! $Id: 5428,v 6.1 1994/07/27 17:50:54 pepsa Exp $ coverpage: title_1: TESTING THE ACCRETION DISK LINE-PROFILE HYPOTHESIS IN ARP 102B: title_2: CYCLE4MEDIUM sci_cat: QUASARS & AGN sci_subcat: RADIO GALAXIES proposal_for: GO longterm: 1 pi_fname: ALEXEI pi_mi: V. pi_lname: FILIPPENKO pi_inst: UC-BERKELEY pi_country: USA pi_phone: 510-642-1813 hours_pri: 6.28 num_pri: 1 fos: Y off_fname: LINDA off_lname: RUTKOWSKI off_title: RES. ADMINISTRATOR off_inst: 1500 off_addr_1: SPONSORED PROJECTS OFFICE off_addr_2: 336 SPROUL HALL off_addr_3: UNIVERSITY OF CALIFORNIA off_city: BERKELEY off_state: CA off_zip: 94720 off_country: USA off_phone: 510-643-6113 ! end of coverpage abstract: line_1: Arp 102B is the prototype of a set of ten broad-line radio galaxies whose line_2: hydrogen Balmer line profiles are double-peaked, and which share several line_3: additional distinguishing optical characteristics. We recently established line_4: the reality of this class through a comprehensive optical spectroscopic survey line_5: of radio-loud AGNs at z < 0.4 (Eracleous & Halpern 1992, 1993). We now propose line_6: to obtain moderate-resolution spectra to study the UV emission lines and line_7: nonstellar continuum of Arp 102B. Several theories have been suggested to line_8: explain the unusual line profiles; the most detailed is a model for emission line_9: from the photoionized atmosphere of an accretion disk. The Balmer lines are the line_10: only broad lines detected in ground-based spectra, and the optical nucleus is line_11: dominated by starlight. Both of these limitations restrict further progress in line_12: understanding the nature of this peculiar spectrum. But observations of the line_13: UV emission lines and continuum could test the models by (1) measuring line line_14: profiles of species with different ionization potentials, and (2) measuring line_15: the nonstellar continuum, which seems different from that of most AGNs. Disk line_16: photoionization models predict line shapes which are different among the UV line_17: lines. The same model predicts an ionizing continuum which is nonthermal, line_18: arising in an optically thin, ion-supported torus, rather than a blackbody line_19: accretion disk. If supported by the results of HST spectra, our study of line_20: Arp 102B could provide the most direct view of an accretion disk in an AGN. ! ! end of abstract general_form_proposers: lname: FILIPPENKO fname: ALEXEI mi: V. inst: 1500 country: USA ! lname: HALPERN fname: JULES mi: P. inst: 1770 country: USA ! lname: ERACLEOUS fname: MICHAEL inst: 3470 country: USA ! lname: CHEN fname: KAIYOU inst: 2500 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: To detect faint lines, to model in detail the profiles of broad lines, and line_2: to determine the overall shape of the continuum, we require spectra having good line_3: S/N ratio and modest resolution over the entire accessible UV wavelength range. line_4: We will connect the red end of the UV spectrum (around 3150 A) with our optical line_5: spectra, obtained at ground-based observatories. This will give a reliable line_6: continuum shape over the range 1150-10000 A, and it will allow us to derive line_7: accurate emission-line intensity ratios between UV and optical lines. Three line_8: HST grating settings are needed, as follows: line_9: (1) FOS, G130H grating, 1150-1608 A, 1.0 A/diode, blue digicon. line_10: (2) FOS, G190H grating, 1573-2323 A, 1.5 A/diode, blue digicon. line_11: (3) FOS, G270H grating, 2227-3306 A, 2.1 A/diode, red digicon. line_12: The FOS spectra will be obtained through the 1" circular aperture. This yields line_13: excellent throughput and very good resolution; it also helps minimize the line_14: contribution of starlight. line_15: The first setting above gives us Ly-alpha and the blue half of C IV 1549, line_16: two very important lines. Most of the Ly-alpha profile will be redshifted away line_17: from the geocoronal emission. The second setting includes the red half of line_18: C IV 1549, He II 1640, and C III] 1909; the blue side of FOS is requested line_19: in order to get sufficient counts in the red half of the C IV profile (which line_20: falls in a very insensitive region of the FOS red side). The most important line_21: lines in the third setting are C II] 2326, [Ne IV] 2423, and Mg II 2800. We line_22: might also detect Fe II blends. Together, these grating settings will allow line_23: us to determine whether there is a UV bump in the continuum. ! question: 4 section: 1 line_1: Only about 10 known AGNs have the double-peaked, broad emission lines which line_2: are characteristic of a rotating disk, but this class offers the most direct line_3: evidence for the reality of accretion disks around supermassive black holes. line_4: They are all too faint for IUE observations to be of great use. Arp 102B is line_5: the nearest and brightest candidate for accretion disk line emission; its line_6: H-alpha line profile is not HIGHLY variable, and its average appearance is line_7: consistent with the simple accretion-disk model. line_8: Until now, the hydrogen lines are the only broad lines which have been seen line_9: in Arp 102B. IUE observations of Arp 102B have resulted in weak detections of line_10: continuum and Ly-alpha. SWP and LWP exposures of duration 265 and 120 minutes, line_11: respectively, barely detected continuum in the 1600-3000 A range (Chen line_12: et al. 1989), consistent with an extrapolation of the optical continuum. The line_13: only UV emission line detected by IUE was Ly-alpha, but the resolution and line_14: S/N ratio are low. We must obtain a much better profile and a more accurate line_15: measurement the continuum shape if meaningful conclusions about the origin of line_16: the emission lines are to be drawn. Other, weaker UV lines must also be line_17: studied. HST is the only telescope that can provide the necessary data on the line_18: emission lines and nonstellar continuum. These data will test the theory of line_19: the origin of emission lines in a photoionized disk atmosphere. line_20: An important supporting piece of data that will aid in the interpretation line_21: of the ionizing continuum is the soft X-ray spectrum. X-ray observations line_22: of Arp 102B have already been obtained with the ROSAT PSPC, and will be line_23: available for archival analysis by the time the HST observations are made. ! question: 4 section: 2 line_1: Arp 102B lies at Galactic coordinates l = 75.5 deg, b = 34.9 deg. According line_2: to Burstein and Heiles (1982, AJ, 87, 1165), Galactic reddening is very small: line_3: E(B-V) = 0.015 mag. From the observed Balmer decrement of the narrow emission line_4: lines in Arp 102B, we deduce that the intrinsic reddening is also small. The line_5: total UV extinction is probably about 0.2 mag. line_6: From the IUE data of Chen et al. (1989), we estimate that the observed line_7: continuum flux density of Arp 102B at 1400 A, 1700 A, and 2300 A is 0.05 mJy, line_8: 0.10 mJy, and 0.18 mJy, respectively. We use these in what follows: line_9: FOS, G130H grating, blue digicon: At 1400 A, the efficiency is 0.055. line_10: The throughput of the 1" aperture is 0.90 for point sources, and we have line_11: 1.0 A/diode. Using equation (5) of Table 1.2.1 in the FOS Instrument Handbook, line_12: we find a count rate of 0.012 per second per diode. Zodiacal light, airglow, line_13: and diffuse Galactic light will not significantly affect our observations. The line_14: dark current is somewhat smaller than the expected signal; thus, the exposure line_15: time must be increased to achieve the desired S/N ratio, compared with the line_16: case of negligible dark current. We therefore require 240 minutes for line_17: S/N = 12 in the continuum at 1400 A. line_18: FOS, G190H grating, blue digicon: At 1700 A, the efficiency is 0.008 and the line_19: throughput it 0.91; there are 1.47 A/diode. For S/N = 16, we require 100 min. line_20: FOS, G270H grating, red digicon: At 2300 A, the efficiency is 0.052. The line_21: point-source throughput is 0.93, and there are 2.09 A/diode. For S/N = 32, we line_22: require only 33 minutes. ! question: 5 section: 1 line_1: None. ! question: 6 section: 1 line_1: None. ! ! question: 8 section: 1 line_1: When our HST observing dates become known, we will request nearly line_2: simultaneous time at Lick and Keck Observatories to obtain optical spectra line_3: and images, IR images, and IR spectra. These data will be combined with the line_4: UV spectra to construct an overall continuum spanning a large wavelength line_5: range. A complete analysis of the data will subsequently be done. ! question: 9 section: 1 line_1: 2590, Deep Imaging of the Site of SN 1961V. -- A. Filippenko, et al. line_2: 3507, UV Spectroscopy and High-Resolution Imaging of NGC 4395. -- A. line_3: Filippenko, W. Sargent, L. Ho line_4: 3519, UV Imaging of Nearby Galaxies. -- D. Maoz, A. Filippenko, et al. line_5: 3810, The Stellar Population of Wolf-Rayet Galaxies. -- P. Conti, line_6: A. Filippenko, W. Sargent, L. Ho, C. Leitherer, C. Robert, W. Vacca line_7: 4302, Supernovae and their Local Environment. -- A. Filippenko, et al. line_8: 4312, Circumstellar Material around Supernovae. -- A. Filippenko, et al. line_9: 4340, Origin of Blue Featureless Continuum in Seyfert 2 Nuclei. -- A. line_10: Filippenko, L. Ho line_11: 4350, FOS Observations of LINER Galaxy Nuclei. -- G. Reichert, A. Filippenko, line_12: L. Ho, J. Shields, R. Mushotzky, K. Mason, G. Branduardi-Raymont, C. Wu. line_13: 4635, Accretion Disk Line-Profile Hypothesis in Arp 102B. -- A. Filippenko, line_14: J. Halpern, M. Eracleous, K. Chen line_15: PUBLICATIONS: line_16: "A Gravitational Lens Candidate Discovered with the Hubble Space Telescope." line_17: D. Maoz, J. N. Bahcall, D. P. Schneider, R. Doxsey, N. A. Bahcall, A. V. line_18: Filippenko, W. M. Goss, O. Lahav, and B. Yanny; Astrophysical Journal line_19: (Letters), 386, L1 (1992). line_20: "HST Observations of NGC 4395, the Least Luminous Seyfert 1 Nucleus: line_21: Evidence Against the Starburst Hypothesis for Broad-Lined Active Galactic line_22: Nuclei." A. V. Filippenko, L. C. Ho, and W. L. W. Sargent; Astrophysical line_23: Journal (Letters), 410, L75 (1993). ! question: 9 section: 2 line_1: "NGC 4395: Evidence Against the Starburst Hypothesis for Seyfert 1 Nuclei line_2: and QSOs." A. V. Filippenko, L. C. Ho, and W. L. W. Sargent; in 16th line_3: Texas Symposium/3rd Symposium on Particles, Strings, and Cosmology; line_4: ed. C. Akerlof and M. Srednicki (New York: New York Academy of Sciences), line_5: 707 (1993). line_6: "Was SN 1961V a Genuine Supernova?" G. C. Bower, A. V. Filippenko, et al. line_7: BAAS, 25, 819 (1993). ! question: 10 section: 1 line_1: Both U. C. Berkeley and Columbia University have extensive computing line_2: facilities (VMS and UNIX) in their Astronomy Departments, as do STScI and line_3: Los Alamos National Laboratory. Image-processing workstations, graphics line_4: terminals, laser printers, large disks, and tape drives are all available. line_5: Many computer programs exist for analysis of data. Both universities also line_6: have many highly capable graduate students and postdoctoral fellows, some line_7: of whom may participate in various aspects of this project. Ground-based line_8: complementary observations can readily be obtained (with short notice) at line_9: Lick Observatory; proposals for Keck time will also be submitted by the PI. line_10: The usual secretarial and technical support is available at Berkeley, line_11: Columbia, Los Alamos, and STScI. ! !end of general form text general_form_address: lname: FILIPPENKO fname: ALEXEI mi: V. category: PI inst: 1500 addr_1: DEPARTMENT OF ASTRONOMY addr_2: 601 CAMPBELL HALL addr_3: UNIVERSITY OF CALIFORNIA city: BERKELEY state: CA zip: 94720 country: USA phone: 510-642-1813 telex: ALEX@BKYAST.BERKELEY.EDU ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: ARP102B descr_1: E,303,315,320,910 pos_1: RA = 17H 17M 56.34S +/- 0.04S, pos_2: DEC = +49D 01' 49.6" +/- 0.6" equinox: 1950.0 pm_or_par: N rv_or_z: Z = 0.02438 comment_1: MAGNITUDES AND FLUXES comment_2: REFER TO NUCLEUS ONLY. comment_3: BRIGHT NUCLEUS SUPERPOSED ON comment_4: FAINTER GALAXY BACKGROUND. comment_5: THE ABOVE COORDINATES ARE comment_6: PREFERRED OVER GASP COORDS. fluxnum_1: 1 fluxval_1: V = 16.0 +/- 0.3 fluxnum_2: 2 fluxval_2: B-V = 1.0 +/- 0.2 fluxnum_3: 3 fluxval_3: F-CONT(1400) = 7.6 +/- 2.3 E-16 fluxnum_4: 4 fluxval_4: F-CONT(1600) = 1.0 +/- 0.3 E-15 fluxnum_5: 5 fluxval_5: F-CONT(2300) = 1.0 +/- 0.3 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: ARP102B config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.4S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 2; req_3: GROUP 1-7 WITHIN 3D; req_4: GROUP 1-6 NO GAP ! linenum: 2.000 targname: ARP102B config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 2.0S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-X=.602, param_2: SCAN-STEP-Y=.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 3; ! linenum: 3.000 targname: ARP102B config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-X=0.30, param_2: SCAN-STEP-Y=0.30, param_3: SEARCH-SIZE-X=3, param_4: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 3.5 ! linenum: 3.500 targname: ARP102B config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-X=0.06 param_2: SCAN-STEP-Y=0.06 param_3: SEARCH-SIZE-X=5 param_4: SEARCH-SIZE-Y=5 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 4 ! linenum: 4.000 targname: ARP102B config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2760 num_exp: 1 time_per_exp: 33M s_to_n: 32 fluxnum_1: 5 priority: 1 req_1: CYCLE 4; comment_1: IF THERE IS EXTRA TIME BEFORE comment_2: EARTH OCCULTATION NEAR END OF comment_3: EXPOSURE, CAN INCREASE EXPOSURE comment_4: TIME TO INCREASE S/N RATIO. ! linenum: 5.000 targname: ARP102B config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 30S fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: SCAN-STEP-X=0.06 param_2: SCAN-STEP-Y=0.06 param_3: SEARCH-SIZE-X=5 param_4: SEARCH-SIZE-Y=5 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 6 ! linenum: 6.000 targname: ARP102B config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1950 num_exp: 1 time_per_exp: 100M s_to_n: 16 fluxnum_1: 4 priority: 2 req_1: CYCLE 4; comment_1: IF THERE IS EXTRA TIME BEFORE comment_2: EARTH OCCULTATION NEAR END OF comment_3: EXPOSURE, CAN INCREASE EXPOSURE comment_4: TIME TO INCREASE S/N RATIO. ! linenum: 6.100 targname: ARP102B config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 4.2S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 6.2 ! linenum: 6.200 targname: ARP102B config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6.0S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-X=.602, param_2: SCAN-STEP-Y=.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 6.3 ! linenum: 6.300 targname: ARP102B config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 30S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-X=0.30, param_2: SCAN-STEP-Y=0.30, param_3: SEARCH-SIZE-X=3, param_4: SEARCH-SIZE-Y=3, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 6.5 ! linenum: 6.500 targname: ARP102B config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 30S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SCAN-STEP-X=0.06 param_2: SCAN-STEP-Y=0.06 param_3: SEARCH-SIZE-X=5 param_4: SEARCH-SIZE-Y=5 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 7 ! linenum: 7.000 targname: ARP102B config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 240M s_to_n: 14 fluxnum_1: 3 priority: 3 req_1: CYCLE 4; comment_1: IF THERE IS EXTRA TIME BEFORE comment_2: EARTH OCCULTATION NEAR END OF comment_3: EXPOSURE, CAN INCREASE EXPOSURE comment_4: TIME TO INCREASE S/N RATIO. ! ! end of exposure logsheet ! No scan data records found