! File: 4909C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:09:54:40 coverpage: title_1: POLARIZATION IMAGING OF THE JET IN MARKARIAN 463: CYCLE3 MEDIUM title_2: (EARLY ACQ FOR 4417) sci_cat: QUASARS & AGN sci_subcat: SEYFERTS proposal_for: GO pi_fname: ALAN pi_mi: K pi_lname: UOMOTO pi_inst: JOHNS HOPKINS UNIVERSITY pi_country: US hours_pri: 0.57 num_pri: 1 foc: Y funds_length: 12 ! end of coverpage abstract: line_1: Markarian 463 is a Seyfert 2 galaxy that shows a Seyfert 1 line_2: spectrum when viewed in polarized light (Miller & Goodrich 1990). line_3: One explanation is that a Seyfert 1 nucleus is heavily obscured line_4: by dust along our line of sight but material external to the line_5: nucleus has a clear view of it and scatters the light in our line_6: direction (polarizing it in the process), giving us a periscopic line_7: view of the Seyfert 1. line_9: From the ground, the nucleus of Mkn 463 is unresolved, but we have line_10: obtained HST/PC images that reveal a 1 arcsec optical jet extending line_11: south of the nucleus. This jet is composed of a string of unresolved line_12: knots and one or more of these is likely to be the scattering site. line_13: We propose to use the FOC to obtain near UV images in polarized light line_14: to locate the scattering site, to discriminate between dust reflection line_15: and electron scattering, and to attempt to understand the jet. ! ! end of abstract general_form_proposers: lname: UOMOTO fname: ALAN title: PI mi: K 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: TSVETANOV fname: ZLATAN inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: ANTONUCCI fname: ROBERT mi: J inst: UCSB country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Markarian 463 is a pair of merging galaxies. This system contains two line_2: nuclei separated by 4 arcsec that lie along an east-west line. The western line_3: nucleus is a LINER with a strong blue continuum and emission lines with FWHM line_4: of about 500 km/s. The eastern nucleus (Mkn 463E) shows a Seyfert 2 spectrum line_5: with the strong, high ionization emission lines typical of this class (Wills line_6: et al. 1977; Hutchings & Neff 1989). line_7: Using Antonucci & Miller's (1985) spectropolarimetric technique, Miller & line_8: Goodrich (1990) discovered a Seyfert 1 spectrum hidden in the polarized light line_9: of Mkn 463E. They observed strong Balmer, weak Fe II, and narrow [O III] line_10: emission in polarized light and surmised that light from a hidden Seyfert 1 line_11: nucleus was scattered by dust or electrons into our line of sight. line_12: Blanco (1991) confirmed this result by directly observing the Seyfert 1 line_13: spectrum in the infrared. He measured broad Paschen emission with Seyfert 1 line_14: profiles superposed on the Seyfert 2 spectrum and concluded that the Seyfert line_15: 1 nucleus was directly observed in the IR. He also used these lines to line_16: compute an approximate visual extinction of 5 mag, and used typical QSO line_17: Paschen/Balmer ratios to deduce that Miller & Goodrich were seeing only 5% of line_18: the Seyfert 1 luminosity. line_19: There is strong evidence, then, that this Seyfert 2 galaxy has a Seyfert 1 line_20: nucleus at its heart and we can see it because of a fortuitously positioned line_21: mirror composed of electrons and/or dust. Identifying this mirror is a line_22: primary goal of the proposed observations. ! question: 2 section: 2 line_1: From the ground, Mkn 463E is a point source with V = 17.3. Since line_2: the small entrance aperture used by Miller & Goodrich excludes the LINER line_3: nucleus 4 arcsec away, we already know that the mirror must be within 2-3 line_4: arcsec of Mkn 463E. Since 1 arcsec is 1 kpc at the distance of Mkn 463, it line_5: was possible, perhaps likely, that the scattering material would be so close line_6: to the nucleus as to be forever unresolved, even with a full-performance HST. line_7: We were delighted, then, to find complex structure near Mkn 463E on early line_8: acquisition images taken with the Planetary Camera (Uomoto et al. 1992). line_9: These pictures show a jet extending 1 arcsec due south of the nucleus, line_10: appearing as a string of 4-5 bright knots along a not-quite-straight line. line_11: The jet accounts for about 1/3 of the total Mkn 463E flux, and the line_12: brighter knots have V ~= 20. The spectral distribution of the jet emission line_13: is continuum dominated, although our limited color information suggests that line_14: some [O III] emission is likely to be included. line_15: We propose to obtain near UV FOC continuum images through polarizing line_16: filters to isolate the structures that scatter the Seyfert 1 light. Miller & line_17: Goodrich found the total polarization of the nucleus+jet complex to be a line_18: large 7.7% in the visual band with values well above 10% in the near UV. line_19: We expect easily to see detailed intrinsic polarization structure in the line_20: nuclear region. ! question: 2 section: 3 line_1: Polarization mechanisms that might confuse our interpretation are line_2: intervening dust and synchrotron emission. Fortunately, neither is line_3: a problem. line_4: We can rule out intervening dust because (1) the Seyfert 2 line emission line_5: is unpolarized, (2) the color excess is too low for the amount of polarization line_6: in Mkn 463E, and (3) there is little Galactic extinction towards Mkn 463. line_7: We can also rule out polarization due to synchrotron processes in the line_8: jet. Although there is considerable activity manifested in radio and optical line_9: emission knots at the bright nucleus and regions south of it (Mazzarella et line_10: al. 1991; Hutchings & Neff 1989), there is no radio emission coincident with line_11: any of the jet's bright spots. If we assume that radio emission from the jet line_12: would have the same spectral index as the nuclear radio source (0.7, Unger et line_13: al. 1986), then it is impossible for an optical synchrotron source in the jet line_14: not to be a radio source. Radio emission from the jet is not observed, so line_15: the optical emission cannot be synchrotron. line_16: We suspect that the jet contains the scattering material. Its position line_17: angle, 182 deg, is almost perpendicular to the electric polarization angle line_18: of 82 deg measured by Miller & Goodrich. This coincidence strongly suggests line_19: the jet as the scattering site, particularly if electron scattering is the line_20: mechanism. Further evidence favoring electron scattering, at least in the line_21: 0.5-2.2 micron range, is an unpublished K-band polarization measurement by line_22: Antonucci and Barvainis of 2.7% for this object. The polarized flux line_23: distribution in this range does not show the imprint of a Rayleigh scattering ! question: 2 section: 4 line_1: law, as seen in the off-nuclear clouds in NGC 1068. Unless nature has been line_2: unusually perverse by making Mkn 463E a confusing collection of many highly line_3: polarized but unrelated sources, we can combine this information with the line_4: spectropolarimetric observations of Miller & Goodrich and our proposed near line_5: UV observations (which will not be contaminated with scattered, possibly line_6: polarized, starlight) to decide between dust (wavelength dependent) and line_7: electron (wavelength independent) scattering. line_8: A large fraction of Seyfert 2 galaxies, perhaps 50% or more, reveal hidden line_9: Seyfert 1 spectra when viewed in polarized light (Miller & Goodrich 1990). line_10: The proposed observations will locate the Seyfert 1 mirror and determine the line_11: scattering mechanism in one of these. If the jet in Mkn 463 turns out to be line_12: the scattering site, then it is possible that many Seyfert 2 galaxies have line_13: similar jets. line_14: The composition and emission mechanism of the jet is unknown, except that line_15: its spectrum is neither locally generated optical synchrotron nor purely line_16: emission lines. The jet may be entirely scattered light like a 1 kpc long line_17: flashlight beam, or perhaps some of the light is from newly formed stars. line_18: If the jet is the Seyfert 1 mirror, then the model of an aligned obscuring line_19: torus at the nucleus neatly explains the observations. The simple FOC line_20: observations proposed here provide a unique opportunity to understand better line_21: the Seyfert phenomenon. ! question: 2 section: 5 line_1: REFERENCES line_3: Antonucci, R. J. & Miller, J. S. 1985, ApJ, 297, 621 line_4: Blanco, P. 1991, PhD thesis, University of Edinburgh line_5: Hutchings, J. B. & Neff, S. G. 1989, AJ, 97, 1306 line_6: Mazzarella, J. M., Gaume, R. A., Soifer, B. T., Graham, J. R., line_7: Neugebauer, G., & Matthews, K. 1991, AJ, 102, 1241 line_8: Miller, J. S. & Goodrich, R. W. 1990, ApJ, 355, 456 line_9: Unger, S. W., Pedlar, A., Booler, R. V., & Harrison, B. A. 1986, line_10: MNRAS, 219, 387 line_11: Uomoto, A., Caganoff, S., Ford, H. C., Rosenblatt, E. I., Evans, line_12: I. N., & Cohen, R. D. 1992, BAAS, 24, 751 Wills, B. J., et al. 1977, BAAS, line_13: 9, 647 line_14: Wills, B. J., Wills, D., Uomoto, A. K., Vogt, S., Tull, R. G., Rybski, P., line_15: Montemayor, T., Kelton, P., Ghigo, F., Douglas, J. N., & Bash, F. 1977, line_16: BAAS, 9, 647 ! question: 3 section: 1 line_1: This proposal describes an early acquisition image for line_2: follow-on polarimetry. This early acquisition image is for line_3: exposure time and coordinate information. We also expect to line_4: execute an FOS program in Cycle 2 on this object that will line_5: provide confirming coordinate, but no exposure time, information. line_6: The procedure is to take a short exposure in the 11x11 arcsec line_7: FOV of FOC/96. This information will be used for follow-on line_8: exposures in the 5.6x5.6 arcsec FOV of FOC/96. ! question: 4 section: 1 line_1: HST is needed for these observations for its spatial resolving line_2: power and UV capabilities. The components (knots) of the jet in line_3: Mkn 463 are unresolved at the 0.1 arcsec level, and are physically line_4: located within an arcsec of the nucleus. Furthermore, the nucleus line_5: is almost 3 mag brighter than the individual unresolved knots in line_6: the jet. The problem reduces to finding the polarization of 20th line_7: mag point sources that are about 0.5 arcsec away from a 17.5 mag line_8: nucleus with a required spatial resolution of about 0.1 arcsec. line_9: This cannot be done from the ground. Despite its less-than-optimum line_10: imaging performance, HST can easily approximate these requirements. line_11: We also want to observe in the near UV, where contamination line_12: from possibly polarized starlight could hamper our interpretation. ! question: 4 section: 2 line_1: The observed count rate for the nucleus+jet complex in the near UV line_2: is 7.6x10**-5 phot/cm**2/s/A (based on Miller & Goodrich 1990). The line_3: jet accounts for about 1/3 of this flux (2.5x10**-5) and this flux is line_4: distributed amongst 4-5 individual knots. Thus, each knot has a flux line_5: of about 5x10**-6 phot/cm**2/s/A. For unpolarized objects, this line_6: results in a count rate of about 5 Hz through the polarizers (eq 4 in line_7: the FOC Handbook). Because we need high spatial resolution, we really line_8: want the count rate within the central core of the image, about 0.07 line_9: arcsec, which contains 15% of the light. This region gives a count line_10: rate of ~1 Hz. Dark count and background are negligible in this case. line_11: If we assume the worst, any knot in the nuclear region might have line_12: only 10% polarization. A S/N of 10 in a single exposure then requires line_13: 5 hours (apply eq 1 in the FOC Handbook, substituting the unpolarized line_14: object flux for background rate). Since it is likely that the polarized line_15: parts will have considerably higher polarization than 10%, we feel safe line_16: in cutting the exposure time to 3.3 hours per filter. This would still line_17: give S/N = 8 for 10% polarization and is adequate to map the polarization line_18: in the nuclear region. For 20% polarization, a likely value, 3.3 hours line_19: gives S/N = 16. ! question: 7 section: 1 line_1: The data obtained from STScI will be calibrated and analyzed at line_2: Johns Hopkins University using current FOS/IDT computer equipment, line_3: augmented by peripherals supported by this proposal. All line_4: coinvestigators plus a TBD graduate student will be directly involved line_5: in the data analysis and publication of the results. ! 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 (FOS 14) line_4: These proposals lead in part to the development of the ideas in this proposal, line_5: but they do not address the specific problem posed here. ! question: 9 section: 2 line_1: With the data in this GTO program we have line_2: 1) resolved the narrow-line region of NGC 1068 and found that the apex of the line_3: ionization cone is coincident with the peak of the CO emission and the OH line_4: megamaser, making them likely candidates for the obscuring molecular torus; line_5: 2) determined that the scattering region or "mirror" in NGC 1068 is extended on line_6: a scale of 1 arc second; line_7: 3) resolved the biconical structure of the narrow-line region in NGC 4151; line_8: 4) discovered an optical jet in the Seyfert 2 galaxy Mrk 463; line_9: 5) resolved the narrow-line regions of additional Seyfert 1's, Seyfert 2's, line_10: and LINERS. The systematic differences in the morphologies of the line_11: narrow-line regions in Seyfert 1's and 2's suggest that an additional free line_12: parameter in unified models is the orientation of the axis of the central line_13: engine reltive to the disk of the host galaxy, in addition to the orientation line_14: relative to the observer. ! question: 9 section: 3 line_1: HST Imaging of the Inner 3 Arcseconds of NGC 1068 in the Light of [O III] 5007, line_2: Evans, I. N., Ford, H. C., Kinney, A. L., Antonucci, R. R. J., Armus, L., line_3: and Caganoff, S., ApJ, 369, L27, 1991. line_4: Faint Object Spectrograph Spectroscopy of Resolved Structure in the Nucleus of line_5: NGC1068, Caganoff, S., et al., ApJ, 377, L9, 1991. line_6: Faint Object Spectrograph Observations of the Low-Luminosity Seyfert Galaxy line_7: NGC 1566, G. A. Kriss, G. F. Hartig, L. Armus, W. P. Blair, S. Caganoff, line_8: and L. Dressel, ApJ, 377, L13, 1991. line_9: HST Imaging of Jets and Collimated Radiation in AGN, Kriss, G. A., et al., line_10: to appear in the proceedings of the Space Telescope Symposium line_11: "Astrophysical Jets", 1992. line_12: HST Continuum and Narrow-band Images of AGN, Kinney, A. L., et al., line_13: BAAS, 24, 727, 1992. line_14: HST Imaging of the Biconical Narrow-line Region of NGC 4151, Kriss, G. A., line_15: et al., BAAS, 24, 751, 1992. line_16: The Optical Jet in Markarian 463, Uomoto, A., et al., BAAS, 24, 751, 1992. line_17: Subarcsecond Optical Structure of the Nucleus of Mrk 3, Tsvetanov, et al., line_18: BAAS, 24, 752, 1992. line_19: HST Narrow Band Planetray Camera Observations of M31 and M51, Ford, H. C., line_20: et al., BAAS, 24, 818, 1992. line_21: HST Observations of AGN within the FOS GTO Program, Tsvetanov, Z., et al., to line_22: appear in the proceedings of "Science with the Hubble Space line_23: Telescope", 1992. ! question: 9 section: 4 line_1: Collimated Radiation in NGC 4151: HST Images and HUT Spectra, Kriss, G. A., line_2: et al., to appear in the proceedings of "The Nature of Compact Objects in line_3: AGN", 1992. line_4: FOS Observations of the Extended Scattering Region in NGC 1068, Kriss, G. A., line_5: et al., to appear in the proceedings of "First Light in the Universe: Stars line_6: or QSO's?", 1992. ! question: 10 section: 1 line_1: Computer networking support and contract administration are provided line_2: by the Department. ! !end of general form text general_form_address: lname: Uomoto fname: Alan mi: K category: PI inst: Johns Hopkins University addr_1: Department of Physics & Astronomy addr_2: The Johns Hopkins University city: Baltimore state: MD zip: 21218 country: USA phone: (410) 516-8043 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MKN463 name_2: MRK463 name_3: MARK463 descr_1: E,301,312,315,318,320 pos_1: RA = 13H 53M 39.87S +/- 0.14S, pos_2: DEC = +18D 36' 57.0" +/- 2" equinox: 1950 fluxnum_1: 1 fluxval_1: V=20 +/- 1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: MKN463 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: POL120,F320W num_exp: 1 time_per_exp: 600S s_to_n: 3 fluxnum_1: 1 priority: 1 req_1: CYCLE 3 comment_1: EARLY ACQUISITION FOR FOLLOW-ON comment_2: POLARIMETRY WITH FOC/96 IN 256X256 comment_3: APERTURE ! ! end of exposure logsheet ! No scan data records found