coverpage: title_1: GEOMETRY AND GENERALIZABILITY OF THE REFLECTED LIGHT MODEL FOR title_2: SEYFERT 2 GALAXIES sci_cat: QUASARS & AGN sci_subcat: SEYFERTS proposal_for: GO pi_fname: ROSS pi_mi: D pi_lname: COHEN pi_inst: CENTER FOR ASTROPHYSICS & SPACE SCIENCES pi_country: USA hours_pri: 2.69 num_pri: 2 fos: Y funds_length: 12 off_fname: RICHARD off_mi: E off_lname: ATTIYEH off_title: DEAN, OGSR off_inst: 1560 off_addr_1: OFFICE OF GRADUATE STUDIES AND RESEARCH, 0003 off_addr_2: 9500 GILMAN DRIVE off_city: LA JOLLA off_state: CA off_zip: 920930003 off_country: USA off_phone: 619-534-6654 ! end of coverpage abstract: line_1: The polarized flux spectra of at least 8 Seyfert 2 galaxies look like the flux line_2: spectra of Seyfert 1 nuclei, and the polarization position angles are generally line_3: perpendicular to the radio structure axes. This and other evidence suggests line_4: that all Seyfert 2 galaxies may have Seyfert 1 spectra visible only in line_5: reflected light. The broad-line regions can be viewed directly in the cases line_6: where the otherwise obscuring tori are viewed pole on, and such objects would line_7: be classified as Seyfert 1 galaxies. It is crucial to determine whether this line_8: generalization of the polarization results is correct, and in particular line_9: whether all Seyfert 2 galaxies have polarized nuclear continuua with position line_10: angles perpendicular to the radio source axes. We argue that contamination by line_11: host-galaxy starlight usually renders this virtually impossible to determine line_12: from the ground, while from space, the observations would be easy and line_13: straightforward. We can use the FOS on the HST as a polarimeter, cutting down line_14: drastically on the starlight by observing in the UV where the stellar flux is line_15: weak. We can also determine the geometry of the obscuring regions, and for line_16: many of the objects, we can determine whether the mechanism of the line_17: polarization is dust or electron scattering. We can determine continuum line_18: slopes and identify broad Fe II features from the flux spectra we line_19: receive as a by-product of the polarimetry. ! ! end of abstract general_form_proposers: lname: COHEN fname: ROSS title: PI mi: D inst: CENTER FOR ASTROPHYSICS & SPACE SCIENCES country: USA ! lname: ANTONUCCI fname: ROBERT mi: RJ inst: UCSB country: USA ! lname: KAY fname: LAURA mi: E inst: BARNARD COLLEGE country: USA ! lname: KROLIK fname: JULIAN mi: H inst: JOHNS HOPKINS UNIVERSITY country: USA ! ! end of general_form_proposers block ! No records found general_form_address: lname: COHEN fname: ROSS mi: D category: PI inst: Center for Astrophysics & Space Sciences addr_1: CASS 0111, UCSD addr_2: 9500 GILMAN DRIVE city: LA JOLLA state: CA zip: 920930111 country: USA phone: 619-534-2664 ! ! end of general_form_address records general_form_text: question: 3 section: 1 line_1: We will do broad-band polarimetry of 2 Seyfert 2 galaxies using the FOS, line_2: large aperture, red detector, the G270H grating, and B Waveplate. We will line_3: obtain a S/N of approximately 5 or greater in the polarized flux by line_4: binning the spectrum between 2100 Angstroms and 3000Angstroms , assuming line_5: that P = 3\%. To minimize spacecraft inefficiency, we will take no line_7: exposure shorter than 20m, shorter than the usually available orbital line_8: period. This will allow us multiple wavelength points (from two to 11) for line_9: several objects at the same SNR, enabling us to determine crudely the line_10: wavelength dependence of the polarization. (This should be sufficient to line_11: distinguish electron scattering from dust scattering.) line_12: The total sample is large enough to enable us to determine unambiguously whether line_13: Seyfert 2 galaxies have reflected featureless continua and what the line_14: geometry of the occulting region is (if any). The SNR of 5 in the polarized line_15: flux will produce a PA accurate to 6 degrees, allowing us to determine line_16: unambiguously whether P is large or small and whether the PA are aligned line_17: (like Seyfert 1 galaxies and quasars) or perpendicular to the radio line_18: structure axis. question: 3 section: 2 line_1: Target acquisition will be non-standard. We have line_2: derived coordinates in the guide star system from published coordinates line_3: for the objects and for the reference stars (which are all in line_4: the guide star catalog). For these objects, three stage peak-up line_5: to center the objects to within 0.21" in Y (suitable for observing line_6: in the large aperture (see CAL/FOS 132). An earlier technique line_7: using offsets followed by small peak-ups was found not to be line_8: completely successfull. Integration times are arbitrarily set to line_9: 5 seconds because of uncertainty in the fraction of total flux line_10: in the compact nucleus. question: 3 section: 3 line_1: No special requirements are placed on the operation of the spacecraft, line_2: and there will be no requirements for calibration beyond the routine line_3: FOS calibration procedure. The polarization sequence itself should not line_4: be interrupted. question: 4 section: 1 line_1: The number of Seyfert 2 galaxies for which featureless continuum line_2: polarization may be determined from ground--based observations is strictly line_3: limited to the nearest objects and those with the strongest continuum line_4: polarizations. This technique has been pushed to its limits by one of us line_5: (L. K.). Thus, it is not known whether the finding of Miller and line_6: collaborators that a few Seyfert 2 galaxies show a reflected Type 1 line_7: spectrum applies to only a small subset of Seyfert 2s or to all of them. line_8: Our sample will yield an unbiased, unambiguous result for a large enough line_9: sample to settle the question of whether Seyfert 2 galaxies have an line_10: occulted source of non--stellar continuum. For the majority of Seyfert 2 line_11: galaxies, continuum polarization is impossible to determine from the line_12: ground due to contamination by polarized starlight, regardless of S/N. No line_13: space--based polarimeter capable of making these measurements exists other line_14: than on the HST. The unique ability of the HST to perform ultraviolet line_15: polarimetry will enable us to resolve this important question. This ability line_16: will be lost after the installation of the COSTAR. question: 4 section: 2 line_1: For a given number of detected counts, (C), and modulation efficiency, (E), line_2: the signal--to--noise in a polarization measurement is: line_3: S/N = (E * P * C)/ (sqrt(2) *sqrt(C)) line_4: The factor of sqrt(2) comes from the conversion of Q and U to P. This line_5: formula reproduces the results in the original FOS Instrument Handbook line_6: (page C--9). To determine the count rate, we have used the latest values line_7: for the HST and FOS efficiency determined by the FOS IDT and included in line_8: the FOS simulator program, but we have multiplied the result by a factor of line_9: 0.5 because the FOS polarimeter can measure only one ray at a time and by line_10: another factor of 0.8 for the waveplate transmission at 2500Angstroms . The line_11: modulation efficiency at 2537Angstroms is 0.77 (See the current FOS line_12: handbook, page 22 and 23 for waveplate transmission and modulation line_13: efficiency.) The objects are bright enough that sky and dark are line_14: negligible, even using the large aperture. question: 4 section: 3 line_1: We have estimated the nuclear continuum fluxes at 2500Angstroms from the line_2: IUE measurements. Assuming a power law index of alpha = 1.3, F(nu) line_3: proportional to nu^(-alpha) (the medians from the acceptable quality IUE line_4: data), and a P of 3%, we will aim for a polarized flux SNR of at least 5. line_5: With a dispersion of 2.05Angstroms /diode we will bin over the 425 diodes line_6: between 2125Angstroms and 3000Angstroms . Using the above factors, an line_7: object with F(lambda)=1.0 * 10^(-15) erg cm^(-2) s^(-1) Angstroms ^(-1) at line_8: 2500Angstroms would yield approximately 190 counts s^(-1) in this range, line_9: without the use of the polarimeter. question: 7 section: 1 line_1: The investigators have worked for the FOS IDT and have extensive experience line_2: both with the FOS and astronomical polarimetry. We will analyze the data at line_3: UCSD and UCSB. Processing is basically the same as for FOS spectral data. line_4: It is additionally necessary to add and difference the spectra taken at the line_5: different waveplate position angles to create the unnormalized Q and U line_6: polarized flux spectra, which are then divided by the modulation efficiency line_7: curve and added in quadrature to produce the total polarized flux. (The Q line_8: and U spectra will be binned to increase the S/N.) SDAS and IRAF will line_9: provide most or all of the necessary routines, along with a package of line_10: polarimetry routines written for VISTA, an image and spectral line_11: reduction/analysis package developed at the University of California. We line_12: expect that we can produce P and Theta almost immediately for each line_13: object which is observed. For those which are polarized and which do not line_14: have adequate radio maps, we will undertake to make appropriate maps. line_15: Improved maps can be acquired by using the VLA at 2~cm or 3.6cm (with the line_16: sensitive ``Voyager'' receivers). Results for the data will be published line_17: prior to making these new maps as the P measurements alone yield a valid line_18: scientific result. The distribution of P will be used to construct new line_19: models of the obscuring region. question: 8 section: 1 line_1: Typical sky survey images are burned out in the cores of these bright line_2: objects, hence the accurate coordinates necessary for FOS target line_3: acquisition must be acquired other than from the guide star plates. For line_4: many of these objects Clements and Argyle have measured accurate line_5: coordinates, and Argyle has provided us with the coordinates of the line_6: reference stars, which are measurable on the guide star plates. line_7: Because binary search target acquisition requires fluxes known to better line_8: than a factor of two over the range of wavelength to which the red tube is line_9: sensitive, and within the 4.3" aperture, we will not use it. line_10: See queston 3, section 2. line_11: objects using the derived coordinates, and then center them perpendicular line_12: to the diode array using a peakup in the 1". question: 8 section: 2 line_1: As required, polarimetry of nearby stars to refine measurements of galactic line_2: interstellar polarization can be acquired as necessary at Lick Observatory. line_3: New radio maps may be made as a follow--up. Their acquisition will not line_4: delay the output of our polarimetry results. question: 9 section: 1 line_1: Antonucci and Cohen have worked on FOS--Team GTO data, but they are not line_2: co--investigators. Antonucci has only just received cycle 1 GO data on NGC line_3: 1068 (program 2077), a related project. He has also received data on the line_4: unrelated program 2177. Antonucci, Cohen, Kay and Krolik are also line_5: co--investigators on one or more related cycle 2 proposals from which no line_6: data have been received. line_7: The only data on which we have worked so far are GTO data, which are not line_8: ours. Some of this (on NGC1068: see below) are related to this proposal. line_9: We are working on a range of AGN and Quasar data taken by the FOS IDT with line_10: H. Ford or M. Burbidge as P.I. question: 9 section: 2 line_1: Antonucci has worked on NGC1068 emission line imaging and nuclear line_2: spectrophotometry in which much has been learned about the line_3: occultation/reflection model for this prototype, eg that we can pinpoint line_4: the obscured nucleus at the emission line cone apex, and that it is line_5: located at the megamaser position. We are now using VLBI velocity field line_6: observations of the maser in an attempt to detect dynamically and to weigh line_7: the putative supermassive black hole. The small--aperture line_8: spectrophotometry and the imaging have provided evidence that the mirror line_9: is spatially extended, verifying a theoretical prediction by Miller, line_10: Mathews, and Goodrich (Ap. J., in press). question: 9 section: 3 line_1: ``FOS Spectroscopy of Resolved Structure in the Nucleus of NGC~1068'', S. line_2: Caganoff, R.R.J. Antonucci, H.C. Ford, G.A. Kriss, G. Hartig, L. Armus, line_3: I.N. Evans, E. Rosenblatt, R.C. Bohlin and A.L. Kinney, {\bit Ap. J. line_4: Lett.}, in press, 1992. line_5: ``HST Line Imaging of the Inner 3 Arcseconds NGC~1068 in the Light of line_6: [O~III]$\lambda$5007'', I. Evans, H. Ford, A. Kinney, R. Antonucci, S. line_7: Caganoff and L. Armus, {\bit Ap. J. Lett.} {\bbf 369}, L27, 1991). line_8: ``Far UV Spectroscopy of the QSO UM 675 with the FOS on the Hubble Space line_9: Telescope'', E. Beaver, E. Burbidge, R. Cohen, V. Junkkarinen, R. Lyons, line_10: E. Rosenblatt, G. Hartig, B. Margon, and A. Davidsen, {\bit Ap. J. Lett.} line_11: {\bbf 377}, L1. line_12: ``Faint Object Spectrograph Observations of CSO 251'', R. D. Cohen, E. A. line_13: Beaver, E. M. Burbidge, V. T. Junkkarinen, R. W. Lyons, and E. I. line_14: Rosenblatt'', in {\bit The First Year of HST Observations}, A. L. Kinney line_15: and J. C. Blades, eds., page 204. line_16: ``The Conditions in the z=0.692 Absorber Towards 3CR 286'', R. D. Cohen, E. line_17: A. Beaver, V. T. Junkkarinen, T. A. Barlow, R. W. Lyons, and H. E. Smith'', line_18: \Apj, submitted. question: 10 section: 1 line_1: All computing facilities required for data reduction and analysis and any line_2: theoretical follow--up already exist at our institutions and are available line_3: largely free of charge. Any necessary supporting optical polarimetric line_4: observations will be done at University of California facilities. We hope line_5: to involve students in this work, provided that support is provided by this line_6: grant. fixed_targets: targnum: 1 name_1: MRK463E descr_1: E,312,923,924 pos_1: RA = 13H 56M 2.920S +/- 0.3", pos_2: DEC = 18D 22' 18.83" +/- 0.3", pos_3: PLATE-ID=019M equinox: 2000 rv_or_z: Z = .0505 fluxnum_1: 1 fluxval_1: V = 14.2 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 4.0 +/- 1.0 E-15 targnum: 2 name_1: MARK34 descr_1: E,312,923,924 pos_1: RA = 10H 34M 8.573S +/- 0.3", pos_2: DEC = 60D 1' 52.01" +/- 0.3", pos_3: PLATE-ID=01S0 equinox: 2000 rv_or_z: Z = .0515 fluxnum_1: 1 fluxval_1: V = 14.7 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 1.3 +/- 0.5 E-15 ! No solar system records found ! No generic target records found exposure_logsheet: ! linenum: 1.0 targname: MRK463E config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 2.0; req_2: SEQ 1.0-4.0 NO GAP; req_3: CYCLE 4 / 1.0-4.0; param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=1.23, ! linenum: 2.0 targname: MRK463E config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 3.0; param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2, param_4: SCAN-STEP-X=0.61, param_5: SCAN-STEP-Y=0.61, ! linenum: 3.0 targname: MRK463E config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 4.0; param_2: SEARCH-SIZE-X=3, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-X=0.29, param_5: SCAN-STEP-Y=0.29, ! linenum: 4.0 targname: MRK463E config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1200S fluxnum_1: 2 priority: 1 param_1: POLSCAN = 4B ! linenum: 11.0 targname: MARK34 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 12.0; req_2: SEQ 11.0-14.0 NO GAP; req_3: CYCLE 4 / 11.0-14.0; param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=1.23, ! linenum: 12.0 targname: MARK34 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 13.0; param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2, param_4: SCAN-STEP-X=0.61, param_5: SCAN-STEP-Y=0.61, ! linenum: 13.0 targname: MARK34 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 14.0; param_2: SEARCH-SIZE-X=3, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-X=0.29, param_5: SCAN-STEP-Y=0.29, ! linenum: 14.0 targname: MARK34 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1200S fluxnum_1: 2 priority: 1 param_1: POLSCAN = 4B ! No scan data records found