! $Id: 88,v 1.1 1994/09/21 11:34:16 pepsa Exp $ coverpage: title_1: UV SPECTRAL DISTRIBUTION IN LOW LUMINOSITY ACTIVE GALAXIES - title_2: IMAGING: CYCLE 4 MEDIUM sci_cat: QUASARS & AGN sci_subcat: OTHER ACTIVE NUCLEI proposal_for: GO pi_fname: ANURADHA pi_mi: P. pi_lname: KORATKAR pi_inst: 3470 pi_country: USA pi_phone: (410) 338-4470 hours_pri: 2.94 num_pri: 4 wf_pc: Y off_fname: HERVEY off_lname: STOCKMAN off_title: DEPUTY DIRECTOR off_inst: 3470 off_addr_1: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: (410) 338-4730 ! end of coverpage abstract: line_1: Observations of activity in the nuclei of galaxies from the most line_2: energetic (QSOs) to the mildly energetic (LINERs) show that many of the line_3: properties are similar and the objects might be related to each other. line_4: A crucial question that arises is, ``Is the basic mechanism that powers line_5: the activity the same in all these galaxies and do the properties of line_6: active nuclei just scale with luminosity\?'' Many studies suggest that line_7: QSOs and luminous Seyfert nuclei have the same basic energy source. line_8: This continuity of properties suggests an extension to still lower line_9: luminosities, but there might be a lower limit to the activity line_10: (analogous to the mass limit in main sequence stars). Hence, it is line_11: important to determine whether Low Luminosity AGNs (LLAGNs; or a line_12: certain sub-class of them) are genuinely related to classical AGNs, or line_13: whether instead their properties might be due to other physical line_14: processes. In this proposal we request FOS and PC observations of 4 line_15: LLAGNs (detected with ROSAT) to determine the physical processes line_16: responsible for UV radiation in these objects. The results of this line_17: analysis will not only help bridge the gap between LLAGNs and normal line_18: galaxies, but answer the following question: How similar are the line_19: LLAGNs to the higher luminosity AGNs\? More specifically, what is the line_20: dominant mechanism for the production of ionizing radiation\? ! ! end of abstract general_form_proposers: lname: KORATKAR fname: ANURADHA mi: P. inst: 3470 country: USA ! lname: DEUSTUA fname: SUSANA mi: E. inst: 2460 country: USA ! lname: EVANS fname: IAN mi: N. inst: 3470 country: USA ! lname: FILIPPENKO fname: ALEXEI mi: V. inst: 1500 country: USA ! lname: HECKMAN fname: TIMOTHY mi: M. inst: 3470 country: USA ! lname: HO fname: LUIS mi: C. inst: 1500 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan to use the WFPC2 PC to observe the objects in our sample using line_2: the F218W filter to determine the spatial extent of the nuclear UV line_3: continuum source for comparison with X-ray imaging data. Since the line_4: spatial resolution of the WFPC2 PC is an order of magnitude better than line_5: the ROSAT HRI resolution, the morphology of the UV continuum source will line_6: enable us to investigate the central source on much smaller spatial line_7: scales than would otherwise be possible. We have selected the F218W line_8: filter because of its high UV efficiency and the absence of strong UV line_9: emission lines in the filter bandpass. The WFPC2 images will also be line_10: used to decide on target acquisition strategies for the subsequent line_11: spectra, based on the observed UV morphology of the target. We will line_12: use the FOS blue detector with the G160L grating to determine the line_13: spectral energy distribution and emission-line properties of the line_14: nuclear source. The G160L exposures are designed to provide a S/N line_15: ratio of approximately 15:1 per pixel in the continuum at 1800 line_16: Angstroms. line_17: We will use the WFPC2 PC with the F218W filter to determine the spatial line_18: extent of the nuclear UV continuum source in the objects in our sample. line_19: The targets should be placed at the PC1 aperture position, with the line_20: exposures split 2:1 to maximize our dynamic range given the uncertain line_21: UV flux distribution. The F218W science exposures will also be used as line_22: EARLY ACQ images for the FOS observations. We currently plan to use a line_23: FOS ACQ/BINARY on an offset star that should be visible in each of the ! question: 3 section: 2 line_1: WFPC2 images and offset directly to the nucleus. If the WFPC2 images line_2: indicate that the nucleus is sufficiently compact, we will instead use line_3: ACQ/BINARY to acquire directly the nucleus. If a suitable offset star line_4: is not visible on the WFPC2 images, we will modify our acquisition line_5: sequence to include a 3x3 peakup on the nucleus using the 0.5 aperture line_6: after the ACQ/BINARY on an offset star. We will obtain an FOS ACQ line_7: image after offsetting to the target to verify the spacecraft pointing. ! question: 4 section: 1 line_1: These observations can only be obtained in the satellite ultraviolet. line_2: We have obtained all relevant IUE data relating to the nuclei of the line_3: objects in this sample. The brightest of the the objects in our sample line_4: was observed by IUE, but the S/N is very low. The UV continua of these line_5: objects is too faint to obtain adequate S/N using IUE. We have observed line_6: the objects in this sample using the ROSAT HRI imager, and have line_7: recently been awarded ROSAT PSPC time to obtain X-ray spectra for these line_8: targets. We also have high resolution optical imaging data and optical line_9: spectra of these objects. line_10: It is possible that the blue bump could be a major contributor to the line_11: energy budget for these objects. Therefore, HST data in the line_12: effectively unobserved UV waveband are critical to understanding the line_13: spectral energy distribution for these objects. line_14: We have estimated the nuclear continuum flux we expect from the nuclei line_15: of these objects from the UV/H-BETA and UV/X-ray luminosity line_16: correlations for AGNs. The predicted flux for all of these objects is line_17: similar to 1.0E-15 erg/cms^2/s/A, consistent with that determined from line_18: the existing NGC 5273 IUE data. We have therefore assumed that the line_19: nuclear continuum flux will be present at this level in our exposure line_20: time calculations. Since we do not have additional UV flux line_21: information for any of the objects in the sample, we have assumed the line_22: same exposure times for each object. The WFPC2 exposure times have line_23: been chosen so as not to saturate the CCD even in the unlikely event ! question: 4 section: 2 line_1: that all of the nuclear flux arises from a point source, and to provide line_2: a mean S/N ratio per pixel of approx. 20:1 if the emission is extended line_3: 1". line_4: The FOS/BL G160L exposures are designed to obtain approximately 250 line_5: counts per pixel in the continuum at 1800 Angstroms, and approximately line_6: 130 counts per pixel in the continuum at 1400 Angstroms. This signal line_7: level is the minimum required to accurately determine the continuum line_8: spectral energy distribution and measure the emission lines with line_9: reasonable accuracy. ! question: 5 section: 1 line_1: None. ! question: 6 section: 1 line_1: None. ! ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: 3591 - "Massive Stars in Starburst Galaxies" (Heckman, PI) line_2: 3837 - "Sectropolarimetry of Low Red-shift Active Galactic Nuclei: Test line_3: of the Quasar Emission Mechanism" (Koratkar, PI) line_4: 4302 - "Supernovae and their Local Environment" (Filippenko, PI) line_5: 4312 - "Circumstellar Matter around Supernovae" (Filippenko, PI) line_6: 4340 - "Origin of Blue Featureless Continuum in Seyfert 2 Nuclei" line_7: (Filippenko, PI; Ho, Co-I) line_8: 4350 - "FOS Observations of LINER Galaxy Nuclei" (Filippenko & Ho, Co-I) line_9: 4364 - "Ultraviolet and Optical Nebular Diagnostics for Photoionization line_10: and Shock Heated Emission Line Gas" (Evans PI, Koratkar Co-I) line_11: 4370 - "Space-UV Imaging of Nearby Powerful Radio Galaxies" (Heckman, line_12: PI) line_13: 4967 - "Carbon, Nitrogen, and Oxygen abundances in Nearby Seyfert line_14: Galaxies" (Koratkar, PI, Evans Co-I) line_15: Except for 4350 none of the above programs are related to this line_16: proposal. The main emphasis of 4350 is on measuring emission to line_17: determine excitation mechanism and absorption lines to detect hot, line_18: young stars. Observations for the program 3837, 4370 have not yet line_19: begun. Observations for 3591 are currently in progress. Data for line_20: programs 4364, and 4967 have only recently been obtained, and are line_21: being analyzed. 2590 and 3507 have been completed and the results are line_22: in press and these programs are not mentioned above. Data for others line_23: have not yet been obtained. ! question: 9 section: 2 line_1: "HST Imaging of the Inner 3 Arcseconds of NGC1068 in the light of line_2: [OIII] 5007", Evans, I.N., Ford, H.C., Kinney, A.L., Antonucci, R.R.J., line_3: Armus, L. & Caganoff, S., Ap.J.Lett., 369, L31, 1991. line_4: "Faint Object Spectrograph Spectroscopy of Resolved Structure in the line_5: Nucleus of NGC1068", Caganoff, S., Antonucci, R.R.J., Ford, H.C., Kriss, line_6: G.A., Hartig, G., Armus, L., Evans, I.N., Rosenblatt, E., Bohlin, R.C., line_7: & Kinney, A.L., Ap.J.Lett., 377, L9, 1991. line_8: "Hubble Space Telescope Imaging of the Narrow Line Region of NGC 4151", line_9: Evans, I.N., Tsvetanov, Z., Kriss, G.A., Ford, H.C., Caganoff, S., & line_10: Koratkar, A.P., Ap. J., in press, 1993. line_11: "A Gravitational Lens Candidate Discovered with the Hubble Space line_12: Telescope," Maoz, D., Bahcall, J.N., Schneider, D.P., Doxsey, R., line_13: Bahcall, N.A., Filippenko, A.V., Goss, W.M., Lahav, O., & Sargent, line_14: W.L.W., Ap.J.Lett., 386, L1, 1992. line_15: "HST Observations of NGC 4395, the Least Luminous Seyfert 1 Nucleus: line_16: Evidence Against the Starburst Hypothesis for Broad-Lined Active line_17: Galactic Nuclei," Filippenko, A.V., Ho, L.C., & Sargent, W.L.W., line_18: Ap.J.Lett., in press. line_19: "NGC 4395: Evidence Against the Starburst Hypothesis for Seyfert 1 line_20: Nuclei and QSOs," Filippenko, A.V., Ho, L.C., & Sargent, W.L.W., in line_21: 16th Texas Symposium/3rd Symposium on Particles, Strings, and line_22: Cosmology, ed. C. Akerlof and M. Srednicki (New York: New York Academy line_23: of Sciences), 1993, in press. ! question: 10 section: 1 line_1: The investigators on this proposal have access to the standard data line_2: analysis and research support facilities provided by their home line_3: institutions. No special support for this project will be provided by line_4: any of the proposers' home institutions. ! !end of general form text general_form_address: lname: KORATKAR fname: ANURADHA mi: P. category: PI inst: 3470 addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA phone: (410) 338-4470 telex: KORATKAR@STSCI.EDU ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC4278 descr_1: E,303,312,910,923,924 pos_1: RA = 12H 20M 06.766S +/- 2.0", pos_2: DEC = +29D 16' 49.27" +/- 2.0", pos_3: PLATE-ID = 00DJ equinox: J2000 rv_or_z: V = +649 fluxnum_1: 1 fluxval_1: V = 16.3 ! targnum: 2 name_1: NGC4639 descr_1: E,301,312,910,923,924 pos_1: RA = 12H 42M 52.326S +/- 2.0", pos_2: DEC = +13D 15' 25.80" +/- 2.0", pos_3: PLATE-ID = 00IY equinox: J2000 rv_or_z: V = +1010 fluxnum_1: 1 fluxval_1: V = 16.3 ! targnum: 3 name_1: NGC5033 descr_1: E,303,312,910,923,924 pos_1: RA = 13H 13M 27.536S +/- 2.0", pos_2: DEC = +36D 35' 37.12" +/- 2.0", pos_3: PLATE-ID = 01PR equinox: J2000 rv_or_z: V = +878 fluxnum_1: 1 fluxval_1: V = 16.3 ! targnum: 4 name_1: NGC5273 descr_1: E,303,312,910,923,924 pos_1: RA = 13H 42M 08.354S +/- 2.0", pos_2: DEC = +35D 39' 15.32" +/- 2.0", pos_3: PLATE-ID = 01QW equinox: J2000 rv_or_z: V = +1054 fluxnum_1: 1 fluxval_1: V = 16.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC4278 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4 / 1-4.0; comment_1: EARLY ACQ FOR 5-7 ! linenum: 2.000 targname: NGC4639 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=NO comment_1: EARLY ACQ FOR 8-10 ! linenum: 3.000 targname: NGC5033 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=NO comment_1: EARLY ACQ FOR 11-13 ! linenum: 4.000 targname: NGC5273 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=NO comment_1: EARLY ACQ FOR 14-16 linenum: 101.000 targname: NGC4278 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.0, req_1: CYCLE 4 / 101-104.0; COMMENT_1: LINES 101-104 ADDED FOR HOPR 223 comment_2: REPEAT. ! linenum: 102.000 targname: NGC4639 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.0, ! linenum: 103.000 targname: NGC5033 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.0, ! linenum: 104.000 targname: NGC5273 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F218W num_exp: 1 time_per_exp: 1800S priority: 1 param_1: CR-SPLIT=0.5, param_2: CR-TOLERANCE=0.0, ! ! end of exposure logsheet ! No scan data records found