! File: 2493C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:07:24:23 coverpage: title_1: NARROW BAND IMAGING OF MARKARIAN 78 sci_cat: QUASARS & AGN proposal_for: GO pi_title: PROF. pi_fname: D. MARK pi_lname: WHITTLE pi_inst: VIRGINIA, UNIVERSITY OF pi_country: USA pi_phone: 804-924-4900 keywords_1: SEYFERT GALAXY, EMISSION LINES, JETS, DYNAMICS hours_pri: 3.00 num_pri: 1 wf_pc: X funds_amount: 51910 funds_length: 12 funds_date: MAY-91 pi_position: ASSIST. PROFESSOR off_fname: D. WAYNE off_lname: JENNINGS off_title: DIRECTOR off_inst: UNIVERSITY OF VIRGINIA off_addr_1: SPONSORED PROGRAMS off_addr_2: P.O. BOX 9003 off_city: CHARLOTTESVILLE off_state: VA off_zip: 22903 off_country: USA ! end of coverpage abstract: line_1: NOTE: Due to the reduced image quality of HST, we have deleted the FOC line_2: spectroscopic observations from this project. The original abstract follows line_3: We aim to study the interaction between jets and the interstellar medium in the line_4: central few kpc of the Seyfert galaxy Markarian 78. In a recent long-slit line_5: survey of Seyfert galaxies, MKN 78 was identified as the outstanding example in line_6: which [OIII] lambda5007 profile structure clearly reveals the interaction line_7: between radio jets and the interstellar medium. Even in this optimum case, line_8: however, the important structures are within a few arcsec of the nucleus, and line_9: HST resolution is needed to trace the interaction in detail. We shall take a line_10: narrow band [OIII] image with the PC and, using image reconstruction, line_11: identify emission structures on equivalent scales tothe radio structure line_12: revealed by a new 2 cm VLA radio map (0."1 resolution). line_13: These observations will allow us to define the intensity line_14: distributions of the emission components over the nuclear regions. We line_15: aim to test two current models: acceleration and compression behind the lobe line_16: bow shock and entrainment along the length of the jet. line_17: In a number of ways, these observations will match those of NGC1068 line_18: recently made by HST. ! ! end of abstract general_form_proposers: lname: WHITTLE fname: D. MARK title: P.I. inst: VIRGINIA, UNIVERSITY OF country: USA ! lname: WILSON fname: ANDREW mi: S. inst: MARYLAND, UNIVERSITY OF country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: See original phase I proposal for scientific case for support. line_3: Note that this Phase II proposal has been modified to reflect line_4: the decreased allocation of spacecraft time (3.0 Hours, from line_5: 5.6 hours), and the removal of the FOC spectra. ! question: 3 section: 1 line_1: It is very fortunate that, with a redshift cz = 11,136 km/s, the entire line_2: profile of [OIII] lambda 5007 falls well within the half power points of PC line_3: narrow filter F517N (effective width = 88 A, designed for zero redshift line_4: Mgb). Three exposures of 30m duration will be obtained with this filter to line_5: image the high excitation gas. We are interested in both the small scale line_6: emission cospatial with the radio structure, as well as the larger scale line_7: (about 30 arcsec) emission which gives clues to the nuclear UV collimation line_8: geometry. An exposure of shorter duration will be made through F588N to line_9: obtain an off-band image for continuum subtraction. (Unfortunately the line_10: adjacent medium band filters will be contaminated by H beta or [OIII] line_11: lambda 4959, 5007 which have very high equivalent width). We feel the line_12: marginal loss in spatial resolution of the PC over the FOC--F/96 is line_13: outweighed by the narrowness of the filter, the increased throughput, line_14: and the much larger field of view. ! question: 4 section: 1 line_1: Typical sizes of linear double or triple radio structures in Seyfert line_2: galaxies are <= 0.1 - 3 arcsec. To understand the interaction of the radio line_3: ejecta with the emission line gas, we MUST spatially resolve these scales. line_5: We have recently pursued long-slit and line-imaging of Seyfert galaxies to line_6: the limit of ground based resolution. The study by Whittle et al (1988 line_7: ApJ 326 125) used a 0.63 arcsec square pixels in 1.5 arcsec seeing and 45 line_8: km/s resolution. Whittle and Wilson were recently awarded visitors time at line_9: CFHT --- arguing the need for the best possible seeing. We had 0.8 arcsec line_10: seeing with 0.4 arcsec pixels and were able to observe MKN 78 (and other line_11: objects) at [OIII], H alpha, [OI] lambda 6300, and [SII] lambda 6717,6731. line_12: These additional lines will enable us to trace the ionisation conditions line_13: across the regions. Although this data is not fully analysed, it seems the line_14: [OIII] components are just resolved spatially along the radio axis. The line_15: jump to 0.1 arcsec resolution would be a critical improvement. line_17: Similarly, we have pushed narrow band imaging of Seyferts to the limit of line_18: ground based conditions --- using the University of Hawaii 88 inch line_19: telescope on Mauna Kea (Haniff, Wilson and Ward 1988 ApJ 334 104, 10 line_20: objects), also with the Image Stabilization Instrument System (ISIS) to line_21: further reduce the effective seeing (Whittle et al 1986 MN 222 189). Once line_22: again, the restrictions imposed by seeing are critical, and prevent a line_23: detailed pursuit of the emission line -- radio link. Radio resolution is ! question: 4 section: 2 line_1: not the problem. 2 cm VLA radio maps with 0.1 arcsec resolution already line_2: exist for many Seyferts (including MKN 78, see Figure 4). If awarded HST line_3: time, we would attempt a 1.3 cm map of MKN 78 with 0.07 arcsec resolution. line_5: In summary, until the limits imposed by ground based seeing are overcome, line_6: it is unlikely that substantial further progress will be made in the study line_7: of the interaction of radio ejecta with line emitting material in the line_8: nuclear regions of Seyfert galaxies. ! question: 5 section: 1 line_1: PC Imaging in [OIII] lambda 5007 and adjacent continuum line_3: Since the line is narrower than the width of the filter (F517N), the number line_4: of electrons per resolution element will be : N_el(line) = 2.27 x 1E12 x line_5: t(secs) x QT(at line) x Fl(erg/cm2/s/(res. el.)) x lambda(A) where Fl is the line_6: integrated line brightness per resolution element. The total flux in [OIII] line_7: lambda 5007 is 4.7 E-13 erg/cm2/s (Whittle et al 1988 ApJ 326 130). This line_8: emission is extended over a region of size 4 arcsec in P.A. 90 deg and is line_9: unresolved (<1 arcsec) in P.A. 0 deg (Haniff, Wilson & Ward 1988 ApJ 334 line_10: 104). If we assume that the emission will cover 1 arcsec in extent in P.A. line_11: 0 deg and has uniform brightness over the 4 arcsec in P.A. 90 deg, we have line_12: Fl = 2.1 E-16 erg/cm2/s/pix. Putting QT(at line = 0.13 as a line_13: weighted average filter QT product over the line (see [OIII] line profile line_14: in Figure 1), we obtain N_el = 882/pix in t = 30 m. The noise is [N(el) + line_15: 80+(RN)^2]^(1/2) = 34 electrons and the S/N = 26. ! question: 5 section: 2 line_1: For the off-band image, we should ideally prefer to save time by using a line_2: medium band filter. Unfortuantely, none of these would be free of line line_3: contamination, given the very high equivalent widths of H beta, [OIII] line_4: lambda 4959,5007 and the redshift cz = 11,136 km/s. We have, therefore, line_5: chosen to obtain a 30m exposure through filter F588N, which will be line_6: completely line free. ! question: 6 section: 1 line_1: Because we require a nearby field star to lie in the PC field, line_2: we must use the ORIENT special requirement. This defines a wide line_3: angular range. However, within this range there are two angles we line_4: do NOT want to have because the star is close to the boundaries of the line_5: PCs. ! question: 7 section: 1 line_1: We have several options for the basic data reduction. At the University of line_2: Virginia Astronomy Department we have an image processing facility based line_3: around a MicroVax which currently runs IRAF, AIPS and DAOPHOT. We aim to line_4: port SDAS before HST launch. At the University of Maryland Astronomy line_5: Program, image processing is based on a networked system of Sun 3 line_6: workstations. The Astronomy Program is also currently purchasing a super line_7: minicomputer (Convex C1 class or better). This will certainly be available line_8: by the time HST data is obtained. We plan to run AIPS, IRAF and hopefully line_9: SDAS on this machine (AIPS and IRAF currently run on the Suns). Thus we may line_10: also visit STScI to use the data analysis systems there. We do not line_11: anticipate any difficulties in performing the basic reduction to calibrated line_12: image and spectral data. ! question: 7 section: 2 line_1: We anticipate that much of the physical inferences will be self-evident line_2: from the intensity distributions and their relation to the line_3: radio map. For more detailed physical analysis, we have several powerful line_4: tools. We have running the photoionization code of Gary Ferland (we are line_5: already fairly sure most of gas is photoionized --- despite being shock line_6: accelerated). We have, in addition, a 3--D computer model framework into line_7: which it is possible to define a wide range of kinematic configurations, line_8: gas distributions and gas densities --- accessing detailed photoionization line_9: calculations to synthesize emission line profiles as `seen' through a line_10: long-slit (a superficial description is in Whittle 1985 MN 216 817). We line_11: shall use existing numerical hydrodynamic models of jet interactions as an line_12: input into the kinematic line profile simulation. In this way we hope to line_13: combine direct inference from the data with more detailed model line_14: simulations. ! question: 8 section: 1 line_1: The positions of the radio and optical nuclei of MKN 78 have both been line_2: measured to an accuracy of +/- 0.2 arcsec, and are in good agreement. ! question: 9 section: 1 line_1: N/A -- First proposal period. ! question: 10 section: 1 line_1: Image processing systems at both University of Virginia and line_2: University of Maryland. ! !end of general form text general_form_address: lname: WHITTLE fname: MARK title: PROF. category: PI inst: UNIVERSITY OF VIRGINIA addr_1: P.O. BOX 3818 city: CHARLOTTESVILLE state: VA zip: 22903 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MARK78 descr_1: GALAXY; SEYFERT GALAXY; NUCLEUS; descr_2: EMISSION; JET pos_1: RA = 7H 37M 56.83S +/- 0.2", pos_2: DEC = +65D 17' 42.2" +/- 0.2" equinox: 1950 rv_or_z: V = 11052 comment_1: FOR PC IMAGES : F517 ([OIII] LINE) comment_2: AND F588N (CONTINUUM). FLUX VALUES comment_3: ARE FOR NUCLEAR REGIONS, 5007 FLUX comment_4: ASSUMES 5 X 0.2 ARCSEC REGION. fluxnum_1: 1 fluxval_1: SURF(V) = 18.0 +/- 1.0 fluxnum_2: 2 fluxval_2: SURF-CONT(4900) = 2.0 +/- 0.5 E-16 fluxnum_3: 3 fluxval_3: SURF-CONT(5860) = 2.0 +/- 0.5 E-16 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 10 +/- 3 E-14 fluxnum_5: 4 fluxval_5: W-LINE(5007) = 200 ! targnum: 2 name_1: SAO14321 descr_1: STAR; TYPE=K0; CALIBRATION TARGET pos_1: RA = 7H 41M 54.51S +/- 0.4", pos_2: DEC = +65D 34' 40.5" +/- 0.4" equinox: 1950 comment_1: FOR POINT SPREAD FUNCTION, comment_2: AKA DM+65 593, GC 10420 comment_3: PROPER MOTION INCLUDED, FROM AGK3. comment_4: OFFSET 29.9702 ARCMIN AT comment_5: PA 55.0592D FROM MKN78 fluxnum_1: 1 fluxval_1: V = 6.0 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 1.0 +/- 0.1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: MARK78 config: PC opmode: IMAGE aperture: P6 sp_element: F517N wavelength: 5171 num_exp: 1 time_per_exp: 30M s_to_n: 25 fluxnum_1: 4 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES, param_3: CLOCKS=YES req_1: SEQ 1-4 NO GAP; req_2: ORIENT 350D +/- 60D / 1-4; req_3: CYCLE 1 / 1-4 comment_1: /OIII/ LINE IMAGE CENTERED IN PC6 comment_2: NEED 32 KBIT GUIDESTAR TELEMETRY comment_3: USED U3=X-AXIS IE OFFSET=0D comment_4: AVOID ORIENT 327D +/- 5D AND comment_5: 10D +/- 5D STAR HITS PC EDGES ! linenum: 1.100 targname: MARK78 config: PC opmode: IMAGE aperture: P6 sp_element: F517N wavelength: 5171 num_exp: 2 time_per_exp: 30M s_to_n: 25 fluxnum_1: 4 priority: 1 param_1: CR-SPLIT=NO,PRE-FLASH=YES, param_2: CLOCKS=YES req_1: SAME ORIENT FOR 1.1 AS 1; req_2: SAME POS FOR 1.1 AS 1; ! linenum: 2.000 targname: MARK78 config: PC opmode: IMAGE aperture: P6 sp_element: F588N wavelength: 5880 num_exp: 2 time_per_exp: 15M s_to_n: 3 fluxnum_1: 3 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES, param_3: CLOCKS=YES req_1: SAME ORIENT FOR 2 AS 1; req_2: SAME POS FOR 2 AS 1 comment_1: CONTINUUM IMAGE CENTERED IN PC6 comment_2: NEED 32 KBIT GUIDESTAR TELEMETRY ! linenum: 3.000 targname: SAO14321 config: PC opmode: IMAGE aperture: P6 sp_element: F517N wavelength: 5171 num_exp: 1 time_per_exp: 0.14S s_to_n: 150 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES, req_1: GUID TOL 0.020" comment_1: GYROHOLD comment_2: PSF FOR ON-LINE FILTER ! linenum: 4.000 targname: SAO14321 config: PC opmode: IMAGE aperture: P6 sp_element: F588N wavelength: 5880 num_exp: 1 time_per_exp: 0.40S s_to_n: 150 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES, req_1: SAME ORIENT FOR 4 AS 3; req_2: SAME POS FOR 4 AS 3; req_3: GUID TOL 0.020" comment_1: GYROHOLD comment_2: PSF FOR OFF-LINE FILTER ! ! end of exposure logsheet ! No scan data records found