! File: 1219C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:06:34:33 coverpage: title_1: POLARIZATION MAPPING OF THE INNER STRUCTURE OF THE SEYFERT GALAXY NGC title_2: 1068 TO SEARCH FOR A NON-THERMAL SOURCE sci_cat: QUASARS, AGN proposal_for: GTO/FOC pi_fname: ALEC pi_lname: BOKSENBERG pi_inst: ROYAL GREENWICH OBSERVATORY pi_country: UNITED KINGDOM pi_phone: 0223 374000 keywords_1: POLARIMETRY, NUCLEUS, SEYFERT GALAXY NGC1068 hours_pri: 6.00 num_pri: 1 time_crit: X pi_position: PROFESSOR ! end of coverpage abstract: line_1: Several Seyfert galaxies, including NGC 1068, are known to be intrinsically line_2: polarized. The source of this polarization may be synchrotron emission from a line_3: jet or electron scattering from an accretion disk or dust scattering from an line_4: extended aggregate of clouds surrounding the nucleus. Images with the Space line_5: Telescope at a resolution of 0.02" should resolve structure down to a scale of line_6: ~1 parsec in NGC 1068. High signal-to-noise images in polarized light should line_7: then enable one to discriminate between bright (unpolarized) HII regions, line_8: extended polarizing dust clouds and a compact polarized non-thermal source. In line_9: the UV, where residual galaxy dilution is weakest, polarizations of ~15% can be line_10: expected. The combination of UV sensitivity and high spatial resolution make line_11: the FOC well suited to this experiment. This proposal to use the FOC follows line_12: naturally from our extensive programme of ground-based observations and line_13: modelling of Seyfert nuclei. ! ! end of abstract general_form_proposers: lname: WARD fname: M. inst: OXFORD UNIVERSITY country: UNITED KINGDOM esa: X ! lname: AXON fname: D. mi: J. inst: MANCHESTER, UNIVERSITY OF country: UNITED KINGDOM esa: X ! lname: MCLEAN fname: IAN mi: S. inst: ROYAL OBSERVATORY, EDINBURGH country: UNITED KINGDOM esa: X ! lname: BOKSENBERG fname: ALEC inst: ROYAL GREENWICH OBSERVATORY country: UNITED KINGDOM esa: X ! lname: HEATHCOTE fname: S. mi: R. inst: NOAO, CERRO TOLOLO INTERAMERICAN OBSERVATORY country: UNITED KINGDOM esa: X ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: At the distance of NGC 1068 (~16 Mpc assuming Ho = 75 km s-1 Mps-1), 2pc~= line_2: 0.03" and this should be within the capabilities of ST. The FOC in the f/96 line_3: mode would yield 0.022 arcsec/pixel and a format of 512 x 512 would give 11.2" line_4: x 11.2" or 860 x 860 pc. Since the effective magnitude of the unresolved line_5: central source will be ~ 16-17, the central pixels will saturate but the wings line_6: and all other sources, such as jets, will be below saturation. A second set of line_7: observations using the f/288 mode on the unresolved central source should line_8: enable its polarization to be determined accurately. line_10: 3.2 Errors line_12: For pixel receiving flux at near the maximum counting rate of 0.6 count/s/ line_13: pixel then an integration time of 2 hours per Rochon polarizer (0d, 60d, 120d) line_14: will yield errors ~ 1%. If the count rate is ten times smaller then the line_15: polarization error will be ~ 3%. The latter will still be a 5SIGMA result (per line_16: pixel) if te expected polarization of 15% is indeed present. ! question: 4 section: 1 line_1: ST Justification line_3: Because we are searching for compact, polarized sources in the innermost line_4: regions of the Seyfert nucleus then high spatial (angular) resolution is line_5: essential. The ST resolution is clearly beyond the bounds of any ground-based line_6: technique except perhaps speckle. But the speckle techniques are difficult line_7: and in any case, polarization images are the main requirements here. ! question: 6 section: 1 line_1: Roll orientation must be known for polarimetry ! question: 7 section: 1 line_1: Reduction and Analysis of Data line_3: The required software for analysis of polarization images already exists at the line_4: Royal Observatory, Edinburgh on the STARLINK VAX 11/780 system. All that is line_5: required is that the ST FOC data be available in FITS format on a magnetic line_6: tape. A description of our polarimetry package (IMPOL) has been supplied to line_7: STScI and to the FOC team (Dr C Blades); it could probably be transferred to line_8: the ECF VAX computer system. line_10: A detailed functional specification for the reduction of polarization data line_11: under SDAS has been prepared by Dr Olivia Lupie (STScI) and this would appear line_12: to embody all the basic requirements (including display) and many additional line_13: features. line_15: It would, however, be very useful to receive TEST DATA (e.g. polarized flat line_16: fields through each Rochon prism) on magnetic tape at an early date to test for line_17: compatibility of the existing softwsre with the type of data produced by the line_18: FOC. ! question: 10 section: 1 line_1: Resources Supplied line_3: These would mainly be in the form of data analysis capabilities and travel line_4: support. ! question: 13 section: 1 line_1: High angular resolution polarization images of NGC1068 to search for spatially line_2: extended and/or compact sources of polarixation within the nucleus of this line_3: Seyfert galaxy. ! !end of general form text general_form_address: lname: MCLEAN fname: IAN mi: S. category: CON inst: ROYAL OBSERVATORY addr_1: BLACKFORD HILL city: EDINBURGH country: UNITED KINGDOM phone: 031 668 8100 telex: 72383 ! lname: BOKSENBERG fname: ALEC title: PROF. category: PI inst: ROYAL GREENWICH OBSERVATORY addr_1: MADINGLEY ROAD addr_2: CB3 0EZ city: CAMBRIDGE country: UNITED KINGDOM phone: 44 223 374000 telex: 817235 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1068-NUC descr_1: SEYFERT GALAXY NUCLEUS pos_1: RA = 2H 40M 7.06S +/- 0.1S, pos_2: DEC = -0D 13' 31.46" +/- 0.05" equinox: 1950 pm_or_par: N rv_or_z: Z=0.0037 acqpr_1: EXT comment_1: UNRESOLVED POINT SOURCE SHOULD BE comment_2: APPROXIMATELY V=16.0 comment_3: REF TO PLATE_REQ/PLATE_AVAIL comment_4: DELETED TO GET A VALIDATION comment_5: NOT GASP. TOO BRIGHT fluxnum_1: 1 fluxval_1: SURF(V)=13.0 ! targnum: 2 name_1: HD16970-CALIB descr_1: CALIBRATION pos_1: RA = 2H 40M 42.060S +/- 0.1S, pos_2: DEC = +03D 01' 29.14" +/- 0.5" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.009400 ra_pm_unct: 0.001333 dec_pm_val: -0.1470 dec_pm_unct: 0.0200 an_prlx_val: 0.0480 an_prlx_unct: 0.0100 plate_req: N plate_avail: N comment_1: GASP MEASURE comment_2: THIS IS A HIGH PROPER comment_3: STAR. DOUBLE, 3 & 6.8 MAG comment_4: SEPARATION 3" fluxnum_1: 1 fluxval_1: V = 3.46, TYPE = A3V, E(B-V) = 0.01 fluxnum_2: 2 fluxval_2: F-CONT(1965) = 1.35 +/- 0.14E-10 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEF sequence_2: FOC-POL-1 targname: NGC1068-NUC config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F307M,POL0 wavelength: 3080 num_exp: 1 time_per_exp: 1800S fluxnum_1: 1 priority: # req_1: GROUP 1-3 WITHIN 1D; req_2: SAME ORIENT FOR 2-3 AS 1; req_3: CYCLE 2 /1-14; req_4: GUID TOL 0.020" / 1-14; req_5: COND IF TAC OK / 1-14; ! linenum: 2.000 sequence_1: DEF sequence_2: FOC-POL-1 targname: NGC1068-NUC config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F307M,POL60 wavelength: 3080 num_exp: 1 time_per_exp: 1800S fluxnum_1: 1 priority: # ! linenum: 3.000 sequence_1: DEF sequence_2: FOC-POL-1 targname: NGC1068-NUC config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F307M,POL120 wavelength: 3080 num_exp: 1 time_per_exp: 1800S fluxnum_1: 1 priority: # comment_1: SIGMA(P)~2% FOR 4 HOURS. ! linenum: 4.000 sequence_1: USE sequence_2: FOC-POL-1 priority: 1 ! linenum: 5.000 sequence_1: USE sequence_2: FOC-POL-1 priority: 1 req_1: SAME ORIENT FOR 5 AS 4; ! linenum: 6.000 sequence_1: DEF sequence_2: FOC-POL-2 targname: NGC1068-NUC config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F307M,POL0 wavelength: 3080 num_exp: 1 time_per_exp: 1300S fluxnum_1: 1 priority: # req_1: GROUP 6-8 WITHIN 1D; req_2: SAME ORIENT FOR 7-8 AS 6; comment_1: REMOVED GROUP TO GET A VERIFY ! linenum: 7.000 sequence_1: DEF sequence_2: FOC-POL-2 targname: NGC1068-NUC config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F307M,F1ND,POL60 wavelength: 3080 num_exp: 1 time_per_exp: 1300S fluxnum_1: 1 priority: # ! linenum: 8.000 sequence_1: DEF sequence_2: FOC-POL-2 targname: NGC1068-NUC config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F307M,POL120 wavelength: 3080 num_exp: 1 time_per_exp: 1300S fluxnum_1: 1 priority: # comment_1: SIGMA(P)~3% FOR 1.5 HOURS. ! linenum: 9.000 sequence_1: USE sequence_2: FOC-POL-2 priority: 2 req_1: SAME ORIENT FOR 9 AS 4 ! linenum: 11.000 targname: NGC1068-NUC config: FOC/96 opmode: IMAGE aperture: 256X256 sp_element: F190M wavelength: 1975 num_exp: 1 time_per_exp: 500S priority: 1 req_1: ORIENT 220D +/- 10D; req_2: GROUP 11-13 WITHIN 1D; comment_1: ORIENT 40D +/- 10D IS EQUALLY GOOD. ! linenum: 12.000 targname: NGC1068-NUC config: FOC/96 opmode: IMAGE aperture: 256X256 sp_element: F190M wavelength: 1975 num_exp: 1 time_per_exp: 500S priority: 1 req_1: ORIENT 260D +/- 10D; comment_1: ORIENT 80D +/- 10D IS EQUALLY GOOD. ! linenum: 13.000 targname: NGC1068-NUC config: FOC/96 opmode: IMAGE aperture: 256X256 sp_element: F190M wavelength: 1975 num_exp: 1 time_per_exp: 500S priority: 1 req_1: ORIENT 300D +/- 10D; comment_1: ORIENT 120D +/- 10D IS EQUALLY GOOD. ! linenum: 14.000 targname: HD16970-CALIB config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F190M, F8ND wavelength: 1975 time_per_exp: 300S fluxnum_1: 2 priority: 1 req_1: CALIB FOR 13; req_2: SEQ 11-14 NO GAP; req_3: SAME ORIENT FOR 14 AS 13; comment_1: NOTE HIGH PROPER MOTION comment_2: STAR WHICH IS CLOSE comment_3: DOUBLE. ! ! end of exposure logsheet ! No scan data records found