE-ID=01RV equinox: 2000 rv_or_z: Z = 0.125 comment_1: BV PHOTOMETRY fluxnum_1: 1 fluxval_1: SURF(B)=15.21 fluxnum_2: 2 fluxval_2: SURF(V)=14.7 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: MRK1014 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W,F1ND num_exp: 1 time_per_exp: 10M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: GROUP1-2 NO GAP; req_2: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 2.000 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F480LP num_exp: 1 time_per_exp: 10M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 3.000 targname: IRAS05189-2524 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W num_exp: 1 time_per_exp: 10M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: GROUP3-4 NO GAP; req_2: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 4.000 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F480LP num_exp: 1 time_per_exp: 10M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 5.000 targname: IRAS12071-0444 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W num_exp: 1 time_per_exp: 20M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: GROUP5-6 NO GAP; req_2: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 6.000 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F480LP num_exp: 1 time_per_exp: 20M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 7.000 targname: UGC8058 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W,F1ND,F2ND num_exp: 1 time_per_exp: 10M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: GROUP7-8 NO GAP; req_2: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 8.000 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F480LP,F2ND num_exp: 1 time_per_exp: 10M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 9.000 targname: IRAS15206+3342 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F430W,F1ND num_exp: 1 time_per_exp: 20M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: GROUP9-10 NO GAP; req_2: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! linenum: 10.000 targname: IRAS15206+3342 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F480LP num_exp: 1 time_per_exp: 15M s_to_n: 10 s_to_n_time: 1M fluxnum_1: 1 priority: 1 req_1: CYCLE2 comment_1: SEARCH FOR DOUBLE NUCLEI ! ! end of exposure logsheet ! No scan data records found