! File: 4371C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:23:38:28 coverpage: title_1: FOS SPECTROSCOPY OF RESOLVED STRUCTURE IN THE NUCLEUS OF MARKARIAN 3 sci_cat: QUASARS & AGN sci_subcat: SEYFERTS proposal_for: GO pi_fname: ZLATAN pi_mi: I pi_lname: TSVETANOV pi_inst: JOHNS HOPKINS UNIVERSITY pi_country: USA pi_phone: 410-516-8585 hours_pri: 4.00 num_pri: 3 fos: Y funds_amount: 30000 funds_length: 12 off_fname: CHERYL-LEE off_lname: HOWARD off_title: ASSISTANT DEAN off_inst: 2380 off_addr_1: HOMEWOOD REASEARCH ADMINISTARTION off_addr_2: 105 AMES HALL off_addr_3: 34TH & NORTH CHARLES STREET off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 410-516-8668 ! end of coverpage abstract: line_1: The narrow-band images of the Seyfert 2 galaxy Mrk 3 taken with the Planetary line_2: Camera on board HST reveal a remarkable sequence of emission-line clouds line_3: arranged along an S-shaped structure in close correspondence with the cm line_4: wavelength radio map. We propose to carry out optical and UV FOS spectroscopy line_5: of some of the discrete clouds. Our goals are to (1) locate and establish line_6: the physical properties of the ``mirrors'' which scatter light from the line_7: hidden broad line region, and (2) study the kinematics of the emission line gas line_8: and compare it with the stellar velocity field. Previous ground-based line_9: studies have shown evidence for the presence of a hidden Seyfert 1 nucleus in line_10: Mrk 3, in accordance with the unified models of AGN. To study this in more line_11: detail we will compare cloud spectra with state-of-the-art photoionization line_12: models to estimate properties such as the intensity of the ionizing radiation line_13: impinging on the clouds. In particular, we will be looking for broad-wings of line_14: the Balmer and other permitted lines due to scattering into our line of sight line_15: of light from the obscured nuclear region, and for signatures of shock waves line_16: and high velocity gas motions (outflow/inflow), which may be a characteristic line_17: of the interaction of the radio plasma with the ambient ISM. With its nuclear line_18: structure completely resolved by the HST and favorable cloud sizes and line_19: intercloud distances Mrk 3, offers one of the best cases for testing unified line_20: models of AGN with the current HST performance. ! ! end of abstract general_form_proposers: lname: TSVETANOV fname: ZLATAN title: PI mi: I inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: FORD fname: HOLLAND mi: C inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: KRISS fname: GERARD mi: A inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: EVANS fname: IAN mi: N inst: STSCI country: USA ! lname: DAVIDSEN fname: ARTHUR mi: F inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: UOMOTO fname: ALAN inst: JOHNS HOPKINS UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The 0.3" aperture of the FOS will be used to isolate the resolved line_2: emission line clouds in the nucleus of the Seyfert 2 galaxy Mrk 3. line_3: UV spectra of the brightest and innermost cloud (E1) will be obtained line_4: with gratings G130H and G190H. Exposure times are set for accumulating line_5: at least 1000 counts in the brightest UV lines. line_6: The sequence for acquiring individual clouds will be as follows: line_7: (1) Binary search on the star roughly 50" away, which appears on our line_8: PC images in chip PC_8; (2) Offset to the position of the brightest line_9: cloud (E1 in Fig. 1); (3) Do a peak-up with a small step size to center line_10: the cloud in the aperture. We have run peak-up simulations using our PC line_11: to check this procedure. ! question: 4 section: 1 line_1: Mrk 3 offers one of the best chances to study the circumnuclear region line_2: in a Seyfert 2 galaxy in detail with the current PSF of the HST. With line_3: their typical dimensions of 0.2"-0.3" and intercloud distances of line_4: 0.5"--0.6" the emission clouds themselves are impossible targets for line_5: ground-based spectrographs. On the other hand, because of these line_6: relatively large (by HST standards) separations, the contamination from line_7: the neighboring clouds due to the spherical aberration is relatively line_8: small, and so the 0.3" FOS aperture will isolate individual clouds line_9: quite well. The UV spectra of the clouds can be obtained only with the line_10: HST. line_11: Positions and sizes of individual clouds are measured from the HST line_12: images. All clouds are resolved with sizes in the range 0.2"-0.3". line_13: Therefore, the 0.3" aperture is chosen, which both isolates the clouds line_14: and does not compromise the spectral resolution. ! question: 5 section: 1 line_1: We have no special requests. ! question: 6 section: 1 line_1: We have no special calibration requirements. ! question: 7 section: 1 line_1: We expect to reduce the FOS spectra at the JHU Center for Astrophysical line_2: Sciences. We have an extensive network of Sun Workstations and most of us line_3: have been part of the FOS team for a number of years, so there is ample line_4: local experience in handling the HST data. line_5: We have already obtained emission line and continuum Planetary Camera images line_6: of Mrk 3, which were used for locating the clouds and estimating the line_7: exposure times. We also have access to previously obtained ground-based line_8: spectroscopy and images which are and will be used for calibration purposes. line_9: The analysis of the data will involve modeling with state-of-the-art line_10: photoionization codes. We have access to CLOUDY, developed by G.Ferland, line_11: and to MAPPINGS, developed by L.Binette. For example, the latest version line_12: of MAPPINGS includes dust in the gas clouds and accounts for the additional line_13: heating from grain photoemission. We will attempt to model the emission line line_14: spectrum over a wide wavelength range and to ascertain the physical line_15: conditions in the emission gas. In particular, we will look for signatures line_16: of shocks and clues for relation with the radio jet plasma, such as high line_17: velocity outflows/inflows. ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: 1036: Imaging and Spectrophotometry of Seyfert Nuclei (FOS 14). line_2: 3274: Continuation of Imaging and Spectrophotometry of Seyfert Nuclei. line_3: 3671: UV Spectroscopy of Hydrogen-Poor Planetary Nebulae. Not related to this line_4: proposal. line_5: HST images of Mrk3 were taken as part of proposals 1036 and 3274 and lead in line_6: part to the development of this proposal. line_7: With the data in this GTO program we have: (1) resolved the narrow-line region line_8: of NGC 1068 and found that the apex of the ionization cone is coincident with line_9: the peak of the CO emission and the OH megamaser, making them likely candidates line_10: for the obscuring molecular torus; (2) determined that the scattering region or line_11: "mirror" in NGC 1068 is extended on a scale of 1 arc second; (3) resolved the line_12: biconical structure of the narrow-line region in NGC 4151; (4) discovered an line_13: optical jet in the Seyfert 2 galaxy Mrk 463; (5) resolved the narrow-line line_14: regions of additional Seyfert 1's, Seyfert 2's, and LINERS. The systematic line_15: differences in the morphologies of the narrow-line regions in Seyfert 1's and line_16: 2's suggest that an additional free parameter in unified models is the line_17: orientation of the axis of the central engine relative to the disk of the host line_18: galaxy, in addition to the orientation relative to the observer. ! question: 10 section: 1 line_1: At the Center for Astrophysical Sciences, the Johns Hopkins University, we line_2: have access to a network of Sun Workstations and the appropriate software line_3: (IRAF, STSDAS) is installed. This network maintenance and other supporting line_4: technical assistance is provided through group maintenance contracts for line_5: computer equipment. The university provides opportunities for undergraduates line_6: and graduaters to assist in research projects for academic credit. ! !end of general form text general_form_address: lname: TSVETANOV fname: ZLATAN mi: I category: PI inst: Johns Hopkins University addr_1: Center of Astrophysical Sciences addr_2: Department of Physics and Astronomy addr_3: 34th & N. Charles Street city: BALTIMORE state: MD zip: 21218 country: USA phone: 410-516-8585 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MRK3-OFFSET name_2: UGC3426-OFFSET descr_1: A,138 pos_1: PLATE-ID=00M8, pos_2: RA = 6H 15M 26.353S +/- 0.3", pos_3: DEC = +71D 02' 33.17" +/- 0.3" equinox: 2000 comment_1: R MAG IS MEASURED FROM comment_2: GROUND-BASED CCD IMAGES fluxnum_1: 1 fluxval_1: R=14.58 +/- 0.02 fluxnum_2: 1 fluxval_2: V-R=0.25 +/- 0.05 ! targnum: 2 name_1: MRK3-CLOUD-E1 name_2: UGC3426-CLOUD-E1 descr_1: E,312,927,924 pos_1: RA-OFF = 9.927S +/- 0.004S, pos_2: DEC-OFF = -17.51" +/- 0.02", pos_3: FROM 1 equinox: 2000 rv_or_z: V = 3998 comment_1: LINE FLUX FROM MEASURED FROM comment_2: PC F502N IMAGE fluxnum_1: 1 fluxval_1: F-LINE(4959)=1.2 +/- 0.1 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: MRK3-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 28S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.2 ! linenum: 1.200 targname: MRK3-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: SCAN-STEP=0.2 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.3 ! linenum: 1.300 targname: MRK3-CLOUD-E1 config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 120S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: SCAN-STEP=0.12 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 1.4-1.5; req_3: GROUP 1.4-1.5 NO GAP ! linenum: 1.400 targname: MRK3-CLOUD-E1 config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H num_exp: 1 time_per_exp: 5000S priority: 1 req_1: CYCLE 3 ! linenum: 1.500 targname: MRK3-CLOUD-E1 config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G190H num_exp: 1 time_per_exp: 4500S priority: 1 req_1: CYCLE 3 ! ! end of exposure logsheet ! No scan data records found