! File: 4500C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:15:00:12 coverpage: title_1: GEOMETRY AND GENERALIZABILITY OF THE REFLECTED LIGHT MODEL FOR title_2: SEYFERT 2 GALAXIES -CYC3 SUPPLEMENTAL 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: 12.00 num_pri: 18 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 general_form_text: question: 3 section: 1 line_1: We will do broad-band polarimetry of 10 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\%. Using the FOS for broad--band polarimetry is faster than line_6: using the HSP. 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: This 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. For 8 of the object we have line_2: derived coordinates in the guide star system from published coordinates line_3: along with measured coordinates for the reference stars (which are all in line_4: the guide star catalog). For these objects, we will use a binary search on line_5: a nearby star in the guide star catalog and then offset to the derived line_6: position of the seyfert galaxy. We will then do a 5 step (Y) by two step line_7: (X) peak-up with the one arc second aperture. The steps will be 0.4 line_8: seconds apart to achieve the desired goal of centering accuracy line_9: perpendicular to the diode array of 0.2". The only reason to do two steps line_10: in X is to insure that errors in the offset do not lead to missing the line_11: object with the peak-up in Y. Our goal for the peak-ups is to distinguish line_12: between 0.3" off center and 0.1" off center to 3 sigma accuracy. This line_13: would normally require 1600 counts (the calculated throughput differs by line_14: 8%) but we are arbitrarily including at least a factor of two safety line_15: margin to account for (unknown) shot noise from the background galaxy line_16: in the 4"aperture. All peak-up exposure times will be 6s. line_17: For two objects we have only radio coordinates. The guide star catalog line_18: shows that differences between radio positions and guide star system line_19: positions are usually less than 1". We will do a 3 stage peak-up on line_20: these two objects, with the last stage limited to a peak-up in Y. line_21: Binary searcy won't work on these objects because the flux in the 4.3 line_22: aperture is not known well enough. ! 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. line_10: For example, for Mrk 34, which has F(2500Angstroms ) = 1.3 * 10^(-15) erg line_11: cm^(-2) s^(-1) Angstroms ^(-1) the time required is 950s. Because each line_12: observation requires 4 positions of the waveplate, we set the shortest line_13: total exposure times to 20m (1200s) to limit spacecraft inefficiency. The line_14: total exposure time for 10 objects is 3.33h, while the total spacecraft line_15: time including all overhead for guide star acquisition and target line_16: acquisition, as well as 2.1~m overhead for each of 4 polarizer positions (a line_17: significant overestimate for FOS spectropolarimetry) totals 12h, for an line_18: efficiency of 28%. ! 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. Because high line_10: accuracy in the wavelength setting is not required, we will offset to the 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. ! !end of general form text 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 fixed_targets: targnum: 1 name_1: NGC3982 descr_1: E,312,923,924 pos_1: RA = 11H 56M 28.131S +/- 0.3", pos_2: DEC = 55D 7' 30.09" +/- 0.3", pos_3: PLATE-ID=00LK equinox: 2000 rv_or_z: Z = .003 fluxnum_1: 1 fluxval_1: V = 11.7 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 4.8 +/- 0.5 E-15 ! targnum: 2 name_1: NGC3982-OFFSET descr_1: A,137 pos_1: RA = 11H 56M 23.78S +/- 0.3", pos_2: DEC = 55D 4' 8" +/- 0.3", pos_3: PLATE-ID=00LK equinox: 2000 fluxnum_1: 1 fluxval_1: V = 13 +/- 0.5, TYPE=G2V ! targnum: 3 name_1: NGC7674 descr_1: E,312,923,924 pos_1: RA = 23H 27M 56.697S +/- 0.3", pos_2: DEC = 8D 46' 43.87" +/- 0.3", pos_3: PLATE-ID=0100 equinox: 2000 rv_or_z: Z = .029 fluxnum_1: 1 fluxval_1: V = 14.4 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 4.0 +/- 0.5 E-15 ! targnum: 4 name_1: NGC7674-OFFSET descr_1: A,137 pos_1: RA = 23H 27M 58.75S +/- 0.3", pos_2: DEC = 8D 46' 57.4" +/- 0.3", pos_3: PLATE-ID=0100 equinox: 2000 fluxnum_1: 1 fluxval_1: V = 13.9 +/- 0.5, TYPE=G2V ! targnum: 5 name_1: MARK266SW descr_1: E,312,923,924 pos_1: RA = 13H 38M 17.798S +/- 0.3", pos_2: DEC = 48D 16' 41.23" +/- 0.3", pos_3: PLATE-ID=008S equinox: 2000 rv_or_z: Z = .028 fluxnum_1: 1 fluxval_1: V = 13.4 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 3.1 +/- 0.5 E-15 ! targnum: 6 name_1: MARK266SW-OFFSET descr_1: A,137 pos_1: RA = 13H 38M 34.71S +/- 0.3", pos_2: DEC = 48D 14' 41.4" +/- 0.3", pos_3: PLATE-ID=008S equinox: 2000 fluxnum_1: 1 fluxval_1: V = 12.4 +/- 0.5, TYPE=G2V ! targnum: 7 name_1: MARK573 descr_1: E,312,923,924 pos_1: RA = 1H 43M 57.742S +/- 0.3", pos_2: DEC = 2D 20' 59.66" +/- 0.3", pos_3: PLATE-ID=00GZ equinox: 2000 rv_or_z: Z = .017 fluxnum_1: 1 fluxval_1: V = 14.1 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 2.1 +/- 0.5 E-15 ! targnum: 8 name_1: MARK573-OFFSET descr_1: A,137 pos_1: RA = 1H 44M 8.22S +/- 0.3", pos_2: DEC = 2D 23' 41.9" +/- 0.3", pos_3: PLATE-ID=00GZ equinox: 2000 fluxnum_1: 1 fluxval_1: V = 13.7+/- 0.5, TYPE=G2V ! targnum: 9 name_1: MARK348 descr_1: E,312,923,924 pos_1: RA = 0H 48M 47.204S +/- 0.3", pos_2: DEC = 31D 57' 24.98" +/- 0.3", pos_3: PLATE-ID=02HD equinox: 2000 rv_or_z: Z = .014 fluxnum_1: 1 fluxval_1: V = 14.6+/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 1.9 +/- 0.5 E-15 ! targnum: 10 name_1: MARK348-OFFSET descr_1: A,137 pos_1: RA = 0H 48M 39.26S +/- 0.3", pos_2: DEC = 31D 57' 20.3" +/- 0.3", pos_3: PLATE-ID=02HD equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14.3 +/- 0.5, TYPE=G2V ! targnum: 11 name_1: MARK78 descr_1: E,312,923,924 pos_1: RA = 7H 42M 41.667S +/- 0.3", pos_2: DEC = 65D 10' 37.38" +/- 0.3", pos_3: PLATE-ID=00MC equinox: 2000 rv_or_z: Z = .038 fluxnum_1: 1 fluxval_1: V = 14.6 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 1.5 +/- 0.5 E-15 ! targnum: 12 name_1: MARK78-OFFSET descr_1: A,137 pos_1: RA = 7H 42M 36.23S +/- 0.3", pos_2: DEC = 65D 11' 1" +/- 0.3", pos_3: PLATE-ID=00MC equinox: 2000 fluxnum_1: 1 fluxval_1: V = 12.9 +/- 0.5, TYPE=G2V ! targnum: 13 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 = .051 fluxnum_1: 1 fluxval_1: V = 14.7 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 1.3 +/- 0.5 E-15 ! targnum: 14 name_1: MARK34-OFFSET descr_1: A,137 pos_1: RA = 10H 33M 55.94S +/- 0.3", pos_2: DEC = 60D 2' 8.0" +/- 0.3", pos_3: PLATE-ID=01S0 equinox: 2000 fluxnum_1: 1 fluxval_1: V = 13.1 +/- 0.5, TYPE=G2V ! targnum: 15 name_1: MARK270 descr_1: E,312,923,924 pos_1: RA = 13H 41M 5.642S +/- 0.3", pos_2: DEC = 67D 40' 20.00" +/- 0.3", pos_3: PLATE-ID=01BR equinox: 2000 rv_or_z: Z = .009 fluxnum_1: 1 fluxval_1: V = 14.1 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 1.3 +/- 0.5 E-15 ! targnum: 16 name_1: MARK270-OFFSET descr_1: A,137 pos_1: RA = 13H 41M 18.76S +/- 0.3", pos_2: DEC = 67D 42' 21.4" +/- 0.3", pos_3: PLATE-ID=01BR equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14.1 +/- 0.5, TYPE=G2V ! targnum: 17 name_1: NGC5135 descr_1: E,312,923,924 pos_1: RA = 13H 25M 43.9S +/- 1.0", pos_2: DEC = -29D 50' 2.66" +/- 1.0", equinox: 2000 rv_or_z: Z = .013 comment_1: PRECESSED FROM RADIO COORDINATES comment_2: 13H22M56.460S, -29D,34',27.5" comment_3: USING IRAF FOR 1950->2000. fluxnum_1: 1 fluxval_1: V = 13.4+/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 9.5 +/- 0.5 E-15 ! targnum: 18 name_1: TOL1238-364 descr_1: E,312,923,924 pos_1: RA = 12H 40M 52.81S +/- 1.0", pos_2: DEC = -36D 45' 20.95" +/- 1.0", equinox: 2000 rv_or_z: Z = .011 comment_1: PRECESSED FROM RADIO COORDINATES comment_2: 12H38M10.568S,-36D,28',53.56" comment_3: USING IRAF FOR 1950->2000. fluxnum_1: 1 fluxval_1: V = 13.5 +/- .5 fluxnum_2: 2 fluxval_2: F-CONT(2500) = 6.5 +/- 0.5 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC3982-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.09S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 1.5; req_2: SEQ 1-1.9 NO GAP; req_3: CYCLE 3 / 1-1.9 comment_1: THE OFFSET WILL BE 3.4 ARCMIN. comment_2: IF THIS IS TOO FAR, A CLOSER comment_3: OFFSET STAR WITH LESS ACCURATE comment_4: COORDINATES IS AVAILABLE. ! linenum: 1.500 targname: NGC3982 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 1.9; ! linenum: 1.900 targname: NGC3982 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: 2.000 targname: NGC7674-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 2.51S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 2.5; req_2: SEQ 2.0-2.9 NO GAP; req_3: CYCLE 3 / 2.0-2.9; comment_1: THE OFFSET WILL BE 33 ARCSEC ! linenum: 2.500 targname: NGC7674 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 2.9; ! linenum: 2.900 targname: NGC7674 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: 3.000 targname: MARK266SW-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: 1 param_1: BRIGHT = 720000, param_2: FAINT = 700 req_1: ONBOARD ACQ FOR 3.5; req_2: SEQ 3.0-3.9 NO GAP; req_3: CYCLE 3 / 3.0-3.9; ! linenum: 3.500 targname: MARK266SW config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 3.9; ! linenum: 3.900 targname: MARK266SW 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: 4.000 targname: MARK573-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 2.08S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 4.5; req_2: SEQ 4.0-4.9 NO GAP; req_3: CYCLE 3 / 4.0-4.9; comment_1: THE OFFSET WILL BE 3.8 ARCSEC comment_2: IF THIS IS TOO FAR, A CLOSER comment_3: OFFSET STAR WITH LESS ACCURATE comment_4: COORDINATES IS AVAILABLE. ! linenum: 4.500 targname: MARK573 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 4.9; ! linenum: 4.900 targname: MARK573 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: MARK348-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.62S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 5.5; req_2: SEQ 5.0-5.9 NO GAP; req_3: CYCLE 3 / 5.0-5.9; comment_1: THE OFFSET WILL BE 1.7 ARCMIN. ! linenum: 5.500 targname: MARK348 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 5.9; ! linenum: 5.900 targname: MARK348 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: 6.000 targname: MARK78-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.00S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 6.5; req_2: SEQ 6.0-6.9 NO GAP; req_3: CYCLE 3 / 6.0-6.9; comment_1: THE OFFSET WILL BE 40ARCSEC. ! linenum: 6.500 targname: MARK78 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 6.9; ! linenum: 6.900 targname: MARK78 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: 7.000 targname: MARK34-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.20S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 7.5; req_2: SEQ 7.0-7.9 NO GAP; req_3: CYCLE 3 / 7.0-7.9; comment_1: THE OFFSET WILL BE 1.6ARCMIN. ! linenum: 7.500 targname: MARK34 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 7.9; ! linenum: 7.900 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 ! linenum: 8.000 targname: MARK270-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.01S fluxnum_1: 1 priority: 1 param_1: BRIGHT = 720000 req_1: ONBOARD ACQ FOR 8.5; req_2: SEQ 8.0-8.9 NO GAP; req_3: CYCLE 3 / 8.0-8.9; comment_1: THE OFFSET WILL BE 2.4ARCMIN. ! linenum: 8.500 targname: MARK270 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=2, param_3: SEARCH-SIZE-Y=5, param_4: SCAN-STEP-X=0.4, param_5: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 8.9; ! linenum: 8.900 targname: MARK270 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: 9.000 targname: NGC5135 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=1.4, req_1: ONBOARD ACQ FOR 9.5; req_2: SEQ 9.0-9.9 NO GAP; req_3: CYCLE 3 / 9.0-9.9; ! linenum: 9.500 targname: NGC5135 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2, param_4: SCAN-STEP-X=0.7, param_5: SCAN-STEP-Y=0.7, req_1: ONBOARD ACQ FOR 9.6; ! linenum: 9.600 targname: NGC5135 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 9.9; ! linenum: 9.900 targname: NGC5135 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: 10.000 targname: TOL1238-364 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=1.4, req_1: ONBOARD ACQ FOR 10.5; req_2: SEQ 10.0-10.9 NO GAP; req_3: CYCLE 3 / 10.0-10.9; ! linenum: 10.500 targname: TOL1238-364 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2, param_4: SCAN-STEP-X=0.7, param_5: SCAN-STEP-Y=0.7, req_1: ONBOARD ACQ FOR 10.6; ! linenum: 10.600 targname: TOL1238-364 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=0.4, req_1: ONBOARD ACQ FOR 10.9; ! linenum: 10.900 targname: TOL1238-364 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 ! ! end of exposure logsheet ! No scan data records found