! File: 3732C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:17:43:38 coverpage: title_1: SPECTRPOLARIMETRY OF HIGH REDSHIFT QUASARS sci_cat: QUASARS & AGN sci_subcat: QUASAR EMISSION proposal_for: GO pi_fname: CHRIS pi_mi: D. pi_lname: IMPEY pi_inst: UNIVERSITY OF ARIZONA pi_country: USA pi_phone: 602-621-6522 hours_pri: 10.00 num_pri: 2 fos: Y funds_amount: 89894 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 request 10.0 hours to obtain FOS UV spectropolarimetry of 2 luminous line_2: high-redshift normal radio-quiet quasars, selected from a large survey line_3: to have exceptional UV brightness and clearly detectable polarization. line_4: By obtaining spectropolarimetry to much shorter rest wavelengths than line_5: have ever before been measured, these observations offer a unique line_6: opportunity to (a) identify the polarizing mechanism(s), and possibly line_7: (b) detect the signature of a black hole accretion flow, and (c) make line_8: the first test of general relativity outside of the weak-field limit. line_9: New measurements of wavelength-dependent optical polarization show two line_10: competing models to be consistent with our spectropolarimetry of a dozen line_11: quasars. Choosing between these requires the extended spectral coverage line_12: (particularly to the shortest wavelengths) which can only be obtained by line_13: combining HST data with quasi-simultaneous ground-based polarimetry. line_14: The proposed observations will determine whether the polarization is line_15: produced by scattering from dust grains or free electrons, and indicate line_16: their location and properties. In AGNs where the contamination from line_17: starlight is, we can measure, for the first time, the polarization of the line_18: strong UV excess. If this component is thermal emission from an accretion line_19: flow, we will infer its physical properties (e.g. geometry and opacity), line_20: and search for the short wavelength posn. angle rotation predicted by GR. ! ! end of abstract general_form_proposers: lname: IMPEY fname: CHRIS title: PI mi: D. inst: UNIVERSITY OF ARIZONA country: USA ! lname: MALKAN fname: MATTHEW mi: A. inst: U. CALIFORNIA, LOS ANGELES country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Two QSOs will observed in spectropolarimetry mode with the line_2: blue side of the FOS. Each POLSCAN-B cycle will involve line_3: 22 minutes of integration and will fit within a single orbit. line_4: Both targets are bright, isolated point sources that can be line_5: acquired in ACQ/BINARY mode. The brighter QSO will be observed line_6: with both the G190H and G270H gratings, and the fainter QSO line_7: with just the G270H grating. Observations can be made in the line_8: large 4.3 arcsecond aperture, and QSO positions are accurate line_9: enough for reliable acquisition. ! question: 4 section: 1 line_1: ST observations are required in order to do polarimtry of line_2: the strong ultraviolet continua of bright QSOs down to line_3: unprecedented rest wavelengths. Line and continuum line_4: polarizations can be measured separately. ! question: 7 section: 1 line_1: Data reduction and analysis will be performed at both Steward line_2: Observatory and UCLA, using software created by the FOS line_3: spectropolarimetry team at Steward. ! question: 10 section: 1 line_1: Computing support and graduate student support will be line_2: available at both Steward Observatory and UCLA. ! !end of general form text general_form_address: lname: IMPEY fname: CHRIS mi: D. category: PI inst: UNIVERSITY OF ARIZONA 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: PG1634+706 name_2: PG descr_1: E,313 pos_1: RA=16H 34M 51.70S+/-0.10", pos_2: DEC=+70D 37' 37.0"+/-1.0", equinox: 1950 rv_or_z: Z=1.334 comment_1: BRIGHT QUASAR, comment_2: FOS SPECTROPOLARIMETRY fluxnum_1: 1 fluxval_1: V=14.9+/-0.1 fluxnum_2: 2 fluxval_2: F-CONT(3000)=100+/-15E-17 ! targnum: 2 name_1: PG2302+029 name_2: PG descr_1: E,313 pos_1: RA=23H 02M 12.00S+/-0.10", pos_2: DEC=+02D 55' 34.0"+/-1.0", equinox: 1950 rv_or_z: Z=1.044 comment_1: BRIGHT QUASAR, comment_2: FOS SPECTROPOLARIMETRY fluxnum_1: 1 fluxval_1: V=16.0+/-0.1 fluxnum_2: 2 fluxval_2: F-CONT(3000)=43+/-9E-17 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PG1634+706 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 6.6S s_to_n: 50 fluxnum_1: 2 priority: 1 req_1: CYCLE 2 / 1.0-5.0; req_2: ONBOARD ACQ FOR 2-3 comment_1: BRIGHT QUASARS, FOS comment_2: SPECTROPOLARIMETRY ! linenum: 2.000 targname: PG1634+706 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1600-2300 num_exp: 4 time_per_exp: 22M s_to_n: 30 fluxnum_1: 2 priority: 1 param_1: POLSCAN=8B ! linenum: 3.000 targname: PG1634+706 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2230-3300 num_exp: 4 time_per_exp: 22M s_to_n: 30 fluxnum_1: 2 priority: 1 param_1: POLSCAN=8B ! linenum: 4.000 targname: PG2302+029 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 18.5S s_to_n: 50 fluxnum_1: 2 priority: 2 req_1: ONBOARD ACQ FOR 5 ! linenum: 5.000 targname: PG2302+029 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2230-3300 num_exp: 6 time_per_exp: 22M s_to_n: 20 fluxnum_1: 2 priority: 2 param_1: POLSCAN=8B ! ! end of exposure logsheet ! No scan data records found