! File: 4941C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:11:29:56 coverpage: title_1: GEOMETRY AND GENERALIZABILITY OF THE REFLECTED LIGHT MODEL FOR title_2: SEYFERT 2 GALAXIES - ANOTHER PART sci_cat: QUASARS & AGN sci_subcat: SEYFERTS proposal_for: GO pi_fname: ROSS pi_mi: D pi_lname: COHEN pi_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO pi_country: USA pi_phone: 619-534-2664 hours_pri: 7.00 num_pri: 7 fos: Y funds_amount: 73224 funds_length: 12 off_fname: RICHARD off_mi: E off_lname: ATTIYEH off_title: DEAN, OGSR off_inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO 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 a few Seyfert 2 galaxies look like the line_2: flux spectra of Seyfert 1 nuclei, and the polarization position angles are 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: about half 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: UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA ! lname: ANTONUCCI fname: ROBERT mi: RJ inst: UNIVERSITY OF CALIFORNIA, SANTA BARBARA country: USA ! lname: KAY fname: LAURA mi: E inst: BARNARD COLLEGE country: USA ! lname: KROLIK fname: JULIAN mi: H inst: THE JOHNS HOPKINS UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will do broad--band polarimetry of 7 Seyfert 2 galaxies using the line_2: FOS, large aperture, Blue detector, the G270H grating, and B line_3: Waveplate. We will obtain a S/N of 4 in the polarized flux by binning line_4: the spectrum between about 2100A and 3000A, assuming that P = 3%. line_5: The polarization measurement will use 4 waveplate settings, to line_6: minimize overhead. Exposure times for four objects with known UV line_7: flux levels will be observed for 1200s, the other three for 1445s. line_8: Target acquisition will be by blind offset followed by peak up in the line_9: 0.5" aperture, after doing a binary search target acq on a star line_10: (in the guide star cat.) with a known offset from the Seyfert nucleus. line_15: The SNR of 4 in the polarized flux will produce a PA accurate to 7D, line_16: allowing us to determine unambiguously whether P is large or small and line_17: whether the PA are aligned (like Seyfert 1 galaxies and quasars) or line_18: perpendicular to the radio structure axis. ! question: 4 section: 1 line_1: The number of Seyfert 2 galaxies for which continuum polarization may line_2: be determined from ground--based observations is strictly limited to line_3: the nearest objects and those with the strongest continuum line_4: polarizations. This technique has been pushed to its limits by one of line_5: us (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 subset of Seyfert 2s or to all of them. Our line_8: 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 line_11: 2 galaxies, continuum polarization is impossible to determine from the line_12: ground due to contamination by polarized starlight, regardless of S/N. line_13: No space--based polarimeter capable of making these measurements line_14: exists other than on the HST. The unique ability of the HST to perform line_15: ultraviolet polarimetry will enable us to resolve this important line_16: question. ! question: 7 section: 1 line_1: The investigators have worked for the FOS IDT and have extensive line_2: experience both with the FOS and astronomical polarimetry. We will line_3: analyze the data at UCSD and UCSB. Processing is basically the same as line_4: for FOS spectral data. It is additionally necessary to add and line_5: difference the spectra taken at the different waveplate position line_6: angles to create the unnormalized Q and U polarized flux spectra, line_7: which are then divided by the modulation efficiency curve and added in line_8: quadrature to produce the total polarized flux. (The Q and U spectra line_9: will be binned to increase the S/N.) SDAS and IRAF will provide most line_10: or all of the necessary routines, along with a package of polarimetry line_11: routines written for VISTA, an image and spectral reduction/analysis line_12: package developed at the University of California. We expect that we line_13: can produce P and $\Theta$ almost immediately for each object which is line_14: observed. For those which are polarized and which do not have adequate line_15: radio maps, we will undertake to make appropriate maps. Improved maps line_16: can be acquired by using the VLA at 2~cm or 3.6cm (with the sensitive line_17: ``Voyager'' receivers). Results for the data will be published prior line_18: to making these new maps as the P measurements alone yield a valid line_19: scientific result. The distribution of P will be used to construct line_20: new 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. line_4: This has been done. line_9: As required, polarimetry of nearby stars to refine measurements of line_10: galactic interstellar polarization can be acquired as necessary at line_11: Lick Observatory. line_12: New radio maps may be made as a follow--up. Their acquisition will not line_13: delay the output of our polarimetry results. ! question: 9 section: 1 line_1: Antonucci and Cohen have worked on FOS--Team GTO data, but are not line_2: Co--investigators. Antonucci expects to receive CYCLE 1 GO data. The line_3: only data received so far are GTO data, some of which (on NGC 1068: line_4: see below) are related to this proposal. We are working on a broad line_5: range of AGN and Quasar data taken by the FOS IDT with H. Ford or M. line_6: Burbidge as P.I. line_7: Antonucci has worked on NGC 1068 emission line imaging and nuclear line_8: spectrophotometry in which much has been learned about the line_9: occultation/reflection model for this prototype, eg that we can line_10: pinpoint the obscured nucleus at the emission line cone apex, and that line_11: it is located at the megamaser position. We are now using VLBI line_12: velocity field observations of the maser in an attempt to detect line_13: dynamically and to weigh the putative supermassive black hole. The line_14: small--aperture spectrophotometry and the imaging have provided line_15: evidence that the mirror is spatially extended, verifying a line_16: theoretical prediction by Miller, Mathews, and Goodrich (Ap. J., in line_17: press). ! question: 9 section: 2 line_1: ``FOS Spectroscopy of Resolved Structure in the Nucleus of NGC 1068'', line_2: S. Caganoff, R.R.J. Antonucci, H.C. Ford, G.A. Kriss, G. Hartig, L. line_3: Armus, I.N. Evans, E. Rosenblatt, R.C. Bohlin and A.L. Kinney, Ap. J. line_4: Lett., in press, 1991. line_5: ``HST Line Imaging of the Inner 3 Arcseconds NGC 1068 in the Light of line_6: [O III]lambda5007'', I. Evans, H. Ford, A. Kinney, R. Antonucci, S. line_7: Caganoff and L. Armus, Ap. J. Lett. 369, L27, 1991). line_8: ``Far UV Spectroscopy of the QSO UM 675 with the FOS and the HST'', E. line_9: Beaver, E. Burbidge, R. Cohen, V. Junkkarinen, R. Lyons, E. line_10: Rosenblatt, G. Hartig, B. Margon, and A. Davidsen, Ap. J. Lett. in line_11: press, 1991. ! question: 10 section: 1 line_1: All computing facilities required for data reduction and analysis and line_2: any theoretical follow--up already exist at our institutions. Any line_3: necessary supporting optical polarimetric observations will be done at line_4: University of California facilities. ! !end of general form text general_form_address: lname: COHEN fname: ROSS mi: D category: PI inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO addr_1: CASS 0111, UCSD addr_2: 9500 GILMAN DRIVE city: SAN DIEGO state: CA zip: 920930111 country: USA phone: 619 534 2664 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MRK3 descr_1: E,312,923,924 pos_1: RA-OFF = 3.60S +/- 0.02S, pos_2: DEC-OFF = -1' 15.71" +/- 0.1", pos_3: FROM 11, pos_4: PLATE-ID=00M8 equinox: 2000 rv_or_z: Z=.014 fluxnum_1: 1 fluxval_1: V = 13.3 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 2.6 +/- 1.0 E-15 ! targnum: 2 name_1: MRK477 descr_1: E,312,923,924 pos_1: RA-OFF = -4.249S +/- 0.011S, pos_2: DEC-OFF = -16.78" +/- 0.1", pos_3: FROM 12, pos_4: PLATE-ID=01AL equinox: 2000 rv_or_z: Z = .038 fluxnum_1: 1 fluxval_1: V = 15.0 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 3.1 +/- 1.0 E-15 ! targnum: 3 name_1: MRK1066 descr_1: E,312,923,924 pos_1: RA-OFF = 11.90S +/- 0.008S, pos_2: DEC-OFF = 31.91" +/- 0.1", pos_3: FROM 13, pos_4: PLATE-ID=036R equinox: 2000 rv_or_z: Z = .012 fluxnum_1: 1 fluxval_1: V = 14.0 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 2.3 +/- 2.3 E-15 ! targnum: 4 name_1: NGC4388 descr_1: E,312,923,924 pos_1: RA-OFF = -2.13S +/- 0.007S, pos_2: DEC-OFF = +2' 54.05" +/- 0.1", pos_3: FROM 14, pos_4: PLATE-ID=00IY equinox: 2000 rv_or_z: Z = .008 fluxnum_1: 1 fluxval_1: V = 13.9 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 4.1 +/- 2.0 E-15 ! targnum: 5 name_1: MRK1073 descr_1: E,312,923,924 pos_1: RA-OFF = 5.48S +/- 0.009S, pos_2: DEC-OFF = 1' 24.14" +/- 0.1", pos_3: FROM 15, pos_4: PLATE-ID=02RZ equinox: 2000 rv_or_z: Z = .023 fluxnum_1: 1 fluxval_1: V = 14.2 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 1.3 +/- 1.3 E-15 ! targnum: 6 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 = .051 fluxnum_1: 1 fluxval_1: V = 14.2 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 2.0 +/- 1.5 E-15 ! targnum: 8 name_1: MRK1 descr_1: E,312,923,924 pos_1: RA-OFF = 8.10S +/- 0.008S, pos_2: DEC-OFF = -21.18" +/- 0.1", pos_3: FROM 18, pos_4: PLATE-ID=00DV equinox: 2000 rv_or_z: Z = .016 fluxnum_1: 1 fluxval_1: V = 15.0 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 1.1 +/- 1.1 E-15 ! targnum: 11 name_1: MRK3-OFFSET name_2: GSC4349-884 descr_1: A,137 pos_1: RA = 06H 15M 32.695S +/- 0.3", pos_2: DEC = +71D 03' 31.02" +/- 0.3", pos_3: PLATE-ID=00M8 equinox: 2000 fluxnum_1: 1 fluxval_1: V = 12.23 +/- 0.04, TYPE=G6-G8V ! targnum: 12 name_1: MRK477-OFFSET name_2: GSC3860-523 descr_1: A,137 pos_1: RA = 14H 40M 42.309S +/- 0.3", pos_2: DEC = 53D 30M 32.51" +/- 0.3", pos_3: PLATE-ID=01AL equinox: 2000 fluxnum_1: 1 fluxval_1: V = 12.26 +/- 0.01, TYPE=G6-G8V ! targnum: 13 name_1: MRK1066-OFFSET name_2: GSC2338-890 descr_1: A,137 pos_1: RA = 02H 59M 46.711S +/- 0.3", pos_2: DEC = 36D 48' 42.19" +/- 0.3", pos_3: PLATE-ID=036R equinox: 2000 fluxnum_1: 1 fluxval_1: V = 12.40 +/- 0.13, TYPE=G6-G8V ! targnum: 14 name_1: NGC4388-OFFSET name_2: GSC880-517 descr_1: A,139 pos_1: RA = 12H 25M 48.859S +/- 0.3", pos_2: DEC = +12D 36' 46.920" +/- 0.3", pos_3: PLATE-ID=00IY equinox: 2000 fluxnum_1: 1 fluxval_1: V = 11.68 +/- 0.48, TYPE=K3-K4V ! targnum: 15 name_1: MRK1073-OFFSET name_2: GSC2856-2121 descr_1: A,139 pos_1: RA = 03H 14M 55.920S +/- 0.3", pos_2: DEC = 42D 00' 45.28" +/-0.3", pos_3: PLATE-ID=02RZ equinox: 2000 fluxnum_1: 1 fluxval_1: V = 11.04 +/- 0.22, TYPE=K4-K5V ! targnum: 16 name_1: MRK463E-OFFSET name_2: GSC1470-633 descr_1: A,137 pos_1: RA = 13H 56M 1.854S +/- 0.3", pos_2: DEC = 18D 23' 27.52" +/- 0.3", pos_3: PLATE-ID=019M equinox: 2000 fluxnum_1: 1 fluxval_1: V = 12.48 +/- 0.26, TYPE=G2V ! targnum: 18 name_1: MRK1-OFFSET name_2: GSC2295-1251 descr_1: A,124 pos_1: RA = 01H 15M 59.182S +/- 0.3", pos_2: DEC = 33D 5' 42.86" +/- 0.3", pos_3: PLATE-ID=00DV equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14.06 +/- 0.18, TYPE=A3-A4V ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: MRK3-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.68S fluxnum_1: 1 priority: 2 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 1.5; req_2: SEQ 1-2 NO GAP; req_3: CYCLE 2 / 1-16; ! linenum: 1.500 targname: MRK3 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 15.0S fluxnum_1: 1 priority: 2 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 2.0; req_2: SPATIAL SCAN ! linenum: 2.000 targname: MRK3 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1200S fluxnum_1: 2 priority: 2 param_1: POLSCAN = 4B ! linenum: 3.000 targname: MRK477-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.69S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 3.5; req_2: SEQ 3-4 NO GAP; ! linenum: 3.500 targname: MRK477 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 15.0S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 4.0; req_2: SPATIAL SCAN ! linenum: 4.000 targname: MRK477 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: 5.000 targname: MRK1066-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.79S fluxnum_1: 1 priority: 3 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 5.5; req_2: SEQ 5-6 NO GAP ! linenum: 5.500 targname: MRK1066 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 15.0S fluxnum_1: 1 priority: 3 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 6.0; req_2: SPATIAL SCAN ! linenum: 6.000 targname: MRK1066 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1445S fluxnum_1: 2 priority: 3 param_1: POLSCAN = 4B ! linenum: 7.000 targname: NGC4388-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S fluxnum_1: 1 priority: 3 param_1: BRIGHT = 720000 param_2: FAINT = 820 req_1: ONBOARD ACQ FOR 7.5; req_2: SEQ 7-8 NO GAP ! linenum: 7.500 targname: NGC4388 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 15.0S fluxnum_1: 1 priority: 3 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 8.0; req_2: SPATIAL SCAN ! linenum: 8.000 targname: NGC4388 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1200S fluxnum_1: 2 priority: 3 param_1: POLSCAN = 4B ! linenum: 9.000 targname: MRK1073-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.66S fluxnum_1: 1 priority: 2 param_1: BRIGHT = 720000 param_2: FAINT = 1740 req_1: ONBOARD ACQ FOR 9.5; req_2: SEQ 9-10 NO GAP ! linenum: 9.500 targname: MRK1073 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 20.0S fluxnum_1: 1 priority: 2 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 10.0; req_2: SPATIAL SCAN ! linenum: 10.000 targname: MRK1073 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1445S fluxnum_1: 2 priority: 2 param_1: POLSCAN = 4B ! linenum: 11.000 targname: MRK463E-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.73S fluxnum_1: 1 priority: 4 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 11.5; req_2: SEQ 11-12 NO GAP; ! linenum: 11.500 targname: MRK463E config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 15.0S fluxnum_1: 1 priority: 4 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 12.0; req_2: SPATIAL SCAN ! linenum: 12.000 targname: MRK463E config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1200S fluxnum_1: 2 priority: 4 param_1: POLSCAN = 4B ! linenum: 15.000 targname: MRK1-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 2.05S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 15.5; req_2: SEQ 15-16 NO GAP ! linenum: 15.500 targname: MRK1 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 20.0S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 16.0; req_2: SPATIAL SCAN ! linenum: 16.000 targname: MRK1 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 1445S fluxnum_1: 2 priority: 1 param_1: POLSCAN = 4B ! ! end of exposure logsheet scan_data: line_list: 1.5,3.5,5.5,7.5,9.5,11.5,15.5 fgs_scan: cont_dwell: D dwell_pnts: 5 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.8000 sides_angle: 0.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 0.4 wid_offset: ! ! end of scan data